A 450 Day Light Curve of the Radio Afterglow of GRB 970508: Fireball Calorimetry

Frail, D. A.; Waxman, Eli; Kulkarni, S. R.

doi:10.1086/309024

Cited by 271 publications

(394 citation statements)

References 42 publications

(62 reference statements)

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“…We set these parameters as ǫe = ǫB = 0.1. These values are consistent with those evaluated from late radio afterglows in long GRBs (Frail et al 2000(Frail et al , 2005. For our purposes the radio emission is always below the cooling frequency hence the system has only two characteristic frequencies, the synchrotron frequency of the "typical" electron and the self absorption frequency.…”

Section: Ultra-relativistic Beamed Jetsupporting

confidence: 89%

Mass ejection from neutron star mergers: different components and expected radio signals

Hotokezaka

Piran

2015

Monthly Notices of the Royal Astronomical Society

131

137

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In addition to producing a strong gravitational signal, a short gamma-ray burst (GRB), and a compact remnant, neutron star mergers eject significant masses at significant kinetic energies. This mass ejection takes place via dynamical mass ejection and a GRB jet but other processes have also been suggested: a shock-breakout material, a cocoon resulting from the interaction of the jet with other ejecta, and viscous and neutrino driven winds from the central remnant or the accretion disk. The different components of the ejected masses include up to a few percent of a solar mass, some of which is ejected at relativistic velocities. The interaction of these ejecta with the surrounding interstellar medium will produce a long lasting radio flare, in a similar way to GRB afterglows or to radio supernovae. The relative strength of the different signals depends strongly on the viewing angle. An observer along the jet axis or close to it will detect a strong signal at a few dozen days from the radio afterglow (or the orphan radio afterglow) produced by the highly relativistic GRB jet. For a generic observer at larger viewing angles, the dynamical ejecta, whose contribution peaks a year or so after the event, will generally dominate. Depending on the observed frequency and the external density, other components may also give rise to a significant contribution. We also compare these estimates with the radio signature of the short GRB 130603B. The radio flare from the dynamical ejecta might be detectable with the EVLA and the LOFAR for the higher range of external densities n 0.5cm −3 .

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Section: Ultra-relativistic Beamed Jetsupporting

confidence: 89%

Mass ejection from neutron star mergers: different components and expected radio signals

Hotokezaka

Piran

2015

Monthly Notices of the Royal Astronomical Society

131

137

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“…While a transition to nonrelativistic expansion does allow for such a late-time rise in the radio light curve for n n n < < a m (Frail et al 2000), the expected transition to nonrelativistic expansion based on our best-fit model parameters is » t 500 NR days (Waxman et al 1998). One possible explanation for an early transition to nonrelativistic expansion is a late encounter of the blast wave with a density enhancement, which decelerates the outflow rapidly and results in a rebrightening; however, there are no other observations to test this hypothesis.…”

Section: F T 1 3 a Mmentioning

confidence: 99%

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Laskar

Berger

Chornock

et al. 2018

ApJ

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We present the first results from a recently concluded study of GRBs at z  5 with the Karl G. Jansky Very Large Array (VLA). Spanning 1 to 85.5 GHz and 7 epochs from 1.5 to 82.3 days, our observations of GRB140311A are the most detailed joint radio and millimeter observations of a GRB afterglow at z  5 to date. In conjunction with optical/near-IR and X-ray data, the observations can be understood in the framework of radiation from a single blast wave shock with energy »É 8.5 10 K,iso 53 erg expanding into a constant density environment with density, » n 8 0 -cm 3 . The X-ray and radio observations require a jet break at » t 0.6 jet days, yielding an opening angle of q »  4 jet and a beaming-corrected blast wave kinetic energy of »É 2.2 10 K 50 erg. The results from our radio follow-up and multiwavelength modeling lend credence to the hypothesis that detected high-redshift GRBs may be more tightly beamed than events at lower redshift. We do not find compelling evidence for reverse shock emission, which may be related to fast cooling driven by the moderately high circumburst density.

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“…This choice is motivated by observations of late radio afterglows in long GRBs and typical radio supernovae (Chevalier 1998;Frail et al 2000Frail et al , 2005.…”

Section: Synchrotron Radiation Of Expanding Outflowsmentioning

confidence: 99%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

113

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Mergers of binary neutron stars and black hole-neutron star binaries produce gravitational-wave(GW) emission and outflows with significant kinetic energies. These outflows result in radio emissions through synchrotron radiation. We explore the detectability of these synchrotron-generated radio signals by follow-up observations of GW merger events lacking a detection of electromagnetic counterparts in other wavelengths. We model radio light curves arising from (i) sub-relativistic merger ejecta and (ii) ultra-relativistic jets. The former produce radio remnants on timescales of a few years and the latter produce γ-ray bursts in the direction of the jet and orphan-radio afterglows extending over wider angles on timescales of weeks. Based on the derived light curves, we suggest an optimized survey at 1.4 GHz with five epochs separated by a logarithmic time interval. We estimate the detectability of the radio counterparts of simulated GW-merger events to be detected by advanced LIGO and Virgo by current and future radio facilities. The detectable distances for these GW merger events could be as high as 1 Gpc. Around 20%-60% of the long-lasting radio remnants will be detectable in the case of the moderate kinetic energy of 3 10 50 · erg and a circum-merger density of -0.1 cm 3 or larger, while 5%-20% of the orphan-radio afterglows with kinetic energy of 10 48 erg will be detectable. The detection likelihood increases if one focuses on the well-localizable GW events. We discuss the background noise due to radio fluxes of host galaxies and false positives arising from extragalactic radio transients and variable activegalacticnuclei, and we show that the quiet radio transient sky is of great advantage when searching for the radio counterparts.

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A 450 Day Light Curve of the Radio Afterglow of GRB 970508: Fireball Calorimetry

Cited by 271 publications

References 42 publications

Mass ejection from neutron star mergers: different components and expected radio signals

Mass ejection from neutron star mergers: different components and expected radio signals

A VLA Study of High-redshift GRBs. I. Multiwavelength Observations and Modeling of GRB 140311A

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

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