Icranet
The 2013 Scientific Report
Presented to
The Scientific Committee
by
Remo Ruffini
Director of ICRANet
ICRANet has been created by a law of the Italian Government, ratified unanimously by the Italian Parliament and signed by the President of the Republic of Italy on February 10^{th }2005. The Republic of Armenia, the Republic of Italy, the Vatican State, ICRA, the University of Arizona and the University of Stanford have been the Founding Members. All of them have ratified the Statute of ICRANet (see Enclosure 1). On September 12^{th }2005 the Board of Governors was established and had its first meeting. Professors Remo Ruffini and Fang LiZhi were appointed respectively Director and Chairman of the Board. On December 19^{th }2006 the Scientific Committee was established and had its first meeting in Washington DC. Prof. Riccardo Giacconi was appointed Chairman and John Mester CoChairman. On September 21^{st }2005 the Director of ICRANet signed with the Ambassador of Brazil Dante Coelho De Lima the adhesion of Brazil to ICRANet. The entrance of Brazil, requested by the President of Brazil Luiz Ignácio Lula Da Silva has been unanimously ratified by the Brazilian Parliament. On February 2009 the board renewed the position of Prof. Fang LiZhi as the Chairman of the Board. On December 2009 the Scientific Committee renewed the position of Prof. Riccardo Giacconi as the Chairman of the Committee. On February 2010 the board renewed the position of Prof. Remo Ruffini as the Director of the ICRANet. On August 12^{th}, 2011 the President of Brazil Dilma Rousseff signed the entrance of Brazil in ICRANet. On October 15^{th}, 2012, following the death of Prof. Fang LiZhi, Prof. Francis Everitt was appointed Chairman of the Board and Prof. XiaoHui Fan and Prof. ShuFang Su were indicated as temporary substitutes of Prof. Fang. On June 12^{th }, 2013, following the completion of his second mandate, Prof. Riccardo Giacconi has resigned as Chairman of the Scientific Committee for health reasons. Prof. João Braga was then appointed Chairman of the Scientific Committee and Prof. Massimo Della Valle was appointed CoChairman (details on
http://www.icranet.org/
). In December 2013, during the visit at the University of Arizona of Prof. Remo Ruffini, Director of ICRANet, it was agreed with the Dean of the University of Arizona to appoint Prof. XiaoHui Fan as the successor of Prof. Fang LiZhi in representing the University of Arizona in the ICRANet Board. During the 2013, we have:
1) adjourned and recruited the Scientific Staff of ICRANet, including the adjunct Faculty, Lecturers, Research Scientists, Visiting Scientists; adjourned and recruited the Administrative Staff of ICRANet;
2) further developed the Brazilian Science Data Center (BSDC) and signed a Cooperation Agreement with FAPERJ (Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro) (see Enclosure 2);
3) started the operations of the Seats of ICRANet in Nice at Villa Ratti, in Yerevan at the National Academy of Sciences and in Brazil at CBPF (see Enclosure 3);
4) prepared the proceedings of the meetings of 2012 and organized meetings and PhD schools (see Enclosure 4);
5) updated and signed cooperation agreements with Universities and Research Centers, including ASI (Italian Space Agency, Italy), BSU (Belarusian State University, Belarus), CAPES (Brazilian Fed. Agency for Support and Evaluation of Grad. Education), CBPF (Brazil), Cearà State (Brazil), ENEA (National Agency for new technologies, energy and the economic sustainable development, Italy), FAPERJ (Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Brazil), GARR (Italy), ICTP (The Abdus Salam International Center for Theoretical Physics, Italy), IHEP (Institute of High Energy Physics, Chinese Academy of Sciences, China), IHES (Institut des Hautes Études Scientifiques, France), INPE (Instituto Nacional de Pesquisas Espaciais, Brasil), INFN (National Institute for Nuclear Physics, Italy), ITA (Instituto Tecnológico de Aeronáutica, Brazil), LeCosPa (Leung Center for Cosmology and Particle Astrophysics, Taiwan), NASB (National Academy of Sciences, Belarus), NAS RA (National Academy of Science, Armenia), Nice University Sophia Antipolis (France), Pescara University “D’Annunzio” (Italy), Physics Department of University of Rome “Sapienza” (Italy), SCSA (State Committee of Science of Armenia), UERJ (Rio de Janeiro State University, Brazil), UFPB (Universidade Federal da Paraíba, Brazil), UIS (Universidad Industrial de Santander, Colombia), UNAM (Universidad Nacional Autonoma De Mexico), UNIFEI (Universidade Federal de Itajubà, Brazil), University of Rome “Sapienza” (Italy), UNS (Universidad Nacional del Sur, Argentina) (see Enclosure 5);
6) recruited new students, organized the teaching programs and the Thesis works of the International Relativistic Astrophysics Doctoral program (IRAPPhD), jointly sponsored by ICRANet and ICRA in collaboration with AEI – Albert Einstein Institute – Potsdam (Germany), Bremen University (Germany), Carl von Ossietzky University of Oldenburg (Germany), CBPF – Brazilian Centre for Physics Research (Brazil), Ferrara University (Italy), IHES (France), Indian centre for space physics (India), INPE (Instituto Nacional de Pesquisas Espaciais, Brasil), Nice University Sophia Antipolis (France), Observatory of the Côte d'Azur (France), Rome University – “Sapienza” (Italy), Savoie University (France), Shanghai Astronomical Observatory (China), Stockholm University (Sweden), Tartu Observatory (Estonia) (see Enclosure 6);
7) developed the Erasmus Mundus program of the European Commission and recruited additional nine students (see Enclosure 7);
8) started the CAPESICRANet program for PhD students, PostDoc Researchers and Visiting professors (see Enclosure 8);
9) followed the project for the ICRANet Center at the Casino de Urca in Rio de Janeiro, Brazil (see Enclosure 9);
10) started the process for adhesion of South Korea and Hungary to ICRANet (see Enclosure 10);
11) connected the ICRANet headquarters in Pescara to the highspeed optical fiber network of GARR, the Italian network of Universities and Research Centers;
12) fostered the lines of research and publication activities which are the objects of the present report.
1) The ICRANet Staff
In the establishment of the ICRANet Scientific Staff we have followed the previously adopted successful strategy: 1) To appoint talented young scientists, as well as senior scientists who have already contributed significantly to those areas which led to the establishment of ICRANet.
2) To create an adjunct Faculty containing many renowned scientists who have made internationally recognized contributions to the field of relativistic astrophysics and whose research interests are closely related to those of ICRANet. These scientists spend from one to six months at the Pescara Center, thereby linking it with their home institutions.
3) To develop a program of Lecturers, Research Scientists and Visiting Scientists, necessary to the scientific operations of the Center.
This strategy has created an outstanding research institute with strong connections to some of the most advanced Research Centers in the world. It also promotes the vital connections between all the ICRANet Member Institutions. The Curricula of the ICRANet Staff are given in the Accompanying Document “The ICRANet Staff, Visiting Scientists and Graduate Students at the Pescara Center”
PROFESSORS OF THE FACULTY
 Belinski Vladimir  ICRANet
 Bianco Carlo Luciano  Università di Roma “Sapienza” and ICRANet
 Einasto Jaan  Tartu Observatory, Estonia
 Izzo Luca  ICRANet
 Novello Mario  Cesare Lattes ICRANet Chair  CBPF and ICRABR, Rio de Janeiro, Brazil
 Rueda, Jorge A.  Università di Roma “Sapienza” and ICRANet
 Ruffini Remo  Università di Roma “Sapienza” and ICRANet
 Vereshchagin Gregory  ICRANet
 Xue SheSheng  ICRANet
ADJUNCT PROFESSORS OF THE FACULTY
Typically and Adjunct Professor spends at ICRANet a period varying from one month to six months every year and keeps ongoing collaborations for the rest of the year.
 Aharonian Felix Albert  (Benjamin Jegischewitsch Markarjan ICRANet Chair)  Dublin Institute for Advanced Studies, Dublin, Ireland  MaxPlanckInstitut für Kernphysis, Heidelberg, Germany
 Amati Lorenzo  Istituto di Astrofisica Spaziale e Fisica Cosmica,  University of Arizona, Tucson, USA
 Chakrabarti Sandip K.  Center for Space Physics, India
 Chardonnet Pascal  Université de la Savoie, France and ICRANet
 Chechetkin Valeri  (Mstislav Vsevolodich Keldysh ICRANet Chair)  Keldysh Institute for Applied Mathematics Moscow, Russia
 Damour Thibault  (JosephLouis Lagrange ICRANet Chair)  IHES, Bures sur Yvette, France
 Della Valle Massimo  Osservatorio di CapodiMonte, INAFNapoli, Italy
 Everitt Francis  (William Fairbank ICRANet Chair)  Stanford University, USA
 Frontera Filippo  University of Ferrara
 Giavalisco Mauro  Department of Astronomy, University of Massachusetts, USA
 Jantzen Robert  (Abraham Taub ICRANet Chair)  Villanova University USA
 Jetzer Philippe  Institute of Theoretical Physics, University of Zurich, Switzerland
 Khalatnikov Markovich  (Lev Davidovich Landau ICRANet Chair)  Isaak  Landau Institute for Theoretical Physics, Russia
 Kerr Roy  (Yevgeny Mikhajlovic Lifshitz ICRANet Chair)  University of Canterbury, New Zealand
 Kleinert Hagen  (Richard Feynmann ICRANet Chair)  Freie Universität Berlin
 Lee Hyung Won  (Yong Duk Kim ICRANet Chair)  School of Computer Aided Science, Inje, Korea
 Madey John  University of Hawaii
 Misner Charles  (John Archibald Wheeler ICRANet Chair)  University of Maryland, USA
 Mo Houjun  Department of Astronomy, University of Massachusetts, USA
 Nicolai Herman  Albert Einstein Institute – Potsdam, Germany
 Pelster Alex  Institute for Advanced Study, Germany
 Pian Elena  INAF and Osservatorio Astronomico di Trieste
 Piran Tsvi  (Yuval Neeman ICRAnet Chair)  The Hebrew University  Jerusalem
 Popov Vladimir  ITEP, Russia
 Punsly Brian Matthew  California University, Los Angeles USA
 Quevedo C. Hernando  Institute of Nuclear Science, UNAM
 Rafelski Johann  University of Arizona, USA
 Rosati Piero  University of Ferrara, Italy
 Rosquist Kjell  (Karl Gustav Jacobi ICRANet Chair)  Stockholm University, Sweden
 ’t Hooft Gerard  Institut for Theoretical Physics, Utrecht Universiteit, Holland
 Titarchuk Lev  (Victor Sobolev ICRANet Chair)  University of Ferrara, Italy
LECTURERS
The Lecturers participate in the many schools and meetings organized by ICRANet, as well as in the International Relativistic Astrophysics Ph.D. program (IRAPPhD), sponsored by ICRANet and ICRA (see below). The Lecture series span from a minimum of a few weeks to the entire year.
 Aksenov Alexey  Institute for CAD, Russian Academy of Sciences
 Alekseev Georgy  Steklov Mathematical Institute – Russian Academy of Sciences
 Bini Donato  CNR and ICRANet, Italy
 Boccaletti Dino  ICRANet and Università di Roma "Sapienza"
 Chen Pisin  National Taiwan University  Kavli Instit. Particle Astrophysics and Cosmology
 Chieffi Alessandro  INAF, Rome, Italy
 Coullet Pierre  Université de Nice  Sophia Antipolis, France
 Di Castro Carlo  Università di Roma "Sapienza", Italy
 Filippi Simonetta  ICRANet and Campus Biomedico, Italy
 Jing YiPeng  Shangai Astronomy Observatory
 Kim Sang Pyo  Kunsan National University, Korea
 Kim SungWon  Institute of Theor. Physics for AsiaPacific, Korea
 Lee Chul Hoon  Hanyang University, Korea
 Limongi Marco  INAF, Rome, Italy
 Lou You Qing  Tsinghua University, Beijing
 Malheiro Manuel  ITA, Brazil
 Mester John  Stanford University, USA
 Mignard François  Observatoire de la Côte d‘Azur, Nice, France
 Ohanian Hans  Rensselaer Polytechnic Institute, New York, USA
 Pacheco José  Observatoire de la Côte d ‘Azur, Nice, France
 Perez Bergliaffa Santiago  Univesidade do Estado de Rio de Janeiro, Brasil
 Pucacco Giuseppe  Università di Tor Vergata Roma
 Sepulveda Alonso  University of Antioquia, Columbia
 Song Doo Jong  National Institute of Astronomy Korea
 Starobinsky Alexei  Landau Institute for Theoretical Physics, Russia
 Vissani Francesco  Gran Sasso National Laboratory, Italy
 Wiltshire David  University of Canterbury, New Zealand
RESEARCH SCIENTISTS
The research scientists are generally at a postdoctoral level and they are extremely active in all research topics.
 Bernardini Maria Grazia  ICRANet and OAB–Merate, Italy
 Cherubini Christian  Campus Biomedico, Rome, Italy
 Geralico Andrea
 Lattanzi Massimiliano
 Patricelli Barbara
 Rotondo Michae
VISITING SCIENTISTS
ICRANet and Università di Roma “Sapienza”, Italy ICRANet and Università di Roma “Sapienza”, Italy ICRANet and UNAM, México ICRANet and Università di Roma “Sapienza”, Italy.
They include experts who have given essential contributions in ongoing activities at ICRANet.
 Abishev Medeu  AlFarabi Kazakh National University, Kazakhstan
 BisnovatyiKogan G.S.  Space Research Institute, Moscow
 Bittencourt Eduardo  CBPF, Brasil
 Corvino Giovanni  University of Rome La Sapienza, Italy
 GellMann Murray  Sante Fe Institute, USA
 Kim Hyuong Yee  INJE, South Korea
 Mohammadi Rohollah  Isfahan University of Technology, Pakistan
 Mosquera Cuesta Herman  CBPF, Brasil
 Perez Martinez Aurora  Instituto de Cibernetica Matematica Y Fisica, Cuba
 Piechocki Wlodzimierz  Institute for Nuclear Studies, Poland
 Qadir Asgar  National Univ. Of Sciences And Technology, Pakistan
 Raffaelli Bernard  Université de Corse, France
 Romero Gustavo E.  Instituto Argentino de Radioastronomia IAR  CONICET, Argentina
 Van Putten Maurice  Korean Institute for Advanced Study, South Korea
ADMINISTRATIVE STAFF
The administrative and secretarial staff of the Center is:
 Adamo Cristina  Administrative Office (Pescara)
 Barbaro Pina  ICRANet Nice (until August 31st)
 Brandolini Gabriele  System Manager (Pescara, starting by July 1st)
 Del Beato Annapia  Documentation Office (Pescara, until August 31st)
 Di Berardino Federica  Head of the Secretarial Office (Pescara)
 Di Niccolo Cinzia  Secretariat (Pescara, starting by August 1st)
 Latorre Silvia  Administrative Office (Pescara)
 Pirone Maria Elena  Secretariat (Pescara, starting by October 1st)
 Schaller Flavia  ICRANet BR – Rio de Janeiro
2) The Collaboration with Brazil (see Enclos. 2)
Following the agreement signed in 2012 between ICRANet and CAPES (Brazilian Fed. Agency for Support and Evaluation of Grad. Education), in 2013 it started the CAPESICRANet program for PhD students, PostDoc Researchers and Visiting professors (see also point 8 below). During 2013 the Brazilian Science Data Center (BSDC) is being expanded. Prof. Remo Ruffini, Director of ICRANet, also signed a Cooperation Agreement with Dr. Ruy Garcia Marques, President of FAPERJ (Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro). Particularly important has been the meeting of the ItalyBrazil Joint Committee for Scientific and Technological Cooperation (Commissione Mista di Cooperazione Scientifica e Tecnologica Italia – Brasile), where an ample discussion has pointed out the importance of ICRANet activities in Brazil.
3) Inauguration of the Seat in Nice at Villa Ratti, in Yerevan at the National Academy of Sciences and in Brazil at CBPF (see Enclos. 3)
We have completed the restructuring of Villa Ratti for the ICRANet Seat in Nice. We been very pleased to receive the invitation by the Municipality of Nice to open ICRANet activities in France, in order to maximize our contacts with other European Countries and more generally with Countries all over the world. We are planning the inauguration in the first semester of 2014. We have also the express our gratitude for the decision of the Municipality of Nice to take care of the maintenance of the park surrounding Villa Ratti. The appeal for the town of Nice and his surroundings, the existence of a modern and efficient airport, the electronic backbones for internet communications are all important elements which add to the splendid decision of the Nice Municipality to offer the historical Villa Ratti as a seat for ICRANet in Nice. The first stone for the restructuring of the Villa has been laid down on November 23^{rd }2007. Since, an important finding of wall paintings of circa 1750 occurred in the Villa. A large amount of activities has been carried out in renovating the building and the park around. The headquarter of the IRAPPhD program will be in Villa Ratti. We were pleased to have, as the first visitors of the freshly opened ICRANet Seat in Villa Ratti, the Nobel Laureate Murray GellMann as well as Prof. Felix Aharonian, Prof. Thibault Damour and Prof. Tom Kibble. We have also started the activities of the ICRANet Seat in Armenia, at the Headquarter of the National Academy of Sciences in Yerevan and at the Byurakan Observatory. Particularly important has been the attribution by the Armenian State Science Committee of five positions: three researchers, one technical support and one secretariat. We have also started the ICRANet Seat in Rio de Janeiro at the CBPF Headquarters and possibly expanding at the Casino de Urca.
4) International Meetings (see Enclos. 4)
We are completing the proceedings of:
 12^{th} ItalianKorean Symposium, Pescara, Italy, July 48, 2011.

