ICRANet Newsletter

ICRANet Newsletter
Novembre/Dicembre 2014 – Gennaio 2015

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Questa newsletter sarà presentata al pubblico dal direttore di ICRANet, prof. Remo Ruffini, e dai membri docenti presso la Sede Centrale ICRANet in Piazza della Repubblica, 10, a Pescara (Italia), nelle prossime settimane. La data esatta verrà annunciata con anticipo a tutte le istituzioni.
Gli interessati a partecipare alla presentazione dovranno registrarsi qui.
Poiché il numero dei partecipanti ammessi è limitato a 100, si raccomanda di registrarsi quanto prima.

SOMMARIO
- Riunione 2014 del Comitato Scientifico
- Discussione della tesi e diplomi degli studenti di dottorato
- Ricercatori in visita e nuovi studenti all’ICRANet
- Ultime pubblicazioni e atti di convegno
- Sviluppi recenti all’ICRANet di Rio de Janeiro
- Prossime conferenze

Riunione 2014 del Comitato Scientifico

Il 27 e 28 Novembre, 2014, presso la sede ICRANet di Pescara, si è tenuto il 12° Meeting del Comitato Scientifico ICRANet.
I risultati scientifici e le pubblicazioni nel 2014 relativi alle diverse linee di ricerca ICRANet sono stati discussi con i rappresentanti degli Stati e Università membri di ICRANet riuniti a Pescara: il Prof. Felix Aharonian (Armenia), il Dr. Carlo Luciano Bianco (ICRA), il Prof . Massimo della Valle (Italia), il Dr. Gabriele Gionti (Città del Vaticano), il Dr. Luca Izzo con delega del Prof. John Mester (Università di Stanford), la Prof.ssa Débora Peres Menezes (rappresentante temporaneo del Brasile), il Prof. Jorge Rueda con delega del Prof. David Arnett (Università dell’Arizona) e il Prof. Remo Ruffini (direttore di ICRANet).
Sono state presentate anche le attività scientifiche e didattiche di ICRANet nel 2014: ad esempio, l'organizzazione di incontri scientifici internazionali e scuole di dottorato, la firma di accordi scientifici e la collaborazione con importanti istituzioni, in particolare del programma di Dottorato Internazionale in Astrofisica Relativista (IRAP-PhD Program).
Il Rapporto Scientifico 2014 completo, presentato dal direttore ICRANet al comitato scientifico ICRANet, può essere consultato al seguente link: www.icranet.org/report_2014

Discussione della tesi e diplomi degli studenti di dottorato

Yuanbin WU, "Forti campi elettromagnetici in fisica e astrofisica: stelle di neutroni, buchi neri, e campi laser intensi", discussione: 10 ottobre 2014 presso l'Università di Roma "Sapienza"

Fundamental phenomena of quantum electrodynamics (QED) and other fundamental interactions in strong electromagnetic fields are among the important topics in physics and astrophysics. In the thesis, we study various phenomena of strong electromagnetic fields in physics and astrophysics, from neutron stars and black holes to intense laser fields. The core-crust interface of neutron stars with global charge neutrality is studied; in this core-crust interface, a very strong electric field which is overwhelming the critical value is developed. This study is generalized to the case of heavy atoms. Extracting energy from black holes has been an interesting topic for decades. Taking into account one loop nonperturbative QED effects of strong fields, the Einstein-Euler-Heisenberg theory is formulated and the properties of black holes such as the maximally extractable energy are studied. Turning to the laboratory experiments, we studied the Breit-Wheeler process which is one of most relevant elementary processes in astrophysics, in the case that a photon colliding with a bifrequent field. High multiphoton phenomena has been shown.

On the left: The core-crust interface of neutron stars with global charge neutrality, see [Rueda, Ruffini, Wu, and Xue, Phys. Rev C 89, 035804 (2014)]. On the right: One-loop Feynman diagrams related to the Euler-Heisenberg effective Lagrangian.

The thesis is based on following publications:
1) "Nonlinear Breit-Wheeler process in the collision of a photon with two plane waves", Y. B. Wu, S. S. Xue, Phys. Rev. D90, 013009 (2014).
2) "Einstein-Euler-Heisenberg Theory and Charged Black Holes", R. Ruffini, Y. B. Wu, S. S. Xue, Phys. Rev. D 88, 085004 (2013).
3) "Surface tension of the core-crust interface of neutron stars with global charge neutrality Rueda", Jorge A. R. Ruffini, Y. B. Wu, S. S. Xue, Phys. Rev. C89 (2014) 3, 035804.
4) "On the surface tension and Coulomb energy of neutron-star matter Wu", Yuan-Bin J. Korean Phys. Soc. 65 (2014) 6, 850-854.

Wu continua la sua carriera scientifica come Post Doc all'Istituto Max Planck di Fisica Nucleare, Heidelberg, Germania.

Damien BEGUE "L'emissione fotosferica di lampi di raggi gamma: dall'analisi teorica ai vincoli osservativi", discussione: 28 ottobre 2014 presso l'Università di Roma "Sapienza"

The deals with the most luminous sources in the universe: gamma-ray bursts. It is known that the emission of these events originate from a plasma moving nearly at the speed of light. Initially, the plasma is opaque, which means that photons can not escape: they are scattered by the electrons of the plasma many times. As the plasma expands, the density decreases and photons can escape the plasma. The resulting emission, called photospheric emission, can be used to constrain the properties of the plasma, and especially its speed. However, these estimates rely on the assumption that the observed spectrum of the photospheric emission is a black-body. In this thesis the light-curves and spectra of the photospheric emission in different situations is studied: when the transparency takes place in the accelerating phase, in the coasting phase or when the dynamics is mediated by magnetic reconnection.

