2014  -   2015  -   2016  -   2017

2018
March/April - August/September - Octobre/Novembre

2019

Fig. 1 - Photo de group du MG15 dans l’Aula Magna, Université Sapienza, Rome.

3. Visite du Professeur Ruffini en Albanie, 23 – 24 Mai 2018

Le 23 et 24 Mai 2018, le Professeur Ruffini, grâce à la collaboration de la Professeur Mimoza Hafizi, s’est rendu en Albanie afin de rencontrer Monsieur Mynyr Koni, Recteur de l’Université de Tirana : ce rencontre à été l’occasion pour eux de discuter la possibilité pour l’institut de devenir membre de plein droit du Doctorat international IRAP-PhD, avec tous les droits envisagés par son statut. La visite a suivi donnait suite à la proposition unanime de l’Université de Tirana en tant que membre potentiel du doctorat conjoint, pendant la réunion de la IRAP-PhD Faculty qui s’est tenue à Rome le 30 Avril 2018.

4. Le Professeur Ruffini est devenu membre du Horizon 2020 Advisory Group for the Marie Sklodowska-Curie actions on skills, training and career development (MSCA) programme – Bruxelles, 28 Juin 2018

Le Professeur Ruffini est officiellement devenu member de l’“Horizon 2020 Advisory Group for the Marie Sklodowska-Curie actions on skills, training and career development (MSCA) programme” pour la période 2018-2020 (3em mandat). La Commission Européenne a renouvelé la membership de ses groups consultatifs qui apportent une contribution de haut niveau fondamental pour informer, évaluer, enrichir et tenir à jour ses idées et réélections sur l’élaboration et le suivi du Horizon 2020 Work Programme. Le Professeur Ruffini a été sélectionné pour ses connaissances sectorielles, ses compétences et son expérience dans le champ de la science. Sa biographie a été aussi inséré dans le Who’s Who booklet du group.
Le MSCA soutien financièrement les chercheurs à tous les points de leur carrières, sans distinction de nationalité et discipline. Le financements peuvent être attribué à des chercheurs individuels, à des groups, à des programs d’échange pour le staff et pour les programmes de doctorat/PhD. En plus, le MSCA donne la possibilité aux scientifiques de gagner expérience internationale, intersectorielle et interdisciplinaire, ainsi que compléter leur parcours avec beaucoup de compétences, qui favoriseront leur employabilité et leur perspective de carrière. Pour informations supplémentaires sur le MSCA Advisory Group: http://ec.europa.eu/research/mariecurieactions/

5. Accord de Collaboration entre la Sun Yat-Sen University et ICRANet, 4 Juillet 2018

Le 4 Juillet 2018, l’ ICRANet a signé un accord de coopération avec la Sun Yat-Sen University de Guangzhou – Chine, qui demeurera valide pendant cinq années. Le document a été signé par Luo Jun, Président de l’Université, et par le Professeur Remo Ruffini, Directeur d’ICRANet, à l’occasion de la participation du professeur Luo en tant que orateur plénière du MG15 à Rome.

Des éminent Professeurs et chercheurs de l’Université Sun Yat-Sen (Chine) ont présenté leur institut et ont célébré la signature de l’accord de coopération avec ICRANet en organisant un intéressant événement, la “SYSU Connection reception” à L’université Sapienza de Rome.

Programme officiel de la cérémonie de clôture – ICRANet, 4 Mai 2018

7. Relation technique et scientifique du projet “Del Talento e della curiosità. Quando l’aquila e il passero volano insieme” (ICRA,ICRANET, Fondazione Marco Besso, ECIPA)

Entre les objectes qui ont bien contribué au développement des êtres humaines, le plus important a été la "Crab Nebula", choisi à symbole du projet. Découverte en 1054 comme une “étoile visitatrice”, elle est maintenant appelée “Crab Nebula” pour sa morphologie comme un crabe, qui a à l’intérieur une Pulsar NPO532, qui tourne dans une période de 33 millisecondes et qui a été identifié en 1968 comme une étoile à neutrons tournante.

