2013ApJ...762L..18G


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST19:35:29

2013ApJ...762L..18G - Astrophys. J., 762, L18 (2013/January-2)

Compact binary progenitors of short gamma-ray bursts.

GIACOMAZZO B., PERNA R., REZZOLLA L., TROJA E. and LAZZATI D.

Abstract (from CDS):

In recent years, detailed observations and accurate numerical simulations have provided support to the idea that mergers of compact binaries containing either two neutron stars (NSs) or an NS and a black hole (BH) may constitute the central engine of short gamma-ray bursts (SGRBs). The merger of such compact binaries is expected to lead to the production of a spinning BH surrounded by an accreting torus. Several mechanisms can extract energy from this system and power the SGRBs. Here we connect observations and numerical simulations of compact binary mergers, and use the current sample of SGRBs with measured energies to constrain the mass of their powering tori. By comparing the masses of the tori with the results of fully general-relativistic simulations, we are able to infer the properties of the binary progenitors that yield SGRBs. By assuming a constant efficiency in converting torus mass into jet energy, εjet= 10%, we find that most of the tori have masses smaller than 0.01 M, favoring "high-mass" binary NSs mergers, i.e., binaries with total masses ≳ 1.5 the maximum mass of an isolated NS. This has important consequences for the gravitational wave signals that may be detected in association with SGRBs, since "high-mass" systems do not form a long-lived hypermassive NS after the merger. While NS-BH systems cannot be excluded to be the engine of at least some of the SGRBs, the BH would need to have an initial spin of ∼0.9 or higher.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - gamma-ray burst: general - gravitational waves - methods: numerical - stars: neutron

Simbad objects: 24

goto Full paper

goto View the reference in ADS

Number of rows : 24

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 GRB 100117A gB 00 45 04.56 -01 35 41.7           ~ 97 0
2 GRB 111117A gB 00 50 46.220 +23 00 39.22           ~ 74 0
3 GRB 070724A gB 01 51 14.08 -18 35 38.8           ~ 133 0
4 GRB 070729 gB 03 45 16.04 -39 19 19.9           ~ 52 0
5 GRB 070714B gB 03 51 22.30 +28 17 51.3           ~ 159 1
6 GRB 071227 gB 03 52 31.09 -55 59 03.3           ~ 136 0
7 GRB 101219A gB 04 58 20.43 -02 32 23.0           ~ 91 0
8 GRB 061006 gB 07 24 07.660 -79 11 55.10           ~ 153 1
9 GRB 061210 gB 09 38 05.270 +15 37 17.30           ~ 108 0
10 GRB 061217 gB 10 41 39.320 -21 07 22.11           ~ 100 0
11 GRB 090515 gB 10 56 41.0 +14 27 22           ~ 75 0
12 GRB 050509B gB 12 36 18.000 +29 01 24.00           ~ 268 1
13 GRB 070809 gB 13 35 04.2 -22 07 07           ~ 96 0
14 GRB 060801 gB 14 12 01.290 +16 58 54.00           ~ 129 0
15 GRB 050724 gB 16 24 44.400 -27 32 27.90     19.70     ~ 367 1
16 GRB 060502B gB 18 35 46.060 +52 37 51.45           ~ 113 1
17 GRB 080905A gB 19 10 39.10 -18 51 55.4           ~ 124 0
18 GRB 070429B gB 21 52 03.820 -38 49 42.20           ~ 86 0
19 GRB 051221 gB 21 54 48.626 +16 53 27.16 19.49         ~ 292 1
20 GRB 051210 gB 22 00 40.930 -57 36 47.10           ~ 105 0
21 GRB 061201 gB 22 08 32.060 -74 34 47.90           ~ 145 0
22 GRB 090510 gB 22 14 12.60 -26 35 51.1           ~ 385 1
23 GRB 080123 gB 22 35 46.100 -64 54 03.24           ~ 65 0
24 GRB 050709 gB 23 01 26.960 -38 58 39.50           ~ 245 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2013ApJ...762L..18G and select 'bookmark this link' or equivalent in the popup menu


2019.10.20-19:35:29

© Université de Strasbourg/CNRS

    • Contact