In figure: Time-integrated spectra of the photospheric emission of a coasting outflow computed with different methods. A black-body (curve 1) is displayed for comparison. It appears clearly that the observed spectrum is broader than the Planck spectrum.

The thesis is based on following publications:
1) "Monte Carlo Simulations of the Photospheric Emission in Gamma-Ray Bursts", D. Bégué, I.A. Siutsou and G.V. Vereshchagin, ApJ 767 (2013) 139.
2) "Transparency of an instantaneously created electron-positron-photon plasma", D. Bégué and G.V. Vereshchagin, MNRAS 439 (2014) 924.
3) "Transparency Parameters from Relativistically Expanding Outflows", D. Bégué and S. Iyyani, ApJ 792 (2014) 42.
Poynting flux dominated jets challenged by their photospheric emission, D. Bégué and A. Pe’er, ApJ (2015), in press; arXiv:1410.2730.

Begue continua la sua carriera scientifica come Post Doc all’Università di Stoccolma, in Svezia.

Marco MUCCINO, "Il ruolo dei sistemi binari come progenitori di GRB brevi e GRB lunghi associati alle Supernovae", discussione: 26 novembre 2014 presso l'Università di Roma "Sapienza"

The thesis addressed the physical origin of the emission of very energetic short and long Gamma-ray bursts (GRBs) associated with supernovae (SNe). From detailed data analyses performed within timescales from milliseconds up to several days, from the X-rays to gamma-rays (up to 100 GeV), the proposal is that both systems originate from binary systems. Very energetic short GRBs originate from merging of neutron stars (NSs). The total mass of these systems must be larger than the NS critical mass, namely 2.67 times the mass of our Sun, to form a black hole (BH) and emit a GRB. For long GRBs the association with SNe is explained within the induced gravitational collapse (IGC) paradigm: a binary progenitor composed of a naked core of an evolved star, depleted by the outer hydrogen and helium, and a companion NS. The naked core explodes as a SN Ic, explaining the lack of the above elements, while its ejected matter accretes onto the NS, triggering the formation of a BH and, again, the GRB emission. The further evolution of the system and the consequent emission of these stages are discussed and explained, allowing to predict the occurrence or not of a SN associated to a GRB.

 

In Figure, the transparency emission (P-GRB) of the first recognized short GRB originating from a NS-NS merger leading to BH formation: GRB 090227B. On the left, the light curve from the NaI-n2 detector (on-board the Fermi satellite) of the P-GRB at a time resolution of 16 milliseconds. On the right, the corresponding spectrum where a thermal component (the narrow dashed function at the center) is evident, as predicted by the Fireshell model, with one of the highest temperature ever inferred.

The thesis is based on following publications:
1) "Evidence for a proto-black hole and a double astrophysical component in GRB 101023", A.V. Penacchioni, R. Ruffini, L. Izzo, M. Muccino, C.L. Bianco, L. Caito, B. Patricelli, L. Amati, A&A, 538, A58 (2012).
2) "GRB 090227B: the missing link between the genuine short and disguised short GRBs", M. Muccino; R. Ruffini; C.L. Bianco; L. Izzo; A.V. Penacchioni. ApJ 763, 125 (2013).
3) "GRB 110709B in the induced gravitational collapse (IGC) paradigm, A.V. Penacchion"i, R. Ruffini, C.L. Bianco, L. Izzo, M. Muccino, G.B. Pisani, J. A. Rueda, A&A, 551, A133 (2013).
4) "On a novel distance indicator for Gamma-Ray Bursts associated with Supernovae", G.B. Pisani, L. Izzo, R. Ruffini, C.L. Bianco, M. Muccino, A.V. Penacchoni, J. A. Rueda, Y. Wang. A&A, 52L, 5 (2013).
5) "GRB 090510: A Disguised Short Gamma-Ray Burst with the Highest Lorentz Factor and Circumburst Medium", M. Muccino, R. Ruffini, C.L. Bianco, L. Izzo, A.V. Penacchioni, G.B. Pisani, ApJ, 772, 62 (2013).
6) "Induced Gravitational Collapse in the BATSE era: the case of GRB 970828", R. Ruffini; L. Izzo; M. Muccino; J.A. Rueda; C. Barbarino; C.L. Bianco; H. Dereli; M. Enderli; A.V. Penacchioni; G.B. Pisani; Y. Wang.,submitted to A&A (arXiv:1311.7432), 2013.
7) "On binary-driven hypernovae and their nested late X-ray emission", R. Ruffini, M. Muccino, C. L. Bianco, M. Enderli, L. Izzo, M. Kovacevic, A. V. Penacchioni, G. B. Pisani, J. A. Rueda, Y. Wang, A&A, 565, L10 (2014).
8) "GRB 130427A and SN 2013cq: A Multiwavelength Analysis of An Induced Gravitational Collapse Event", R. Ruffini, Y. Wang, M. Kovacevic, C. L. Bianco, M. Enderli, M. Muccino, A. V. Penacchioni, G. B. Pisani, J. A. Rueda. ApJ in press (2014).
9) "Induced gravitational collapse at extreme cosmological distances: the case of GRB 090423", R. Ruffini, L. Izzo, M. Muccino, G. B. Pisani, J. A. Rueda, Y. Wang, Barbarino, C. L. Bianco, M. Enderli, M. Kovacevic, A&A, 569, A39, (2014).
10) "A search for Fermi bursts associated with supernovae and their frequency of occurrence", M. Kovacevic, L. Izzo, Y. Wang, M. Muccino, M. Della Valle, L. Amati, C. Barbarino, M. Enderli, G. B. Pisani, L. Li, A&A, 569, A108 (2014)
11) "GRB 140619B: a short GRB from a binary neutron stars leading to the black hole formation", M. Muccino, R. Ruffini, M. Kovacevic, L. Izzo, F. G. Oliveira, J. A. Rueda, C.L. Bianco, M. Enderli, A.V. Penacchioni, G.B. Pisani, Y. Wang, E. Zaninoni, ArXiv:1412.1018, 2014.

