Gamma-Ray Burst Observations by the High-Energy Particle Detector on board the China Seismo-Electromagnetic Satellite between 2019 and 2021

被引：4

作者：

Palma, F. ^{[1
]}

Martucci, M. ^{[1
]}

Neubuser, C. ^{[2
]}

Sotgiu, A. ^{[1
]}

Follega, F. M. ^{[2
,3
]}

Ubertini, P. ^{[4
]}

Bazzano, A. ^{[4
]}

Rodi, J. C. ^{[4
]}

Ammendola, R. ^{[1
]}

Badoni, D. ^{[1
]}

Bartocci, S. ^{[1
]}

Battiston, R. ^{[2
,3
]}

Beole, S. ^{[5
,6
]}

Bertello, I. ^{[4
]}

Burger, W. J. ^{[2
]}

Campana, D. ^{[7
]}

Cicone, A. ^{[8
]}

Cipollone, P. ^{[1
]}

Coli, S. ^{[6
]}

Conti, L. ^{[1
,9
]}

Contin, A. ^{[10
,11
]}

Cristoforetti, M. ^{[2
,12
]}

D'Angelo, G. ^{[4
]}

De Angelis, F. ^{[4
]}

De Donato, C. ^{[1
]}

De Santis, C. ^{[1
]}

Diego, P. ^{[4
]}

Di Luca, A. ^{[2
,12
]}

Fiorenza, E. ^{[4
]}

Gebbia, G. ^{[2
,3
]}

Iuppa, R. ^{[2
,3
]}

Lega, A. ^{[2
,3
]}

Lolli, M. ^{[11
]}

Martino, B. ^{[13
]}

Masciantonio, G. ^{[1
]}

Merge, M. ^{[1
,14
]}

Mese, M. ^{[7
,15
]}

Morbidini, A. ^{[4
]}

Nozzoli, F. ^{[2
]}

Nuccilli, F. ^{[4
]}

Oliva, A. ^{[11
]}

Osteria, G. ^{[7
]}

Palmonari, F. ^{[10
,11
]}

Panico, B. ^{[7
,15
]}

Papini, E. ^{[4
]}

Parmentier, A. ^{[4
]}

Perciballi, S. ^{[5
,6
]}

Perfetto, F. ^{[7
]}

Perinelli, A. ^{[2
,3
]}

Picozza, P. ^{[1
,16
]}

机构：

[1] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy

[2] Ist Nazl Fis Nucl, TIFPA, Via Sommar 14, I-38123 Povo, Trento, Italy

[3] Univ Trento, Via Sommar 14, I-38123 Povo, Trento, Italy

[4] INAF IAPS, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[5] Univ Torino, Via P Giuria 1, I-10125 Turin, Italy

[6] Ist Nazl Fis Nucl, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy

[7] Ist Nazl Fis Nucl, Sez Napoli, Via Cintia, I-80126 Naples, Italy

[8] Univ Aquila, Via Vetoio, I-67100 Laquila, Italy

[9] Uninettuno Univ, Corso V Emanuele II 39, I-00186 Rome, Italy

[10] Univ Bologna, Viale Berti Pichat 6-2, Bologna, Italy

[11] Ist Nazl Fis Nucl, Sez Bologna, Viale Berti Pichat 6-2, Bologna, Italy

[12] Fdn Bruno Kessler, Via Sommar 18, I-38123 Povo, Trento, Italy

[13] CNR, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[14] Italian Space Agcy, Via Politecn, I-00133 Rome, Italy

[15] Univ Napoli Federico II, Via Cintia, I-80126 Naples, Italy

[16] Univ Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy

[17] Ist Nazl Fis Nucl, LNF, VE Fermi 54, I-00044 Rome, Italy

[18] CNR, IFAC, Via Madonna del Piano 10, I-50019 Florence, Italy

[19] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China

[20] Minist Emergency Management China, Natl Inst Nat Hazards, Beijing 100085, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2024年 / 960卷 / 01期

关键词：

CSES-01; SATELLITE; GRB; 190114C; GIANT FLARE; ERROR BOX; EMISSION; PROMPT; IDENTIFICATION; SUPERNOVA; SPECTRA; PROTONS;

D O I：

10.3847/1538-4357/ad06ae

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this paper we report the detection of five strong gamma-ray bursts (GRBs) by the High-Energy Particle Detector (HEPD-01) mounted on board the China Seismo-Electromagnetic Satellite, operational since 2018 on a Sun-synchronous polar orbit at a similar to 507 km altitude and 97 degrees inclination. HEPD-01 was designed to detect high-energy electrons in the energy range 3-100 MeV, protons in the range 30-300 MeV, and light nuclei in the range 30-300 MeV n(-1). Nonetheless, Monte Carlo simulations have shown HEPD-01 is sensitive to gamma-ray photons in the energy range 300 keV-50 MeV, even if with a moderate effective area above similar to 5 MeV. A dedicated time correlation analysis between GRBs reported in literature and signals from a set of HEPD-01 trigger configuration masks has confirmed the anticipated detector sensitivity to high-energy photons. A comparison between the simultaneous time profiles of HEPD-01 electron fluxes and photons from GRB190114C, GRB190305A, GRB190928A, GRB200826B, and GRB211211A has shown a remarkable similarity, in spite of the different energy ranges. The high-energy response, with peak sensitivity at about 2 MeV, and moderate effective area of the detector in the actual flight configuration explain why these five GRBs, characterized by a fluence above similar to 3 x 10(-5) erg cm(-2) in the energy interval 300 keV-50 MeV, have been detected.

引用

页数：8

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