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ICRANet Newsletter
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Ottobre/Novembre 2022
SOMMARIO
1. 4 GCN ICRANet
2. Secondo annuncio del 5° Zeldovich meeting, 12 - 17 Giugno 2023, Yerevan (Armenia)
3. Missione del Prof. Ruffini negli USA, 6-11 Novembre 2022: conferenze al Cosmos Club, all'Institute for Advanced Studies (IAS) ed alla Princeton University
4. Il Prof. Ruffini è tra il 2% degli autori più citati, secondo Elsevier
5. Congratulazioni al Prof. Narek Sahakyan, Direttore del centro ICRANet Armenia e Professore della Faculty ICRANet, che ha conseguito il dottorato di ricerca (DSc) in fisica, 22 Novembre 2022
6. Eclissi solare parziale e misura del diametro solare (25 Ottobre 2022) ed eclissi lunare agli antipodi (8 Novembre 2022), eventi online e podcast
7. Rinnovo dell'accordo di cooperazione tra l'ICRANet e l'Università Campus Bio-Medico di Roma (Italia), 11 Ottobre 2022
8. Seminari presso il centro ICRANet a Pescara, 25 Novembre 2022
9. Visite scientifiche presso l'ICRANet
10. Pubblicazioni recenti
1. 4 GCN ICRANet
2. Secondo annuncio del 5° Zeldovich meeting, 12 - 17 Giugno 2023, Yerevan (Armenia)
3. Missione del Prof. Ruffini negli USA, 6-11 Novembre 2022: conferenze al Cosmos Club, all'Institute for Advanced Studies (IAS) ed alla Princeton University
4. Il Prof. Ruffini è tra il 2% degli autori più citati, secondo Elsevier
5. Congratulazioni al Prof. Narek Sahakyan, Direttore del centro ICRANet Armenia e Professore della Faculty ICRANet, che ha conseguito il dottorato di ricerca (DSc) in fisica, 22 Novembre 2022
6. Eclissi solare parziale e misura del diametro solare (25 Ottobre 2022) ed eclissi lunare agli antipodi (8 Novembre 2022), eventi online e podcast
7. Rinnovo dell'accordo di cooperazione tra l'ICRANet e l'Università Campus Bio-Medico di Roma (Italia), 11 Ottobre 2022
8. Seminari presso il centro ICRANet a Pescara, 25 Novembre 2022
9. Visite scientifiche presso l'ICRANet
10. Pubblicazioni recenti
1. 4 GCN ICRANet
TITLE: GCN CIRCULAR
NUMBER: 32780
SUBJECT: GRB 221009A: A type I BdHN of exceptional energetics
DATE: 22/10/17 11:16:22 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
GRB221009A detected by Swift (Kennea et al. 2022 GCN32635), Fermi-GBM(Veres et al. 2022, GCN32636, Lesage et al. 2022, GCN32642), Fermi-LAT(Bissaldi et al. 2022, GCN32637), with redshift of z=0.151 and an isotropic equivalent energy of Eiso=2x1054 erg (de Ugarte Postigo et al. 2022,GCN32648 and GCN32642) is a typical Binary driven Hypernova of type I (BdHNI), originating from the collapse of a carbon-oxygen core (CO-core) in presence of a companion neutron star (NS) with common feature with three BdHN I: GRB130427A with "pile up" in the prompt phase (Ruffini et al. 2013,GCN14526); GRB190114C (Ruffini et al. 2019, GCN23715); and GRB180720B(Ruffini et al. 2018, GCN23019). As the above three sources, GRB221009Apresents: 1) the optical (Lipunov et al. 2022, GCN32634 and GCN32639;Perley. 2022 GCN32638; Broens. 2022, GCN32640; Hu et al. 2022, GCN32644;Mondy: Belkin et al. 2022, GCN32645; de Wet et al.2022, GCN32646; Xu et al.2022 GCN32647; Odeh 2022, GCN32649; Brivio et al. 2022, GCN32652; Izzo et al. 2022, GCN32765), radio (Bright et al. 2022, GCN32653 and Farah et al.2022, GCN32655) and X-ray (Kennea et al, 2022, GCN32635, and GCN32651)synchrotron afterglow emissions as well as the TeV emission (Yong Huang et al. 2022, GCN32677), which in BdHN I originate from accreting millisecond spinning newborn NS (Rueda et al. 2022, e-Print: 2204.00579 [astro-ph.HE]);2) the ultra-relativistic prompt emission (UPE) phase (Moradi et al. 2021,PRD 104, 063043 and Rastegarnia et al. 2022, EPJC 82, 778) and GeV emission(Rueda et al 2022 ApJ 929 56) originated from the black hole formed by hypercritical accretion of the supernova ejecta on the NS companion; and 3) the optical emission of the nickel decay of the supernova (SN), created bythe collapse of the CO-core. The first evidence of the supernova rise is reported by S. Belkin et al. 2022, (GCN32769). In this GRB the bolometric optical peak of SN is expected to be observed at 15.57+/-2.0 days after the Fermi-GBM trigger (October 24th 2022, uncertainty from October 22nd 2022 to October 26th 2022, with the bolometric optical luminosity of L=(9.45+/-2.8) x1042 erg/s; Aimuratov et al. in preparation).
*******************************
TITLE: GCN CIRCULAR
NUMBER: 32802
SUBJECT: GRB 221009A X-ray light-curve and the indication of TeV light-curve
DATE: 22/10/19 15:28:45 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M. Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
LHAASO observed more than 5000 very high energy (VHE) photons in GRB 221009A, with the highest energy reaching 18 TeV (GCN 32677). Previously, high energy TeV emissions were also observed in GRB 180720B (Abdalla et al. 2019), 190114C (MAGIC Collaboration 2019), 190829A (H.E.S.S. Collaboration 2021) and 201216C (Blanch et al. GCN 29075). A common feature of these bursts is that the TeV light-curve follows a power-law decay with a similar index as the X-ray light-curve, and the TeV luminosity is tens of percent of the X-ray luminosity (see attached figure 1 and the references of Abdalla et al. 2019, MAGIC Collaboration 2019 and H.E.S.S. Collaboration 2021, Ruffini et al. 2021, Rueda et al. 2022, Rastegarnia et al. 2022, Wang et al. 2022). Here we present the X-ray light-curve of GRB 221009A observed by Swift-XRT (GCN 32651), and the t0 is taken from the Fermi-GBM trigger time (GCN 32636), see attached figure 2, a power-law of index -1.58 is fitted. The shadow region shows 20%-60% of the X-ray luminosity, which is expected to be the 0.3-1 TeV luminosity (17% less luminous for 0.5-18 TeV assuming a power-law spectrum of photon index -2) of this new burst if it shares the same behavior as the previous ones. We encourage further observations, especially the VHE observations, because this burst probably is more luminous than the previous ones, and it will be precious to have a late time (after days) VHE luminosity which was never achieved before, as well as the optical observations for the supernova appearance (GCN 32670, GCN 32780).
*******************************
TITLE: GCN CIRCULAR
NUMBER: 32808
SUBJECT: GRB 221009A: Peak luminosity of the supernova vs. synchrotron afterglow
DATE: 22/10/20 14:57:47 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M. Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
GRB 221009A appears to be a rare example (Jean-Luc Atteia et al. 2022, GCN 32793) of a particularly energetic and close GRB (de Ugarte Postigo et al. 2022, GCN 32648 and Lesage et al. 2022, GCN 32642 and N.P.M. Kuin et al. 2022, GCN 32656). Within the BdHN model, we have followed the X-ray, optical, and radio afterglows originating from synchrotron emission powered by fast spinning newborn neutron stars (vNS) with initial periods of fraction of a millisecond, accreting the supernova ejecta, created by the collapse of a carbon-oxygen core (Rueda et al. 2022, arXiv:2204.00579). Figures 1, 2 and 3 show the afterglows of three type I BdHNe, namely GRB 180720B (Ruffini et al. 2018, GCN 23019), GRB 190114C (Ruffini et al. 2019, GCN 23715), and GRB 211023A (Aimuratov et al. 2021, GCN 31056), and the prediction of their associated supernova. We have indicated the expected time of the occurrence of the supernova in GRB 221009A (Aimuratov et al. 2022, GCN 32780). The ongoing observations in optical, radio, and X-ray bands are strongly recommended for allowing the determination of the spin and magnetic field of the vNS. This will probe as well if the optical synchrotron emission, at ~ 106 s from the Fermi-GBM trigger, impedes the observations of the optical emission of the supernova originating from nickel decay (Aimuratov et al. in preparation, see also data from Ilfan Bikmaev et al. 2022, GCN 32752, and Jia. Ren et al. 2022, arXiv:2210.10673, reproduced in Fig. 4).
