Accurate Calorimetry of GRB 030329

Frail, D. A.; Söderberg, A. M.; Kulkarni, S. R.; Berger, E.; Yost, S. A.; Fox, D. B.; Harrison, F.

doi:10.1086/426680

Cited by 98 publications

(134 citation statements)

References 28 publications

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“…Energy considerations show that both the electrons and the magnetic field carry significant fractions of the total internal energy of the shocked gas, e ≈ B ∼ 0.1 . These values are consistent with those inferred from late radio afterglows of long GRBs (e.g., Frail et al 2000Frail et al , 2005. The observed spectra indicate that the distribution of the accelerated electrons Lorentz factor, γ, is a power-law dN/dγ ∝ γ −p at γ > γ m where p ≈ 2.1 − 2.5 in mildly relativistic shocks (e.g., the radio emission from GRB associated SNe and late GRB afterglows) and p ≈ 2.5 − 3 in Newtonian shocks (as seen in typical radio SNe; Chevalier 1998, and references therein).…”

Section: The Radio Signal From Outflow-ism Interactionsupporting

confidence: 90%

Detectable radio flares following gravitational waves from mergers of binary neutron stars

Nakar

Piran

2011

Nature

393

484

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The question "what is the observable electromagnetic (EM) signature of a compact binary merger?" is an intriguing one with crucial consequences to the quest for gravitational waves (GW). Compact binary mergers are prime sources of GW, targeted by current and next generation detectors. Numerical simulations have demonstrated that these mergers eject energetic sub-relativistic (or even relativistic) outflows. This is certainly the case if the mergers produce short GRBs, but even if not, significant outflows are expected. The interaction of such outflows with the surround matter inevitably leads to a long lasting radio signal. We calculate the expected signal from these outflows (our calculations are also applicable to short GRB orphan afterglows) and we discuss their detectability. We show that the optimal search for such signal should, conveniently, take place around 1.4 GHz. Realistic estimates of the outflow parameters yield signals of a few hundred µJy, lasting a few weeks, from sources at the detection horizon of advanced GW detectors. Followup radio observations, triggered by GW detection, could reveal the radio remnant even under unfavorable conditions. Upcoming all sky surveys can detect a few dozen, and possibly even thousands, merger remnants at any give time, thereby providing robust merger rate estimates even before the advanced GW detectors become operational. In fact, the radio transient RT 19870422 fits well the overall properties predicted by our model and we suggest that its most probable origin is a compact binary merger radio remnant.

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Section: The Radio Signal From Outflow-ism Interactionsupporting

confidence: 90%

Detectable radio flares following gravitational waves from mergers of binary neutron stars

Nakar

Piran

2011

Nature

393

484

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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

132

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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“…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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Accurate Calorimetry of GRB 030329

Cited by 98 publications

References 28 publications

Detectable radio flares following gravitational waves from mergers of binary neutron stars

Detectable radio flares following gravitational waves from mergers of binary neutron stars

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

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

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