En regardant la Figure 12, on peut voir:
I. L’inscription en chinois concernant la découverte de l’étoile visitatrice, registrée en Juillet 1054 par des astronomes chinois, coréens et japonais;
II. L’image de la Crab Nebula, prise par le Hubble Space Telescope en 2014 avec ses structures filamenteuses, qui s’étende encore aujourd’hui à une vitesse de 250 km / sec;
III. L’émission X-ray par la Crab pulsar et sa wind nebula, observées par le satellite CHANDRA.

Ca a été le fil rouge des expositions organisées par ICRA et ICRANet, dont les recherches les plus importantes menées dans les derniers 50 années, ont été concentrées sur la compréhension des étoile à neutrons, sur la découverte du premier trou noir (voir Image 13) et, plus récemment, sur la physique des Sursauts gamma. Ca a permis de rejoindre et d’éclairer les parties les plus loin et sombres de l’Univers, revenant à ses premiers stages et au Big Bang. L’énergie émise par un Sursaut gamma est équivalente à celle émise par un milliard de galaxies, chacune composé de 100 milliards d’étoiles, même si pour une durée d’environ des centaines de secondes.

Figure 12 – L’inscription chinoise concernant la découverte de « l’étoile visitatrice » (1054), la photo de la Crab Nebula prise par le Hubble Space Telescope, et l’émission X-ray de la Crab pulsar et sa wind nebula.	Figure 13 – Le Professeur Remo Ruffini en recevant le Cressy-Morrison Award (1972) par la New York Academy of Science, pour la découverte du premier trou noir dans la galaxie.

La compréhension de ces phénomènes a une longue histoire, dans laquelle les résultats les plus relevant ont été possible grâce à la coopération entre l’Est et l’Ouest, et à des révolutions conceptuelles fondamentales, introduites par 3 géants: Albert Einstein, Werner Heisenberg et Enrico Fermi. Tout ç a été possible grâce à la relation spéciale entra l’Italie et la Chine, au rôle crucial joué par l’Italie dan la formulation de la relativité générale et spéciale de Albert Einstein, à la collaboration de Michele Besso et Marcel Grossmann avec les mathématiciens italiens les plus importants (comme Ricci Curbastro et Tullio Levi Civita), et grâce aussi au rôle révolutionnaire de Fermi en Cosmologie, encore inconnu au grand public.
Pour voir le materiel relevant des 2 expositions "ICRANet and China" et "Einstein, Fermi and Heisenberg: the birth of Relativistic Astrophysics", voir: http://www.fondazionemarcobesso.it/3362/inaugurazione-mostre-einstein-fermi-e-heisenberg-e-la-nascita-della-astrofisica-relativistica-e-icranet-e-cina-2/

Pour lire la biographie "Marcel Grosmann. For the love of Mathematics”, voir: https://www.amazon.it/Marcel-Grossmann-Mathematics-Springer-Biographies-ebook/dp/B07DMD4VNH/ref=sr_1_1?ie=UTF8&qid=1532701370&sr=8-1&keywords=Marcel+Grossmann+For+the+Love+of+Mathematics (Anglais)
https://www.amazon.it/Marcel-Grossmann-Aus-Liebe-Mathematik/dp/3905894327/ref=sr_1_fkmr0_1?ie=UTF8&qid=1532701370&sr=8-1-fkmr0&keywords=Marcel+Grossmann+For+the+Love+of+Mathematics (Allemande)

Dans le cadre du projet, ont été aussi complétés les livres "Fermi e l'Astrofisica" (en cours d'impression à Singapore ) et "Einstein, Heisenberg and Fermi and the birth of Relativistic Astrophysics”.
Certains chapitres de ces livres ont été aussi présentés pendant les conférences tenues dans le cadre du projet par le Professeur Roy Patrick Kerr, Prix Crafoord pour l’Astronomie en 2016, décerné par le Roy de Suède (voir figure 14).