*******************************
TITLE: GCN CIRCULAR
NUMBER: 32828
SUBJECT: GRB 221009A: Determination of the black holes mass and spin
DATE: 22/10/24 15:43:08 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M. Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
In GRB 221009A, as in GRB 130427A (Ackermann et al. 2014, Science, 343, 42; and Ruffini et al. 2019, ApJ, 886, 82), the Fermi-GBM data in the prompt phase are piled up (Lesage et al. 2022, GCN 32642). In both cases there are missing the ultra-relativistic prompt emission (UPE) phases originating from quantum electro dynamical process around a Kerr BH (Ruffini et al. 2019, ApJ, 886, 82; and Rueda et al. 2022, ApJ, 929, 56), which were well observed in GRB 190114C (Moradi et al. 2021, Phys Rev D 104, 063043) and GRB 180720B (Rastegarnia et al. 2022, EPJC 82, 77). Under these conditions, for GRB 130427A the 0.1-100 GeV data of Fermi-LAT had allowed to determine only the lower limit on the BH mass, M>2.31 solar masses, and the upper limit of its spin parameter, α<0.4 (Ruffini et al. 2019, ApJ, 886, 82). For the BDHNI GRB 190114C (Ruffini et al. 2019, GCN 23715), the values of the BH mass and spin had been determined by taking into account the UPE contribution: M=4.53 solar masses, α=0.54 (Moradi et al. 2021, Phys Rev D 104, 063043). The analysis of GRB 130427A applied to GRB 221009A gives for the BH mass and spin parameters: M>2.36 solar masses and α<0.5. We identify the spike at 500s as the X-ray flare (see e.g. Ruffini et al. 2021 MNRAS 504, 5301-5326 for similar GRBs). We also identify the trigger in the 10 keV-10 MeV data of Fermi-GBM as the dawn of the supernova (SN-rise), associated with the gravitational collapse of the progenitor CO-core. The SN ejecta, accreting on the binary NS companion, give origin to the BH (BH rise, Rueda & Ruffini 2012, ApJ L, 758, L7) and accreting on the vNS they originate the afterglow (vNS rise, Ruffini et al. 2018, ApJ, 869.101; Becerra, et al. 2022, Phys Rev D 106, 083002). Additional data analysis from AGILE (GCN 32650), Fermi (GCN 32636, 32637, 32642, 32819), Swift (GCN 32635), LHAASO (GCN 32677), HXMT (Atel 15660) are needed to relate the SN-rise to the first appearance of the vNS (the vNS-rise) by the TeV radiation (GCN 32780, 32820, 32808), and also to relate the appearance of the BH (BH-rise) to the identification of the first GeV emission.
NUMBER: 32780
SUBJECT: GRB 221009A: A type I BdHN of exceptional energetics
DATE: 22/10/17 11:16:22 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
GRB221009A detected by Swift (Kennea et al. 2022 GCN32635), Fermi-GBM(Veres et al. 2022, GCN32636, Lesage et al. 2022, GCN32642), Fermi-LAT(Bissaldi et al. 2022, GCN32637), with redshift of z=0.151 and an isotropic equivalent energy of Eiso=2x1054 erg (de Ugarte Postigo et al. 2022,GCN32648 and GCN32642) is a typical Binary driven Hypernova of type I (BdHNI), originating from the collapse of a carbon-oxygen core (CO-core) in presence of a companion neutron star (NS) with common feature with three BdHN I: GRB130427A with "pile up" in the prompt phase (Ruffini et al. 2013,GCN14526); GRB190114C (Ruffini et al. 2019, GCN23715); and GRB180720B(Ruffini et al. 2018, GCN23019). As the above three sources, GRB221009Apresents: 1) the optical (Lipunov et al. 2022, GCN32634 and GCN32639;Perley. 2022 GCN32638; Broens. 2022, GCN32640; Hu et al. 2022, GCN32644;Mondy: Belkin et al. 2022, GCN32645; de Wet et al.2022, GCN32646; Xu et al.2022 GCN32647; Odeh 2022, GCN32649; Brivio et al. 2022, GCN32652; Izzo et al. 2022, GCN32765), radio (Bright et al. 2022, GCN32653 and Farah et al.2022, GCN32655) and X-ray (Kennea et al, 2022, GCN32635, and GCN32651)synchrotron afterglow emissions as well as the TeV emission (Yong Huang et al. 2022, GCN32677), which in BdHN I originate from accreting millisecond spinning newborn NS (Rueda et al. 2022, e-Print: 2204.00579 [astro-ph.HE]);2) the ultra-relativistic prompt emission (UPE) phase (Moradi et al. 2021,PRD 104, 063043 and Rastegarnia et al. 2022, EPJC 82, 778) and GeV emission(Rueda et al 2022 ApJ 929 56) originated from the black hole formed by hypercritical accretion of the supernova ejecta on the NS companion; and 3) the optical emission of the nickel decay of the supernova (SN), created bythe collapse of the CO-core. The first evidence of the supernova rise is reported by S. Belkin et al. 2022, (GCN32769). In this GRB the bolometric optical peak of SN is expected to be observed at 15.57+/-2.0 days after the Fermi-GBM trigger (October 24th 2022, uncertainty from October 22nd 2022 to October 26th 2022, with the bolometric optical luminosity of L=(9.45+/-2.8) x1042 erg/s; Aimuratov et al. in preparation).
*******************************
TITLE: GCN CIRCULAR
NUMBER: 32802
SUBJECT: GRB 221009A X-ray light-curve and the indication of TeV light-curve
DATE: 22/10/19 15:28:45 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M. Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
LHAASO observed more than 5000 very high energy (VHE) photons in GRB 221009A, with the highest energy reaching 18 TeV (GCN 32677). Previously, high energy TeV emissions were also observed in GRB 180720B (Abdalla et al. 2019), 190114C (MAGIC Collaboration 2019), 190829A (H.E.S.S. Collaboration 2021) and 201216C (Blanch et al. GCN 29075). A common feature of these bursts is that the TeV light-curve follows a power-law decay with a similar index as the X-ray light-curve, and the TeV luminosity is tens of percent of the X-ray luminosity (see attached figure 1 and the references of Abdalla et al. 2019, MAGIC Collaboration 2019 and H.E.S.S. Collaboration 2021, Ruffini et al. 2021, Rueda et al. 2022, Rastegarnia et al. 2022, Wang et al. 2022). Here we present the X-ray light-curve of GRB 221009A observed by Swift-XRT (GCN 32651), and the t0 is taken from the Fermi-GBM trigger time (GCN 32636), see attached figure 2, a power-law of index -1.58 is fitted. The shadow region shows 20%-60% of the X-ray luminosity, which is expected to be the 0.3-1 TeV luminosity (17% less luminous for 0.5-18 TeV assuming a power-law spectrum of photon index -2) of this new burst if it shares the same behavior as the previous ones. We encourage further observations, especially the VHE observations, because this burst probably is more luminous than the previous ones, and it will be precious to have a late time (after days) VHE luminosity which was never achieved before, as well as the optical observations for the supernova appearance (GCN 32670, GCN 32780).
 |
 |
| Figure 1:http://www.icranet.org/docs/fig1.png | Figure 2:http://www.icranet.org/docs/fig2.png |
*******************************
TITLE: GCN CIRCULAR
NUMBER: 32808
SUBJECT: GRB 221009A: Peak luminosity of the supernova vs. synchrotron afterglow
DATE: 22/10/20 14:57:47 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M. Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
GRB 221009A appears to be a rare example (Jean-Luc Atteia et al. 2022, GCN 32793) of a particularly energetic and close GRB (de Ugarte Postigo et al. 2022, GCN 32648 and Lesage et al. 2022, GCN 32642 and N.P.M. Kuin et al. 2022, GCN 32656). Within the BdHN model, we have followed the X-ray, optical, and radio afterglows originating from synchrotron emission powered by fast spinning newborn neutron stars (vNS) with initial periods of fraction of a millisecond, accreting the supernova ejecta, created by the collapse of a carbon-oxygen core (Rueda et al. 2022, arXiv:2204.00579). Figures 1, 2 and 3 show the afterglows of three type I BdHNe, namely GRB 180720B (Ruffini et al. 2018, GCN 23019), GRB 190114C (Ruffini et al. 2019, GCN 23715), and GRB 211023A (Aimuratov et al. 2021, GCN 31056), and the prediction of their associated supernova. We have indicated the expected time of the occurrence of the supernova in GRB 221009A (Aimuratov et al. 2022, GCN 32780). The ongoing observations in optical, radio, and X-ray bands are strongly recommended for allowing the determination of the spin and magnetic field of the vNS. This will probe as well if the optical synchrotron emission, at ~ 106 s from the Fermi-GBM trigger, impedes the observations of the optical emission of the supernova originating from nickel decay (Aimuratov et al. in preparation, see also data from Ilfan Bikmaev et al. 2022, GCN 32752, and Jia. Ren et al. 2022, arXiv:2210.10673, reproduced in Fig. 4).
 |
 |
| Fig1:http://www.icranet.org/docs/Fig1.pdf | Fig2:http://www.icranet.org/docs/Fig2.pdf |
 |
 |
| Fig3:http://www.icranet.org/docs/Fig3.pdf | Fig4:http://www.icranet.org/docs/Fig4.pdf |
*******************************
TITLE: GCN CIRCULAR
NUMBER: 32828
SUBJECT: GRB 221009A: Determination of the black holes mass and spin
DATE: 22/10/24 15:43:08 GMT
FROM: Remo Ruffini at ICRA ruffini@icra.it
Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M. Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:
In GRB 221009A, as in GRB 130427A (Ackermann et al. 2014, Science, 343, 42; and Ruffini et al. 2019, ApJ, 886, 82), the Fermi-GBM data in the prompt phase are piled up (Lesage et al. 2022, GCN 32642). In both cases there are missing the ultra-relativistic prompt emission (UPE) phases originating from quantum electro dynamical process around a Kerr BH (Ruffini et al. 2019, ApJ, 886, 82; and Rueda et al. 2022, ApJ, 929, 56), which were well observed in GRB 190114C (Moradi et al. 2021, Phys Rev D 104, 063043) and GRB 180720B (Rastegarnia et al. 2022, EPJC 82, 77). Under these conditions, for GRB 130427A the 0.1-100 GeV data of Fermi-LAT had allowed to determine only the lower limit on the BH mass, M>2.31 solar masses, and the upper limit of its spin parameter, α<0.4 (Ruffini et al. 2019, ApJ, 886, 82). For the BDHNI GRB 190114C (Ruffini et al. 2019, GCN 23715), the values of the BH mass and spin had been determined by taking into account the UPE contribution: M=4.53 solar masses, α=0.54 (Moradi et al. 2021, Phys Rev D 104, 063043). The analysis of GRB 130427A applied to GRB 221009A gives for the BH mass and spin parameters: M>2.36 solar masses and α<0.5. We identify the spike at 500s as the X-ray flare (see e.g. Ruffini et al. 2021 MNRAS 504, 5301-5326 for similar GRBs). We also identify the trigger in the 10 keV-10 MeV data of Fermi-GBM as the dawn of the supernova (SN-rise), associated with the gravitational collapse of the progenitor CO-core. The SN ejecta, accreting on the binary NS companion, give origin to the BH (BH rise, Rueda & Ruffini 2012, ApJ L, 758, L7) and accreting on the vNS they originate the afterglow (vNS rise, Ruffini et al. 2018, ApJ, 869.101; Becerra, et al. 2022, Phys Rev D 106, 083002). Additional data analysis from AGILE (GCN 32650), Fermi (GCN 32636, 32637, 32642, 32819), Swift (GCN 32635), LHAASO (GCN 32677), HXMT (Atel 15660) are needed to relate the SN-rise to the first appearance of the vNS (the vNS-rise) by the TeV radiation (GCN 32780, 32820, 32808), and also to relate the appearance of the BH (BH-rise) to the identification of the first GeV emission.
