Query : 1998A&A...340..447M

1998A&A...340..447M - Astronomy and Astrophysics, volume 340, 447-456 (1998/12-2)

On the true energy budget of GRB 970508 and GRB 971214.


Abstract (from CDS):

We emphasize the already known idea that since GRB970508 released an energy of Qγ≃1051δΩergs in soft gamma rays alone, where δΩ is the solid angle of the beam, the actual energy of the e+e p fireball driving the blast wave could be considerably higher than this value, QFB>Qγ. We further argue that, for reasonably large values of δΩ, as is probably suggested by the radio observations, the value of QFB∼5x1051tm3n1erg, for GRB 970508; where n1 is the number density of the ambient medium in units of 1 proton/cm3 and tm is the epoch in months when the associated radio-blastwave degrades to become mildly relativistic. Thus the value of QFB for GRB 970508 could be as large as 1053erg or even much higher. This idea is corroborated by GRB 971214 for which the value of Qγ≃2x1052δΩ is much higher than the corresponding value for GRB 970508. It is likely that GRB971214 has a correspondingly higher value of QFB. We discuss that it is unlikely that this energy, QFB∼1053erg was liberated by the central engine by a direct electromagnetic mode. On the other hand, as conceived by several previous authors and as is suggested by supernova theories, the e+e p fireball (FB) driving the blast wave is likely to be preceded by a much stronger neutrino burst: ν+ν ->e+ +e. Although, the efficiency for e+ e production by this latter route is usually found to be as low as η±∼10–3, we point out that for very high values of neutrino energy release Qν>QFB, it is possible that, the value of η± increses substantially. By considering that, the value of QFB for such GRBs is indeed ∼1053erg, we envisage that the energy of the actual neutrino burst/wind could be as high as ∼1054-1055erg (here we ignore likely loss of energy by gravitational energy mode). This energy might be had from general relativistic collapse of a massive stellar core having initial gravitational mass, say, Mi∼few M to a stage having a potential well much deeper than what is present on a canonican neutron star surface. Accordingly, we predict that the new generation large neutrino telescopes may detect neutrino burst of energy Qν∼1054-1055 ergs, with neutrino energies touching ∼1GeV, in coincidence with GRBs.

Abstract Copyright:

Journal keyword(s): gamma rays: bursts - black hole physics

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
1 GRB 970508 gB 06 53 49.2 +79 16 19           ~ 854 1
2 GRB 980329 gB 07 02 41 +38 50.7           ~ 267 1
3 GRB 971214 gB 11 56 26.4 +65 12 01           ~ 437 1
4 V* V818 Sco LXB 16 19 55.0692669024 -15 38 25.017666540 11.60 12.40 11.1     Oev 1570 0
5 SS 433 HXB 19 11 49.5647697480 +04 58 57.827127648   16.3 13.0     A7Ib: 2012 4
6 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1725 2
7 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1857 2

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