3^{rd} Galileo – Xu Guangqi Meeting, Beijing, China, October 1115, 2011.

XIII Marcel Grossmann Meeting, Stockholm, Sweden July 17, 2012
We have also organized the following meetings:

Second Bego Scientific Rencontre, Nice, France, May 1631, 2013.

The 2013 yearly ICRANet Scientific Meeting on Relativistic Astrophysics, Pescara, Italy, June 321, 2013.

The first URCA meeting on Relativistic Astrophysics, Rio de Janeiro, Brazil, June 2429, 2013.

13^{th} ItalianKorean Meeting, Seoul, South Korea, July 1519, 2013.

IRAP Ph.D. School, Nice, France, September 220, 2013.
5) Scientific Agreements (see Enclos. 5)
The following Agreements have been signed, updated and renewed by the Director (see Fig. 1):
 ASI (Italian Space Agency, Italy)
 BSU (Belarusian State University, Belarus)
 CAPES (Brazilian Fed. Agency for Support and Evaluation of Grad. Education)
 CBPF (Brazil)
 Cearà State (Brazil)
 ENEA (National Agency for new technologies, energy and the economic sustainable development, Italy)
 FAPERJ (Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Brazil)
 GARR (Italy)
 ICTP (The Abdus Salam International Center for Theoretical Physics, Italy)
 IHEP (Institute of High Energy Physics, Chinese Academy of Sciences, China)
 IHES (Institut des Hautes Études Scientifiques, France)
 INFN (National Institute for Nuclear Physics, Italy)
 INPE (Instituto Nacional de Pesquisas Espaciais, Brasil)
 ITA (Instituto Tecnológico de Aeronáutica, Brazil)
 LeCosPa (Leung Center for Cosmology and Particle Astrophysics, Taiwan)
 NASB (National Academy of Sciences, Belarus)
 NAS RA (National Academy of Science, Armenia)
 Nice University Sophia Antipolis (France)
 Pescara University “D’Annunzio” (Italy)
 Physics Department of University of Rome “Sapienza” (Italy)
 SCSA (State Committee of Science of Armenia)
 UERJ (Rio de Janeiro State University, Brazil)
 UFPB (Universidade Federal da Paraíba, Brazil)
 UIS (Universidad Industrial de Santander, Colombia)
 UNAM (Universidad Nacional Autonoma De Mexico)
 UNIFEI (Universidade Federal de Itajubà, Brazil)
 University of Rome “Sapienza” (Italy)
 UNS (Universidad Nacional del Sur, Argentina)
Figure 1
These collaborations are crucial in order to give ICRANet scientists the possibility to give courses and lectures in the Universities and, vice versa, to provide to the Faculty of such Universities the opportunity to spend research periods in ICRANet institutions.
6) The International Relativistic Astrophysics Ph.D. (IRAPPhD) program (see Enclos. 6)
One of the major success of ICRANet has been to participate in the International competition of the Erasmus Mundus Ph.D. program and the starting of this program from the 2010 (see Fig. 2).
Figure 2
The participating institutions are:
 AEI – Albert Einstein Institute – Potsdam (Germany)
 Bremen University (Germany)
 Carl von Ossietzky University of Oldenburg (Germany)
 CBPF – Brazilian Centre for Physics Research (Brazil)
 Ferrara University (Italy)
 Indian centre for space physics (India)
 INPE (Instituto Nacional de Pesquisas Espaciais, Brasil)
 Institut Hautes Etudes Scientifiques – IHES (France)
 Nice University Sophia Antipolis (France)
 Observatory of the Côte d'Azur (France)
 Rome University – “Sapienza” (Italy)
 Savoie University (France)
 Shanghai Astronomical Observatory (China)
 Stockholm University (Sweden)
 Tartu Observatory (Estonia)
The IRAP PHD program intends to create conditions for high level education in Astrophysics mainly in Europe to create a new generation of leading scientists in the region. No single university in Europe today has the expertise required to attain this ambitious goal by itself. For this reason we have identified universities which offers a very large complementarity expertise. The students admitted and currently following courses and doing research in such a program are given in the following:
Third Cycle 200407 
Chiappinelli Anna 
France 

Cianfrani Francesco 
Italy 

Guida Roberto 
Italy 

Rotondo Michael 
Italy 

Vereshchagin Gregory 
Belarus 

Yegoryan Gegham 
Armenia 
Fourth Cycle 200508 
Battisti Marco Valerio 
Italy 

Dainotti Maria.Giovanna 
Italy 

Khachatryan Harutyun 
Armenia 

Lecian Orchidea Maria 
Italy 

Pizzi Marco 
Italy 

Pompi Francesca 
Italy 
Fifth Cycle 200609 
Caito Letizia 
Italy 

De Barros Gustavo 
Brasil 

Khachatryan Harutyun 
Switzerland 

Patricelli Barbara 
Italy 

Rangel Lemos Luis Juracy 
Brasil 

Rueda Hernandez Jorge Armando 
Colombia 
Sixth Cycle 20072010 
Ferroni Valerio 
Italy 