2. Secondo annuncio del 5° Zeldovich meeting, 12 - 17 Giugno 2023, Yerevan (Armenia)
Siamo lieti di informarvi che la sottomissione degli abstract per il 5° Zeldovich meeting è aperta.
La lista degli invited speakers comprende:
• Gennady Bisnovatyi-Kogan, Space Research Institute (IKI), Russia
• Massimo Della Valle, Osservatorio Astronomico di Capodimonte e INAF, Italia (TBC)
• Marat Gilfanov, Max-Planck Institute for Astrophysics, Germania e IKI, Russia (TBC)
• Paolo Giommi, Italian Space Agency (ASI), Italia
• Luca Izzo, Niels Bohr Institute, Danimarca (TBC)
• Michael Kramer, Max-Planck-Institut fuer Radioastronomie, Germania (TBC)
• Jutta Kunz, Università di Oldenburg, Germania (TBC)
• Klaus Laemmerzahl, Università di Brema, Germania
• Di Li, National Astronomical Observatories of China, Cina
• Ruoyu Liu, Nanjing University, Cina
• Andrea Merloni, Max Planck Institute for extraterrestrial Physics, Germania (TBC)
• Razmik Mirzoyan, Max-Planck-Institute for Physics, Germania
• Tsvi Piran, The Hebrew University, Israele
• Konstantin Postnov, Sternberg Astronomical Institute, Moscow State University, Russia
• Rashid Sunyaev, Max-Planck Institute for Astrophysics, Germania e IKI, Russia (TBC)
• Alexei Starobinsky, Landau Institute for Theoretical Physics, Russia
• Lev Titarchuk, University di Ferrara, Italy and Astro Space Center, Lebedev Physical Institute, Russia
• Nan Zhang, Institute of High Energy Physics, Cina
Durante questo meeting, saranno presentate le nuove scoperte fatte dalle principali missioni scientifiche in Astrofisica relativistica:
• Telescopio russo - tedesco Spektr-RG (SRG)
• Telescopio americano - europeo - canadese James Webb Space Telescope (JWST)
• L'italo - americano Imaging X-ray Polarimetry Explorer (IXPE)
• La missione sino - europea enhanced X-ray Timing and Polarimetry (eXTP)
• L'Osservatorio cinese Large High Altitude Air Shower Observatory (LHAASO)
• Il telescopio cinese Five-hundred-meter Aperture Spherical Telescope (FAST)
• Il telescopio europeo Major Atmospheric Gamma Imaging Cherenkov Telescope (MAGIC)
Il costo dell'iscrizione anticipata è di 300 euro (100 euro per gli studenti). Il costo dell'iscrizione in ritardo sarà di 400 euro (150 euro per gli studenti). Queste quote coprono il costo del kit della conferenza, delle pause caffè e della pubblicazione degli atti della conferenza.
Per il poster del meeting: https://indico.icranet.org/event/6/attachments/382/560/poster.pdf
Per il sito web del meeting: http://www.icranet.org/zeldovich5
La lista degli invited speakers comprende:
• Gennady Bisnovatyi-Kogan, Space Research Institute (IKI), Russia
• Massimo Della Valle, Osservatorio Astronomico di Capodimonte e INAF, Italia (TBC)
• Marat Gilfanov, Max-Planck Institute for Astrophysics, Germania e IKI, Russia (TBC)
• Paolo Giommi, Italian Space Agency (ASI), Italia
• Luca Izzo, Niels Bohr Institute, Danimarca (TBC)
• Michael Kramer, Max-Planck-Institut fuer Radioastronomie, Germania (TBC)
• Jutta Kunz, Università di Oldenburg, Germania (TBC)
• Klaus Laemmerzahl, Università di Brema, Germania
• Di Li, National Astronomical Observatories of China, Cina
• Ruoyu Liu, Nanjing University, Cina
• Andrea Merloni, Max Planck Institute for extraterrestrial Physics, Germania (TBC)
• Razmik Mirzoyan, Max-Planck-Institute for Physics, Germania
• Tsvi Piran, The Hebrew University, Israele
• Konstantin Postnov, Sternberg Astronomical Institute, Moscow State University, Russia
• Rashid Sunyaev, Max-Planck Institute for Astrophysics, Germania e IKI, Russia (TBC)
• Alexei Starobinsky, Landau Institute for Theoretical Physics, Russia
• Lev Titarchuk, University di Ferrara, Italy and Astro Space Center, Lebedev Physical Institute, Russia
• Nan Zhang, Institute of High Energy Physics, Cina
Durante questo meeting, saranno presentate le nuove scoperte fatte dalle principali missioni scientifiche in Astrofisica relativistica:
• Telescopio russo - tedesco Spektr-RG (SRG)
• Telescopio americano - europeo - canadese James Webb Space Telescope (JWST)
• L'italo - americano Imaging X-ray Polarimetry Explorer (IXPE)
• La missione sino - europea enhanced X-ray Timing and Polarimetry (eXTP)
• L'Osservatorio cinese Large High Altitude Air Shower Observatory (LHAASO)
• Il telescopio cinese Five-hundred-meter Aperture Spherical Telescope (FAST)
• Il telescopio europeo Major Atmospheric Gamma Imaging Cherenkov Telescope (MAGIC)
Il costo dell'iscrizione anticipata è di 300 euro (100 euro per gli studenti). Il costo dell'iscrizione in ritardo sarà di 400 euro (150 euro per gli studenti). Queste quote coprono il costo del kit della conferenza, delle pause caffè e della pubblicazione degli atti della conferenza.
Per il poster del meeting: https://indico.icranet.org/event/6/attachments/382/560/poster.pdf
Per il sito web del meeting: http://www.icranet.org/zeldovich5
3. Missione del Prof. Ruffini negli USA, 6-11 Novembre 2022: conferenze al Cosmos Club, all'Institute for Advanced Studies (IAS) ed alla Princeton University
Dal 6 all'11 Novembre 2022, il Prof. Remo Ruffini, Direttore ICRANet, ha visitato gli USA. Nel corso di questa visita, è stato invitato a presentare un seminario presso il prestigioso Cosmos Club a Washington DC nella giornata di lunedì 7 Novembre alle h 11:30 AM EST, dal titolo "The Role of Supernovae in Triggering the Formation of a Black Hole in Gamma Ray Bursts"; di seguito l'abstract:
Supernovae of constant luminosities, with a tight neutron star companion, trigger complex systems leading to the formation of fast rotating Kerr Black Holes. Their rotational energy feeds gamma ray bursts which are extremely luminous. This presentation identifies extensions of known physical laws, inquiring on the unique role of these cosmic events. We follow their implications for the life evolution of our universe. We also present recent understanding on the largest ever GRB221009A exploded on last October 19 and followed by the largest number of Observatories in all wavelengths from the ground and from space, from radio all the way to MeV , GeV and TeV radiation and UHCR.
Il giorno successive, l'8 Novembre, il Prof. Ruffini si è spostato a Princeton, poiché è stato invitato a partecipale al tradizionale Bahcall lunch presso l'Institute for Advanced Studies (IAS), uno speciale pranzo congiunto per gli astrofisici ed i fisici, i membri e la Faculty dell'istituto che si tiene nella Dilworth Room, Simons Hall.
Subito dopo il pranzo, il Prof. Ruffini si è recato presso l'università di Princeton, dove è stato invitato a presentare nuovamente il suo seminario dal titolo "The Role of Supernovae in Triggering the Formation of a Black Hole in Gamma Ray Bursts" presso la Jadwin Hall, nella nuova Gravity Initiative section.
Mentre si trovava presso l'Università di Princeton, il Prof. Ruffini ha incontrato anche, tra gli altri, la Prof. ssa Neta Bahcall, il Prof. Lyman Page ed il Prof. Bruce Partridge, e ha colto questa occasione per avere con loro delle interessanti conversazioni scientifiche.
Nei giorni successive, il Prof. Ruffini ha incontrato il Dr David Nirenberg, Direttore dello IAS, per discutere con lui dei questioni scientifiche e per presentargli gli ultimi risultati di ricerca ottenuti dal gruppo ICRANet. Ha anche visitato la biblioteca dell'Università di Princeton ed incontrato la Dott.ssa Abigail Johnson, della Princeton University Press, con la quale ha discusso di importanti questioni editoriali.
Supernovae of constant luminosities, with a tight neutron star companion, trigger complex systems leading to the formation of fast rotating Kerr Black Holes. Their rotational energy feeds gamma ray bursts which are extremely luminous. This presentation identifies extensions of known physical laws, inquiring on the unique role of these cosmic events. We follow their implications for the life evolution of our universe. We also present recent understanding on the largest ever GRB221009A exploded on last October 19 and followed by the largest number of Observatories in all wavelengths from the ground and from space, from radio all the way to MeV , GeV and TeV radiation and UHCR.
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| Fig. 1: annuncio del seminario del Prof. Remo Ruffini presso il Cosmos Club, Washington DC, il giorno 7 Novembre 2022. | Fig. 2: Il Prof. Remo Ruffini di fronte alla parete con tutti i membre che hanno ricevuto il Premio Nobel, che si trova presso il Cosmos Club a Washington. |
Il giorno successive, l'8 Novembre, il Prof. Ruffini si è spostato a Princeton, poiché è stato invitato a partecipale al tradizionale Bahcall lunch presso l'Institute for Advanced Studies (IAS), uno speciale pranzo congiunto per gli astrofisici ed i fisici, i membri e la Faculty dell'istituto che si tiene nella Dilworth Room, Simons Hall.
