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Luminosity of a quark-star undergoing torsional oscillations and the problem of gamma ray bursts | | J. Heyvaerts
; S. Bonazzola
; M. Bejger
; P. Haensel
; | | Date: |
7 Nov 2008 | | Abstract: | We discuss whether the process of winding-up the magnetic field by
differential rotation in a new-born quark-star can cause an energy emission
rate high enough and lasting sufficiently long to explain long gamma ray
bursts. Within the magneto-hydrodynamics, we study the torsional oscillations
and the extraction of energy from a new-born, hot, differentially rotating
quark-star.
The new-born compact star is a fast rotator which blows a relativistic
leptonic wind. The star’s torsional oscillation considerably modulates this
wind emission when it is odd and of a sufficient amplitude, which is relatively
easy to reach. Odd oscillations may occur just after the formation of a
quark-star.Other asymmetries can cause similar effects. The buoyancy of
wound-up magnetic fields is inhibited, or its effects are limited, by a variety
of different mechanisms described in the paper. Direct electromagnetic emission
by the torsional oscillation in an outside vacuum or in the leptonic wind
surrounding the compact object is found to be insignificant.
On the contrary, the twist given to the outer magnetic field by an odd
torsional oscillation is generally sufficient to break the star’s magnetosphere
open. The Poynting emission of the star in its leptonic environment is then
radiated from all its surface and is considerably enhanced during these open
episodes, tapping at the bulk rotational energy of the star. This results in
intense energy shedding in the first tens of minutes after the collapse for
magnetized quark-stars with an initial poloidal field of order of 10**14 Gauss,
sufficient to explain long gamma-ray bursts. | | Source: | arXiv, 0811.1090 | | Services: | Forum | Review | PDF | Favorites | |
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