Mergers of black hole-neutron star binaries and rates of associated electromagnetic counterparts

被引:20
作者
Bhattacharya, Mukul [1 ]
Kumar, Pawan [2 ]
Smoot, George [3 ,4 ,5 ,6 ,7 ,8 ]
机构
[1] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA
[2] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA
[3] Hong Kong Univ Sci & Technol, Inst Adv Study, Kowloon, Clear Water Bay, Hong Kong 999077, Peoples R China
[4] Univ Sorbonne Paris Cite, Univ Paris Diderot, PCCP, F-75013 Paris, France
[5] Univ Sorbonne Paris Cite, Univ Paris Diderot, APC, F-75013 Paris, France
[6] Univ Calif Berkeley, BCCP, Berkeley, CA 94720 USA
[7] Univ Calif Berkeley, LBNL, Berkeley, CA 94720 USA
[8] Univ Calif Berkeley, Phys Dept, Berkeley, CA 94720 USA
关键词
accretion; accretion discs; equation of state; gravitational waves; gamma-ray burst: general; stars: neutron; GAMMA-RAY BURSTS; DISC WIND; ACCRETION; EVOLUTION; OUTFLOWS;
D O I
10.1093/mnras/stz1147
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Black hole-neutron star (BHNS) binaries are amongst promising candidates for the joint detection of electromagnetic (EM) signals with gravitational waves (GWs) and arc expected to be detected in the near future. Here we study the effect of the BHNS binary parameters on the merger ejecta properties and associated EM signals. We estimate the remnant disc and unbound ejecta masses for BH mass and spin distributions motivated from the observations of transient low-mass X-ray binaries and a specific NS equation of slate (EoS). The amount of r-process elements synthesized in BHNS mergers is estimated to be a factor of-102-104 smaller than BNS mergers, due to the smaller dynamical ejecta and merger rates for the former. We compute the EM luminosities and light curves for the early- and late-time emissions from the ultrarelativistic jet, sub-relativistic dynamical ejecta and wind, and the mildly relativistic cocoon for typical ejecta parameters. We then evaluate the low-latency EM follow-up rates of the CiW triggers in terms of the GW detection rate iVciw for current telescope sensitivities and typical BUNS binary parameters to rind that most of the EM counterparts are detectable for high BH spin, small Bll mass, and a stiffer NS EoS when NS disruption is significant. Based on the relative detection rates for given binary parameters, we rind the ease of EM follow-up to be: ejecta afterglow > cocoon afterglow greater than or similar to jet prompt > ejecta macronova > cocoon prompt > jet afterglow >> wind macronova >> wind afterglow.
引用
收藏
页码:5289 / 5309
页数:21
相关论文
共 94 条
[1]   Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors [J].
Abadie, J. ;
Abbott, B. P. ;
Abbott, R. ;
Abernathy, M. ;
Accadia, T. ;
Acerneseac, F. ;
Adams, C. ;
Adhikari, R. ;
Ajith, P. ;
Allen, B. ;
Allen, G. ;
Ceron, E. Amador ;
Amin, R. S. ;
Anderson, S. B. ;
Anderson, W. G. ;
Antonuccia, F. ;
Aoudiaa, S. ;
Arain, M. A. ;
Araya, M. ;
Aronsson, M. ;
Arun, K. G. ;
Aso, Y. ;
Aston, S. ;
Astonea, P. ;
Atkinson, D. E. ;
Aufmuth, P. ;
Aulbert, C. ;
Babak, S. ;
Baker, P. ;
Ballardin, G. ;
Ballmer, S. ;
Barker, D. ;
Barnum, S. ;
Baroneac, F. ;
Barr, B. ;
Barriga, P. ;
Barsotti, L. ;
Barsuglia, M. ;
Barton, M. A. ;
Bartos, I. ;
Bassiri, R. ;
Bastarrika, M. ;
Bauchrowitz, J. ;
Bauera, Th S. ;
Behnke, B. ;
Beker, M. G. ;
Benacquista, M. ;
Bertolini, A. ;
Betzwieser, J. ;
Beveridge, N. .
CLASSICAL AND QUANTUM GRAVITY, 2010, 27 (17)
[2]   GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral [J].