Pendant ces conférences, tenues auprès de la Fondation Besso à Rome, plusieurs éminents astrophysiques (voir figure 5, 16, 17, 18) comme Marco Tavani (https://youtu.be/E7t0TkuK6Bc), Massimo Della Valle (https://youtu.be/9rjA-5ZgkOE), Fulvio Ricci (https://youtu.be/BXUH2hxlZGU), Roy Kerr (https://youtu.be/9rjA-5ZgkOE), Paolo de Bernardis (https://youtu.be/dJGBH6cuaXA) et Paolo Giommi, ainsi que certains étudiants de doctorat ICRANet (voir Figures 19, 20, 21, 22), ont présenté leur travaux scientifiques, qui ont été au8ssi filmées afin de pouvoir être utiles pour les recherches futures.

Figure 15 – Le Professor Marco Tavani pendant sa conférence “Radiazioni di GeV osservate da AGILE”.	Figure 16 – Le Professeur Massimo Della Valle pendant sa conférence “L’arcobaleno e le stelle d’oro”.
Figure 17 – Le Professeur Fulvio Ricci pendant sa Lectio Magistralis “Gravitational Waves observations”.	Figure 18 – Le Professeur Paolo De Bernardis pendant sa Lectio Magistralis “La luce più antica dell’universo”.

Figures 19, 20, 21, 22 – De gauche à droite: les étudiants de doctorat ICRANet Daria Promorac, Rahim Moradi, Wang Yu e Yerlan Aimuratov, pendant leur présentations à la Fondation Besso.

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Du 17 au 30 Juin 2018, le Professeur Shadi Tahvildar-Zadeh (Rutgers, The State University of New Jersey – USA), a visité le centre ICRANet de Pescara, et a tenu plusieurs séminaires pour les faculty members et les étudiants. Les sujets abordés dans ses conferences étaient: Theories of matter: Weyl, Einstein and Mie, the classification of singularities, the Bianchi identities and equations of motion, the Born-In field non linear electrodynamics, the Bopp-Landé-Thomas-Podolsky linear electrodynamics, the zero-gravity space times and Ring-like particles, the general relativistic hydrogen, the ground state of positronium and dark matter, the photons as particles and the electron-photon systems.

* Séminaire de Sergio Andrés Vallejo Peña, 24 Juillet 2018

Le 24 Juillet 2018, Sergio Andrés Vallejo Peña, un étudiant invité de l’Universidad de Antioquia (UDEA) – Colombie, a tenu 2 séminaires sur “The effects of anisotropy and non-adiabaticity on the evolution of the curvature perturbation”(https://arxiv.org/abs/1804.05005) et "The MESS of cosmological perturbations" (https://arxiv.org/abs/1806.01941).


* Séminaire de Mikalai Prakapenia, 24 Juillet 2018

Le 24 Juillet 2018, Mikalai Prakapenia (Chercheur au centre ICRANet-Minsk et étudiant de doctorat à l’Université d’Etat bélarusse), a tenu un important séminaire intitulé “Thermalization of electron-positron plasma with quantum degeneracy”. He reported on the analysis of the non-equilibrium electron-positron-photon plasma thermalization process studied using relativistic Boltzmann solver, taking into account quantum corrections both in non-relativistic and relativistic cases. Collision integrals are computed from exact QED matrix elements for all binary and triple interactions in the plasma. It is shown that in non-relativistic case binary interaction rates dominate over triple ones, resulting in establishment of kinetic equilibrium prior to final relaxation towards thermal equilibrium, in agreement with previous studies. On the contrary, in relativistic case triple interaction rates are fast enough to prevent establishment of kinetic equilibrium. It is shown that thermalization process strongly depends on quantum degeneracy in initial state, but does not depend on plasma composition.

