GRB 120711 A：强烈的INTEGRAL爆发，具有持久的柔和gamma-ray发射和强大的光学闪光
GRB 120711A: an intense INTEGRAL burst with long-lasting soft gamma-ray emission and a powerful optical flash
A. Martin-Carrillo, L. Hanlon, M. Topinka, A. P. LaCluyzé, V. Savchenko, D. A. Kann, A. S. Trotter, S. Covino, T. Krühler, J. Greiner, S. McGlynn, D. Murphy, P.… 展开作者
A. Martin-Carrillo, L. Hanlon, M. Topinka, A. P. LaCluyzé, V. Savchenko, D. A. Kann, A. S. Trotter, S. Covino, T. Krühler, J. Greiner, S. McGlynn, D. Murphy, P. Tisdall, S. Meehan, C. Wade, B. McBreen, D. E. Reichart, D. Fugazza, J. B. Haislip, A. Rossi, P. Schady, J. Elliott, S. Klose
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21 pages, 10 figures. Accepted for publication in Astronomy and Astrophysics
A long and intense gamma-ray burst (GRB) was detected by INTEGRAL on July 11 2012 with a duration of ~115s and fluence of 2.8x10^-4 erg cm^-2 in the 20 keV-8 MeV energy range. GRB 120711A was at z~1.405 and produced soft gamma-ray emission (>20 keV) for at least ~10 ks after the trigger. The GRB was observed by several ground-based telescopes that detected a powerful optical flash peaking at an R-band brightness of ~11.5 mag at ~126 s after the trigger. We present a comprehensive temporal and spectral analysis of the long-lasting soft gamma-ray emission detected in the 20-200 keV band with INTEGRAL, the Fermi/LAT post-GRB detection above 100 MeV, the soft X-ray afterglow from XMM-Newton, Chandra, and Swift and the optical/NIR detections from Watcher, Skynet, GROND, and REM. We modelled the long-lasting soft gamma-ray emission using the standard afterglow scenario, which indicates a forward shock origin. The combination of data extending from the NIR to GeV energies suggest that the emission is produced by a broken power-law spectrum consistent with synchrotron radiation. The afterglow is well modelled using a stratified wind-like environment with a density profile k~1.2, suggesting a massive star progenitor (i.e. Wolf-Rayet). The analysis of the reverse and forward shock emission reveals an initial Lorentz factor of ~120-340, a jet half-opening angle of ~2deg-5deg, and a baryon load of ~10^-5-10^-6 Msun consistent with the expectations of the fireball model when the emission is highly relativistic. Long-lasting soft gamma-ray emission from other INTEGRAL GRBs with high peak fluxes, such as GRB 041219A, was not detected, suggesting that a combination of high Lorentz factor, emission above 100 MeV, and possibly a powerful reverse shock are required. Similar long-lasting soft gamma-ray emission has recently been observed from the nearby and extremely bright Fermi/LAT burst GRB 130427A.
Detection horizon for the neutrino burst from the stellar helium flash
Niels Bohr International Academy and DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Max-Planck-Institut für Physik（马克斯·普朗克物理研究所）
Compton scattering in terrestrial gamma-ray flashes detected with the Fermi gamma-ray burst monitor
地面伽玛射线闪光（英语：Terrestrial gamma ray flashes，缩写为TGFs）是一种与雷暴中的闪电活动相关的短时间强烈伽玛射线闪光。使用蒙特卡罗模拟的相对论逃逸电子雪崩（RREA）的过程中，理论预测的时间和光谱演化的TGFs进行了比较与观测的伽马射线暴监视器（GBM）上的费米伽玛射线太空望远镜。假设一个单一的源高度为15公里，模拟数据的比较进行了一系列的经验选择的源电子变化的时间尺度。数据表现出明显的软化源距离的增加，在定性与理论预测一致。模拟光谱在数据中遵循这一趋势，但往往低估了观察到的硬度。这种差异可能意味着基本的RREA模型是不够的。或者，相对于天顶倾斜的TGF光束可以产生与数据兼容的源距离的演变。基于这些结果，我们提出，通过GBM观察到的TGFs的源电子分布在至少几十微秒的时间尺度上变化，上限约为。100微秒
SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features
Tsinghua University（清华大学）；Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学（SOKENDAI））；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）
SN 2019vxm是一颗峰值亮度高、演化缓慢的IIn型超新星，早期光谱显示闪光电离特征，后期红外超表明新尘埃形成，其光变曲线与SN 2010jl相似。
Minutes-long soft X-ray prompt emission from a compact object merger
Beijing Normal University（北京师范大学）；Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；State Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理国家重点实验室）；University of Chinese Academy of Sciences, Chinese Academy of Sciences（中国科学院大学）；Department of Physics, University of Rome "Sapienza"（罗马第一大学物理系）；Department of Physics, University of Rome "Tor Vergata"（罗马第二大学物理系）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）
Long-term optical and near-infrared photometric evolution of SN 2019vxm, an interacting Type IIn supernova
HUN-REN CSFK, Konkoly Observatory（匈牙利科学院研究网络恒星物理研究所孔科伊天文台）；MTA Centre for Excellence（匈牙利科学院卓越中心）；ELTE Eötvös Loránd University, Institute of Physics and Astronomy（厄特沃什·罗兰大学物理与天文学研究所）；MTA–HUN-REN CSFK Lendület “Momentum” Stellar Pulsation Research Group（匈牙利科学院-匈牙利科学院研究网络恒星物理研究所Lendület“动量”恒星脉动研究组）；Department of Experimental Physics, University of Szeged（塞格德大学实验物理系）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体科学系）
Characterising EP241107a: Multiwavelength Observations of an Einstein Probe-detected Fast X-ray Transient
Indian Institute of Astrophysics（印度天体物理研究所）；Department of Physics, Indian Institute of Technology Bombay（孟买印度理工学院物理系）；Cahill Center for Astrophysics, California Institute of Technology（加州理工学院卡希尔天体物理中心）；Department of Physics and Astronomy, University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校物理与天文系）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森尼天体物理中心）