Abbott, B. P. ;
Abbott, R. ;
Abbott, T. D. ;
Acernese, F. ;
Ackley, K. ;
Adams, C. ;
Adams, T. ;
Addesso, P. ;
Adhikari, R. X. ;
Adya, V. B. ;
Affeldt, C. ;
Afrough, M. ;
Agarwal, B. ;
Agathos, M. ;
Agatsuma, K. ;
Aggarwal, N. ;
Aguiar, O. D. ;
Aiello, L. ;
Ain, A. ;
Ajith, P. ;
Allen, B. ;
Allen, G. ;
Allocca, A. ;
Altin, P. A. ;
Amato, A. ;
Ananyeva, A. ;
Anderson, S. B. ;
Anderson, W. G. ;
Angelova, S. V. ;
Antier, S. ;
Appert, S. ;
Arai, K. ;
Araya, M. C. ;
Areeda, J. S. ;
Arnaud, N. ;
Arun, K. G. ;
Ascenzi, S. ;
Ashton, G. ;
Ast, M. ;
Aston, S. M. ;
Astone, P. ;
Atallah, D. V. ;
Aufmuth, P. ;
Aulbert, C. ;
AultONeal, K. ;
Austin, C. ;
Avila-Alvarez, A. ;
Babak, S. ;
Bacon, P. ;
Bader, M. K. M. .
PHYSICAL REVIEW LETTERS, 2017, 119 (16)
[3]  
Abbott B. P., ApJ, V848, pL12
[4]   Advanced Virgo: a second-generation interferometric gravitational wave detector [J].
Acernese, F. ;
Agathos, M. ;
Agatsuma, K. ;
Aisa, D. ;
Allemandou, N. ;
Allocca, A. ;
Amarni, J. ;
Astone, P. ;
Balestri, G. ;
Ballardin, G. ;
Barone, F. ;
Baronick, J-P ;
Barsuglia, M. ;
Basti, A. ;
Basti, F. ;
Bauer, Th S. ;
Bavigadda, V. ;
Bejger, M. ;
Beker, M. G. ;
Belczynski, C. ;
Bersanetti, D. ;
Bertolini, A. ;
Bitossi, M. ;
Bizouard, M. A. ;
Bloemen, S. ;
Blom, M. ;
Boer, M. ;
Bogaert, G. ;
Bondi, D. ;
Bondu, F. ;
Bonelli, L. ;
Bonnand, R. ;
Boschi, V. ;
Bosi, L. ;
Bouedo, T. ;
Bradaschia, C. ;
Branchesi, M. ;
Briant, T. ;
Brillet, A. ;
Brisson, V. ;
Bulik, T. ;
Bulten, H. J. ;
Buskulic, D. ;
Buy, C. ;
Cagnoli, G. ;
Calloni, E. ;
Campeggi, C. ;
Canuel, B. ;
Carbognani, F. ;
Cavalier, F. .
CLASSICAL AND QUANTUM GRAVITY, 2015, 32 (02)
[5]   The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VI. Radio Constraints on a Relativistic Jet and Predictions for Late-time Emission from the Kilonova Ejecta [J].
Alexander, K. D. ;
Berger, E. ;
Fong, W. ;
Williams, P. K. G. ;
Guidorzi, C. ;
Margutti, R. ;
Metzger, B. D. ;
Annis, J. ;
Blanchard, P. K. ;
Brout, D. ;
Brown, D. A. ;
Chen, H. -Y. ;
Chornock, R. ;
Cowperthwaite, P. S. ;
Drout, M. ;
Eftekhari, T. ;
Frieman, J. ;
Holz, D. E. ;
Nicholl, M. ;
Rest, A. ;
Sako, M. ;
Soares-Santos, M. ;
Viliar, V. A. .
ASTROPHYSICAL JOURNAL LETTERS, 2017, 848 (02)
[6]  
[Anonymous], APJ
[7]  
[Anonymous], 2016, ASTROPHYS J, DOI DOI 10.3847/0004-637X/825/2/128
[8]  
[Anonymous], ARXIV190304543
[9]  
[Anonymous], 2011, ASTROPHYS J, DOI DOI 10.1088/0004-637X/727/1/20
[10]  
[Anonymous], 6 MICR WORKSH MICR S