Izzo Luca 
Italy 

Kanaan Chadia 
Lebanon 

Pugliese Daniela 
Italy 

Siutsou Ivan 
Belarus 

Sigismondi Costantino 
Italy 
Seventh Cycle 20082011 
Belvedere Riccardo 
Italy 

Ceccobello Chiara 
Italy 

Ferrara Walter 
Italy 

Ferrari Francesca 
Italy 

Han Wenbiao 
China 

Luongo Orlando 
Italy 

Pandolfi Stefania 
Italy 

Taj Safia 
Pakistan 
Eight Cycle 20092012 
Boshkayev Kuantay 
Kazakhstan 

Bravetti Alessandro 
Italy 

Ejlli Damian 
Albania 

Fermani Paolo 
Italy 

Haney Maria 
Germany 

Menegoni Eloisa 
Italy 

Sahakyan Narek 
Armenia 

Saini Sahil 
India 
Ninth Cycle 20102013 
Arguelles Carlos 
Argentina 
(including Erasmus Mundus call) 
Benetti Micol 
Italy 

Muccino Marco 
Italy 

Baranov Andrey 
Russia 

Benedetti Alberto 
Italy 

Dutta Parikshit 
India 

Fleig Philipp 
Germany 

Gruber Christine 
Austria 

Liccardo Vincenzo 
Italy 

Machado De Oliveira Fraga Bernardo 
Brazil 

Martins De Carvalho Sheyse 
Brazil 

Penacchioni Ana Virginia 
Argentina 

Valsan Vineeth 
India 
Tenth Cycle 20112014 
Cáceres Uribe Diego Leonardo 
Colombia 
(including Erasmus Mundus call) 
Raponi Andrea 
Italy 

Wang Yu 
China 

Begue Damien 
France 

Dereli Husne 
Turkey 

Gregoris Daniele 
Italy 

Iyyani Shabnam Syamsunder 
India 

Pereira Jonas Pedro 
Brazil 

Pisani Giovanni 
Italy 

Rakshit Suvendu 
India 

Sversut Arsioli Bruno 
Brazil 

Wu Yuanbin 
China 
Eleventh Cycle 20122015 
Barbarino Cristina 
Italy 
(including Erasmus Mundus call) 
Bardho Onelda 
Albania 

Cipolletta Federico 
Italy 

Dichiara Simone 
Italy 

Enderli Maxime 
France 

Filina Anastasia 
Russia 

Galstyan Irina 
Armenia 

Gomes De Oliveira Fernanda 
Brazil 

Khorrami Zeinab 
Iran 

Ludwig Hendrik 
Germany 

Sawant Disha 
India 

Strobel Eckhard 
Germany 
Twelfth Cycle 20132016 
Ahlén Olof 
Sweden 
(including Erasmus Mundus call 
Becerra Bayona Laura 
Colombia 
and CAPESICRANet call) 
Brandt Carlos Henrique 
Brazil 