Muccino continua la sua carriera scientifica come assegnista presso l'Università "La Sapienza", Roma, Italia

Giovanni Battista PISANI, "Un nuovo paradigma per Gamma-Ray Bursts energetici associati alle Supernovae: verso una nuova candela standard", discussione: 26 Novembre 2014, Università di Roma "Sapienza"

The PhD research project included the reduction and analysis of Gamma Ray Bursts (GRBs) data from different satellites, such as Batse, Swift or Fermi. GRBs are flashes in gamma-rays observed in distant galaxies. They can last from milliseconds to several minutes with a released energy of the order of the solar mass. They are indeed the most powerful events ever observed in the Universe. The attention was focused on GRBs associated with Supernovae (SNe). It have been recently proposed the Induced Gravitational Collapse (IGC) occurring in a particular class of binary systems as progenitors for the aforementioned GRB-SN sources. Such phenomena are referred as Binary-driven HyperNovae (BdHNe). We have further developed the BdHN paradigm and enlarged the sample of BdHN candidates. One of the most exciting outcomes of this work is the possibility to consider this class of BdHN events as a standard candle. If confirmed, this result could provide new independent challenges on the current cosmological model back to 600 millions years only after the Big Bang.

In figure: The plot shows the X-ray afterglow luminosity of a sample of GRB sources as a function of the rest-frame time after the GRB explosion. The sample is composed by the six GRB listed in the upper table: they all are associated with a SN, have a measured redshift, have an isotropic explosion energy larger than 10^52 ergs, and have very good quality X-ray data. Furthermore, they have all been classified as binary-driven hypernovae (BdHNe).
The X-ray luminosities of all the considered sources clearly show the same decaying behavior after about 20000 seconds, despite their separate behaviors at earlier times and the different energies of their relative GRB source. We currently use this scaling law to infer the redshifts of similar sources when it is not measured, and to predict the SN arising about 10-15 days after the initial explosion.
If the validity of this law will be confirmed for any redshift, it would open the possibility to use BdHNe as standard candles to test the current cosmological model.

The thesis is based on following publications:
1) "GRB 090510: a disguised short GRB with the highest Lorentz factor and circumburst medium", Muccino, M.; Ruffini, R.; Bianco, C. L.; Izzo, L.; Penacchioni, A. V.; Pisani, G. B.,2013, ApJ, 772, 62.
2) "GRB 110709B in the induced gravitational collapse paradigm", Penacchoni, A.V.; Ruffini, R.; Bianco, C. L.; Izzo, L.; Muccino, M.; Pisani, G. B.; Rueda, J. A., 2013, A&A, 551, A133.
3) "Novel distance indicator for gamma-ray bursts associated with supernovae''", Pisani, G. B.; Izzo, L.; Ruffini, R.; Bianco, C. L.; Muccino, M.; Penacchioni, A. V.; Rueda, J. A.; Wang, Y., 2013, A&A, 552, L5.
4) "On binary-driven hypernovae and their nested late X-ray emission", Ruffini, R.; Muccino, M.; Bianco, C. L.; Enderli, M.; Izzo, L.; Kovacevic, M.; Penacchioni, A. V.; Pisani, G. B.; Rueda, J. A.; Wang, Y., 2014, A&A , 565, L10.
5) "Induced gravitational collapse at extreme cosmological distances: the case of GRB 090423", Ruffini, R.; Izzo, L.; Muccino, M.; Pisani, G. B.; Rueda, J. A.; Wang, Y.; Barbarino, C.; Bianco, C. L.; Enderli, M.; Kovacevic, M., 2014, A&A, 569, A39.
6) "A search for Fermi bursts associated to supernovae and their frequency of occurrence", Kovacevic, M.; Izzo, L.; Wang, Y.; Muccino, M.; Della Valle, M.; Amati, L.; Barbarino, C.; Enderli, M.; Pisani, G. B.; Li, L., 2014, A&A, 569, A180.
7) "GRB 130427A and SN 2013cq: A Multi-wavelenght Analysis of an Induced Gravitational Collapse Event", Ruffini, R.; Wang, Y.; Kovacevic, M.; Bianco, C. L.; Enderli, M.; Muccino, M.; Penacchioni, A. V.; Pisani, G. B.; Rueda, J. A., 2015, ApJ, 798, 10.
8) "Induced Gravitational Collapse in the BATSE era: the case of GRB 970828", Ruffini, R.; Izzo, L.; Muccino, M.; Rueda, J. A.; Barbarino, C.; Bianco, C. L.; Dereli, H.; Enderli, M.; Penacchioni, A. V.; Pisani, G. B.; Wang, Y., in press, Astronomy Reports.