10. Visites scientifiques au centre ICRANet de Pescara

* Visite de Sonila Boçi au centre ICRANet, 30 Avril – 13 Mai 2018
Du 30 Avril au 13 Mai 2018, le Professeur Sonila Boçi de l’Université de Tirana – Albanie, a visité le centre ICRANet de Pescara. Pendant sa visite, elle a eu l’opportunité de discuter de ses travaux de recherché et d’avoir des intéressants échanges d’opinion avec les autres chercheurs ICRANet de toutes les parties du monde.

Pendant l’été, beaucoup d’autres scientifiques et étudiants ont visité le centre ICRANet de Pescara:
* Professeur Clovis Achy Soares Maia (University of Brasilia – Brazil), 7 - 14 Juillet 2018
* Les étudiants de Doctorat Sílvia Pereira Nunes, Ronaldo Vieira Lobato et Marcelo Montenegro Lapola (Instituto Tecnológico de Aeronáutica de São José dos Campos, SP – Brazil), 7 – 12 Juillet 2018
* Professeur Shadi Tahvildar-Zadeh (Rutgers, The State University of New Jersey – USA), 17 – 30 Juin 2018
* Soroush Shakeri (Isfahan University of Technology - Iran), 19 Juin – 17 Juillet 2018
* Professeur Mathews Grant (Center for Astrophysics at Notre Dame University – USA), 7 – 9 Juillet 2018
* Professeur Wenbin Lin (School of Physical Science and Technology, Southwest Jiaotong University – China), 8 – 14 Juillet 2018
* Professeur Hyung Won Lee (Inje University – South Korea), 16 Juillet – 15 August 2018
* Sergio Andrés Vallejo Peña (Universidad de Antioquia – Colombia), 1 Juillet – 9 Septembre 2018
* Mikalai Prakapenia (ICRANet-Minsk center and Belarusian State University – Belarus), 1 – 27 Juillet 2018

Prof. Sonila Boci

Prof. Clovis Achy Soares Maia

Prof. Shadi Tahvildar-Zadeh

Soroush Shakeri

Prof. Mathews Grant

Professor Hyung Won Lee

Mikalai Prakapenia

Pendant et/or avant leur visites, ces scientifiques ont eu aussi la possibilité de participer au 15th Marcel Grossmann meeting à Rome, et de mener des importantes recherches avec les autres scientifiques ICRANet de toutes les parties du monde.

Faisant suite à l’Accord entre ICRANet et l’Université Al-Farabi Kazakh National, 2 groups d’étudiants du Kazakhstan, sous la supervision du Professeur Medeu Abishev, ont visité le centre ICRANet de Pescara. Le premier groupe s’est rendu du 11 au 25 Juin 2018, et était composé par: Fariza Aitzhan, Makpal Akhmetzhanova, Albina Bazarova, Aizhan Duysenbaeva, Mamak Tangsholpan, Ernat Nurtazin, Balzhan Mamadkarimova and Tileuberdi Akhat.
Le deuxieme group, qui s’est rendu du 30 Juin au 11 Juillet, était composé par: Sadirkhanov Zhandos, Abdramanova Gulbanu, Assel Kuanysh, Anel Imangaliyeva, Symbat Nurakhmetova, Anapiya Meruyert, Zaltay Aklen, Gaukhar Askhanova, Niyazov Kaiyrzhan, Yesbol Meirambekuly, Botakoz Seifullina and Fatima Dankenova.

Fig. 24 -Les étudiants Kazakhs pendant leur visite au centre ICRANet de Pescara.