Subito dopo il pranzo, il Prof. Ruffini si è recato presso l'università di Princeton, dove è stato invitato a presentare nuovamente il suo seminario dal titolo "The Role of Supernovae in Triggering the Formation of a Black Hole in Gamma Ray Bursts" presso la Jadwin Hall, nella nuova Gravity Initiative section.
Mentre si trovava presso l'Università di Princeton, il Prof. Ruffini ha incontrato anche, tra gli altri, la Prof. ssa Neta Bahcall, il Prof. Lyman Page ed il Prof. Bruce Partridge, e ha colto questa occasione per avere con loro delle interessanti conversazioni scientifiche.
Nei giorni successive, il Prof. Ruffini ha incontrato il Dr David Nirenberg, Direttore dello IAS, per discutere con lui dei questioni scientifiche e per presentargli gli ultimi risultati di ricerca ottenuti dal gruppo ICRANet. Ha anche visitato la biblioteca dell'Università di Princeton ed incontrato la Dott.ssa Abigail Johnson, della Princeton University Press, con la quale ha discusso di importanti questioni editoriali.
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| Fig. 3: da sinistra a destra: il Prof. Remo Ruffini, la Prof.ssa Neta Bahcall, il Prof. Lyman Page ed il Prof. Bruce Partridge. | Fig. 4: Il Prof. Ruffini insieme alla Dott.ssa Abigail Johnson (Princeton University Press). |
4. Il Prof. Ruffini è tra il 2% degli autori più citati, secondo Elsevier
Il recente aggiornamento del database accessibile al pubblico degli oltre 100.000 eminenti scienziati individuati da Elsevier, ha mostrato che il Prof. Remo Ruffini (Direttore ICRANet), il Prof. Behzad Eslam Panah (ICRANet Mazandaran, Iran) e diversi altri scienziati ICRANet sono presenti in questa lista.
Elsevier ha creato questo database accessibile al pubblico degli scienziati più citati, che fornisce informazioni standardizzate su citazioni, h-index, co-authorship adjusted hm-index e citazioni agli articoli in differenti posizioni di autorialità. Gli scienziati sono classificati in 22 campi differenti ed in 174 sotto campi, che sono forniti per tutti gli scienziati con almeno 5 articoli. I dati sulla lunghezza della carriera sono aggiornati alla fine del 2021 ed i singoli dati dell'ultimo riguardano le citazioni ricevute nel 2021. La selezione si basa sul c-score dei 100.000 eminenti scienziati (con o senza auto citazioni) su una classifica percentile del 2% o più nel sotto campo. Questa versione della lista è basata dallo spaccato di Scopus al 1 Settembre 2022, aggiornata alla fine dell'anno 2021 per le citazioni. Questo lavoro utilizza i dati Scopus forniti da Elsevier attraverso l'ICSR Lab (https://www.elsevier.com/icsr/icsrlab) ed i calcoli sono stati fatti utilizzando tutti i profili Scopus degli autori al 1 Settembre 2022.
Elsevier ha creato questo database accessibile al pubblico degli scienziati più citati, che fornisce informazioni standardizzate su citazioni, h-index, co-authorship adjusted hm-index e citazioni agli articoli in differenti posizioni di autorialità. Gli scienziati sono classificati in 22 campi differenti ed in 174 sotto campi, che sono forniti per tutti gli scienziati con almeno 5 articoli. I dati sulla lunghezza della carriera sono aggiornati alla fine del 2021 ed i singoli dati dell'ultimo riguardano le citazioni ricevute nel 2021. La selezione si basa sul c-score dei 100.000 eminenti scienziati (con o senza auto citazioni) su una classifica percentile del 2% o più nel sotto campo. Questa versione della lista è basata dallo spaccato di Scopus al 1 Settembre 2022, aggiornata alla fine dell'anno 2021 per le citazioni. Questo lavoro utilizza i dati Scopus forniti da Elsevier attraverso l'ICSR Lab (https://www.elsevier.com/icsr/icsrlab) ed i calcoli sono stati fatti utilizzando tutti i profili Scopus degli autori al 1 Settembre 2022.
5. Congratulazioni al Prof. Narek Sahakyan, Direttore del centro ICRANet Armenia e Professore della Faculty ICRANet, che ha conseguito il dottorato di ricerca (DSc) in fisica, 22 Novembre 2022
E' un grande piacere annunciare che il 22 Novembre 2022, il Prof. Narek Sahakyan, Direttore del centro ICRANet in Armenia, ha conseguito il dottorato di ricerca (DSc) in fisica, come annunciato dalla Higher Attestation Commission (VAK) di Armenia (https://www.bok.am/en/node/14246). La sua dissertazione, dal titolo "Study of multiwavelength and neutrino emission from blazars" è stata discussa con successo il 25 Giugno 2022.
Il Professor Sahakyan è così diventato uno dei pochi giovani ricercatori armeni ad aver conseguito, sotto i 40 anni, questo titolo scientifico così alto nella sua nazione.
6. Eclissi solare parziale e misura del diametro solare (25 Ottobre 2022) ed eclissi lunare agli antipodi (8 Novembre 2022), eventi online e podcast
Eclissi solare parziale e misura del diametro solare (25 Ottobre 2022)
In occasione dell'eclissi solare parziale del 25 Ottobre 2022, il Prof. Costantino Sigismondi, collaboratore ICRANet, ha organizzato un evento online e podcast, nel quadro di un progetto portato avanti con gli studenti di liceo di Pescara, Roma e Motta di Liveza (Italy), sulla misura del diametro solare.
Questo studio si inserisce in un progetto di astrometria "Eclissi, equinozi e tramonti: i metodi per domare i cavalli del sole". Il carro mitologico di Febo è condotto attraverso una precisa orbita, i cui parametri sono oggetto di studio della meccanica celeste. Gli astronomi dopo Galileo, con questa frase, alludevano alla comprensione del fenomeno della rifrazione atmosferica, che fu misurata proprio con il Sole tra 20° e 70° dallo zenit da Giandomenico Cassini nel 1655, dopo essere stata misurata da Tycho Brahe nel 1572 con la Supernova in Cassiopea osservata da tutta Europa.
Il Prof. Sigismondi ha illustrato i seguenti metodi osservativi e di analisi dei dati con le misure della posizione e del diametro del Sole meridiane e sull'orizzonte: elementi di astrometria (sistemi di coordinate celesti, ascensione retta e declinazione, longitudine e latitudine eclittica); le stagioni dal punto di vista astronomico (la forma dell'orbita della Terra: eccentricità e linea degli apsidi); la forma e le dimensioni della Terra dai dati sul meridiano da Roma S. Maria degli Angeli e dei Martiri a Motta di Livenza; il timing di un'osservazione astronomica usando il video sincronizzato con UTC; il timing di un'osservazione astronomica da webcam e la sincronizzazione col protocollo NTP; le effemeridi astronomiche NASA, IMCCE ed il programma Stellarium; il fit lineare sui dati dell'equinozio di autunno 2022; il fit quadratico sui dati del solstizio estivo del 2022, il fit quadratico sui dati dell'eclissi parziale di Sole del 25 Ottobre 2022, il database online delle osservazioni alla Meridiana clementina e il foglio di lavoro per la riduzione dati.
Per la base scientifica dell'evento: http://www.icranet.org/index.php?option=com_content&task=view&id=1461
Per i video analizzati nel corso dell'evento: http://www.icranet.org/index.php?option=com_content&task=view&id=1460#EclissiLuna
Per la playlist YouTube sull'eclissi solare del 25 Ottobre 2022: https://www.youtube.com/playlist?list=PLJaer2KV492_Nu3nCaB3LhVxKXsAHhR7S
L'eclissi lunare agli antipodi (8 Novembre 2022)
The lunar eclipse at the antipodes has been seen thanks to the calculations (November 8, 2022).
Infatti, in ogni stagione delle eclissi, ogni sei mesi draconitici le eclissi vengono sempre a coppie, se non addirittura in tre. Tutte queste statistiche sono retaggio della meccanica celeste classica ed il Prof. Costantino Sigismondi, collaboratore ICRANet, ne ha ripercorso le tappe principali attraverso due eventi:
Il primo si è tenuto il 5 Novembre nella Basilica di Santa Maria degli Angeli (Roma). Sulla Linea Clementina sono stati simulati i passaggi meridiani della Luna del 7 e del 9 Novembre 2022 e sono stati svolti i calcoli di interpolazione per l'8 Novembre, imponendo la condizione di allineamento tra i centri di Luna, Terra e Sole. E' stato infine scoperto che la Luna sarebbe stata a quasi 180° dal Sole nella giornata dell'8 Novembre alle h 12:00.
Il secondo si è tenuto l'8 Novembre, tramite un collegamento al sito Timeanddate, dove sono state trasmesse le immagini dell'eclissi: https://www.timeanddate.com/eclipse/lunar/2022-november-8. Nel frattempo, il Prof. Sigismondi ha fatto dei commenti storico - scientifici in italiano..
Le eclissi di Luna furono utilizzate per misurare la longitudine del punto di osservazione, avendo a disposizione una meridiana. Costituiscono il metodo più accurato per questo scopo fino a tutto il XVIII secolo. Anche Cristoforo Colombo valutò la longitudine di Hispaniola con l'eclissi di Luna del 29 Febbraio 1504. Il Prof. Sigismondi ha poi illustrato le eclissi di Luna che lui ha osservato, a partire da quella del 9 Gennaio 1982 a Lanciano, ripetutasi dopo un ciclo di Saros il 21 Gennaio 2000 a Padova, poi ancora dopo un ciclo di Metone il 21 Gennaio 2019 a Pescara ed il 7 Agosto 2017 dal ponte Sant Angelo a Roma. L'ultima eclissi da lui osservata è stata quella del 16 Maggio 2022 a Lanciano.