Jonas Pedro PEREIRA, "Processi elettrodinamici in Astrofisica generale di Stelle di neutroni e buchi neri", discussione: 1° dicembre 2014 presso l'Università di Roma "Sapienza"

In this thesis the investigation of some of the physical consequences associated with the presence of an electrodynamical structure in astrophysical objects is presented. First the thermodynamics of charged black holes within nonlinear Lagrangians to the electromagnetism, the ones that generalize the Maxwellian Lagrangian is scrutinized. The aforementioned formalism into their own description and interactions, elucidating several of their aspects, the ones to be confronted with observations in order to assess their existence is applied. The solution to general relativity minimally coupled with nonlinear electromagnetism in the slowly rotating case and made use of the physics of neutrinos to probe and characterize such spacetimes is also founded. Stability analyses were also formulated and scrutinized for thin-shells interacting with black holes, as well as for stratified stars with surface degrees of freedom, for investigating their subtleties and fingerprints, of fundamental importance for their observational searches.

In figure: When surface degrees of freedom (SDF) are present in a neutron star, for example in a thin layer splitting its core and crust, the stability of such a star changes due to the dynamics of the aforesaid SDF, when compared to a continuous system [see Phys. Rev. D 90, 123011 (2014) for details]. Here we show a numerical catalogue for the stability of thin shells present in globally neutral neutron stars where all the interactions are taken into account [Phys. Lett. A 883, 1 (2012) ]. In the abscissa is a range of densities at the base of the crusts (bcr) in neutron stars, normalized by the neutron drip density (drip), of the order of 10^11g/cc. The ordinate is the squared minimum velocity of the sound (min), related to adiabatic thin shells. For each given density at the base of the crust for each curve (related to a given central density in a neutron star, the number present on the curve in units of the nuclear density, 10^14g/cc), stable shells are those whose velocities of the sound are larger than its associated minimum speed of the sound and smaller than the unit (the velocities here are normalized by the speed of light in vacuum). Negative values of the ordinate for given densities at the base of the crust mean that any equation of state of the shells in the associated neutron stars lead to stable configurations. The density at the base of the crust must not exceed the nuclear density for the aforesaid model. Therefore, the thin shell stabilty only per se leads to a maximum mass of neutron stars within this model: 1.97 solar masses, associated with a density of 2.2 times the nuclear density, as given by the dashed brown curve. Finally, each physical neutron star should be a point in this plot, since it would have a definite equation of state for its shell, a central and at the base of the crust densities and then one could immediately assess whether or not it is stable against radial shell displacements.

The thesis is based on following publications:
1) "On the black hole mass decomposition in nonlinear electrodynamics", Jonas P. Pereira, Herman J. Mosquera-Cuesta, Jorge A. Rueda, and Remo Ruffini, Phys. Lett. B 734, 396 (2014).
2) "Stability of thin-shells interfaces inside compact stars", Jonas P. Pereira, Jaziel G. Coelho, and Jorge A. Rueda, Phys. Rev. D 90, 123011 (2014).
3) "Radial stability in stratified stars", Jonas P. Pereira and Jorge A. Rueda, Accepted for publication in Astrophys. J. (2015).
4) "Energy decomposition within Einstein-Born-Infeld black holes", Jonas P. Pereira and Jorge A. Rueda, submitted to Phys. Rev. D (2015).
5) "Matching arbitrary slowly rotating spacetimes and the issue of energy conditions", Jonas P. Pereira and Jorge A. Rueda, submitted to Phys. Lett. B (2015).
6) "Nonlinear electrodynamics in slowly rotating spacetimes and their probe through the physics of neutrinos", Jonas P. Pereira, Herman J. Mosquera-Cuesta, and Gaetano Lambiase, in preparation (2015).

Bruno SVERSUT ARSIOLI, "Dati multifrequenza da Active Galactic Nuclei", discussione: 1° dicembre 2014 presso l'Università di Roma "Sapienza"

There is growing interest from the Astrophysics community to identify and study γ-ray sources, especially the ones detected at E>100GeV in the so called Very High Energy (VHE) regime. Distant galaxies harboring an Active Nucleus (AGN) were recently detected as major extra-galactic sources of TeV photons, turning to be key component for a variety of studies like understanding AGN’s jet properties and composition, or probing emission mechanism probably in the vicinity of super massive black holes (SMBH). Even more remarkable are the multitude of questions currently being addressed by considering the interaction of VHE photons along its propagation through cosmological distances, such as unveiling the spectral shape of the Extragalactic Background Light (EBL), probing the existence of Intergalactic Magnetic Fields, or even addressing fundamental question related to Quantum Gravity and Stand Model physics. So far, the number of such VHE "Astrophysical laboratories" is not that big, reaching only 148 galactic/extragalactic TeV detected sources.
The present thesis took forward the idea of preparing a large catalog of High Synchrotron Peak blazars (HSP), which shows to be the most abundant population of extragalactic TeV emitters, with the main goal of revealing and characterize promising targets for TeV observatories. HSP blazars are remarkably rare, with only a few hundreds of them expected to be above the sensitivity limits of currently available surveys. To find these very uncommon objects, there was devised a method that combines multifrequency selection criteria based in unique features from HSP’s Spectral Energy Distribution. The so called 1WHSP sample was assembled including ≈1000 TeV candidates, unveiling many new γ-ray emitters in the energy range 300MeV-200GeV. In addition, by correlating the arrival direction of ultra high energy cosmic rays (UHECR) with the position of bright 1WHSP sources, it is shown that HSP blazars could well be part of the population emitting UHE particles. Such result is unique in the sense that it is based on direct source-event chance associations, and particularly interesting since it challenges what was previously expected for direct associations of this kind.