Carvalho Gabriel 
Brazil 

Gómez Gabriel 
Colombia 

Harutyunyan Vahagn 
Armenia 

Kovacevic Milos 
Serbia 

Li Liang 
China 

Lisakov Sergey 
Russia 

Maiolino Tais 
Brazil 

Pereira Lobo Iarley 
Brazil 

Pessina Francesco 
Italy 

Sridhar Srivatsan 
India 

Yang Xiaofeng 
China 
7) The Erasmus Mundus Ph.D. program (see Enclos. 7)
Each student admitted to the Erasmus Mundus program of the IRAP Ph.D. is part of a team inside one of the laboratories of the consortium. Each year they have the opportunity to visit the other laboratories of the consortium and enlighten themselves with new topics in the forefront research from world leading experts. In this way the students come in direct contact with some of the leading scientists in the world working in General Relativity, Relativistic Astrophysics and in Quantum Field Theory. In addition to the theoretical centers, we associate experimental and observational centers. This will provide an opportunity to the Ph.D students to obtain a complete education in theoretical relativistic astrophysics and also an experience on how to carry out a specific astrophysical mission. All the institutions participating in IRAP PhD have an extensive experience in international collaborations including visiting professors, postdoctoral researchers and training of Ph.D. students. All of our partners have enrolled Ph.D. students inside their laboratories in various aspects of astrophysics.
8) CAPESICRANet Program (see Enclos. 8)
Following the Memorandum of Understanding signed in 2012 with CAPES, we started the CAPESICRANet Program on Relativistic Astrophysics and Cosmology to promote the Collaboration between Brazilian and European scientists with five major actions: 1) Fellowships for Brazilian graduate students in the IRAPPhD program; 2) Senior European scientists visiting Brazil for up to 3 months per year for three years; 3) Senior Brazilian scientists visiting ICRANet seats in Asia and Europe for up to 5 months in a year; 4) Postdoctoral Fellowships for International candidates in ICRANet seats, Scientific Institutions associated to ICRANet, and Institutions with scientists associated to ICRANet, both in Europe and Brazil; 5) Organization of workshops and outreach programs. In 2013 we have already recruited the first PhD Students, Senior European scientists, Senior Brazilian scientists and Postdoctoral fellows.
9) Project for the ICRANet Center at Casino de Urca (see Enclos. 9)
We have followed the architectural project for the ICRANet Center at the Casino de Urca in Rio de Janeiro, Brazil.
10) Adhesion of South Korea and Hungary to ICRANet (see Enclos. 10)
We have started the procedure for the adhesion of South Korea to ICRANet, with a Seat at the EWHA University in Seoul, and also for the adhesion of Hungary.
11) Pescara connected to GARR network.
Following the agreement signed with Consortium GARR, the Consortium which manages the network connecting all Universities and Research Centers in Italy to worldwide, in December 2013 the ICRANet headquarters in Pescara have been connected to the GARR highspeed optical fiber network of international research centers.
12) Lines of research
We turn now to the research activity of ICRANet, which by Statute addresses the developments of research in Astrophysics in the theoretical framework of Albert Einstein’s theories of special and general relativity. Thanks to an unprecedented developments of observational techniques from the ground, from Space, and even in underground experiments in astroparticle physics, we are today capturing astrophysical signals from all over the universe never before conceived and received in all the history of homo sapiens. The Einstein theory of relativity, for many years relegated to the boundaries of physics and mathematics, has become today the authentic conceptual and theoretical “backbone” of this exponentially growing field of relativistic astrophysics. In the Reports of previous years, as a testimonial of this developments, I enclosed the paper “The Ergosphere and Dyadosphere of Black Holes” which has appeared in “The Kerr spacetime”, edited by David L. Wiltshire, Matt Visser and Susan M. Scott (Cambridge University Press, 2009). In it, I traced the exciting developments, which started with the understanding on the nuclear evolutions of stars, and had then led to the discovery of neutron stars, and through the work of Riccardo Giacconi and colleagues, to the first identification of a black hole in our galaxy. I also enclosed the paper “Moments with Yakov Borisovich Zeldovich” (appeared in the Proceedings of the International Conference “The Sun, the Stars, the Universe, and General Relativity” in honor of Ya.B. Zeldovich's 95^{th }Anniversary, Editors R. Ruffini and G.V. Vereshchagin, AIP Conference Proceedings, Vol. 1205 (2010) p. 110), recalling some of the crucial moments in the developments of relativistic astrophysics in Soviet Union around the historical figure of
Figure 3  Figure 4
Figure 5  Figure 6
Figure 7
Figure 8
Ya.B. Zeldovich. It is also appropriate to mention that ICRANet will organize an International conference in honor of Ya. B. Zeldovich 100^{th }Anniversary in Minsk (Belaurs) on March 1014, 2014. I recalled how the initial activities of ICRANet were guided by three major scientific components (see Fig. 3), which have indeed seen, in recent times, further important developments:
1) The knowledge made possible by general relativity and especially by the Kerr solution and its electrodynamical generalization in the KerrNewman black hole (see
e.g. the recent development of the dyadotorus concept, Fig. 4).
2) The great knowledge gained in relativistic quantum field theories originating from particle accelerators, colliders and nuclear reactors from laboratories distributed worldwide (see e.g. the recent developments at CERN, Fig. 5).
3) The splendid facilities orbiting in space, from the Chandra to the XMM, to the Swift and Fermi missions as well as many other satellites, the VLT and Keck telescopes on the ground, as well as the radio telescope arrays offer us the possibility, for the first time, of the observations of the most transient and energetic sources in the universe: the GammaRay Bursts (GRBs) (see e.g. the recent developments thanks to additional scientific missions, Fig. 6).
In the previous years Reports I have shown that, thanks to a fortunate number of events and conceptual and scientific resonances, a marked evolution of these topics had occurred. New fields of research had sprouted up from the previous ones at the ICRANet Center in Pescara, at ICRA in Rome and at the other Member Institutions. The synergy created by the theoretical developments and the new astrophysical observations had stimulated novel and important results in a vast range of theoretical topics (see Fig. 7), particularly thanks to the recent introduction of the new Induced Gravitational Collapse (IGC) paradigm (see below).
The topic about the KerrNewman Black Holes had been sprouting up in three new fields: The KerrNewman Black holes (L, M, Q); The solitonic equations of GR; GR solutions with L, M, Q, X.
KerrNewman Black Holes (L, M, Q): We had and we have the opportunity of the presence in Pescara of Prof. Roy Kerr as ICRANet Adjunct Professor and discussed the fundamental issues of the uniqueness of the KerrNewman Black Hole. A distinct progress in this collaboration has appeared in the paper by D. Bini, A. Geralico, R. Kerr, “The KerrShild ansatz revised”, International Journal of Geometric Methods in Modern Physics (IJGMMP) 7 (2010), 693703.
The solitonic equations of GR: An alternative derivation of the Kerr solution had been advanced in a classical paper of 1978 by V. Belinski and V. Zakharov using inverse scattering method. The generalization of this method to the presence of electromagnetic field was constructed in 1980 by G. Alekseev and KerrNewman solution has been derived by him in analogous way at the same year. Prof. V. Belinski is now an ICRANet Faculty Member and has further developed this research with the effective collaboration of Prof.
G. Alekseev which is an ICRANet Lecturer. This activity was presented at the 12^{th }Marcel Grossmann Meeting and at number of other conferences and has reached a new maturity.
GR solutions with L, M, Q, X: The unsolved problem of a physical solution in general relativity of an astrophysical object which must be characterized necessarily by four parameters, mass, charge, angular momentum and quadrupole moment, has also been debated for years and it is yet not satisfactorily solved. The presence of ICRANet of Prof. Quevedo as an Adjunct Professor has shown an important result published by Bini, Geralico, Longo, Quevedo [Class. Quant. Grav., 26 (2009), 225006]. This result has been obtained for the special case of a MashhoonQuevedo solution characterized only by mass, angular momentum and quadrupole moment. It has been shown that indeed such a MashhoonQuevedo solution can be matched to an internal solution solved in the postNewtonian approximation by Hartle and Thorne for a rotating star. Equally important has been the result recently obtained by Belvedere showing that a fast rotating model of neutron star with global charge neutrality within the HartleThorne approximation leads to an internal solution of the Kerr metric.
Similarly, the GammaRay Bursts topic had been sprouting up two additional new fields: Ultra high energy sources and Supernovae.
GammaRay Bursts: The research on GRBs in ICRANet is wide and has been participated by many Members of the Faculty and of the Adjunct Faculty, as well as by many Lecturers, Research Scientists and graduate students. Traditionally, GRBs are divided into two classes, “short” GRBs and “long” GRBs, arranged in a bimodal distribution with a separation around a duration of 2s. In 2001 we proposed that both short and long GRBs are created by the same process of gravitational collapse to a black hole. The energy source is the e^{+}e^{}plasma created in the process of the black hole formation. The two parameters characterizing the GRB are the total energy Ee± ^{tot }of such an e^{+}e^{}plasma and its baryon loading B defined as B=MBc^{2}/Ee± ^{tot}, where MB is the mass of the baryon loading. The e^{+}e^{}plasma evolves as a selfaccelerating optically thick fireshell up to when it become transparent, hence we refer to our theoretical model as the “fireshell model”. We have defined a “canonical GRB” light curve with two sharply different components. The first one is the ProperGRB (PGRB), which is emitted when the optically thick fireshell becomes transparent and consequently has a very well defined time scale determined by the transparency condition. The second component is the emission due to the collision between the accelerated baryonic matter and the CircumBurst Medium (CBM). This comprises what is usually called the “afterglow”. The relative energetics of the two components is a function of B. For B < 10^{5 }the GRB is “PGRB dominated”, since the PGRB is energetically dominant over the second component. The contrary is true for B larger than such a critical value. Since 2001 it has been a major point of our theoretical model that the long GRBs are simply identified with the peak of this second component. In the last year the comprehension of the GRB phenomenon has remarkably increased, thanks to the introduction of the IGC paradigm. The long GRBs associated with Supernovae, which were traditionally considered as an overall single event, are now interpreted as a set of four different Episodes, each one characterized by its own spectral, luminosity and time evolution and corresponding to four different astrophysical processes:
) The “Episode 1” corresponds to the emission from the onset of a Supernova (SN), in a close binary system with a companion neutron star (NS). The initial SN expansion, at nonrelativistic velocities, induces a strong matter accretion onto the NS, which reaches the critical mass and then collapses to a black hole (BH). The observed hard Xray emission is composed of a thermal spectrum plus a powerlaw component, both evolving in time.
) The “Episode 2”, corresponding to the observations of the GRB, is related to the collapse of the NS into a BH.
) The “Episode 3”, in soft Xrays, occurs when the prompt emission from the GRB fades away and it emerges an additional component we discovered in the Swift XRT data. It has been shown that this component, in energetic (Eiso > 10^{52 }erg) GRBsSNe, when referred to the restframe of the source, follows a standard behavior of the light curve evolution. This emission encompasses the SN shock break out and the expanding SN ejecta, and gives origin to an authentic “cosmic candle”.
) The “Episode 4” is represented by the observations of the optical emission of the SN, which has been observed in some IGC sources, with redshift z < 0.9.
This is quite different from the case of the short GRBs. In this year report we have identified the first case of “genuine short GRB” (see below).
Ultra high energy sources: This additional topic was motivated by the interaction with Brian Punsly and was well documented in his volume “Black hole gravitohydromagnetics” (Springer) as well as in the joining of ICRANet by Prof. Felix Aharonian as representative of Armenia in the Scientific Committee and by his appointment as the Adjunct Professor of ICRANet. Many of the observational work done by Prof. Aharonian are crucial for the theoretical understanding of the ultra high energy sources. Prof. Aharonian started also his collaboration with the IRAP PhD program where he is following the thesis of graduate students as thesis advisor.
Supernovae: GRBs have broaden the existing problematic of the study of Supernovae. In some models, e.g. the “collapsar” one, all GRBs are assumed to originate from supernovae. Within our approach, we assume that corecollapse supernovae can only lead to neutron stars, and we also assume that GRBs are exclusively generated in the collapse to a black hole. Within this framework, supernovae and GRBs do necessarily originate in a binary system composed by an evolved main sequence star and a neutron star. The concept of induced gravitational collapse leads to the temporal coincidence between the transition from the neutron star to the black hole and the concurrent transition of the late evolved star into a supernova. This very wide topic has been promoted by the collaboration with Prof. Massimo Della Valle, who is an Adjunct Professor at ICRANet. This kind of research is particularly important for trying to find a coincidence between electromagnetic radiation, highenergy particles, ultra highenergy cosmic rays, neutrinos and gravitational radiation, possible observable for existing or future detectors.
Similarly, the Relativistic Quantum Field Theory topic has been sprouting up two additional new fields: “Von Kernen zu den Sternen” and Plasma Thermalization.
“Von Kernen zu den Sternen” (book in preparation by J. Rueda and R Ruffini): A multiyear study in ICRA and ICRANet has been devoted to the relativistic ThomasFermi equations. The early work was directed to the analysis of superheavy nuclei. In the last years, a special attention has been given to formulate a unified approach which, on one side, describes the superheavy nuclei and, on the other, what we have called “Massive Nuclear Cores”. These last ones are systems of about 10^{57 }nucleons, kept together in beta equilibrium and at nuclear density due to the effect of self gravity. The most surprising result has been that the analytic treatment used by Prof. Popov and his group in their classical work on superheavy nuclei can be scaled to the Massive Nuclear Core regime in presence of gravity. The consequences of this is that an electric field close to the critical value Ec = me^{2}c^{3}/(e) can be found on the surface layer of such Massive Nuclear Cores. This