Per il sito web del meeting e per le referenze sui lavori che trattano delle eclissi lunari: http://www.icranet.org/index.php?option=com_content&task=view&id=1460
In occasione dell'eclissi solare parziale del 25 Ottobre 2022, il Prof. Costantino Sigismondi, collaboratore ICRANet, ha organizzato un evento online e podcast, nel quadro di un progetto portato avanti con gli studenti di liceo di Pescara, Roma e Motta di Liveza (Italy), sulla misura del diametro solare.
Questo studio si inserisce in un progetto di astrometria "Eclissi, equinozi e tramonti: i metodi per domare i cavalli del sole". Il carro mitologico di Febo è condotto attraverso una precisa orbita, i cui parametri sono oggetto di studio della meccanica celeste. Gli astronomi dopo Galileo, con questa frase, alludevano alla comprensione del fenomeno della rifrazione atmosferica, che fu misurata proprio con il Sole tra 20° e 70° dallo zenit da Giandomenico Cassini nel 1655, dopo essere stata misurata da Tycho Brahe nel 1572 con la Supernova in Cassiopea osservata da tutta Europa.
Il Prof. Sigismondi ha illustrato i seguenti metodi osservativi e di analisi dei dati con le misure della posizione e del diametro del Sole meridiane e sull'orizzonte: elementi di astrometria (sistemi di coordinate celesti, ascensione retta e declinazione, longitudine e latitudine eclittica); le stagioni dal punto di vista astronomico (la forma dell'orbita della Terra: eccentricità e linea degli apsidi); la forma e le dimensioni della Terra dai dati sul meridiano da Roma S. Maria degli Angeli e dei Martiri a Motta di Livenza; il timing di un'osservazione astronomica usando il video sincronizzato con UTC; il timing di un'osservazione astronomica da webcam e la sincronizzazione col protocollo NTP; le effemeridi astronomiche NASA, IMCCE ed il programma Stellarium; il fit lineare sui dati dell'equinozio di autunno 2022; il fit quadratico sui dati del solstizio estivo del 2022, il fit quadratico sui dati dell'eclissi parziale di Sole del 25 Ottobre 2022, il database online delle osservazioni alla Meridiana clementina e il foglio di lavoro per la riduzione dati.
Per la base scientifica dell'evento: http://www.icranet.org/index.php?option=com_content&task=view&id=1461
Per i video analizzati nel corso dell'evento: http://www.icranet.org/index.php?option=com_content&task=view&id=1460#EclissiLuna
Per la playlist YouTube sull'eclissi solare del 25 Ottobre 2022: https://www.youtube.com/playlist?list=PLJaer2KV492_Nu3nCaB3LhVxKXsAHhR7S
L'eclissi lunare agli antipodi (8 Novembre 2022)
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| Fig. 5: simulazione del transito meridiano lunare, 7 Novembre 2022. | Fig. 6: simulazione del transito meridiano lunare, 9 Novembre 2022. |
The lunar eclipse at the antipodes has been seen thanks to the calculations (November 8, 2022).
Infatti, in ogni stagione delle eclissi, ogni sei mesi draconitici le eclissi vengono sempre a coppie, se non addirittura in tre. Tutte queste statistiche sono retaggio della meccanica celeste classica ed il Prof. Costantino Sigismondi, collaboratore ICRANet, ne ha ripercorso le tappe principali attraverso due eventi:
Il primo si è tenuto il 5 Novembre nella Basilica di Santa Maria degli Angeli (Roma). Sulla Linea Clementina sono stati simulati i passaggi meridiani della Luna del 7 e del 9 Novembre 2022 e sono stati svolti i calcoli di interpolazione per l'8 Novembre, imponendo la condizione di allineamento tra i centri di Luna, Terra e Sole. E' stato infine scoperto che la Luna sarebbe stata a quasi 180° dal Sole nella giornata dell'8 Novembre alle h 12:00.
Il secondo si è tenuto l'8 Novembre, tramite un collegamento al sito Timeanddate, dove sono state trasmesse le immagini dell'eclissi: https://www.timeanddate.com/eclipse/lunar/2022-november-8. Nel frattempo, il Prof. Sigismondi ha fatto dei commenti storico - scientifici in italiano..
Le eclissi di Luna furono utilizzate per misurare la longitudine del punto di osservazione, avendo a disposizione una meridiana. Costituiscono il metodo più accurato per questo scopo fino a tutto il XVIII secolo. Anche Cristoforo Colombo valutò la longitudine di Hispaniola con l'eclissi di Luna del 29 Febbraio 1504. Il Prof. Sigismondi ha poi illustrato le eclissi di Luna che lui ha osservato, a partire da quella del 9 Gennaio 1982 a Lanciano, ripetutasi dopo un ciclo di Saros il 21 Gennaio 2000 a Padova, poi ancora dopo un ciclo di Metone il 21 Gennaio 2019 a Pescara ed il 7 Agosto 2017 dal ponte Sant Angelo a Roma. L'ultima eclissi da lui osservata è stata quella del 16 Maggio 2022 a Lanciano.
Per il sito web del meeting e per le referenze sui lavori che trattano delle eclissi lunari: http://www.icranet.org/index.php?option=com_content&task=view&id=1460
7. Rinnovo dell'accordo di cooperazione tra l'ICRANet e l'Università Campus Bio-Medico di Roma (Italia), 11 Ottobre 2022
L'11 Ottobre 2022 è stato rinnovato l'accordo di cooperazione tra l'ICRANet e l'Università Campus Bio-medico di Roma. L'accordo sarà valido per ulteriori 2 anni e le principali attività congiunte che saranno portate avanti nel quadro del progetto comprendono: la promozione delle attività teoriche e di osservazione nel campo dell'astrofisica relativistica; lo scambio istituzionale di membri, ricercatori, post-doc, e studenti; lo sviluppo di tecnologie e di dati per l'astrofisica su tutte le bande di frequenza; l'organizzazione di corsi, seminari, conferenze, workshops; lo sviluppo di ricerche inter-instituzionali e pubblicazioni congiunte.
Per il testo dell'accordo: http://www.icranet.org/bio-medico
8. Seminari presso il centro ICRANet a Pescara, 25 Novembre 2022
Seminario del Prof. Gennady Bisnovatyi-Kogan
Venerdì 25 Novembre 2022, il Prof. Gennady Bisnovatyi-Kogan (Space Research Institute dell'Accademia delle Scienze russa - SRI RAS) ha presentato un seminario dal titolo "About the Observational Check of the Mechanism of Gamma Radiation in Soft Gamma Repeaters (SGR)"; di seguit l'abstract:
Soft gamma repeaters (SGR) are identified as single neutron stars (NS) inside the Galaxy, or nearby galaxies, with sporadic transient gamma radiation. A total number of discovered SGR, including relative Anomalous X-ray pulsars (AXP), is a few tens of objects. Many of them show periodic radiation, connected with NS rotation, with periods 2-12 s. The slow rotation is accompanied by small rate of loss of rotational energy, which is considerably smaller than the observed sporadic gamma ray luminosity, and is many orders less than the luminosity during giant bursts, observed in 4 SGR. Therefore the energy source is usually connected with annihilation of a very strong NS magnetic field. Another model is based on the release of nuclear energy stored in the NS non-equilibrium layer. We suggest here an observational test which could distinguish between these two models.
L'annuncio del seminario è stato anche pubblicato sul sito web dell'ICRANet: http://www.icranet.org/index.php?option=com_content&task=blogcategory&id=89&Itemid=781
Per il video del seminario: https://youtu.be/1lZLqJ_pogk
Seminario del Prof. Marco Merafina
Venerdì 25 Novembre 2022, il Prof. Marco Merafina (Università di Roma La Sapienza) ha presentato un seminario dal titolo "Multimass King models with Kroupa mass function"; di seguito l'abstract:
Statistical analysis on Milky Way globular clusters distribution is developed in order to extract the best fit function and carry out the critical value of the onset of gravothermal catastrophe, connected with the maximum of the distribution function. Results show that gravothermal collapse for globular clusters onsets earlier than commonly believed and in accordance with theoretical results obtained by considering the presence of the effective potential which describes the effects of the tidal forces induced by the hosting galaxy. N-body simulations confirm the presence of the effective potential with the predicted form. Theoretical model is generalized to multimass one by using Kroupa mass function. A detailed description of the projected densities at different W0 indicates similar luminosity profiles in complete accordance with observations. We also consider the effects of the mass segregation on the distribution of stars and the consequences on the equipartition process. N-body simulations in connection with mass distribution and segregation as well the computational development applied to multimass model are also shown at the present state of the art.
L'annuncio del seminario è stato anche pubblicato sul sito web dell'ICRANet: http://www.icranet.org/index.php?option=com_content&task=blogcategory&id=89&Itemid=781
Per il video del seminario: https://youtu.be/gW4yGYbLdNA
Venerdì 25 Novembre 2022, il Prof. Gennady Bisnovatyi-Kogan (Space Research Institute dell'Accademia delle Scienze russa - SRI RAS) ha presentato un seminario dal titolo "About the Observational Check of the Mechanism of Gamma Radiation in Soft Gamma Repeaters (SGR)"; di seguit l'abstract:
Soft gamma repeaters (SGR) are identified as single neutron stars (NS) inside the Galaxy, or nearby galaxies, with sporadic transient gamma radiation. A total number of discovered SGR, including relative Anomalous X-ray pulsars (AXP), is a few tens of objects. Many of them show periodic radiation, connected with NS rotation, with periods 2-12 s. The slow rotation is accompanied by small rate of loss of rotational energy, which is considerably smaller than the observed sporadic gamma ray luminosity, and is many orders less than the luminosity during giant bursts, observed in 4 SGR. Therefore the energy source is usually connected with annihilation of a very strong NS magnetic field. Another model is based on the release of nuclear energy stored in the NS non-equilibrium layer. We suggest here an observational test which could distinguish between these two models.