In figure: Centaurus A, the closest radio-loud AGN. Top left, optical image taken by the Wide Field Imager (WFI) ESO 2.2m; Top right, mid-infrared image taken by Spitzer satellite; Down left, the jet feature seen in X-rays as measured by Chandra satellite; Down right, the jet feature seen in Radio by the Very Large Array VLA.

Sversut Arsioli continua la sua carriera scientifica come assegnista presso ASI - Agenzia Spaziale Italiana, Italia.

Husne DERELI, "Studio di una popolazione di lampi di raggi gamma con afterglows a bassa luminosità", discussione: 16 dicembre 2014 presso l’Università di Nizza "Sophia Antipolis"

Gamma-ray bursts (GRB) are extreme events. They are crudely classified into two groups based on their duration, namely the short and long bursts. Such a classification has proven to be useful to determine their progenitors: the merger of two compact objects for short bursts and the explosion of a massive star for long bursts. Further classifying the long GRBs might give tighter constraints on their progenitor and on the emission mechanism(s).
In this thesis the evidence for the existence of a sub-class of long GRBs, based on their faint afterglow emission is presented. These bursts were named low-luminosity afterglow (LLA) GRBs. The data analysis and the selection method, and their main properties are described. Their link to supernova is strong as 64% of all the bursts firmly associated to SNe are LLA GRBs.
Finally, additional properties of LLA GRBs are presented: the study of their rate density, which seems to indicate a new distinct third class of events, the properties of their host galaxies, which show that they take place in young star-forming galaxies. Additionally, the difficulties to reconcile all differences between normal long GRBs and LLA GRBs only by considering instrumental or environmental effects are showed, a different ejecta content or a different geometry for the burst. Thus, the conclusion is that LLA GRBs and normal long GRBs should have different properties.
It is indicated that a binary system is favored in the case of LLA GRB. The argument is based on the initial mass function of massive stars, on the larger rate density of LLA GRBs compared to the rate of normal long GRBs and on the type of accompanying SNe.

In figure: The light-curves of all GRBs taken from X-ray afterglow observations were corrected for time dilation, K-correction and distance correction and they were rescaled at a common redshift z=1. Finally, all the bursts below a threshold of 10-13 erg s-1 cm-2 were selected at one day (Dereli et al. 2014) corresponding to 90% confidence level of group II Gendre et al. 2008. These bursts were named Low-Luminosity Afterglow (LLA) GRBs which are shown by blue diamonds while red dots show the remaining GRBs, which were used as a control sample in this study
Ref.: B. Gendre, A. Galli, and M. Boer ApJ, vol. 683, pp. 620-629, Aug. 2008
H. Dereli, M. Boer, B. Gendre, L. Amati, and S. Dichiara, “Properties of Low Luminosity Afterglow Gamma-ray Bursts,” Submitted to MNRAS, 2014.

Ricercatori in visita e nuovi studenti all’ICRANet

Due studentesse iraniane presso la sede centrale ICRANet

Due dottorande iraniane dell'Università Politecnica di Isfahan, Saghar Batebi e Seddigheh Tizchang, sostenute dal governo iraniano, sono arrivate all’ICRANet di Pescara per un periodo di ricerca di sei mesi. Durante questa visita conosceranno i campi di ricerca dell’ICRANet e approfondiranno la loro conoscenza dei Gamma Ray Bursts.

Nuovi studenti del programma di dottorato IRAP

	AIMURATOV Yerlan Kazakistan Studente di dottorato presso l’Università di Roma "Sapienza", e l’ICRANet, Pescara.
	CHANG Yu-Ling Taiwan Studente di dottorato presso l’ASI, Roma, e l’ICRANet, Pescara.
	KARLICA Mile Croazia Studente di dottorato presso l’Università di Roma "Sapienza", e l’ICRANet, Pescara.
	MORADI Rahim Iran studente di dottorato presso l’Università di Roma "Sapienza", e l’ICRANet, Pescara.

Ultime pubblicazioni e atti di convegno

Saggio selezionato per la Menzione d'onore 2014 della Gravity Research Foundation

"Sulla distribuzione del core-alone di materia oscura nelle galassie"
(Authors: Remo Ruffini, Carlos Raúl Argüelles, Jorge Armando Rueda) IJMPD 23 No. 12, 1442020; arXiv:astro-ph/1409.7365

Galaxies such as dwarf and spirals are known to be surrounded by huge spherical halos of dark matter, this is, halos which are composed of particles which only feel the gravitational force, but do not emit any kind of electromagnetic radiation. By the other hand, there is observational evidence which suggest that the center of the majority of these galaxies harbor massive black holes. The nature of these massive and compact dark central objects is still an open issue in astrophysics. Moreover, the actual understanding of these two dark galactic components are studied independently, and associated to completely different physical phenomena. In this work we address these issues from a more unified perspective, by proposing a theoretical model based on two physical pillars such as quantum statistics and general relativity.
We investigate the distribution of dark matter in galaxies by solving in the more general way the relativistic equations of equilibrium of a self-gravitating system of massive fermions at finite temperature. This model is contrasted phenomenologically with galactic observables ranging from dwarf to big spiral galaxies, evidencing that a fermion mass of about 10 keV, implies DM profiles in agreement with the observed and Universal constant DM halo surface density; as well as predicts dense central degenerate cores at sub-parsec scales, as alternative to IMBHs to SMBHs with masses Mc ∼ 10^4 to Mc ∼ 10^7 respectively.