fortunate result has triggered a great interest and has opened what it can be considered a new approach to the electrodynamics of neutron stars within ICRANet.
Relativistic Quantum Field Theory: A major effort in the last years has been to review the electronpositron creation and annihilation processes in physics and astrophysics. Particularly in the paper by Ruffini, Vereshchagin, Xue [Phys. Rep. 487 (2010) 1140] there are reviewed the conceptual developments which led Dirac to describe the system e^{+}e ^{} 2g, Breit Wheeler to describe the system 2g e^{+}e ^{}and the classical papers of Sauter, Euler, Heisenberg and Schwinger to the analysis of vacuum polarization and pair creation in an overcritical electric field Ec = me^{2}c^{3}/(e). In addition three ultrarelativistic
processes have been in depth reviewed. They deal with (1) the vacuum polarization process in the field of a KerrNewman black hole; (2) the feedback of the electronpositron pair creation on the overcritical electric field; and (3) the thermalization process of the created e^{+}e^{}plasma. This reports, with more than 500 references, gives the background necessary to initiate the study of the quantum field theory description of the electrodynamical approach in the process of gravitational collapse.
Plasma thermalization: The physics of electronpositron plasma has appeared to be relevant for GRBs, but also for the Early Universe, in laboratory experiments with ultraintense lasers etc. We study both nonequilibrium effects such as thermalization and associated timescales, as well as dynamical effects such as accelerated expansion in the optically thick regime. Relativistic numerical codes are designed and widely implemented in this research. The basic outcomes include: determination from the first principles of relaxation timescales of optically thick electronpositron plasma with baryonic loading in the wide range of plasma parameters; conclusion that deviations from a simple "frozen radial profile" in spatial distributions of energy and matter densities of expanding electronpositron plasma with baryonic loading are possible. The last conclusion imply in particular the possibility to recover the spatial distribution of matter and energy in the process of collapse of a GRB progenitor to a black hole.
All the topics have further developed and strengthened and additional topics have sprouted, as it is shown in Fig. 8 and in Fig. 9a, where the projection of these researches are represented. This has led to a deeper understanding of the initial field of research, but has led as well to a wider number of fundamental topics covered by the scientific programs developed at ICRANet.
Figure 9a
Figure 9b
I here report the consolidation of this program, also thanks to the involvement of all the IRAPPhD students (see Fig. 9b). I will review here just a few topics, which will also be presented in the oral contributions of this Scientific Meeting.
Particularly important is the report on Gammarays and Neutrinos from Cosmic Accelerators, on Page 1, which summarizes the activities traditionally carried on by the ICRANet Armenian Scientists in the MAGIC and HESS collaborations. The evolution and future prospects on the analysis of the highenergy emission for GRBs are presented in this report by Prof. Aharonian and Dr. Sahakyan. In parallel, in 2013 has been completed the coating of the telescope in the .Byurakan Observatory, which will give a crucial support to the GRBSN followup observations traditionally addressed as afterglow.
The topic of BKL cosmology is one of the most important and classical contributions of Einstein theory to the study of cosmology. This classic work, developed by Belinski, Kalatnikov and Lifshitz, has already been reviewed in all the major treaties on general relativity, but only recently a new insight has come from the impressive discoveries made by Thibault Damour at the IHES in Paris, by Prof. Mark Henneaux at the University of Bruxelles, and by Herman Nicolai at the Albert Einstein Institute in Potsdam, on the way to generalize the BKL theory of cosmological singularity to the string theories. The new results can be of essential importance for understanding the problem of cosmological singularity and for the identification of hidden internal symmetries in fundamental physics. Prof. Belinski has already finished his part of a new book on “Cosmological singularities” which will written in coauthorship with Prof. Damour. The book has planned to be published by Cambridge University Press. A shortened and adapted version of this book has already been presented in the AIP conference proceedings of XIV Brazilian School of Cosmology and Gravitation (V. Belinski “On the Singularity Phenomenon in Cosmology”, in: Chapter 2, Cosmology and Gravitation: XIV Brazilian School of Cosmology and Gravitation, Cambridge Scientific Publishers, 2011). Three graduate students of the IRAP PhD program are actually working on this topic for their theses with Profs. Hagen Kleinert and Hermann Nicolai in Berlin (Dutta, Fleig, and Gruber). Among the completely new results achieved during the last year, first it should be mentioned the exact description of the quantum dynamics of a supersymmetric version of the Bianchi IX cosmological model and identification the basic role of the KacMoody algebra in the structure of the quantum Hamiltonian (T.Damour et al.). The second result is the proof of the existence of the general cosmological solution with the Friedman initial singularity if the influence of the dissipative processis near singularity will be taken into account in the framework of the IsraelStewart theory (V.Belinski).
On a different topic, during the last year the solitonic solutions of GR has received new interest in respect of the exact solutions of Einstein and EinsteinMaxwell equations: a) The old problem how to generate the exact stationary axisymmetric solutions corresponding to the charged masses with horizons in the framework of Inverse Scattering Method (ISM) was investigated. It was shown that applicability of the ISM in presence of electromagnetic field is not restricted only to the cases with naked singularities (as it have been erroneously stated by some authors). In fact solutions of EinsteinMaxwell equations with horizon also follows from ISM and they are of the same solitonic character. The mathematical procedure of analytical continuations of the nakedsingularity solitonic solutions in the space of their parameters which procedure results in solitonic solutions with horizon has been described (G. Alekseev and V. Belinski “Soliton Nature of Equilibrium State of Two Charged Masses in General Relativity”, arXiv:grqc/1103.0582, IJMP(D) in press, 2011); b) It was found the new way of derivation of the Kerr solution by adding to the Schwarzchild black hole the solitonic vortex made from the pure gravitational field. With this method, one can figure out how rotational energy can contribute to the mass of the resulting Kerr black hole. Also the relation of the HansonRegge type between the mass and angular momentum of a Kerr black hole has been established and its connection with the ChristodoulouRuffini concept of irreducible mass was analyzed (V. Belinski and H. W. Lee “Kerr rotation as solitonic whirl around Schwarzschild black hole”, Nuovo Cimento, submitted, 2011). During the last year all these constructions was generalized also for the electrically charged black holes. It was shown how one can derive the KerrNewman solution by adding a solitonic vortex to the ReissnerNordstrom black hole. The report is on Page 53.
The report on GammaRay Bursts starts on page 71. Major progresses have been accomplished this years in the following aspects (see Figs. 1018):
1) Particularly exciting is the new possibility of having components yet to be observed in GRB sources. In fact, we have shown that it is not possible to interpret GRB 090618 and GRB 101023 within the framework of the traditional single component GRB model. We argue that the observation of the first episode of duration of around 50s could not be a part of a canonical GRB, while the residual emission could be modeled easily with the models existing in literature. This led to the definition of the novel concept of “protoblack hole emission”.
2) Thanks to this new understanding, we studied the Xray emission shown by GRBs associated to SNe as due to the newly born neutron star, introducing the concept of the “neo neutron stars” and further developing the Induced Gravitational Collapse (IGC) scenario. This led us on May 2^{nd }to predict, from the observations of the prompt emission of GRB 130427A, the occurrence of an associated supernova between May 10^{th }and May 13^{th}. This prediction has been indeed confirmed by the observations. This field is evolving so rapidly that “usual” publications in Scientific Journals are no longer fast enough to keep pace. We therefore issued a number of GCN Circulars to quickly inform the Scientific Community of the discoveries:
) GCN 14526: “GRB 130427A: Predictions about the occurrence of a supernova”;
) GCN 14888: “GRB 130609B: Theoretical redshift estimation”;
) GCN 14913: “GRB 130603B: Analogy with GRB 090510A and possible connection with a supernova”;
) GCN 15322: “GRB 130925A: Possible signatures of binary nature in the afterglow  Request for observations”;
) GCN 15560: “GRB 060614: theoretical derivation of the redshift and need for deeper search of the host galaxy”;
) GCN 15576: “GRB 131202A: theoretical estimation of the redshift”.
3) The new developments of the IGC scenario led us to explore the possibility to introduce a new redshift estimator, which we called “cosmic candle by a binary driven hypernova”, for members of the subclass of IGCGRBs.
4) We identified the first example of genuine short GRBs and we identified the new class of GRBs “disguised by excess”. Particularly interesting is also the possible collaboration with Brazil on space projects
Figure 10: A candidate Genuine Short GRB  Figure 11: Spectrum of the genuine short
Figure 12: GRB 090618 light curve  Figure 13: GRB 101023 light curve
Figure 14: Temperature evolution in Episode 1 of GRB 090618  Figure 15: Radius evolution in Episode 1 of GRB 090618
Figure 16: An universal behaviour of restframe Xray luminosity after 20.000  Figure 17: The nested structure of GRBSN Xray afterglows
Figure 18: Arnett and Meakin 2D computations of core collapse
In the report “Relativistic effects in Physics and Astrophysics” (see page 553) it is studied the distribution of the GRB bolometric luminosity over the EQTSs, with special attention to the prompt emission phase. We analyze as well the temporal evolution of the EQTS apparent size in the sky. We use the analytic solutions of the equations of motion of the fireshell and the corresponding analytic expressions of the EQTSs which have been presented in recent works and which are valid for both the fully radiative and the adiabatic dynamics. We find the novel result that at the beginning of the prompt emission the most luminous regions of the EQTSs are the ones closest to the line of sight. On the contrary, in the late prompt emission and in the early afterglow phases the most luminous EQTS regions are the ones closest to the boundary of the visible region (see Fig. 19). We find as well an expression for the apparent radius of the EQTS in the sky, valid in both the fully radiative and the adiabatic regimes. Such considerations are essential for the theoretical interpretation of the prompt emission phase of GRBs.
Figure 19: Evolution of luminosity over the EQTSs
The collaboration on Supernovae is mainly centered from almost daily scientific contact with Prof. Massimo Della Valle, who is currently PI of a VLT proposal “A spectroscopic study of the supernova/GRB connection”. A short summary of the internationally wellknown activities of Prof. Della Valle, who is an Adjunct Professor at ICRANet, is given in the report on page 2175, which contains the many publications in international journals. Prof. Della Valle is also very actively following one graduate student of the IRAP PhD program. A new stimulus has come from the recent understanding of the IGC paradigm, which allows a completely new understanding of the relation between the supernovae and the GRBs
The Report on “Cosmology and Large Scale Structures” on page 621, led by Prof. Fang LiZhi, manifests the progress made by the ICRANet group at the University of Arizona. It deals with three different topics. A. Turbulence behavior of cosmic baryon gas. With hydrodynamic simulation sample of the LCDM universe produced by the WENO algorithm, we show that the intermittency of the velocity field of cosmic baryon fluid at redshift z=0 in the scale range from the Jeans length to about 16h^{1 }Mpc can be extremely well described by the SheLévĕque's scaling formula, which is used to describe a fully developed turbulence. We also found that the nonGaussian features of the cosmic baryon fluid and Lya transmitted flux of quasar absorption spectrum can be well described by a logPoisson hierarchy. B. WouthuysenField coupling. With a stateoftheart numerical method, we show that the resonant scattering of Lya photons with neutral hydrogen atoms will lock the color temperature of the photon spectrum around the Lya frequency to be equal to the kinetic temperature of hydrogen gas. The time scales of the onset of WouthuysenField coupling, the profile of frequency distribution of photons in the state of local thermal equilibrium, the effects of the expansion of the universe on the WouthuysenField coupling in a optical thick halos have also been found. These results are essential for studying the 21 cm signal from high redshift sources. C. Timedependent behavior of Lya photon transfer. Lya photons have been widely applied to study cosmological problems in high redshifts. Since the time scales of high redshift sources, such as GRBs, generally are short, timedependent solutions of Lya photon transfer becomes serious. However, no reliable numerical solvers of the timedependent problem of radiative transfer equation with resonant scattering have been developed till 2006. The timedependent solver (Meiksin, MN, 370, (2006), 20252037) still cannot pass the test of analytical solutions (Field, ApJ, 129, (1959), 551). The solver based on the WENO scheme has been established. It can very well pass various tests (Roy et al ApJ, 716, 2010, 604). It reveals many interesting features of the time evolution of resonant photons Lya in optical thick medium. It provides the solutions of studying the timedependent effect of resonant scattering on the profile of red damping wing of GRBs. It is crucial to understand the halos of GRBs. This report is going to be updated thanks to the new contributions of Prof. XiaoHui Fan.