L'annuncio del seminario è stato anche pubblicato sul sito web dell'ICRANet: http://www.icranet.org/index.php?option=com_content&task=blogcategory&id=89&Itemid=781
Per il video del seminario: https://youtu.be/1lZLqJ_pogk
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| Fig. 7 e 8: Il Prof. Gennady Bisnovatyi-Kogan mentre presenta il suo seminario presso il centro ICRANet a Pescara, 25 Novembre 2022. | |
Seminario del Prof. Marco Merafina
Venerdì 25 Novembre 2022, il Prof. Marco Merafina (Università di Roma La Sapienza) ha presentato un seminario dal titolo "Multimass King models with Kroupa mass function"; di seguito l'abstract:
Statistical analysis on Milky Way globular clusters distribution is developed in order to extract the best fit function and carry out the critical value of the onset of gravothermal catastrophe, connected with the maximum of the distribution function. Results show that gravothermal collapse for globular clusters onsets earlier than commonly believed and in accordance with theoretical results obtained by considering the presence of the effective potential which describes the effects of the tidal forces induced by the hosting galaxy. N-body simulations confirm the presence of the effective potential with the predicted form. Theoretical model is generalized to multimass one by using Kroupa mass function. A detailed description of the projected densities at different W0 indicates similar luminosity profiles in complete accordance with observations. We also consider the effects of the mass segregation on the distribution of stars and the consequences on the equipartition process. N-body simulations in connection with mass distribution and segregation as well the computational development applied to multimass model are also shown at the present state of the art.
L'annuncio del seminario è stato anche pubblicato sul sito web dell'ICRANet: http://www.icranet.org/index.php?option=com_content&task=blogcategory&id=89&Itemid=781
Per il video del seminario: https://youtu.be/gW4yGYbLdNA
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| Fig. 9 e 10: Il Prof. Marco Merafina mentre presenta il suo seminario presso il centro ICRANet a Pescara, 25 Novembre 2022. | |
9. Visite scientifiche presso l'ICRANet
• Prof. Seyed Mohammad Taghi Mirtorabi (Alzahra University - Iran), 1 - 18 Ottobre 2022
• Prof. Massimo Della Valle (Osservatorio di Capodimonte - Italia), 30 Ottobre - 1 Novembre 2022
• Prof. Gennady Bisnovatyi-Kogan (Space Research Institute dell'Accdemia delle Scienze russa - SRI RAS), 25 - 27 Novembre 2022
• Prof. Marco Merafina (Università di Roma La Sapienza), 25 Novembre 2022
Durante la loro visita, questi scienziati hanno avuto l'opportunità di discutere le loro ricerche scientifiche e di avere interessanti scambi con gli altri ricercatori dell'ICRANet e da diverse parti del mondo.
• Prof. Massimo Della Valle (Osservatorio di Capodimonte - Italia), 30 Ottobre - 1 Novembre 2022
• Prof. Gennady Bisnovatyi-Kogan (Space Research Institute dell'Accdemia delle Scienze russa - SRI RAS), 25 - 27 Novembre 2022
• Prof. Marco Merafina (Università di Roma La Sapienza), 25 Novembre 2022
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| Prof. Seyed Mohammad Taghi Mirtorabi | Prof. Massimo Della Valle | Prof. Gennady Bisnovatyi-Kogan | Prof. Marco Merafina |
Durante la loro visita, questi scienziati hanno avuto l'opportunità di discutere le loro ricerche scientifiche e di avere interessanti scambi con gli altri ricercatori dell'ICRANet e da diverse parti del mondo.
10. Pubblicazioni recenti
J. A. Rueda, Liang Li, R. Moradi, R. Ruffini, N. Sahakyan, and Y. Wang, On the X-Ray, Optical, and Radio Afterglows of the BdHN I GRB 180720B Generated by Synchrotron Emission, published on November 3, 2022 in ApJ, Volume 939, Number 2.
Gamma-ray bursts (GRBs) are systems of unprecedented complexity across all the electromagnetic spectrum, including the radio, optical, X-rays, gamma rays in the MeV and GeV regimes, as well as ultrahigh-energy cosmic rays, each manifested in seven specific physical processes with widely different characteristic evolution timescales ranging from 10−14 s to 107 s or longer. We here study the long GRB 180720B originating from a binary system composed of a massive carbon-oxygen (CO) star of about 10M⊙ and a companion neutron star (NS). The gravitational collapse of the CO star gives rise to a spinning newborn NS (νNS), with an initial period of P0 = 1 ms that powers the synchrotron radiation in the radio, optical, and X-ray wavelengths. We here investigate solely the GRB 180720B afterglows and present a detailed treatment of its origin based on the synchrotron radiation released by the interaction of the νNS and the SN ejecta. We show that in parallel to the X-ray afterglow, the spinning νNS also powers the optical and radio afterglows and allows to infer the νNS and ejecta parameters that fit the observational data.
DOI: http://dx.doi.org/10.3847/1538-4357/ac94c9
J. A. Rueda, R. Ruffini, L. Li, R. Moradi, J. F. Rodriguez, and Y. Wang, Evidence for the transition of a Jacobi ellipsoid into a Maclaurin spheroid in gamma-ray bursts, published on October 7, 2022 in Phys. Rev. D 106, 083004.
In the binary-driven hypernova (BdHN) scenario, long gamma-ray bursts (GRBs) originate in a cataclysmic event that occurs in a binary system composed of a carbon-oxygen (CO) star and a neutron star (NS) companion in close orbit. The collapse of the CO star generates at its center a newborn NS (νNS), and a supernova (SN) explosion. Matter from the ejecta is accreted both onto the νNS because of fallback and onto the NS companion, leading to the collapse of the latter into a black hole (BH). Each of the ingredients of the above system leads to observable emission episodes in a GRB. In particular, the νNS is expected to show up (hereafter νNS−rise) in the early GRB emission, nearly contemporary or superimposed to the ultrarelativistic prompt emission (UPE) phase, but with a different spectral signature. Following the νNS−rise, the νNS powers the afterglow emission by injecting energy into the expanding ejecta leading to synchrotron radiation. We here show that the νNS−rise and the subsequent afterglow emission in both systems, GRB 180720B and GRB 190114C, are powered by the release of rotational energy of a Maclaurin spheroid, starting from the bifurcation point to the Jacobi ellipsoid sequence. This implies that the νNS evolves from a triaxial Jacobi configuration, prior to the νNS−rise, into the axially symmetric Maclaurin configuration observed in the GRB. The triaxial νNS configuration is short-lived (less than a second) due to a copious emission of gravitational waves, before the GRB emission, and it could be in principle detected for sources located at distances closer than 100 Mpc. This appears to be a specific process of emission of gravitational waves in the BdHN I powering long GRBs.
DOI: https://doi.org/10.1103/PhysRevD.106.083004
L. M. Becerra, R. Moradi, J. A. Rueda, R. Ruffini, and Y. Wang, First minutes of a binary-driven hypernova, published on October 3, 2022 in Phys. Rev. D 106, 083002.
We simulate the first minutes of the evolution of a binary-driven hypernova event, with a special focus on the associated accretion processes of supernova ejecta onto the newborn neutron star (νNS) and the NS companion. We calculate the rotational evolution of the νNS and the NS under the torques exerted by the accreted matter and the magnetic field. We take into account general relativistic effects through effective models for the NSs binding energy and the specific angular momentum transferred by the accreted matter. We use realistic hypercritical accretion rates obtained from three-dimensional smoothed-particle-hydrodynamics numerical simulations of the binary-driven hypernova event for a variety of orbital periods. We show that the rotation power of the νNS has a unique double-peak structure while that of the NS has a single peak. These peaks are of comparable intensity and can occur very close in time or even simultaneously depending on the orbital period and the initial angular momentum of the stars. We outline the consequences of the above features in the early emission and their consequent observation in long gamma-ray bursts.
DOI: https://doi.org/10.1103/PhysRevD.106.083002
Carvalho, G. A.; Anjos, R. C. dos; Coelho, J. G.; Lobato, R. V.; Malheiro, M.; Marinho, R. M.; Rodriguez, J. F.; Rueda, J. A.; Ruffini, R., Orbital Decay of Double White Dwarfs: Beyond Gravitational-wave Radiation Effects, published on November 23, 2022 in ApJ, Vol. 940, n. 1.
The traditional description of the orbital evolution of compact-object binaries, like double white dwarfs (DWDs), assumes that the system is driven only by gravitational-wave (GW) radiation. However, the high magnetic fields with intensities of up to gigagausses measured in WDs alert a potential role of the electromagnetic (EM) emission in the evolution of DWDs. We evaluate the orbital dynamics of DWDs under the effects of GW radiation, tidal synchronization, and EM emission by a unipolar inductor generated by the magnetic primary and the relative motion of the nonmagnetic secondary. We show that the EM emission can affect the orbital dynamics for magnetic fields larger than megagausses. We applied the model to two known DWDs, SDSS J0651+2844 and ZTF J1539+5027, for which the GW radiation alone does not fully account for the measured orbital decay rate. We obtain upper limits to the primary's magnetic field strength, over which the EM emission causes an orbital decay faster than observed. The contribution of tidal locking and the EM emission is comparable, and together they can contribute up to 20% to the measured orbital decay rate. We show that the gravitational waveform for a DWD modeled as purely driven by GWs and including tidal interactions and EM emission can have large relative dephasing detectable in the mHz regime of frequencies relevant for space-based detectors like LISA. Therefore, including physics besides GW radiation in the waveform templates is essential to calibrate the GW detectors using known sources, e.g., ZTF J1539+5027, and to infer binary parameters.
DOI: 10.3847/1538-4357/ac9841
S-S. Xue, W boson mass tension caused by its right-handed gauge coupling at high energies?, published on October 16, 2022 in Nuclear Physics B, Volume 985.