"Sul campo magnetico della pulsar con configurazioni realistiche di stelle di neutroni"
(Authors: R. Belvedere, Jorge A. Rueda, and R. Ruffini), published on The Astrophysical Journal (ApJ), volume 799, page 23, January 20 (2015), arXiv:1411.2621

With densities in their interiors that overcome the density in the nucleus of an atom, neutron stars are the densest stars in the Universe. The most known observational evidence of the existence of neutron stars are the pulsars. In the intervening years from the seminal work of Oppenheimer & Volkoff (1939) on the equilibrium configurations of non-rotating neutron stars, based on the equation of state of a degenerate Fermion gas, more has been learned from the physical properties of neutron stars. A more complex knowledge of the nuclear equation of state, structure, and stability conditions of both static and rotating neutron stars has been acquired, leading to the necessity of exploring its implications on the observable properties of neutron stars. We have recently developed a neutron star model fulfilling global and not local charge neutrality, both in the static and in the uniformly rotating cases. The model is described by the coupled Einstein-Maxwell-Thomas-Fermi (EMTF) equations, in which all fundamental interactions are accounted for in the framework of general relativity and relativistic nuclear mean field theory. Uniform rotation was there introduced following the Hartle's formalism.
In this work we show that the use of realistic parameters of rotating neutron stars, obtained from numerical integration of the self-consistent axisymmetric general relativistic equations of equilibrium, leads to an estimate of the magnetic field and radiation efficiency of pulsars very different from estimates based on fiducial parameters of a neutron star, namely the assumption of a neutron star mass, M = 1.4 Msun, radius R = 10 km, and moment of inertia, I = 1045 g cm2. In addition, we compare and contrast the magnetic field inferred from the traditional Newtonian rotating magnetic dipole model with respect to the one obtained from its general relativistic analog which takes into due account the effect of the finite size of the source. We apply these considerations to the specific high-magnetic field pulsars class and show that, indeed, all these sources can be described as canonical pulsars driven by the rotational energy of the neutron star, and with magnetic fields lower than the quantum critical field for any value of the neutron star mass.

"Il processo non lineare Breit-Wheeler nella collisione di un fotone con un campo bifrequent"
(Authors:Y. B. Wu, S. S. Xue), Phys. Rev. D90, 013009 (2014)

Electron-positron pair creation by the collision of two real photons (Breit-Wheeler process [Breit and Wheeler, Phys. Rev. 46, 1087 (1934)]) is one of most relevant elementary processes in high-energy astrophysics. It can lead to observable effects such as cutoff in the high-energy Gamma spectra. In order to access the observations of this fundamental phenomenon in the earth-based experiments, the generalization of the Breit-Wheeler process to the nonlinear Breit-Wheeler process of pair production in the collision a photon with an intensive monochromatic plane wave has been fully analyzed and discussed in the past few decades [e.g., Reiss, J. Math. Phys. 3, 59 (1962) and Ritus, J. Sov. Laser Res. 6, 497 (1985)]. Such a nonlinear Breit-Wheeler process has been detected in the SLAC-E-144 experiment [Burke et al., Phys. Rev. Lett. 79, 1626 (1997)]. In the recent work [Yuan-Bin Wu and She-Sheng Xue, Phys. Rev. D 90, 013009 (2014)], we analyzed the nonlinear Breit-Wheeler process of pair production off a probe photon colliding with a bifrequent field.
The bifrequent field is composed of a low-frequency and a high-frequency electromagnetic wave that propagate in the same direction. We clearly showed the phenomenon of Breit-Wheeler pair production with simultaneous photon emission into the low-frequency wave and the high multiphoton (absorption and emission) phenomena: a large number of photons can be involved in this Breit-Wheeler pair production process. The results show a possible way to access the observations of these phenomena in the laser-based experiments.

Upper panel: normalized pair-production probability for the process with the given number of photon absorbed from (emitted into) the low-frequency wave and one photon absorbed from the high-frequency wave, the inset shows the case when the high-frequency wave is absent. Lower panel: spectra of created pairs.

I partecipanti ICRANet allo SWIFT Meeting

Durante il decimo Swift Meeting (presso l’Università "Sapienza" di Roma, 2-5 dicembre 2014) il prof. Ruffini ha presentato una relazione su "Il modello di collasso indotto gravitazionale rispetto al modello di collasso palla di fuoco" (la presentazione power point è visibile qui). Sette studenti ICRANet hanno inoltre presentato un poster:

A sinistra: Laura BECERRA, Accrescimento ipercritico, collasso gravitazionale indotto, e ipernovae A destra: Maxime ENDERLI, Progenitori binari dei GRB all'interno del modello fireshell - pertinenza dell'osservazione Swift
A sinistra: Milos KOVACEVIC, Lo scenario dell'interpretazione della crescita spike-like nelle Binary-Driven ipernovae A destra: Marco MUCCINO, GRB 140619b: un Grb corto da una stella di neutroni di fusione che porta alla formazione di un buco nero
A sinistra: Giovanni Battista PISANI, Binary-Driven ipernovae e loro tarde emissioni nascoste di raggi x A destra: Yu WANG, Analisi e previsione GRB 130427A / SN 2013cq
Elena ZANINONI, Dieci anni di Swift: una scala universale per GRB brevi e lunghi (Ex,iso-Eγ,iso-Epk)