11. Publications récentes

S. Gasparyan, N. Sahakyan, V. Baghmanyan, D. Zargaryan, “On the multi-wavelength Emission from CTA 102”, accepted for publication on The Astrophysical Journal, on 8 July 2018.
We report on broadband observations of CTA 102 (z=1.037) during the active states in 2016-2017. In the γ-ray band, Fermi LAT observed several prominent flares which followed a harder-when-brighter behavior: the hardest photon index Γ=1.61±0.10 being unusual for FSRQs. The peak γ-ray flux above 100 MeV (3.55±0.55)×10⁻⁵ photon cm⁻²s⁻¹ observed on MJD 57738.47 within 4.31 minutes, corresponds to an isotropic γ-ray luminosity of L_γ=3.25×10⁵⁰ergs⁻¹, comparable with the highest values observed from blazars so far. The analyses of the Swift UVOT/XRT data show an increase in the UV/optical and X-ray bands which is contemporaneous with the bright γ-ray periods. The X-ray spectrum observed by Swift XRT and NuSTAR during the γ-ray flaring period is characterized by a hard photon index of ∼1.30. The shortest e-folding time was 4.08±1.44 hours, suggesting a very compact emission region R≤δ×2.16×10¹⁴ cm. We modeled the spectral energy distribution of CTA 102 in several periods (having different properties in UV/optical, X-ray and γ-ray bands) assuming a compact blob inside and outside the BLR. We found that the high-energy data are better described when the infrared thermal radiation of the dusty torus is considered. In the flaring periods when the correlation between the γ-ray and UV/optical/X-ray bands is lacking, the γ-ray emission can be produced from the interaction of fresh electrons in a different blob, which does not make a dominant contribution at lower energies.
Link: https://arxiv.org/abs/1807.02869v1


P. Padovani, P. Giommi, E. Resconi, T. Glauch, B. Arsioli, N. Sahakyan, M. Huber,“Dissecting the region around IceCube-170922A: the blazar TXS 0506+056 as the first cosmic neutrino source”, accepted for publication in MNRAS on 12 July 2018.
We present the dissection in space, time, and energy of the region around the IceCube-170922A neutrino alert. This study is motivated by: (1) the first association between a neutrino alert and a blazar in a flaring state, TXS 0506+056; (2) the evidence of a neutrino flaring activity during 2014 - 2015 from the same direction; (3) the lack of an accompanying simultaneous γ-ray enhancement from the same counterpart; (4) the contrasting flaring activity of a neighbouring bright γ-ray source, the blazar PKS 0502+049, during 2014 - 2015. Our study makes use of multi-wavelength archival data accessed through Open Universe tools and includes a new analysis of Fermi-LAT data. We find that PKS 0502+049 contaminates the γ-ray emission region at low energies but TXS 0506+056 dominates the sky above a few GeV. TXS 0506+056, which is a very strong (top percent) radio and γ-ray source, is in a high γ-ray state during the neutrino alert but in a low though hard γ-ray state in coincidence with the neutrino flare. Both states can be reconciled with the energy associated with the neutrino emission and, in particular during the low/hard state, there is evidence that TXS 0506+056 has undergone a hadronic flare with very important implications for blazar modelling. All multi-messenger diagnostics reported here support a single coherent picture in which TXS 0506+056, a very high energy γ-ray blazar, is the only counterpart of all the neutrino emissions in the region and therefore the most plausible first non-stellar neutrino and, hence, cosmic ray source.
Link: https://arxiv.org/abs/1807.04461


T. Hayashinaka, S. Xue, “Physical renormalization condition for de Sitter QED”, Published in Rapid communication section of Phys. Rev. D 97, 105010, on 13 February 2018.
We considered a new renormalization condition for the vacuum expectation values of the scalar and spinor currents induced by a homogeneous and constant electric field background in de Sitter spacetime. Following a semiclassical argument, the condition named maximal subtraction imposes the exponential suppression on the massive charged particle limit of the renormalized currents. The maximal subtraction changes the behaviors of the induced currents previously obtained by the conventional minimal subtraction scheme. The maximal subtraction is favored for a couple of physically decent predictions including the identical asymptotic behavior of the scalar and spinor currents, the removal of the infrared (IR) hyperconductivity from the scalar current, and the finite current for the massless fermion.
Link: https://journals.aps.org/prd/abstract/10.1103/PhysRevD.97.105010


