Gamma-ray bursts as the death throes of massive binary stars

Narayan, Ramesh; Paczyński, B.; Piran, Tsvi

doi:10.1086/186493

Cited by 1,412 publications

(1,387 citation statements)

References 23 publications

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“…Some massive stars are also known to exist very far from apparent star forming regions (e.g., Smith, Andrews, & Mauerhan 2016). It is also interesting to note that white dwarf mergers may actually end up as core-collapse SNe and could lead to SNe with similar properties to our ultra-stripped SNe (e.g., Nomoto & Iben 1985;Schwab, Quataert, & Kasen 2016). As we suggest here, Carich gap transients can have different origin.…”

Section: Ca-rich Gap Transients (Ptf10iuv and Sn 2005e)mentioning

confidence: 79%

“…Therefore, ultra-stripped SNe are related to sources of gravitational waves detected by LIGO (e.g., Abadie et al 2010). In addition, double NS systems which merge are suggested to cause short gamma-ray bursts (Blinnikov et al 1984;Paczynski 1986;Narayan, Paczynski, & Piran 1992) and r-process element nucleosynthesis (e.g., Rosswog et al Figure 1. Evolution of the central density and temperature of our ultra-stripped SN progenitor obtained with MESA.…”

Section: Introductionmentioning

confidence: 99%

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Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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Section: Ca-rich Gap Transients (Ptf10iuv and Sn 2005e)mentioning

confidence: 79%

Section: Introductionmentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

105

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“…We also do not rule out the possibility of a gamma-ray burst whose electromagnetic radiation is concentrated in a narrow jet (Eichler et al 1989;Narayan, Paczynski & Piran 1992), which is very unlikely to be detected during the GW event due to the low probability that it is beamed towards the Earth.…”

Section: Introductionmentioning

confidence: 94%

First gravitational-wave burst GW150914: MASTER optical follow-up observations

Липунов

Kornilov

Gorbovskoy

et al. 2016

Mon. Not. R. Astron. Soc.

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The Advanced LIGO observatory recently reported the first direct detection of gravitational waves predicted by Einstein (1916). We report on the first optical observations of the Gravitational Wave (GW) source GW150914 error region with the Global MASTER Robotic Net. We detected several optical transients, which proved to be unconnected with the GW event. Our result is consistent with the assumption that gravitational waves were produced by a binary black hole merger. The detection of the event confirmed the main prediction of the population synthesis performed with the "Scenario Machine" formulated in Lipunov1997b.

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“…Accretion onto the black hole then powers a relativistic transient, a short-duration gamma-ray burst (GRB; Narayan et al 1992;Ruffert & Janka 1999;Aloy et al 2005;Rezzolla et al 2011;Berger et al 2013;Tanvir et al 2013;Berger 2014;Ruiz et al 2016), with a prompt gamma-ray emission duration of  2 s. One of the biggest uncertainties in this canonical picture is how long the NS remnant survives prior to collapse. This depends on the mass of the final remnant and the highly uncertain Equation of State (EOS) of dense nuclear matter Lasky et al 2014;Fryer et al 2015;Lawrence et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Fong

Metzger

Berger

et al. 2016

ApJ

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The merger of a neutron star (NS) binary may result in the formation of a rapidly spinning magnetar. The magnetar can potentially survive for seconds or longer as a supramassive NS before collapsing to a black hole if, indeed, it collapses at all. During this process, a fraction of the magnetar's rotational energy of ∼10 53 erg is transferred via magnetic spin-down to the surrounding ejecta. The resulting interaction between the ejecta and the surrounding circumburst medium powers a year-long or greater synchrotron radio transient. We present a search for radio emission with the Very Large Array following nine short-duration gamma-ray bursts (GRBs) at rest-frame times of ≈1.3-7.6 yr after the bursts, focusing on those events that exhibit early-time excess X-ray emission that may signify the presence of magnetars. We place upper limits of 18-32 μJy on the 6.0 GHz radio emission, corresponding to spectral luminosities of (0.05-8.3)×10 39 erg s −1 . Comparing these limits to the predicted radio emission from a long-lived remnant and incorporating measurements of the circumburst densities from broadband modeling of short GRB afterglows, we rule out a stable magnetar with an energy of 10 53 erg for half of the events in our sample. A supramassive remnant that injects a lower rotational energy of 10 52 erg is ruled out for a single event, GRB 050724A. This study represents the deepest and most extensive search for long-term radio emission following short GRBs to date, and thus the most stringent limits placed on the physical properties of magnetars associated with short GRBs from radio observations.

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Gamma-ray bursts as the death throes of massive binary stars

Cited by 1,412 publications

References 23 publications

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

First gravitational-wave burst GW150914: MASTER optical follow-up observations

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

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