Gli atti del convegno Zeldovich-100

E’ un piacere annunciare che gli atti delle sessioni parallele della conferenza internazionale in onore di Ya. B. Zeldovich nel suo 100° Anniversario sono ora pubblicati nel numero speciale della rivista internazionale Nonlinear Phenomena in Complex Systems Vol. 17, no. 4, pp. 340 – 470, 2014. www.j-npcs.org/abstracts/vol2014no4.html I lavori delle sessioni plenarie sono pubblicati in Astronomy Reports. I redattori delle edizioni speciali sono Sergei Kilin (Accademia Nazionale delle Scienze della Bielorussia), Remo Ruffini (ICRANet) e Gregory Vereshchagin (ICRANet).

Sviluppi recenti all'ICRANet di Rio de Janeiro

1) BSDC - 1WHSP: il più grande catalogo di TeV blazar

Un catalogo di 996 Blazar HSP, il tipo più estremo di Nuclei Galattici Attivi (AGN) noto, è stato assemblato come parte della tesi dottorale di Bruno Arsioli. La ricerca è stata effettuata presso la ASDC nell'ambito della collaborazione tra ICRANet e l'Agenzia Spaziale Italiana (ASI).
I Blazar HSP sono particolarmente interessanti in quanto accelerano le particelle a più alte energie osservate in sorgenti extragalattiche e irradiano fotoni fino a energie molto grandi di raggi gamma e nel dominio TeV.
Molte delle fonti nel catalogo possono essere rilevate con l'attuale generazione di telescopi Cherenkov e un gran numero di essi sarà rilevato in future osservazioni ed esplorazioni CTA.
Una versione interattiva del catalogo sarà presto disponibile on-line sul sito del Science Data Center brasiliano (BSDC) (www.bsdc.org) e dell’ASDC (www.asdc.asi.it) web sites.

2) BSDC - Una versione interattiva del più aggiornato catalogo di nane bianche disponibile on-line sul sito BSDC

Il più aggiornato catalogo di stelle nane bianche, sulla base di dati SDSS-DR10, è appena stato pubblicato da S.O. Kepler e collaboratori (2015, MNRAS, 446, 4078). Questo elenco è stato redatto con il contributo della ASDC dove un certo numero di fonti BL Lac, che mostrano spettri ottici simili ad alcuni tipi di nane bianche ma che mostrano anche emissioni radio, sono state identificate e rimosse sulla base di strumenti software ASDC.
La versione interattiva del catalogo, che dà accesso a tutti gli spettri ottici, dati IR e molto di più, è disponibile sui siti web BSDC e ASDC.

3) Articoli co-scritti da membri del gruppo ICRANet Rio

	Riccardo BELVEDERE - R. Belvedere, K. Boshkayev, Jorge A. Rueda, R. Ruffini; "Uniformly rotating neutron stars in the global and local charge neutrality cases"; Nuclear Physics A 921, 33 (2014). - R. Belvedere, Jorge A. Rueda, R. Ruffini; “On the Keplerian frequency and moment of inertia of neutron stars”; submitted to Phys. Rev. C. - R. Belvedere, Jorge A. Rueda, R. Ruffini; “On the magnetic field of pulsars with realistic neutron star configurations”; ApJ, 799, 23 (2015). - R. Belvedere, S. B. Duarte, Jorge A. Rueda, R. Ruffini; “Rapidly rotating neutron stars with extended hadronic nuclear models with delta‐mesons”; in preparation.
	Jorge RUEDA - J. P. Pereira and J. A. Rueda, “Radial stability in stratified stars”, ApJ, in press; arXiv:1501.02621, Jan. 2015. - R. Belvedere, J. A. Rueda, and R. Ruffini, "On the Magnetic Field of Pulsars with Realistic Neutron Star Configurations", ApJ, vol. 799, p. 23, Jan. 2015. - R. Ruffini, Y. Wang, M. Enderli, M. Muccino, M. Kovacevic, C. L. Bianco, A. V. Penacchioni, G. B. Pisani, and J. A. Rueda, "GRB 130427A and SN 2013cq: A Multi-wavelength Analysis of An Induced Gravitational Collapse Event", ApJ, vol. 798, p. 10, Jan. 2015. - F. G. Oliveira, J. A. Rueda, and R. Ruffini, "X, Gamma-Rays, and Gravitational Waves Emission in a Short Gamma-Ray Burst", Astrophysics and Space Science Proceedings, vol. 40, p. 43, 2015. - J. P. Pereira, J. G. Coelho, and J. A. Rueda, "Stability of thin-shell interfaces inside compact stars", Phys. Rev. D, vol. 90, p. 123011, Dec. 2014. - M. Muccino, R. Ruffini, M. Kovacevic, L. Izzo, F. G. Oliveira, J. A. Rueda, C. L. Bianco, M. Enderli, A. V. Penacchioni, G. B. Pisani, Y. Wang, and E. Zaninoni, "GRB 140619B: a short GRB from a binary neutron stars merger leading to the black hole formation", ArXiv e-prints, Dec. 2014. - S. M. de Carvalho, R. Negreiros, J. A. Rueda, and R. Ruffini, "Thermal evolution of neutron stars with global and local neutrality", Phys. Rev. C, vol. 90, p. 055804, Nov. 2014.
	Ivan SIUTSOU - Carlos R. Argüelles, Remo Ruffini, Ivan Siutsou, Bernardo Fraga; "On the distribution of dark matter in galaxies: quantum treatments"; J. Kor. Phys. Soc.; in press. - I. Siutsou, C. R. Argüelles, R. Ruffini; "Dark Matter Massive Fermions and Einasto Profiles in Galactic Haloes"; submitted to A&A. - U. Barres de Almeida, R. Ruffini, I. Siutsou; "Limits on Lorentz invariance violation from highly variable gamma‐ray data of GRBs and Blazars"; in preparation. - A. Aksenov, I. Siutsou, G. Vereshchagin; "Electron‐positron plasmathermalization in optically thick environment"; in preparation.
	Elena ZANINONI - M. Muccino, R. Ruffini, M. Kovacevic, L. Izzo, F. G. Oliveira, J. A. Rueda, C. L. Bianco, M. Enderli, A. V. Penacchioni, G. B. Pisani, Y. Wang, E. Zaninoni; "GRB 140619B: a short GRB from a binary neutron stars merger leading to the black hole formation"; ArXiv e-prints, Dec. 2014. - E. Zaninoni, M.G. Bernardini, R. Margutti, S. Oates, G. Chincarini; "Gamma‐ray burst optical lightcurve zoo: comparison with X‐ray observations"; A&A 557, A12 (2014). - R. Ruffini, G. B. Pisani, M. Muccino, J. A. Rueda, C. L. Bianco, M. Enderli, L. Izzo, M. Kovacevic, A.V. Penacchioni, Y. Wang, E. Zaninoni; "GRB 090510: the tightest observed binary‐driven hypernova"; submitted to ApJ.