C.R. Argüelles, A. Krut, J.A. Rueda, R. Ruffini, “Novel constraints on fermionic dark matter from galactic observables I: The Milky Way”, accepted for publication on Physics of the Dark Universe, Volume 21, on 12 July 2018.
We have recently introduced a new model for the distribution of dark matter (DM) in galaxies based on a self-gravitating system of massive fermions at finite temperatures, the Ruffini–Argüelles–Rueda (RAR) model. We show that this model, for fermion masses in the keV range, explains the DM halo of the Galaxy and predicts the existence of a denser quantum core at the center. We demonstrate here that the introduction of a cutoff in the fermion phase-space distribution, necessary to account for the finite Galaxy size, defines a new solution with a central core which represents an alternative to the black hole (BH) scenario for SgrA*. For a fermion mass in the range mc²=48-345 keV, the DM halo distribution is in agreement with the Milky Way rotation curve data, while harbors a dense quantum core of about 4x10⁶ solar masses within the S2-star pericenter.
Link: https://www.sciencedirect.com/science/article/pii/S2212686418300815


M.A. Prakapenia, I.A.Siutsou, G.V. Vereshchagin, “Numerical scheme for treatment of Uehling–Uhlenbeck equation for two-particle interactions in relativistic plasma, accepted for publication on the Journal of Computational Physics, on 4 July 2018.
We present a new efficient method to compute Uehling–Uhlenbeck collision integral for all two-particle interactions in relativistic plasma with drastic improvement in computation time with respect to existing methods. Plasma is assumed isotropic in momentum space. The set of reactions consists of: Moeller and Bhabha scattering, Compton scattering, two-photon pair annihilation, and two-photon pair production, which are described by QED matrix elements. In our method exact energy and particle number conservation laws are fulfilled. Reaction rates are compared, where possible, with the corresponding analytical expressions and convergence of numerical rates is demonstrated.
Link: https://www.sciencedirect.com/science/article/pii/S0021999118304650?via%3Dihub


B. Arsioli, U. Barres de Almeida, E. Prandini, B. Fraga, L. Foffano, “Extreme & High Synchrotron Peaked Blazars at the limit of Fermi-LAT detectability: the γ-ray spectrum of 1BIGB sources”, published on Monthly Notices of the Royal Astronomical Society, sty1975, on 24 July 2018.
We present the 1-100 GeV spectral energy distribution for a population of 148 high-synchrotron-peaked blazars (HSPs) recently detected with Fermi-LAT as part of the First Brazil-ICRANet Gamma-ray Blazar catalogue (1BIGB). Most of the 1BIGB sources have their γ-ray spectral properties presented here for the first time, representing a significant new extension of the γ-ray blazar population. Since our sample was originally selected from an excess signal in the 0.3 - 500 GeV band, the sources stand out as promising TeV blazar candidates, potentially in reach of the forthcoming very-high-energy (VHE) γ-ray observatory, CTA. The flux estimates presented here are derived considering PASS8 data, integrating over more than 9 years of Fermi-LAT observations. We also review the full broadband fit between 0.3-500 GeV presented in the original 1BIGB paper for all sources, updating the power-law parameters with currently available Fermi-LAT dataset. The importance of these sources in the context of VHE population studies with both current instruments and the future CTA is evaluated. To do so, we select a subsample of 1BIGB sources and extrapolate their γ-ray SEDs to the highest energies, properly accounting for absorption due to the extragalactic background light. We compare those extrapolations to the published CTA sensitivity curves and estimate their detectability by CTA. Two notable sources from our sample, namely 1BIGB J224910.6-130002 and 1BIGB J194356.2+211821, are discussed in greater detail. All γ-ray SEDs, are made publicly available via the Brazilian Science Data Center (BSDC) service, maintained at CBPF, in Rio de Janeiro.
Link: https://academic.oup.com/mnras/advance-article-abstract/doi/10.1093/mnras/sty1975/5057880


