Could an X-ray flare after GRB 170817A originate from a post-merger slim accretion disc?
Could an X-ray flare after GRB 170817A originate from a post-merger slim accretion disc?
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GRB 170817A 之后的 X 射线耀斑是否源自合并后的细长吸积盘？
DOI：
10.1093/mnras/stz840
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发表时间：
2019-03
影响因子：
4.8
通讯作者：
Gu Wei Min
中科院分区：
文献类型：
--
作者：
Lin Yi Qing;Dai Zi Gao;Gu Wei Min
GRB 170817A, detected by Fermi-GBM 1.7\,s after the merger of a neutron star (NS) binary, provides the first direct evidence for a link between such a merger and a short-duration gamma-ray burst. The X-ray observations after GRB 170817A indicate a possible X-ray flare with a peak luminosity $L_{\rm peak} \sim 2\times 10^{39}\,{\rm erg\,s}^{-1}$ near day 156. Here we show that this X-ray flare may be understood based on a slim disc around a compact object. On the one hand, there exists the maximal accretion rate $\dot M_{\rm max}$ for the slim disc, above which an optically thick outflow is significant and radiation from the disc is obscured. Based on the energy balance analysis, we find that $\dot M_{\rm max}$ is in the range of $\sim 4\dot M_{\rm Edd}$ and $\sim 21\dot M_{\rm Edd}$ when the angular velocity of the slim disc is between $\rm (1/5)^{1/2}\Omega_K$ and $\rm \Omega_K$ (where $\dot M_{\rm Edd}$ is the Eddington accretion rate and $\Omega_K$ is the Keplerian angular velocity). With $\dot M_{\rm max}$, the slim disc can provide a luminosity $\sim L_{\rm peak}$ for a compact object of $2.5 M_{\sun}$. On the other hand, if the merger of two NSs forms a typical neutrino-dominated accretion disc whose accretion rate $\dot M$ follows a power-law decline with an index $-1.8$ , then the system must pass through the outflow regime and enter the slim disc in $\sim 11-355$ days. These results imply that a post-merger slim accretion disc could account for the observed late-time $L_{\rm peak}$.
GRB 170817A, detected by Fermi-GBM 1.7\,s after the merger of a neutron star (NS) binary, provides the first direct evidence for a link between such a merger and a short-duration gamma-ray burst. The X-ray observations after GRB 170817A indicate a possible X-ray flare with a peak luminosity $L_{\rm peak} \sim 2\times 10^{39}\,{\rm erg\,s}^{-1}$ near day 156. Here we show that this X-ray flare may be understood based on a slim disc around a compact object. On the one hand, there exists the maximal accretion rate $\dot M_{\rm max}$ for the slim disc, above which an optically thick outflow is significant and radiation from the disc is obscured. Based on the energy balance analysis, we find that $\dot M_{\rm max}$ is in the range of $\sim 4\dot M_{\rm Edd}$ and $\sim 21\dot M_{\rm Edd}$ when the angular velocity of the slim disc is between $\rm (1/5)^{1/2}\Omega_K$ and $\rm \Omega_K$ (where $\dot M_{\rm Edd}$ is the Eddington accretion rate and $\Omega_K$ is the Keplerian angular velocity). With $\dot M_{\rm max}$, the slim disc can provide a luminosity $\sim L_{\rm peak}$ for a compact object of $2.5 M_{\sun}$. On the other hand, if the merger of two NSs forms a typical neutrino-dominated accretion disc whose accretion rate $\dot M$ follows a power-law decline with an index $-1.8$ , then the system must pass through the outflow regime and enter the slim disc in $\sim 11-355$ days. These results imply that a post-merger slim accretion disc could account for the observed late-time $L_{\rm peak}$.
