TY - JOUR
T1 - Fast Radio Bursts with Extended Gamma-Ray Emission?
AU - Murase, Kohta
AU - Mészáros, Peter
AU - Fox, Derek B.
N1 - Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/2/10
Y1 - 2017/2/10
N2 - We consider some general implications of bright γ-ray counterparts to fast radio bursts (FRBs). We show that even if these manifest in only a fraction of FRBs, γ-ray detections with current satellites (including Swift) can provide stringent constraints on cosmological FRB models. If the energy is drawn from the magnetic energy of a compact object such as a magnetized neutron star, the sources should be nearby and be very rare. If the intergalactic medium is responsible for the observed dispersion measure, the required γ-ray energy is comparable to that of the early afterglow or extended emission of short γ-ray bursts. While this can be reconciled with the rotation energy of compact objects, as expected in many merger scenarios, the prompt outflow that yields the γ-rays is too dense for radio waves to escape. Highly relativistic winds launched in a precursor phase, and forming a wind bubble, may avoid the scattering and absorption limits and could yield FRB emission. Largely independent of source models, we show that detectable radio afterglow emission from γ-ray bright FRBs can reasonably be anticipated. Gravitational wave searches can also be expected to provide useful tests.
AB - We consider some general implications of bright γ-ray counterparts to fast radio bursts (FRBs). We show that even if these manifest in only a fraction of FRBs, γ-ray detections with current satellites (including Swift) can provide stringent constraints on cosmological FRB models. If the energy is drawn from the magnetic energy of a compact object such as a magnetized neutron star, the sources should be nearby and be very rare. If the intergalactic medium is responsible for the observed dispersion measure, the required γ-ray energy is comparable to that of the early afterglow or extended emission of short γ-ray bursts. While this can be reconciled with the rotation energy of compact objects, as expected in many merger scenarios, the prompt outflow that yields the γ-rays is too dense for radio waves to escape. Highly relativistic winds launched in a precursor phase, and forming a wind bubble, may avoid the scattering and absorption limits and could yield FRB emission. Largely independent of source models, we show that detectable radio afterglow emission from γ-ray bright FRBs can reasonably be anticipated. Gravitational wave searches can also be expected to provide useful tests.
UR - http://www.scopus.com/inward/record.url?scp=85013168477&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85013168477&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/836/1/L6
DO - 10.3847/2041-8213/836/1/L6
M3 - Article
AN - SCOPUS:85013168477
SN - 2041-8205
VL - 836
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L6
ER -