The delay time of gravitational wave — gamma-ray burst associations

Zhang, Bing

doi:10.1007/s11467-019-0913-4

Cited by 51 publications

(28 citation statements)

References 95 publications

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“…In the context of GRB170817 our work places strong constraints on the physical origin of the observed γ-ray signals, assuming that the statistical limit on t w found in this work applies also for this specific GRB. We find that the observed delay between the GW and the γ-ray signal is dominated by the time it takes the jet to reach the location at which it will radiate (see also Zhang 2019). The consequence of this interpretation is that the γ-ray duration may naturally (depending on the prompt emission model; see Section 4.6) be of the same order of the observed delay, which is the case for GRB170817.…”

Section: Discussionmentioning

confidence: 60%

Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

Beniamini

Duran

Πετροπούλου

et al. 2020

ApJL

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The joint detection of GW170817/GRB 170817 confirmed the long-standing theory that binary neutron star mergers produce short gamma-ray burst (sGRB) jets that can successfully break out of the surrounding ejecta. At the same time, the association with a kilonova provided unprecedented information regarding the physical properties (such as masses and velocities) of the different ejecta constituents. Combining this knowledge with the observed luminosities and durations of cosmological sGRBs detected by the Burst Alert Telescope onboard the Neil Gehrels Swift Observatory, we revisit the breakout conditions of sGRB jets. Assuming self-collimation of sGRB jets does not play a critical role, we find that the time interval between the binary merger and the launch of a typical sGRB jet is 0.1 s. We also show that for a fraction of at least~30% of sGRBs, the usually adopted assumption of static ejecta is inconsistent with observations, even if the polar ejecta mass is an order of magnitude smaller than that in GRB 170817. Our results disfavor magnetar central engines for powering cosmological sGRBs, limit the amount of energy deposited in the cocoon prior to breakout, and suggest that the observed delay of ∼1.7s in GW170817/GRB 170817 between the gravitational wave and gamma-ray signals is likely dominated by the propagation time of the jet to the gamma-ray production site.Unified Astronomy Thesaurus concepts: Gamma-ray bursts (629); Relativistic jets (1390); Neutron stars (1108); Gravitational wave sources (677); Astrophysical black holes (98)

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Section: Discussionmentioning

confidence: 60%

Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

Beniamini

Duran

Πετροπούλου

et al. 2020

ApJL

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“…The joint electromagnetic and gravitational-wave detection of GW170817-like events with the addition of a NEMO will enable significant further insight into gamma-ray burst physics. For example, the delay time between the collapse and the prompt emission will drive studies into the jet-launching mechanism (e.g., Zhang 2019;Beniamini et al 2020) that is currently ill-understood (Zhang 2018), and the existence and lifetime of the remnant will reveal the impact of neutrino radiation on heavy-element formation through the rapid neutroncapture process in kilonovae (Metzger & Fernández 2014;Martin et al 2015;Fernández et al 2019;Kawaguchi, Shibata, & Tanaka 2020).…”

Section: Other Sciencementioning

confidence: 99%

Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

Ackley

Adya

Agrawal

et al. 2020

Publ. Astron. Soc. Aust.

188

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Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly rotating remnant neutron stars that emit gravitational waves. These will provide clues to the extremely hot post-merger environment. This signature of nuclear matter in gravitational waves contains most information in the 2–4 kHz frequency band, which is outside of the most sensitive band of current detectors. We present the design concept and science case for a Neutron Star Extreme Matter Observatory (NEMO): a gravitational-wave interferometer optimised to study nuclear physics with merging neutron stars. The concept uses high-circulating laser power, quantum squeezing, and a detector topology specifically designed to achieve the high-frequency sensitivity necessary to probe nuclear matter using gravitational waves. Above 1 kHz, the proposed strain sensitivity is comparable to full third-generation detectors at a fraction of the cost. Such sensitivity changes expected event rates for detection of post-merger remnants from approximately one per few decades with two A+ detectors to a few per year and potentially allow for the first gravitational-wave observations of supernovae, isolated neutron stars, and other exotica.

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“…The total intrinsic time delay is expected to be a few seconds (e.g., Zhang 2019), and potentially up to 10 s in extreme scenarios. Separately constraining the different contributions to the intrinsic time delay unveils great insight into these events (e.g., Li et al 2016;Abbott et al 2017b;Zhang 2019). The more precisely we can determine the intrinsic time delay the greater our constraints on fundamental physics.…”

Section: The Time Delay From Merger To Prompt Gamma-ray Burst Emissionmentioning

confidence: 99%

“…Multimessenger observations of GWs and SGRBs provide new information to investigate the viable jet launching mechanisms. In the magnetar case you would expect a longer time delay from the GW-inferred merger time to the on-set of GRBs emission (Zhang 2019). Remnant classification (Sect.…”

Section: Ultrarelativistic Jet Formationmentioning

confidence: 99%

Neutron star mergers and how to study them

Burns

2020

Living Rev Relativ

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Neutron star mergers are the canonical multimessenger events: they have been observed through photons for half a century, gravitational waves since 2017, and are likely to be sources of neutrinos and cosmic rays. Studies of these events enable unique insights into astrophysics, particles in the ultrarelativistic regime, the heavy element enrichment history through cosmic time, cosmology, dense matter, and fundamental physics. Uncovering this science requires vast observational resources, unparalleled coordination, and advancements in theory and simulation, which are constrained by our current understanding of nuclear, atomic, and astroparticle physics. This review begins with a summary of our current knowledge of these events, the expected observational signatures, and estimated detection rates for the next decade. I then present the key observations necessary to advance our understanding of these sources, followed by the broad science this enables. I close with a discussion on the necessary future capabilities to fully utilize these enigmatic sources to understand our universe.

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The delay time of gravitational wave — gamma-ray burst associations

Cited by 51 publications

References 95 publications

Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

Neutron star mergers and how to study them

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