The Report “Theoretical Astroparticle Physics” on page 671 represents the summary of activities during the last year on this topic by the group including: Carlo Luciano Bianco, Remo Ruffini, Gregory Vereshchagin, SheSheng Xue. Students working within the group include: Alberto Benedetti, Micol Benetti, Damien Begue, Ivan Siutsou. Astroparticle physics is a new field of research emerging at the intersection of particle physics, astrophysics and cosmology. We focused on several topics with three major directions of research: a) electronpositron plasma, b) transparency of relativistically expanding plasma and GRBs, c) neutrinos and large scale structure formation in cosmology, d) the role of dark matter in galaxies and its cosmological counterpart and e) cosmological data and indications for new physics. Electronpositron plasma appear relevant for GRBs and also for the Early Universe, in laboratory experiments with ultraintense lasers, etc. We examine quantum corrections to the collision integrals and determine timescales of relaxation towards thermal equilibrium for high temperature electronpositronphoton plasma. (A.G. Aksenov, R. Ruffini. I.A. Siutsou and G.V. Vereshchagin, “Bose enhancement and Pauli blocking in the pair plasma”, in preparation). We investigate the behaviour of the electronpositron pairs created by a strong electric field. We show how the energy conversion from initial electric field to thermal electronpositron plasma occurs in a complicated sequence of processes starting with Schwinger pair production which is followed by oscillations of created pairs due to back reaction on initial electric field, then production of photons due to annihilation of pairs and finally isotropization of created electron–positron–photon plasma (A. Benedetti, R. Ruffini and G.V. Vereshchagin, “Phase space evolution of pairs created in strong electric fields”, Physics Letters A, Vol. 377 (2013) 206–215). We also consider analogies and differences of physical conditions of electronpositron plasma in GRBs and in cosmology. (R. Ruffini and G.V. Vereshchagin, ”Electronpositron plasma in GRBs and in cosmology”, Il Nuovo Cimento C, Vol. 36, Issue 1, (2013) pp.255266). We study the photospheric emission from ultrarelativistic outflows, which is relevant for understanding GRB emission when ultrarelativistically expanding plasma becomes optically thin. In order to find the observed spectrum we proceed in several different directions: a) approximations to the radiative transfer equations (R. Ruffni, I. A. Siutsou and G. V. Vereshchagin, ”Theory of photospheric emission from relativistic outflows”, the Astrophysical Journal, Vol. 772, Issue 1 (2013) article id. 11) b) Monte Carlo simulations of photon scattering at the dynamical ”photosphere” (D. Begue, I. A. Siutsou and G. V. Vereshchagin, ”Monte Carlo simulations of the photospheric emission in GRBs”, the Astrophysical Journal, Vol. 767, Issue 2 (2013) article id. 139); c) Kompaneets equation with anisotropic photon field (A.G. Aksenov, R. Ruffni and G. V. Vereshchagin, ”Comptonization of photons near the photosphere of relativistic outflows”, MNRAS Letters, Vol. 436, Issue 1 (2013) pp. L54L58) and d) relativistic Boltzmann equations (A. Benedetti and G.V. Vereshchagin, in preparation, 2013). All these results indicate that the photospheric spectrum from ultrarelativistic sources is wider than the Planck one, see Figure 20. In particular, we found α=1, as typically observed in GRBs for temperature decreasing inversely proportional to radius squared.
Figure 20. The spectrum of photospheric emission from photon thick outflow obtained with different approximations. Dotted curve shows the Planck spectrum. Dasheddotted curve shows the result from Ruffini et al. (2013b) obtained using the fuzzy photosphere approximation. Dotted curve shows the result from Begue et al. (2013) obtained from Monte Carlo simulations. Solid curve shows the result from Aksenov et al. (2012) obtained by the solution of the radiative transfer equation with the FokkerPlanck approximation to the collision integral.
In the framework of cosmology we show that in modelling the distribution of dark matter in galaxies in terms of equilibrium configurations of semidegenerate selfgravitating fermions, it allow us to determine a novel corehalo morphology for the dark matter density profiles, as well as an associated novel particle mass bound in the keV range. The most general corehalo solution presents a segregation of three new physical regimes: 1) an inner core governed by a degenerate quantum state of the ‘inos’. 2) At larger radii a low degenerate physical regime exist with a sharply decreasing density distribution followed by an extended plateau. 3) Finally a third regime in which the fermions follow the classical Boltzmann statistics with flat rotation curves. We further check the predicted circular velocity profiles against a sample of high quality rotation curves obtained from recent observations by The HI Nearby Galaxy Survey (THINGS). After extraction of ordinary matter contributions (stellar disk, bulge and gas), we obtain the rotational curves purely due to dark matter and fit with our rotational velocity profiles and with Einasto profiles by least square method. We find that, for the larger part of the sample corresponding to cored
(i.e. not cuspy) Einasto curves, our model is preferred in the majority of the cases. Another relevant observational aspect we consider to check on galactic halos, is the so called Universality laws. This law found by Donato et. al. (2009) implies a constant acceleration due to dark matter at a given halo radius, and is valid for a wide range of galaxies, ranging from dwarf to ellipticals. We then show that it always exists a given set of the free parameters of our model (with ‘ino’ masses beyond the lower bound previously found) which is in agreement with this observational universal result. More observational data coming from the center of some galaxies (i.e. the compact region in the center of our galaxy Sgr A*), compels us to study an extension within the model which includes a new interaction (other than gravitational) between the ‘inos’. For this aim, the minimal standard model extension candidate for dark matter, i.e. the sterile neutrino is considered. The fact that the keVmass range for the sterile neutrinos be in agreement with all current astrophysical/cosmological constraints makes it an excellent candidate. We present future perspectives on how this generalized model of interacting selfgravitating fermions may deal with the distribution of dark matter in galaxies at all scales, from the very center up to the outer halos in a selfconsistent way. Cosmological data and indications for new physics: This year we work on constraint cosmological parameters starting from the minimal model ΛCDM called HarrisonZel'dovich (HZ) model and increasing the number of parameters going to explore several interesting models.
The most important metrics in general relativity is the KerrNewman solution which describes the gravitational and electromagnetic fields of a rotating charged mass, characterized by its mass M, charge Q and angular momentum L in geometrical units. This solution characterizes the field of a black hole. For astrophysical purposes, however, it is necessary to take into account the effects due to the moment of inertia of the object. To attack this problem, an exact solution of the EinsteinMaxwell equations have been proposed by Mashhoon and Quevedo which posses an infinite set of gravitational and electromagnetic multipole moments. It is not clear, however, how this external solution to an astrophysical object can be matched to a physical internal solution corresponding to a physically acceptable rotating mass. The report “Generalization of the KerrNewman solution” on page 1031 reports on current progresses in using an explicit solution of the HartleThorne equation to an eternal solution with N independent quadrupole moments. Equally important has been the result recently obtained by Belvedere showing that a fast rotating model of neutron star with global charge neutrality within the HartleThorne approximation leads to an internal solution of the Kerr metric.
The Report from ICRABR on page 1157 covered a wide range thematic in cosmology and non linear relativistic field theory studied by Prof. M. Novello and his group. This include the geometrical description of quantum mechanics where it is shown that quantum mechanics could be interpreted as a modification of the euclidean nature of a 3D space into a particular affine space. In this formulation, deformation of physical distances are in the core of quantum effects allowing a geometrical formulation of the uncertainty principle. Prof. Novello also studied the Higgs mechanism without Higgs boson. The purpose of this work is to show that the gravitational interaction is able to generate mass for all body. A main part of his activity is related to bouncing cosmology.
The report on Black Holes and Quasars refers to the activity of Prof. Brian Punsly (see page 1171), who is actively participating within ICRANet with the publication of his internationally recognized book on “Black hole gravitohydromagnetics”, the first and second edition (2010) being published with Springer. In addition, Prof. Punsly have been interested in observational properties of quasars such as broad line emission excess in radio loud quasars accentuated for polar line of sight and excess narrow line widths of broad emission lines in broad absorption line quasars, showing that this is best explained by polar lines of sight.
The problem “The electronpositron pairs in physics and astrophysics: from heavy nuclei to black holes” has been the subject of a physics reports of more than 500 references, which is inserted on page 1351, by Ruffini, Vereshchagin and Xue. There, all the different aspects of the field has been reviewed: The fundamental contributions to the electronpositron pair creation and annihilation and the concept of critical electric field; Nonlinear electrodynamics and rate of pair creation; Pair production and annihilation in QED; Semiclassical description of pair production in a general electric field; Phenomenology of electronpositron pair creation and annihilation; The extraction of blackholic energy from a black hole by vacuum polarization processes; Plasma oscillations in electric fields; Thermalization of the mildly relativistic pair plasma. Due to the interaction of physics and astrophysics we are witnessing in these years a splendid synthesis of theoretical, experimental and observational results originating from three fundamental physical processes. They were originally proposed by Dirac, by Breit and Wheeler and by Sauter, Heisenberg, Euler and Schwinger. For almost seventy years they have all three been followed by a continued effort of experimental verification on Earth based experiments. The Dirac process, e^{+}e →2 g, has been by far the most successful. It has obtained extremely accurate experimental verification and has led as well to an enormous number of new physics in possibly one of the most fruitful experimental avenues by introduction of storage rings in Frascati and followed by the largest accelerators worldwide: DESY, SLAC etc. The BreitWheeler process, 2g → e^{+}e^{}, although conceptually simple, being the inverse process of the Dirac one, has been by far one of the most difficult to be verified experimentally. Only recently, through the technology based on free electron Xray laser and its numerous applications in Earthbased experiments, some first indications of its possible verification have been reached. The vacuum polarization process in strong electromagnetic field, pioneered by Sauter, Heisenberg, Euler and Schwinger, introduced the concept of critical electric field. It has been searched without success for more than forty years by heavyion collisions in many of the leading particle accelerators worldwide. In view of the recent developments in the free electron lasers, we have invited at ICRANet Prof. John Madey, the inventor of the free electron lasers, to give a set of lectures and to explore the possibility to have, by focusing the free electron laser signals, the realization in the laboratory of the BreitWheeler process. Prof. Madey has also accepted the position of Adjunct Professor at ICRANet, and he is planning a collaboration with us in the forthcoming years.
In the report on page 1181, using the formula obtained for the rate of pair production in spatially varying external electric field dynamical equations describing the space and time evolutions of pairinduced electric charges, currents and fields bounded within a given spatial region are solved. These results imply the wave propagation of the pairinduced electric field and wavetransportation of the electromagnetic energy in the strong field region. Analogously to the electromagnetic radiation emitted from an alternating electric current, the space and time variations of pairinduced electric currents and charges emit an electromagnetic radiation. We show that this radiation has a peculiar energyspectrum that is clearly distinguishable from the energyspectra of the bremsstrahlung radiation, electron–positron annihilation and other possible background events. This possibly provides a distinctive way to detect the radiation signatures for the production and oscillation of electron–positron pairs in ultrastrong electric fields that can be realized in either ground laboratories or astrophysical environments. (W.B. Han, R. Ruffini, S.S. Xue, Physics Letters B 691 (2010) 99). We focus our attention on studying how this oscillation frequency approaches the plasma frequency. The spectrum of this dipole radiation shows a unique linelike feature, as discussed above. The position of this feature, is determined as a function of the initial value of electric field strength. (A. Benedetti , W. B. Han, R. Ruffini, G.V. Vereshchagin, Physics Letters B6 98 (2011) 75). The ee^{− }pairs generated by the vacuum polarization process around a gravitationally collapsing charged core are entangled in the electromagnetic field (R. Ruffini, L. Vitagliano, S.S. Xue, Phys. Lett. B 573, (2003) 33), and thermalize in an electron–positron–photon plasma on a time scale ~ 10^{4 }t_{C }(R. Ruffini, L. Vitagliano, S.S. Xue, Phys. Lett. B 559, (2003) 12). As soon as the thermalization has occurred, the hydrodynamic expansion of this electrically neutral plasma starts (R. Ruffini, J. Salmonson, J. Wilson, S.S. Xue, A&A Vol. 335 (1999) 334; Vol. 359 (2000) 855). While the temporal evolution of the ee^{− }gravitationally collapsing core moves inwards, giving rise to a further amplified supercritical field, which in turn generates a larger amount of ee^{− }pairs leading to a yet higher temperature in the newly formed e^{+}e^{−}g plasma. We study this theoretically challenging process, which is marked by distinctive and precise quantum and general relativistic effects, and follow the dynamical phase of the formation of Dyadosphere and of the asymptotic approach to the horizon by examining the time varying process at the surface of the gravitationally collapsing core. We conclude that the core is not discharged or, in other words, the electric charge of the core is stable against vacuum polarization and electric field is amplified during the gravitational collapse. As a consequence, an enormous amount of pairs is left behind the collapsing core and Dyadosphere (G. Preparata, R. Ruffini, S.S. Xue, A&A Vol. 338 (1998) L87) is formed. Recently, we study this pairproduction process in a neutral collapsing stellar cores at or over nuclear densities，and show an overcritical electric field on the surface of baryon core. It is shown that in gravitational corecollapse, such an electric field dynamically evolves in the spacetime and electronpositron pairs are produced, leading to the Dyadosphere of electronpositron pairs. This result has been published in (W. B. Han, R. Ruffini, S.S. Xue, Physics Review D86,084004(2012). In order to understand the backreaction of such electric energy building and radiating on collapse, we further adopt a simplified model describing the collapse of a spherically thin capacitor to give an analytical description how gravitational energy is converted to both kinetic and electric energies in collapse. It is shown that (i) averaged kinetic and electric energies are the same order, about an half of gravitational energy of spherically thin capacitor in collapse; (ii) caused by radiating and rebuilding electric energy, gravitational collapse undergoes a sequence of ``on and off'' hopping steps in the microscopic Compton scale. This has been published (R. Ruffini, and SS. Xue , Physics Letters A377 (2013) 2450). Taking into account the EulerHeisenberg effective Lagrangian of oneloop nonperturbative QED contributions, we formulate the EinsteinEulerHeisenberg theory and study the solutions of nonrotating black holes with electric and magnetic charges in spherical geometry. In the limit of strong and weak electromagnetic fields of black holes, we calculate the black hole horizon radius, area, and total energy up to the leading order of QED corrections and discuss the black hole irreducible mass, entropy, and maximally extractable energy as well as the ChristodoulouRuffini mass formula. This result has been published (R. Ruffini, Y.B. Wu and S.S. Xue, Physics Review D88, 085004 (2013)). An interesting aspect of effective field theories in the strongfield limit has recently been emphasized in a completely different class of quantum field theories. These have the property of developing in the strongfield limit an anomalous power behavior. We study and conclude that in the strong fields expansion, the leading order behavior of the EulerHeisenberg effective Lagrangian is logarithmic, and can be formulated as a power law. These results have been published in (H. Kleinert, E. Strobel and SS. Xue, Phys. Rev. D88, 025049 (2013)).