The CDF collaboration's recent high-precision measurement of the W mass is in 7.0σ disagreement with the Standard Model expectation. This tension will be relieved if the W boson has a non-trivial right-handed gauge coupling at high energies. At TeV scales, the SM gauge symmetric four-fermion interactions induce a right-handed gauge coupling, and SM fermions compose massive composite particles. We investigate the top-quark mass produced by spontaneous symmetry breaking and compute the W and Z boson propagators and decays. The right-handed coupling corrections to their masses and widths are consistent with experimental measurements. We discuss how SM gauge bosons and composite particles can restore parity-preserving gauge symmetries at TeV scales.
DOI: https://doi.org/10.1016/j.nuclphysb.2022.115992
N. Sahakyan, D. Israyelyan, G. Harutyunyan, S. Gasparyan, V. Vardanyan, M. Khachatryan, Modelling the time variable spectral energy distribution of the blazar CTA 102 from 2008 to 2022, published on October 2, 2022 in Monthly Notices of the Royal Astronomical Society.
We present long-term multiwavelength observations of blazar CTA 102 (z = 1.037). Detailed temporal and spectral analyses of γ-ray, X-ray, and UV/optical data observed by Fermi-LAT, Swift XRT, NuSTAR, and Swift-UVOT over a period of 14 yr, between 2008 August and 2022 March, were performed. We found strong variability of source emission in all the considered bands; especially in the γ-ray band it exhibited extreme outbursts when the flux crossed the level of 10−5 photon cm−2 s−1. Using the Bayesian Blocks algorithm, we split the adaptively binned γ-ray light curve into 347 intervals of quiescent and flaring episodes and for each period built corresponding multiwavelength spectral energy distributions (SEDs), using the available data. Among the considered SEDs, 117 high-quality (quasi) contemporaneous SEDs, which have sufficient multiwavelength data, were modelled using JETSET framework within a one-zone leptonic synchrotron and inverse-Compton emission scenario assuming the emitting region is within the broad-line region and considering internal and external seed photons for the inverse-Compton up scattering. As a result of modelling, the characteristics of the relativistic electron distribution in the jet as well as jet properties are retrieved and their variation in time is investigated. The applied model can adequately explain the assembled SEDs and the modelling shows that the data in the bright flaring periods can be reproduced for high Doppler boosting and magnetic field. The obtained results are discussed in the context of particle cooling in the emitting region.
DOI: https://doi.org/10.1093/mnras/stac2875
B. Eslam Panah, Two-dimensional Lifshitz-like AdS black holes in F(R) gravity, published on November 2 in the Journal of Mathematical Physics 63, 112502 (2022).
Two-dimensional (2D) Lifshitz-like black holes in special F(R) gravity cases are extracted. We indicate an essential singularity at r = 0, covered by an event horizon. Then, conserved and thermodynamic quantities, such as temperature, mass, entropy, and the heat capacity of 2D Lifshitz-like black holes in F(R) gravity, are evaluated. Our analysis shows that 2D Lifshitz-like black hole solutions can be physical solutions, provided that the cosmological constant is negative (Λ < 0). Indeed, there is a phase transition between stable and unstable cases by increasing the radius of AdS black holes. In other words, the 2D Lifshitz-like AdS black holes with large radii are physical and enjoy thermal stability. The obtained 2D Lifshitz-like AdS-black holes in F(R) gravity turn into the well-known 2D Schwarzschild AdS-black holes when the Lifshitz-like parameter is zero (s = 0). Moreover, correspondence between these black hole solutions and the 2D rotating black hole solutions is found by adjusting the Lifshitz-like parameter.
DOI: https://doi.org/10.1063/5.0104272
A. Bagheri Tudeshki, G. H. Bordbar, and B. Eslam Panah, Dark Energy Star in Gravity's Rainbow, published on October 19 in Physics Letters B. 835, 137523 (2022).
The concept of dark energy can be a candidate for preventing the gravitational collapse of compact objects to singularities. According to the usefulness of gravity's rainbow in UV completion of general relativity (by providing a new description of spacetime), it can be an excellent option to study the behavior of compact objects near phase transition regions. In this work, we obtain a modified Tolman-Openheimer-Volkof (TOV) equation for anisotropic dark energy as a fluid by solving the field equations in gravity's rainbow. Next, to compare the results with general relativity, we use a generalized Tolman-Matese-Whitman mass function to determine the physical quantities such as energy density, radial pressure, transverse pressure, gravity profile, and anisotropy factor of the dark energy star. We evaluate the junction condition and investigate the dynamical stability of dark energy star thin shell in gravity's rainbow. We also study the energy conditions for the interior region of this star. We show that the coefficients of gravity's rainbow can significantly affect this non-singular compact object and modify the model near the phase transition region.
DOI: https://doi.org/10.1016/j.physletb.2022.137523
García, Cristhian; Santa, Camilo; Romano, Antonio Enea, Deep learning reconstruction of the large scale structure of the Universe from luminosity distance, published on October 19, 2022 in Monthly Notices of the Royal Astronomical Society.
Supernovae Ia (SNe) can provide a unique window on the large-scale structure (LSS) of the Universe at redshifts where few other observations are available, by solving the inversion problem (IP) consisting in reconstructing the LSS from its effects on the observed luminosity distance. So far the IP was solved assuming some restrictions about space-time, such as spherical symmetry for example, while we obtain for the first time solutions of the IP problem for arbitrary space-time geometries using deep learning. The method is based on the use of convolutional neural networks (CNN) trained on simulated data. The training data set is obtained by first generating random density and velocity fields, and then computing their effects on the luminosity distance. The CNN, based on an appropriately modified version of U-Net to account for the tridimensionality of the data, is then trained to reconstruct the density and velocity fields from the luminosity distance. We find that the velocity field inversion is more accurate than the density field, because the effects of the velocity on the luminosity distance only depend on the source velocity, while in the case of the density it is an integrated effect along the line of sight, giving rise to more degeneracy in the solution of the IP. Improved versions of these neural networks, modified to accommodate the non-uniform distribution of the SNe, can be applied to observational data to reconstruct the LSS of the Universe at redshifts at which few other observations are available.
DOI: https://doi.org/10.1093/mnras/stac2916
Cadavid, Alexander Gallego; Romano, Antonio Enea; Liddle, Andrew R., Reconstructing homospectral inflationary potentials, published on October 13, 2022 in Phys. Rev. D 106, 083512.
Purely geometrical arguments show that there exist classes of homospectral inflationary cosmologies, i.e., different expansion histories producing the same spectrum of comoving curvature perturbations. We develop a general algorithm to reconstruct the potential of minimally coupled single scalar fields from an arbitrary expansion history. We apply it to homospectral expansion histories to obtain the corresponding potentials, providing numerical and analytical examples. The infinite class of homospectral potentials depends on two free parameters, the initial energy scale and the initial value of the field, showing that, in general, it is impossible to reconstruct a unique potential from the curvature spectrum unless the initial energy scale and the field value are fixed, for instance, through observation of primordial gravitational waves.
DOI: https://doi.org/10.1103/PhysRevD.106.083512
Gamma-ray bursts (GRBs) are systems of unprecedented complexity across all the electromagnetic spectrum, including the radio, optical, X-rays, gamma rays in the MeV and GeV regimes, as well as ultrahigh-energy cosmic rays, each manifested in seven specific physical processes with widely different characteristic evolution timescales ranging from 10−14 s to 107 s or longer. We here study the long GRB 180720B originating from a binary system composed of a massive carbon-oxygen (CO) star of about 10M⊙ and a companion neutron star (NS). The gravitational collapse of the CO star gives rise to a spinning newborn NS (νNS), with an initial period of P0 = 1 ms that powers the synchrotron radiation in the radio, optical, and X-ray wavelengths. We here investigate solely the GRB 180720B afterglows and present a detailed treatment of its origin based on the synchrotron radiation released by the interaction of the νNS and the SN ejecta. We show that in parallel to the X-ray afterglow, the spinning νNS also powers the optical and radio afterglows and allows to infer the νNS and ejecta parameters that fit the observational data.
DOI: http://dx.doi.org/10.3847/1538-4357/ac94c9
J. A. Rueda, R. Ruffini, L. Li, R. Moradi, J. F. Rodriguez, and Y. Wang, Evidence for the transition of a Jacobi ellipsoid into a Maclaurin spheroid in gamma-ray bursts, published on October 7, 2022 in Phys. Rev. D 106, 083004.
In the binary-driven hypernova (BdHN) scenario, long gamma-ray bursts (GRBs) originate in a cataclysmic event that occurs in a binary system composed of a carbon-oxygen (CO) star and a neutron star (NS) companion in close orbit. The collapse of the CO star generates at its center a newborn NS (νNS), and a supernova (SN) explosion. Matter from the ejecta is accreted both onto the νNS because of fallback and onto the NS companion, leading to the collapse of the latter into a black hole (BH). Each of the ingredients of the above system leads to observable emission episodes in a GRB. In particular, the νNS is expected to show up (hereafter νNS−rise) in the early GRB emission, nearly contemporary or superimposed to the ultrarelativistic prompt emission (UPE) phase, but with a different spectral signature. Following the νNS−rise, the νNS powers the afterglow emission by injecting energy into the expanding ejecta leading to synchrotron radiation. We here show that the νNS−rise and the subsequent afterglow emission in both systems, GRB 180720B and GRB 190114C, are powered by the release of rotational energy of a Maclaurin spheroid, starting from the bifurcation point to the Jacobi ellipsoid sequence. This implies that the νNS evolves from a triaxial Jacobi configuration, prior to the νNS−rise, into the axially symmetric Maclaurin configuration observed in the GRB. The triaxial νNS configuration is short-lived (less than a second) due to a copious emission of gravitational waves, before the GRB emission, and it could be in principle detected for sources located at distances closer than 100 Mpc. This appears to be a specific process of emission of gravitational waves in the BdHN I powering long GRBs.
DOI: https://doi.org/10.1103/PhysRevD.106.083004
L. M. Becerra, R. Moradi, J. A. Rueda, R. Ruffini, and Y. Wang, First minutes of a binary-driven hypernova, published on October 3, 2022 in Phys. Rev. D 106, 083002.
