The multi-messenger picture of compact binary mergers

Rosswog, Stephan

doi:10.1142/s0218271815300128

Cited by 161 publications

(142 citation statements)

References 304 publications

(505 reference statements)

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“…First, the rate of SGRBs (corrected for beaming, as estimated in Fong et al 2012) could be greater than the rate of just binary NS mergers (e.g., Kalogera et al 2004), and we may expect NS-BH mergers to be a significant GW source in the near future (Maselli & Ferrari 2014;Li et al 2016bLi et al , 2016c. Next, NS-BH mergers cannot have BH masses that are too large, otherwise there may not be sufficient material for an accretion disk to power the prompt SGRB emission ( M 8 10   -, Shibata & Taniguchi 2011;Foucart 2012;Rosswog 2015). This affects the production of r-process material from the mergers and the rate of SGRBs needed to produce the observed abundances (for reviews, see Arnould et al 2007;Qian & Wasserburg 2007;Sneden et al 2008;Thielemann et al 2011).…”

Section: Resultsmentioning

confidence: 99%

The Fate of Neutron Star Binary Mergers

Piro

Giacomazzo

Perna

2017

ApJL

100

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Following merger, a neutron star (NS) binary can produce roughly one of three different outcomes: (1) a stable NS, (2) a black hole (BH), or (3) a supramassive, rotationally supported NS, which then collapses to a BH following angular momentum losses. Which of these fates occur and in what proportion has important implications for the electromagnetic transient associated with the mergers and the expected gravitational wave (GW) signatures, which in turn depend on the high density equation of state (EOS). Here we combine relativistic calculations of NS masses using realistic EOSs with Monte Carlo population synthesis based on the mass distribution of NS binaries in our Galaxy to predict the distribution of fates expected. For many EOSs, a significant fraction of the remnants are NSs or supramassive NSs. This lends support to scenarios in which a quickly spinning, highly magnetized NS may be powering an electromagnetic transient. This also indicates that it will be important for future GW observatories to focus on high frequencies to study the post-merger GW emission. Even in cases where individual GW events are too low in signal to noise to study the post merger signature in detail, the statistics of how many mergers produce NSs versus BHs can be compared with our work to constrain the EOS. To match short gamma-ray-burst (SGRB) X-ray afterglow statistics, we find that the stiffest EOSs are ruled out. Furthermore, many popular EOSs require a significant fraction of ∼60%-70% of SGRBs to be from NS-BH mergers rather than just binary NSs.

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Section: Resultsmentioning

confidence: 99%

The Fate of Neutron Star Binary Mergers

Piro

Giacomazzo

Perna

2017

ApJL

100

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“…Thus, the mass ratio has a clear observational imprint on the EM counterparts. 4 Notice that the model of [75] was tested for ejecta masses above 0.01M and that higher uncertainties and errors might be present for low mass ejecta. …”

Section: A Macronovaementioning

confidence: 99%

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the mass ratio

et al. 2017

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We present new (3+1)D numerical relativity simulations of the binary neutron star (BNS) merger and postmerger phase. We focus on a previously inaccessible region of the binary parameter space spanning the binary's mass-ratio q ∼ 1.00 − 1.75 for different total masses and equations of state, and up to q ∼ 2 for a stiff BNS system. We study the mass-ratio effect on the gravitational waves (GWs) and on the possible electromagnetic emission associated to dynamical mass ejecta. We compute waveforms, spectra, and spectrograms of the GW strain including all the multipoles up to l = 4. The mass-ratio has a specific imprint on the GW multipoles in the late-inspiral-merger signal, and it affects qualitatively the spectra of the merger remnant. The multipole effect is also studied by considering the dependency of the GW spectrograms on the source's sky location. Unequal mass BNSs produce more ejecta than equal mass systems with ejecta masses and kinetic energies depending almost linearly on q. We estimate luminosity peaks and light curves of macronovae events associated to the mergers using a simple approach. For q ∼ 2 the luminosity peak is delayed for several days and can be up to four times larger than for the q = 1 cases. The macronova emission associated with the q ∼ 2 BNS is more persistent in time and could be observed for weeks instead of few days (q = 1) in the near infrared. Finally, we estimate the flux of possible radio flares produced by the interaction of relativistic outflows with the surrounding medium. Also in this case a large q can significantly enhance the emission and delay the peak luminosity. Overall, our results indicate that BNS merger with large mass ratio have EM signatures distinct from the equal mass case and more similar to black hole -neutron star binaries.

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“…Within the black hole accretion disk (BHAD) class of models, long-duration bursts are believed to arise from accreting black holes at the center of massive stars, e.g., from collapsars (Woosley 1993) or he-mergers ). Short-duration bursts are believed to be produced by the merger of two compact objects: consisting either of a binary neutron star (NS-NS) or a neutron star and a black hole (BH-NS): for reviews see, for example, Fryer et al (1999), Popham et al (1999), Lee & Ramirez-Ruiz (2007), Berger (2014), Rosswog (2015). These compact mergers are produced in close binaries and the kicks imparted onto these compact remnants cause these systems to have high space velocities.…”

Section: Introductionmentioning

confidence: 99%

The Fate of the Compact Remnant in Neutron Star Mergers

Fryer

Belczyński

Ramírez-Ruiz

et al. 2015

ApJ

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Neutron star (binary neutron star and neutron star-black hole) mergers are believed to produce short-duration gamma-ray bursts (GRBs). They are also believed to be the dominant source of gravitational waves to be detected by the advanced LIGO and advanced VIRGO and the dominant source of the heavy r-process elements in the universe. Whether or not these mergers produce short-duration GRBs depends sensitively on the fate of the core of the remnant (whether, and how quickly, it forms a black hole). In this paper, we combine the results of Newtonian merger calculations and equation of state studies to determine the fate of the cores of neutron star mergers. Using population studies, we can determine the distribution of these fates to compare to observations. We find that black hole cores form quickly only for equations of state that predict maximum non-rotating neutron star masses below 2.3-2.4 solar masses. If quick black hole formation is essential in producing GRBs, LIGO/Virgo observed rates compared to GRB rates could be used to constrain the equation of state for dense nuclear matter.

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The multi-messenger picture of compact binary mergers

Cited by 161 publications

References 304 publications

The Fate of Neutron Star Binary Mergers

The Fate of Neutron Star Binary Mergers

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the mass ratio

The Fate of the Compact Remnant in Neutron Star Mergers

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