Particularly important is the report From nuclei to compact stars on page 1651. This activity has been carried out by a collaboration between D. Arnett, H. Kleinert, V. Popov, M. Rotondo, J. Rueda, R. Ruffini and S.S. Xue. One of the most active field of research has been to analyze a general approach to Compact Stars like WhiteDwarfs and Neutron Stars, based on the ThomasFermi ultrarelativistic equations amply adopted in the study of superheavy nuclei. The analysis of superheavy nuclei has historically represented a major field of research, developed by Prof. V. Popov and Prof. W. Greiner and their schools. In 2007 the ICRANet group found the welcome result that all the analytic work developed by Prof. V. Popov and the Russian school can be applied using scaling laws satisfied by the relativistic ThomasFermi equation to the case of nuclear matter cores of stellar dimensions, if the beta equilibrium condition is properly taken into account. Since then, a large variety of problems has emerged, which have seen the direct participation of the above mentioned ICRANet Faculty and Adjunct Faculty staff. In a set of seven appendixes, they have been presented the recent progresses made in the intervening years. First, the consideration made for an isolated core with constant proton density whose boundary has been sharply defined by a step function. No external forces are exerted. Then when the assumption of a sharp proton density profile has been relaxed and, consequently, a smooth surface modeled by a WoodsSaxonlike proton distribution has been introduced. The analysis of globally neutral and compressed configurations composed by a relativistic fluid of degenerate neutrons, protons, and electrons in beta equilibrium has been recently accomplished. It has been generalized the FeynmanMetropolisTeller treatment of compressed atoms to relativistic regimes, and the concept of compressed nuclear matter cores of stellar dimensions has been introduced. Finally we studied the construction of neutron star configurations within a fully consistent formulation of the equations of equilibrium in general relativity and strong interactions, which has been covered in the Ph. D. thesis of D. Pugliese, R. Belvedere and S. Martins de Carvalho (see Fig. 21). This work has been successfully generalized to the case of uniformly rotating neutron stars, and it has been part of the Ph. D. thesis of R. Belvedere. The stability of neutron stars against massshedding and secular axisymmetric instabilities have been addressed. The analysis of the properties of the corecrust interface of a neutron star, such as its surface and Coulomb energies, and stability against perturbations have been studied by Y.~Wu and J. Pereira in their Ph. D. theses. This entire program has been developed in order to identify the initial boundary conditions for the electrodynamical process occurring at the onset of gravitational collapse leading to a black hole.
Figure 21: The corecrust transition in a fully general relativistic treatment of a neutron star considering strong, weak, electromagnetic and gravitational interactions
In parallel to this work on the neutron star, the introduction of the techniques for solving a compressed atom in a WignerSeitz cell has allowed to give a new approach to the study of degenerate matter in white dwarfs. This problem presents, still today, open issues of great interest such as the equilibrium of the electron gas and the associated nuclear component, taking into account the electromagnetic, the gravitational and the weak interactions formulated in a correct special and general relativistic framework. A complete analysis of the properties of such configurations as a function of the compression can be duly done through the relativistic generalization of the FeynmanMetropolisTeller approach. It is then possible to derive a consistent equation of state for compressed matter which generalizes both the uniform freeelectron fluid approximation, adopted for instance by Chandrasekhar in his famous treatment of whitedwarfs, and the wellknown work of Salpeter which describes the electrodynamical and relativistic effects by a sequence of approximations. Apart from taking into account all possible electromagnetic and special relativistic corrections to the equation of state of whitedwarf matter, the new equation of state, which incorporates the beta equilibrium condition, leads to a selfconsistent calculation of the onset for inverse betadecay of a given nuclear composition as function of the Fermi energy of electrons or equivalently, as a function of the density of the system. This important achievement, leads to a selfconsistent calculation of the critical mass of whitedwarfs with heavy nuclear composition. In addition, the numerical value of the mass, of the radius, and of the critical mass of whitedwarfs turn to be smaller with respect to the ones obtained with approximate equations of state. Therefore, the analysis of compressed atoms following the relativistic FeynmanMetropolisTeller treatment has important consequences in the determination of the massradius relation of white dwarfs, leading to the possibility of a direct confrontation of these results with observations, in view of the current great interest for the cosmological implications of the type Ia supernovae. The generalization of the above FeynmanMetropolisTeller treatment to the case of finite temperatures has been one of the subjects of the Ph. D. thesis of S. M. de Carvalho. The consequences of the thermal effects on the massradius relation of white dwarfs have been then scrutinized. The particular case of the lowmass white dwarfs that form binary systems with neutron stars, e.g. PSR J1738+0333, has been analyzed in detail. The equation of state obtained from the FeynmanMetropolisTeller approach at finite temperatures has been tested in this lowmass (lowdensity) objects, where large from the zero temperature approximation are expected.
These two topics are leading to the preparation of a new book with Springer with the title “Von Kernen zu den Sternen” by J. Rueda and R. Ruffini.
The generalization of the general relativistic theory of white dwarfs to the rotating case has been successfully achieved in the thesis work of K. Boshkayev. The entire family of uniformly rotating stable white dwarfs has been already obtained by studying the massshedding, the inverse bdecay, pycnonuclear, and axisymmetric instabilities. The maximum mass and the minimum (maximum) rotation period (frequency) have been obtained for selected nuclear compositions. These results are relevant both for the theory of type Ia supernovae as well as for the recent work of M. Malheiro, J. Rueda and R. Ruffini on the description of SoftGammaRay Repeaters (SGRs) and Anomalous XRay Pulsars (AXPs) as rotation powered white dwarfs, following a pioneer idea of M. Morini et al. (1988) and of B. Paczynski (1990) on the AXP 1E 2259+586. The recent observation of SGR 0418+5729 promises to be an authentic Rosetta Stone, a powerful discriminant for alternative models of SGRs and AXPs. The loss of rotational energy of a neutron star cannot explain the Xray luminosity of SGR 0418+5729, excluding the possibility of identifying this source as an ordinary spindown powered neutron star. The inferred upper limit of the surface magnetic field of SGR 0418+5729 B < 7.5x10^{12 }G, describing it as a neutron star within the magnetic braking scenario, is well below the critical magnetic field B =2pmc^{3}/(he) ~ 4.4x10^{13 }Gauss, challenging the power mechanism based on magnetic field decay purported in the magnetar scenario. We have shown that the observed upper limit on the spindown rate of SGR 0418+5729 is, instead, perfectly in line with a model based on a massive fast rotating highly magnetized white dwarf of fiducial mass M=1.4M_{Sun}, radius R=10^{3 }km, and moment of inertia I ~ 10^{49 }g cm. We have analyzed the energetics of all SGRs and AXPs including their steady emission, the glitches and their subsequent outburst activities. It can be then shown that the occurrence of the glitch, the associated sudden shortening of the period, as well as the corresponding gain of rotational energy, can be explained by the release of gravitational energy associated to a sudden contraction and decrease of the moment of inertia of the white dwarfs, consistent with the conservation of their angular momentum. The energetics of the steady emission as well as the one of the outbursts following the glitch can be simply explained in term of the loss of the rotational energy in view of the moment of inertia of the white dwarfs, much larger than the one of neutron stars. There is no need here to invoke the decay of ultrastrong magnetic fields of the magnetar model (see Fig. 22). A more exhaustive analysis of SGR 0418+5729 within the white dwarf model has been recently achieved in the Ph. D. thesis of K. Boshkayev. The request of the rotational stability of the white dwarf gives bounds for the mass, radius, moment of inertia and magnetic field, through the analysis of constant rotation period sequences of uniformly rotating white dwarfs. We have also analyzed the emission properties in the optical band, and inferred the cyclotron frequencies associated to their magnetic fields which might cause absorption features in the optical wavelengths. The same analysis has been accomplished for Swift J1822.31606 and 1E 2259+586. We are in addition considering the possible progenitors of these massive fast rotating highly magnetized white dwarfs. We have considered the possibility that white dwarfs mergers could be the progenitor of white dwarfs with the above desirable properties, hence of SGRs and AXPs. In collaboration with P. Loren from University of Exeter in UK, and the group led by Prof. GarciaBerro at Universitat Politecnica de Catalunya and Institute for Space Studies of Catalonia in Barcelona, we have performed numerical simulations of white dwarf mergers. We have shown that the products of these mergers consist of a hot central magnetized white dwarf surrounded by a heavy rapidly rotating disk. The evolution of the postmerger massive rapidly rotating magnetized white dwarf and its emission properties in the optical bands, have been computed. We have shown that these properties are consistent with AXPs such as 4U 0142+61, which show an infrared excess explainable via the existence of a dust disk, whereas the surface black body emission well describes the observations in the UV bands. The emission by these white dwarfs in the Xray band is currently under consideration and it is the subject of the Ph. D. thesis of D. Cáceres.
Figure 22: Rotation period derivative versus the rotation period of SGRs and AXPs (red, blue and green). The dashed curves are contours of constant magnetic field, for a model based on white dwarfs.
The thermal evolution of neutron stars has been one of the thesis topics of S. M. de Carvalho. This work has been done in collaboration with R. Negreiros from Universidade Federal Fluminense in Brazil. The cooling curves of the novel neutron stars satisfying the condition of global charge neutrality have been obtained by full numerical integration of the radiative and transport equations in general relativity. A detailed comparison with the traditional case of locally neutral neutron stars has been performed.
The understanding of the theory of neutron stars has allowed the analysis of their role in astrophysical systems such as the GRBs, the GRBSupernova, and the short GRBs. It has been analyzed in detail the binary progenitors of these systems with particular emphasis on the role played by neutron stars.
Concerning short GRBs, we had the first example that they are the result of the merger of neutron star binaries. F. Gomes Oliveira, as part of her Ph. D. thesis, has computed the evolution of binary neutron stars up to the merger point to evaluate the emission of gravitational waves in these systems. The dynamics has been simulated via the effective onebody formalism of Prof. Thibault Damour, up to fourth postNewtonian order. The detectability of this emission by second generation detectors such as Advanced LIGO has been assessed, and the total energy output in gravitational waves has been compared with the observed emission in both X and gamma rays. This work has been possible thanks to the analysis of the first genuinely short GRB, GRB 090227B by Muccino et al. (2013), where it has been shown that the properties of this GRB indeed are consistent with a binary neutron star progenitor.
There are other aspects of GRBs where the physics of neutron stars plays an important role and where the different aspects of a detailed description of the neutron star interior described above acquire a specific value. This is the case of the process of induced gravitational collapse of a neutron star to a black hole by a supernova in a binary system. I come back to this point later on, to the distinction between long and short GRBs, as well as the GRBSN connection.