We simulate the first minutes of the evolution of a binary-driven hypernova event, with a special focus on the associated accretion processes of supernova ejecta onto the newborn neutron star (νNS) and the NS companion. We calculate the rotational evolution of the νNS and the NS under the torques exerted by the accreted matter and the magnetic field. We take into account general relativistic effects through effective models for the NSs binding energy and the specific angular momentum transferred by the accreted matter. We use realistic hypercritical accretion rates obtained from three-dimensional smoothed-particle-hydrodynamics numerical simulations of the binary-driven hypernova event for a variety of orbital periods. We show that the rotation power of the νNS has a unique double-peak structure while that of the NS has a single peak. These peaks are of comparable intensity and can occur very close in time or even simultaneously depending on the orbital period and the initial angular momentum of the stars. We outline the consequences of the above features in the early emission and their consequent observation in long gamma-ray bursts.
DOI: https://doi.org/10.1103/PhysRevD.106.083002
Carvalho, G. A.; Anjos, R. C. dos; Coelho, J. G.; Lobato, R. V.; Malheiro, M.; Marinho, R. M.; Rodriguez, J. F.; Rueda, J. A.; Ruffini, R., Orbital Decay of Double White Dwarfs: Beyond Gravitational-wave Radiation Effects, published on November 23, 2022 in ApJ, Vol. 940, n. 1.
The traditional description of the orbital evolution of compact-object binaries, like double white dwarfs (DWDs), assumes that the system is driven only by gravitational-wave (GW) radiation. However, the high magnetic fields with intensities of up to gigagausses measured in WDs alert a potential role of the electromagnetic (EM) emission in the evolution of DWDs. We evaluate the orbital dynamics of DWDs under the effects of GW radiation, tidal synchronization, and EM emission by a unipolar inductor generated by the magnetic primary and the relative motion of the nonmagnetic secondary. We show that the EM emission can affect the orbital dynamics for magnetic fields larger than megagausses. We applied the model to two known DWDs, SDSS J0651+2844 and ZTF J1539+5027, for which the GW radiation alone does not fully account for the measured orbital decay rate. We obtain upper limits to the primary's magnetic field strength, over which the EM emission causes an orbital decay faster than observed. The contribution of tidal locking and the EM emission is comparable, and together they can contribute up to 20% to the measured orbital decay rate. We show that the gravitational waveform for a DWD modeled as purely driven by GWs and including tidal interactions and EM emission can have large relative dephasing detectable in the mHz regime of frequencies relevant for space-based detectors like LISA. Therefore, including physics besides GW radiation in the waveform templates is essential to calibrate the GW detectors using known sources, e.g., ZTF J1539+5027, and to infer binary parameters.
DOI: 10.3847/1538-4357/ac9841
S-S. Xue, W boson mass tension caused by its right-handed gauge coupling at high energies?, published on October 16, 2022 in Nuclear Physics B, Volume 985.
The CDF collaboration's recent high-precision measurement of the W mass is in 7.0σ disagreement with the Standard Model expectation. This tension will be relieved if the W boson has a non-trivial right-handed gauge coupling at high energies. At TeV scales, the SM gauge symmetric four-fermion interactions induce a right-handed gauge coupling, and SM fermions compose massive composite particles. We investigate the top-quark mass produced by spontaneous symmetry breaking and compute the W and Z boson propagators and decays. The right-handed coupling corrections to their masses and widths are consistent with experimental measurements. We discuss how SM gauge bosons and composite particles can restore parity-preserving gauge symmetries at TeV scales.
DOI: https://doi.org/10.1016/j.nuclphysb.2022.115992
N. Sahakyan, D. Israyelyan, G. Harutyunyan, S. Gasparyan, V. Vardanyan, M. Khachatryan, Modelling the time variable spectral energy distribution of the blazar CTA 102 from 2008 to 2022, published on October 2, 2022 in Monthly Notices of the Royal Astronomical Society.
We present long-term multiwavelength observations of blazar CTA 102 (z = 1.037). Detailed temporal and spectral analyses of γ-ray, X-ray, and UV/optical data observed by Fermi-LAT, Swift XRT, NuSTAR, and Swift-UVOT over a period of 14 yr, between 2008 August and 2022 March, were performed. We found strong variability of source emission in all the considered bands; especially in the γ-ray band it exhibited extreme outbursts when the flux crossed the level of 10−5 photon cm−2 s−1. Using the Bayesian Blocks algorithm, we split the adaptively binned γ-ray light curve into 347 intervals of quiescent and flaring episodes and for each period built corresponding multiwavelength spectral energy distributions (SEDs), using the available data. Among the considered SEDs, 117 high-quality (quasi) contemporaneous SEDs, which have sufficient multiwavelength data, were modelled using JETSET framework within a one-zone leptonic synchrotron and inverse-Compton emission scenario assuming the emitting region is within the broad-line region and considering internal and external seed photons for the inverse-Compton up scattering. As a result of modelling, the characteristics of the relativistic electron distribution in the jet as well as jet properties are retrieved and their variation in time is investigated. The applied model can adequately explain the assembled SEDs and the modelling shows that the data in the bright flaring periods can be reproduced for high Doppler boosting and magnetic field. The obtained results are discussed in the context of particle cooling in the emitting region.
DOI: https://doi.org/10.1093/mnras/stac2875
B. Eslam Panah, Two-dimensional Lifshitz-like AdS black holes in F(R) gravity, published on November 2 in the Journal of Mathematical Physics 63, 112502 (2022).
Two-dimensional (2D) Lifshitz-like black holes in special F(R) gravity cases are extracted. We indicate an essential singularity at r = 0, covered by an event horizon. Then, conserved and thermodynamic quantities, such as temperature, mass, entropy, and the heat capacity of 2D Lifshitz-like black holes in F(R) gravity, are evaluated. Our analysis shows that 2D Lifshitz-like black hole solutions can be physical solutions, provided that the cosmological constant is negative (Λ < 0). Indeed, there is a phase transition between stable and unstable cases by increasing the radius of AdS black holes. In other words, the 2D Lifshitz-like AdS black holes with large radii are physical and enjoy thermal stability. The obtained 2D Lifshitz-like AdS-black holes in F(R) gravity turn into the well-known 2D Schwarzschild AdS-black holes when the Lifshitz-like parameter is zero (s = 0). Moreover, correspondence between these black hole solutions and the 2D rotating black hole solutions is found by adjusting the Lifshitz-like parameter.
DOI: https://doi.org/10.1063/5.0104272
A. Bagheri Tudeshki, G. H. Bordbar, and B. Eslam Panah, Dark Energy Star in Gravity's Rainbow, published on October 19 in Physics Letters B. 835, 137523 (2022).
The concept of dark energy can be a candidate for preventing the gravitational collapse of compact objects to singularities. According to the usefulness of gravity's rainbow in UV completion of general relativity (by providing a new description of spacetime), it can be an excellent option to study the behavior of compact objects near phase transition regions. In this work, we obtain a modified Tolman-Openheimer-Volkof (TOV) equation for anisotropic dark energy as a fluid by solving the field equations in gravity's rainbow. Next, to compare the results with general relativity, we use a generalized Tolman-Matese-Whitman mass function to determine the physical quantities such as energy density, radial pressure, transverse pressure, gravity profile, and anisotropy factor of the dark energy star. We evaluate the junction condition and investigate the dynamical stability of dark energy star thin shell in gravity's rainbow. We also study the energy conditions for the interior region of this star. We show that the coefficients of gravity's rainbow can significantly affect this non-singular compact object and modify the model near the phase transition region.
DOI: https://doi.org/10.1016/j.physletb.2022.137523
García, Cristhian; Santa, Camilo; Romano, Antonio Enea, Deep learning reconstruction of the large scale structure of the Universe from luminosity distance, published on October 19, 2022 in Monthly Notices of the Royal Astronomical Society.
Supernovae Ia (SNe) can provide a unique window on the large-scale structure (LSS) of the Universe at redshifts where few other observations are available, by solving the inversion problem (IP) consisting in reconstructing the LSS from its effects on the observed luminosity distance. So far the IP was solved assuming some restrictions about space-time, such as spherical symmetry for example, while we obtain for the first time solutions of the IP problem for arbitrary space-time geometries using deep learning. The method is based on the use of convolutional neural networks (CNN) trained on simulated data. The training data set is obtained by first generating random density and velocity fields, and then computing their effects on the luminosity distance. The CNN, based on an appropriately modified version of U-Net to account for the tridimensionality of the data, is then trained to reconstruct the density and velocity fields from the luminosity distance. We find that the velocity field inversion is more accurate than the density field, because the effects of the velocity on the luminosity distance only depend on the source velocity, while in the case of the density it is an integrated effect along the line of sight, giving rise to more degeneracy in the solution of the IP. Improved versions of these neural networks, modified to accommodate the non-uniform distribution of the SNe, can be applied to observational data to reconstruct the LSS of the Universe at redshifts at which few other observations are available.
DOI: https://doi.org/10.1093/mnras/stac2916
Cadavid, Alexander Gallego; Romano, Antonio Enea; Liddle, Andrew R., Reconstructing homospectral inflationary potentials, published on October 13, 2022 in Phys. Rev. D 106, 083512.
Purely geometrical arguments show that there exist classes of homospectral inflationary cosmologies, i.e., different expansion histories producing the same spectrum of comoving curvature perturbations. We develop a general algorithm to reconstruct the potential of minimally coupled single scalar fields from an arbitrary expansion history. We apply it to homospectral expansion histories to obtain the corresponding potentials, providing numerical and analytical examples. The infinite class of homospectral potentials depends on two free parameters, the initial energy scale and the initial value of the field, showing that, in general, it is impossible to reconstruct a unique potential from the curvature spectrum unless the initial energy scale and the field value are fixed, for instance, through observation of primordial gravitational waves.
DOI: https://doi.org/10.1103/PhysRevD.106.083512