Prossime Conferenze

MG14 - Apertura delle registrazioni

E’ con grande piacere che annunciamo l'apertura di registrazione on-line (http://www.icra.it/mg/mg14/registration.htm) per il 14° Meeting Marcel Grossmann, che si terrà a Roma presso l’Università "Sapienza" tra il 12 e il 18 luglio 2015.
La quota di iscrizione è 350 € sino al 25 maggio, dopo di che la quota sarà di € 400. La quota per gli studenti è 150 €, in qualsiasi momento (con la certificazione di "Student Status").
Il poster preliminare è: http://www.icra.it/mg/mg14/MG14_poster.pdf
Gli abstracts per le presentazioni delle sessioni parallele devono essere presentati entro il 1° Giugno 2015, ma di preferenza al momento della registrazione.
L'attuale elenco preliminare delle sessioni parallele e relativi chair sono disponibili all'indirizzo: http://www.icra.it/mg/mg14/par_sessions_chairs.htm
Un primo elenco di plenary speakers confermati è disponibile qui: http://www.icra.it/mg/mg14/invited_speakers.htm
Tutte le richieste possono essere indirizzate alla casella di posta del meeting: mg14@icra.it

Il 2° ICRANet César Lattes Meeting

L'incontro, dedicato al coordinamento delle attività scientifiche ICRANet in Brasile prima della riunione de MGXIV a Roma nel luglio 2015, celebrerà il 100° anniversario delle equazioni di Einstein. L'incontro scientifico si svolgerà alle UFF e al CBPF. Conferenze pubbliche saranno programmate al Museo di Arte Contemporanea (MAC), al Cassino da Urca, all’UFPE, all’ UFPB e all’IFCE.
L'incontro riguarderà le attività di osservazione dei raggi X, gamma e UHECR, il progresso teorico in astrofisica relativistica di stelle di neutroni, buchi neri, onde gravitazionali e Cosmologia, nonché lo sviluppo del Science Data Center brasiliano (BSDC): da sorgenti galattiche ed extragalattiche sarà possibile andare molto indietro nel tempo, sino alla comparsa delle prime strutture nel nostro Universo. Saranno rivisti lo stato e le prospettive per i progetti ICRANet, all'interno del dottorato IRAP, i post-doc associati, e la presenza di scienziati di alto livello all'interno di tutti i Centri ICRANet.
La registrazione è ora aperta all’indirizzo: http://www.icranet.org/2cl/registration.htm
Il sito web della conferenza è: http://www.icranet.org/2cl/
Un poster preliminare può essere scaricato all'indirizzo: http://www.icranet.org/2cl/img/poster.pdf

Il 4° Galileo - Xu GuangQi meeting

La "Conferenza Internazionale sulla Gravitazione e Cosmologia – il quarto meeting Galileo-Xu GuangQi" è stata creata per celebrare i forti legami scientifici tra Italia e Cina, sotto il segno di Galileo Galilei (1564-1642) e Xu GuangQi (1562-1633), amico e discepoli di padre Matteo Ricci Maria (1552-1610), che più di tutti ha contribuito a portare nuove scoperte scientifiche europee in Cina. L'incontro avrà luogo a Pechino, dal 4 all’8 Maggio, 2015. Le precedenti edizioni si sono tenute a Shanghai nel 2009, a Nizza / Ventimiglia nel 2010 e a Pechino nel 2011. Il convegno sarà caratterizzato dalla presenza di molti scienziati occidentali e delle principali istituzioni scientifiche e accademiche in Cina.