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DOI：
10.1088/0004-637x/693/1/670
发表时间：
2008-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Cheng-Liang Jiao;L. Xue;Weimin Gu;Ju-fu Lu
通讯作者：
Cheng-Liang Jiao;L. Xue;Weimin Gu;Ju-fu Lu
DOI：
10.3847/1538-4357/aabaec
发表时间：
2017-11
期刊：
The Astrophysical Journal
影响因子：
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作者：
D. Siegel;B. Metzger
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D. Siegel;B. Metzger
DOI：
10.1086/500655
发表时间：
2005-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Falcone;D. Burrows;D. Lazzati;S. Campana;S. Kobayashi;Bing Zhang;P. Mészáros;K. Page;J. Ken
通讯作者：
A. Falcone;D. Burrows;D. Lazzati;S. Campana;S. Kobayashi;Bing Zhang;P. Mészáros;K. Page;J. Ken
影响因子：
56.9
作者：
M. Kasliwal;E. Nakar;L. Singer;D. Kaplan;D. Cook;A. Van Sistine;R. Lau;C. Fremling;O. Gottlieb;J. Jencson;S. Adams;U. Feindt;K. Hotokezaka;S. Ghosh;D. Perley;P. Yu;T. Piran;J. Allison;G. Anupama;A. Balasubramanian;K. Bannister;J. Bally;J. Barnes;S. Barway;E. Bellm;V. Bhalerao;D. Bhattacharya;N. Blagorodnova;J. Bloom;P. Brady;C. Cannella;D. Chatterjee;S. Cenko;B. Cobb;C. Copperwheat;A. Corsi;K. De;D. Dobie;S. Emery;P. Evans;O. Fox;D. Frail;C. Frohmaier;A. Goobar;G. Hallinan;F. Harrison;G. Helou;T. Hinderer;A. Ho;A. Horesh;W. Ip;R. Itoh;D. Kasen;H. Kim;N. Kuin;T. Kupfer;C. Lynch;K. Madsen;P. Mazzali;A. Miller;K. Mooley;T. Murphy;C. Ngeow;D. Nichols;S. Nissanke;P. Nugent;E. Ofek;H. Qi;R. Quimby;S. Rosswog;Florin Rusu;E. Sadler;P. Schmidt;J. Sollerman;I. Steele;A. Williamson;Y. Xu;L. Yan;Y. Yatsu;C. Zhang;W. Zhao
通讯作者：
M. Kasliwal;E. Nakar;L. Singer;D. Kaplan;D. Cook;A. Van Sistine;R. Lau;C. Fremling;O. Gottlieb;J. Jencson;S. Adams;U. Feindt;K. Hotokezaka;S. Ghosh;D. Perley;P. Yu;T. Piran;J. Allison;G. Anupama;A. Balasubramanian;K. Bannister;J. Bally;J. Barnes;S. Barway;E. Bellm;V. Bhalerao;D. Bhattacharya;N. Blagorodnova;J. Bloom;P. Brady;C. Cannella;D. Chatterjee;S. Cenko;B. Cobb;C. Copperwheat;A. Corsi;K. De;D. Dobie;S. Emery;P. Evans;O. Fox;D. Frail;C. Frohmaier;A. Goobar;G. Hallinan;F. Harrison;G. Helou;T. Hinderer;A. Ho;A. Horesh;W. Ip;R. Itoh;D. Kasen;H. Kim;N. Kuin;T. Kupfer;C. Lynch;K. Madsen;P. Mazzali;A. Miller;K. Mooley;T. Murphy;C. Ngeow;D. Nichols;S. Nissanke;P. Nugent;E. Ofek;H. Qi;R. Quimby;S. Rosswog;Florin Rusu;E. Sadler;P. Schmidt;J. Sollerman;I. Steele;A. Williamson;Y. Xu;L. Yan;Y. Yatsu;C. Zhang;W. Zhao
DOI：
10.1086/500723
发表时间：
2005-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Bing Zhang;Yizhong Fan;Yizhong Fan;J. Dyks;S. Kobayashi;S. Kobayashi;P. Mészáros;D. Burrows
通讯作者：
Bing Zhang;Yizhong Fan;Yizhong Fan;J. Dyks;S. Kobayashi;S. Kobayashi;P. Mészáros;D. Burrows