The topic about Symmetries in General Relativity (the full report is on page 2193) has been developed as an intense collaboration between various research groups. Profs. R.T. Jantzen, L. Stella (Observatory of Monte Porzio, Rome), O. Semerak (Czech Republic), D. Bini and Dr. A. Geralico have studied the problem of motion of test particles in black hole spacetimes, in presence of a superposed radiation field. The scattering of radiation by the test particles causes a frictionlike drag force which forces particles on certain equilibrium orbits outside the black hole horizon. This interesting effect, known as PoyntingRobertson effect, has been deeply investigated in many different contexts: besides the Schwarzschild and Kerr black hole, novel results have been published for the case of a Vaidya radiation metric. In the latter case, in fact, one takes the advantages of having an exact solution of the Einstein’s field equations whose source is a null field. Among the various consequences we mention that while a unique equilibrium circular orbit exists if the photon flux has zero angular momentum, multiple such orbits appear if the photon angular momentum is sufficiently high. Furthermore other solutions of the Weyl class with cylindrical symmetry as well as solutions within the class of exact gravitational plane waves and electromagnetic plane waves have been examined in the context of PoyntingRobertson like effects obtaining a number of physically relevant situations. Bini and Geralico have also considered the motion of spinning test particles in Kerr spacetime in full generality with the aim to study deviations between the world lines of spinning objects in comparison with those of geodesic test particles, generalizing some recent works on the same topic where motion were but constrained on the equatorial plane. Bini, Geralico and Jantzen have been able to obtain new foliations in spacetimes admitting separable geodesics. These “separable geodesic action slicing” have been used then to explore certain geometrical properties of horizon penetrating coordinates in black hole spacetimes. Other collaborations, again for what concerns the topics included in symmetries in General Relativity, have been started with Profs. A. Ortolan (INFN Legnaro, Padova, Italy) and P. Fortini (University of Ferrara, Italy) to study of the interaction of electromagnetic waves with gravitational waves, with the gravitational waves considered in the exact theory and not in its linear approximation.
In collaboration with Campus BioMedico in Rome there are ongoing researches on galactic structures. The Reports “Self Gravitating Systems, Galactic Structures and Galactic Dynamics” on page 2305 is focused on analytical and numerical methods for the study of classical selfgravitating fluid/gaseous masses. A series of papers of this group have been devoted in the past to the generalization of the classical theory of ellipsoidal figures of equilibrium using virial methods. The research activities of the group have focused subsequently on functional methods for obtaining equilibrium solutions for polytropic selfgravitating systems that rotate and have a non uniform vorticity. The group has recently published a novel and important result in the context of analogous geometry theory. It is well known that the wave equation for the perturbations of given a perfect barotropic and irrotational Newtonian fluid can be rewritten as an “effective General Relativity”. They have extended this result including the possibility for the fluid to be selfgravitating. This work opens the path for a new interpretation of classical whitedwarf theory in terms of curved spacetime techniques. The group has also studied the perturbations of classical compressible rotating but not gravitating fluids as occurring in generalized acoustic black holes. It has also analyzed the Analog Gravity formalism at full nonlinear level through Von Mises’ Wave Equation for irrotational configurations.
We recall the successful attempt of applying methodologies developed in Relativistic Astrophysics and Theoretical Physics to researches in the medicine domain. The Report “Interdisciplinary Complex Systems” on page 2335 adopts analytical and numerical methods for the study of problems of nonlinear dynamics focusing on biological systems and using a theoretical physics approach. It is well established both numerically and experimentally that nonlinear systems involving diffusion, chemotaxis, and/or convection mechanisms can generate complicated timedependent spiral waves, as in happens in chemical reactions, slime molds, brain and in the heart. Because this phenomenon is global in Nature and arises also in astrophysics with spiral galaxies, the goal of this research activity has been to clarify the role of this universal spiraling pattern. The group has studied numerically the nonlinear partial differential equations of the theory (ReactionDiffusion) using finite element methods. The group has recently published moreover a novel and important result: an electromechanical model of cardiac tissue, on which spiral moves and causes the domain to deform in space and time (see Fig. 23). This model is a real breakthrough in the context of theoretical biophysics, leading to new scenarios in the context of computational cardiology. In 2011 the group has focused its research on classical hydrodynamics, evaluating the stress exerted by the fluid on the domain walls and introducing an indicator of risk for their damage. Such a methodology, named as “threeband decomposition analysis of wall shear stress in pulsatile flows”, has been immediately applied to hemodynamical problems which have been numerically integrated (see Fig. 24), but results promising also for other problems of physical and biological sciences and for engineering.
Figure 23: Electrical activity map of an electroelastic deformed patch of cardiactype tissue
Figure 24: Turbulent flow structure (specifically the velocity amplitude) in a deformed vessel, obtained by numerical integration through finite elements of the incompressible NavierStokes equations.
The next contribution is the one by Jaan Einasto of the Tartu Astronomical Observatory. Prof. Einasto has been collaborating in the previous year intensively within ICRA about the large scale structure of the Universe and its possible fractal structure. With Prof. Einasto there is also the collaboration of Prof. G. Hutsi. Since two years Prof. Einasto is an Adjunct Professor of ICRANet and an active member of the Faculty of the IRAP PhD. In this role Prof. Einasto has delivered a set of lectures in the months of February and September 2010 on “The large scale structure of the universe: a powerful probe for fundamental physics”. This topic was covered with a quantitative analysis of the distribution of galaxies, on dark matter, on the cosmological parameters and dark energy. At the moment, Prof. Einasto has completed a book reviewing the status of the dark matter and the large scale structure of the universe published by World Scientific as Volume 14^{th }in the Advanced Series in Astrophysics and Cosmology Series edited by L.Z. Fang and R. Ruffini. This book covers the material of the lectures delivered in the IRAP PhD program as well as an historical perspective between the different approaches to the study of the dark matter content of the universe in the west and in the former Soviet union. The full report is on page 1177.
An important fundamental research topic is the investigation of “analogue models of gravity”. Such models have been used to understand many aspect of gravitational phenomena, in particular the mechanism of Hawkingand UnruhRadiation, by studying in supersonic flow nozzles. These were of great help in dispersing criticism of these radiations based on our ignorance of the divergences of local quantum field theory at ultrashort distances. Another important analogy is bases on the relation between EinsteinCartan Physics and the theory of defects in solids, worked out in detail in the textbook by our adjunct faculty members H. Kleinert: <
http://users.physik.fu
berlin.de/~kleinert/kleinert/?p=booklist&details=1
>. This analogy has recently allowed to understand the equivalence of Einstein's theory of gravitation with his Teleparallel Theory of Gravitation as a result of a novel gauge symmetry. The first uses only the curvature of spacetime to explain gravitational forces, while the second uses only torsion. The equivalence relies on the fact that crystalline defects of rotation and translation (disclinations and dislocations, respectively) are not independent of each other, but the ones can be understood as superpositions of the other. Moreover, the analogy has allowed to set up an infinite family of intermediate theories in which curvature and torsion appear both <
http://klnrt.de/385/385.pdf
>. Finally, all geometries relevant in gravitational physics has been derived from a completely new theory of multivalued fields <
http://www.physik.fuberlin.de/~kleinert/kleinert/?p=booklist&details=9
>.
A volume dedicated to Fermi and Astrophysics has been edited in the recent years and has been finally completed (“Fermi and Astrophysics”, edited by D. Boccaletti and R. Ruffini, World Scientific, 2011). This book has some different goals: 1) to present some papers which were published at ICRA in the occasion of the centenary of the birth of Enrico Fermi; 2) to translate into English a set of papers by Fermi which were available only in Italian; 3) to try to understand the reason why, having been one of the greatest experts on Einstein theory in the earliest years of his life, after his transfer to Rome and later on to the United States Fermi never published anything on Einstein theory. In the latest part of his life Fermi realized that astrophysics offers a great future to physics. The only paper by Fermi mastering general relativity and cosmology was to prove George Gamow work being wrong. On the contrary, he managed in matter of fact to give one of the greatest contribution to cosmology and to Gamow theory and to Einstein theory of general relativity.
Other books which are currently in preparation are:
 J. Einasto, “Dark Matter and Large Scale Structure Story”, World Scientific, 2013.
 J. Rueda and R. Ruffini, “Von Kernen zu den Sternen”, Springer, expected in 2014.
 R. Ruffini, G.V. Vereshchagin and S.S. Xue, “Oscillations and radiation from electronpositron plasma”, World Scientific, expected in 2014.
 V. Belinski and E. Verdaguer, “Gravitational Solitons”, Second Edition, Cambridge University Press, expected in 2014.
 V. Belinski, “Cosmological Singularity”, Cambridge University Press, expected in 2014.
 D. Bini, S. Filippi and R. Ruffini, “Rotating Physical Solutions”, Springer, expected in 2014.
 C.L. Bianco, L. Izzo, R. Ruffini and S.S. Xue, “The Canonical GRBs”, World Scientific, expected in 2014.
 H.C. Ohanian, R. Ruffini, “Gravitation and Spacetime”, Third Edition, Norton and Company 2013.
An oral presentation by Pascal Chardonnet of the current situation of the IRAP PhD and the Erasmus Mundus program cosponsored by the European Commission, as well as a report on the first 28 graduate students enrolled in the program (see enclosure 7).
Acknowledgements
I am very happy to express, on behalf of all the Members of ICRANet and myself, our profound gratitude to the Minister of Foreign Affairs, to the Minister of Economy and Finances of Italy. Special gratitude to the Ragioneria Generale of the Ministry of Economy and Finances, for their attention in the activities of ICRANet. A special recognition goes to the activities of the many Ambassadors and Consuls who have greatly helped in the intense series of activities carried out by ICRANet in Belarus, Brazil, France, China, Korea and New Zealand. Special gratitude to the Foreign Ministries of Armenia and of Brazil for drafting the Seat Agreements for the ICRANet seats in Yerevan and in Rio.
This year has been marked by an intense series of lectures organized by ICRANet at the University of Nice Sofia Antipolis for the graduate students and by the completion of the seat of Villa Ratti in Nice. We are grateful for this common effort to the President, Frédérique Vidal, and the Vice President, Stéphane Ngô Maï, of the University of Nice Sofia Antipolis. We are grateful to the Mayor of Pescara, to the Mayor of Nice, Christian Estrosi, to the Adjunct for Science, Research and Culture, Dr. Agnes Rampal, and to the President of the Conseil Général des AlpesMaritimes, Eric Ciotti, for their generous support in granting to ICRANet the logistics of the Centers in their respective townships.
We are equally very grateful to the Brazilian Institutions, the Foreign Minister of Brazil, the Minister of Science of Brazil, the Governor of the State of Cearà, the Mayor of Rio for their essential support in the establishment of the ICRANet seat in Brazil. All this has been made possible thanks to the very effective presence of Mario Novello and Joao Braga in the board and in the Scientific Committee of ICRANet. A special sign of gratitude goes to Minister Roberto Amaral and to Prof. Francisco José Amaral Vieira for their continuous support. All this work could not have been achieved without the help of all Members institutions of ICRANet.
Special gratitude goes also to the Armenian Ambassador in Rome, H.E. Mr. Sargis Ghazaryan, and to the Brazilian Ambassador in Rome, H.E. Ricardo Neiva Tavares.
We look forward to the school “Search for life beyond the Solar System” (March 1621, 2014, Tucson, Arizona), organized thanks to the collaboration with the Specola Vatican and in particular his Director Fr. José Funes, SJ.
Clearly, a special mention of satisfaction goes to all the Scientific Institutions and Research Centers which have signed with us a collaboration agreement which include ASI (Italian Space Agency, Italy), BSU (Belarusian State University, Belarus), CAPES (Brazilian Fed. Agency for Support and Evaluation of Grad. Education), CBPF (Brazil), Cearà State (Brazil), ENEA (National Agency for new technologies, energy and the economic sustainable development, Italy), FAPERJ (Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Brazil), GARR (Italy), ICTP (The Abdus Salam International Center for Theoretical Physics, Italy), IHEP (Institute of High Energy Physics, Chinese Academy of Sciences, China), IHES (Institut des Hautes Études Scientifiques, France), INPE (Instituto Nacional de Pesquisas Espaciais, Brasil), INFN (National Institute for Nuclear Physics, Italy), ITA (Instituto Tecnológico de Aeronáutica, Brazil), LeCosPa (Leung Center for Cosmology and Particle Astrophysics, Taiwan), NASB (National Academy of Sciences, Belarus), NAS RA (National Academy of Science, Armenia), Nice University Sophia Antipolis (France), Pescara University “D’Annunzio” (Italy), Physics Department of University of Rome “Sapienza” (Italy), SCSA (State Committee of Science of Armenia), UERJ (Rio de Janeiro State University, Brazil), UFPB (Universidade Federal da Paraíba, Brazil), UIS (Universidad Industrial de Santander, Colombia), UNAM (Universidad Nacional Autonoma De Mexico), UNIFEI (Universidade Federal de Itajubà, Brazil), University of Rome “Sapienza” (Italy), UNS (Universidad Nacional del Sur, Argentina).
ICRANet, as sponsor of the IRAPPhD program, expresses its gratitude to AEI – Albert Einstein Institute – Potsdam (Germany), Bremen University (Germany), Carl von Ossietzky University of Oldenburg (Germany), CBPF – Brazilian Centre for Physics Research (Brazil), Ferrara University (Italy), IHES (France), Indian centre for space physics (India), INPE (Instituto Nacional de Pesquisas Espaciais, Brasil), Nice University Sophia Antipolis (France), Observatory of the Côte d'Azur (France), Rome University – “Sapienza” (Italy), Savoie University (France), Shanghai Astronomical Observatory (China), Stockholm University (Sweden), Tartu Observatory (Estonia), for their joint effort in creating and activating this first European Ph.D. program in Relativistic Astrophysics which has obtained the official recognition of the Erasmus Mundus program of the European Community. All these activities were achieved thanks to the dedicated work of Prof. Pascal Chardonnet.
Finally, thanks goes to the Physics Department of the University of Rome “Sapienza” for all the collaboration with ICRA in the teaching, in the electronic links and in the common research.
A special mention of gratitude, of course, goes to the administrative, secretarial and technical staff of ICRANet and ICRA for their essential and efficient daily support.