R. Ruffini, J. Rodriguez, M. Muccino, J. A. Rueda, Y. Aimuratov, U. Barres de Almeida, L. Becerra, C. L. Bianco, C. Cherubini, S. Filippi, D. Gizzi, M. Kovacevic, R. Moradi, F. G. Oliveira, G. B. Pisani, and Y. Wang, “On the Rate and on the Gravitational Wave Emission of Short and Long GRBs” published on The Astrophysical Journal, Volume 859, Number 1 on 18 May 2018.
On the ground of the large number of gamma-ray bursts (GRBs) detected with cosmological redshift, we classified GRBs in seven subclasses, all with binary progenitors which emit gravitational waves (GWs). Each binary is composed of combinations of carbon–oxygen cores (COcore), neutron stars (NSs), black holes (BHs), and white dwarfs (WDs). The long bursts, traditionally assumed to originate from a BH with an ultrarelativistic jetted emission, not emitting GWs, have been subclassified as (I) X-ray flashes (XRFs), (II) binary-driven hypernovae (BdHNe), and (III) BH–supernovae (BH–SNe). They are framed within the induced gravitational collapse paradigm with a progenitor COcore–NS/BH binary. The SN explosion of the COcore triggers an accretion process onto the NS/BH. If the accretion does not lead the NS to its critical mass, an XRF occurs, while when the BH is present or formed by accretion, a BdHN occurs. When the binaries are not disrupted, XRFs lead to NS–NS and BdHNe lead to NS–BH. The short bursts, originating in NS–NS, are subclassified as (IV) short gamma-ray flashes (S-GRFs) and (V) short GRBs (S-GRBs), the latter when a BH is formed. There are (VI) ultrashort GRBs (U-GRBs) and (VII) gamma-ray flashes (GRFs) formed in NS–BH and NS–WD, respectively. We use the occurrence rate and GW emission of these subclasses to assess their detectability by Advanced LIGO-Virgo, eLISA, and resonant bars. We discuss the consequences of our results in view of the announcement of the LIGO/Virgo Collaboration of the source GW 170817 as being originated by an NS–NS.
Link: http://iopscience.iop.org/article/10.3847/1538-4357/aabee4/meta


D. Bini, T. Damour, A. Geralico, “Spin-orbit precession along eccentric orbits: Improving the knowledge of self-force corrections and of their effective-one-body counterparts”, published on Phys. Rev. D 97, 104046 (2018) on 25 May 2018.
The (first-order) gravitational self-force correction to the spin-orbit precession of a spinning compact body along a slightly eccentric orbit around a Schwarzschild black hole is computed through the ninth post-Newtonian order, improving recent results by Kavanagh et al. [Phys. Rev. D 96, 064012 (2017).] This information is then converted into its corresponding Effective-One-Body counterpart, thereby determining several new post-Newtonian terms in the gyrogravitomagnetic ratio gS∗.
Link: https://journals.aps.org/prd/abstract/10.1103/PhysRevD.97.104046


D. Bini, T. Damour, A. Geralico, C. Kavanagh, “Detweiler’s redshift invariant for spinning particles along circular orbits on a Schwarzschild background”, published on Phys. Rev. D 97, 104022 (2018) on 18 May 2018.
We study the metric perturbations induced by a classical spinning particle moving along a circular orbit on a Schwarzschild background, limiting the analysis to effects which are first order in spin. The particle is assumed to move on the equatorial plane and has its spin aligned with the z-axis. The metric perturbations are obtained by using two different approaches, i.e., by working in two different gauges: the Regge-Wheeler gauge (using the Regge-Wheeler-Zerilli formalism) and a radiation gauge (using the Teukolsky formalism). We then compute the linear-in-spin contribution to the first-order self-force contribution to Detweiler's redshift invariant up to the 8.5 post-Newtonian order. We check that our result is the same in both gauges, as appropriate for a gauge-invariant quantity, and agrees with the currently known 3.5 post-Newtonian results.
Link: https://journals.aps.org/prd/abstract/10.1103/PhysRevD.97.104022