Cooling of young neutron stars in GRB associated to supernovae

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Volume 540 (April 2012)

A&A, 540 (2012) A12

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Table 1

GRBs associated to SNe and URCAs.

GRB				E_URCA			R_NS	z^e
GRB	(erg)	(erg)^a	(erg)^b	(erg)^c			(km)^d	z^e

980425	1.2 × 10⁴⁸	2.3 × 10⁴⁹	1.0 × 10⁵²	3 × 10⁴⁸	0.4	1.7 × 10⁴	8	0.0085
030329	2.1 × 10⁵²	1.8 × 10⁴⁹	8.0 × 10⁵¹	3 × 10⁴⁹	6 × 10²	1.2 × 10³	14	0.1685
031203	1.8 × 10⁵⁰	3.1 × 10⁴⁹	1.5 × 10⁵²	2 × 10⁴⁹	8.2	3.0 × 10³	20	0.105
060218	1.8 × 10⁵⁰	9.2 × 10⁴⁸	2.0 × 10⁵¹	?	?	?	?	0.033

Notes. Here is the total energy of GRB, and are the bolometric and the kinetic energy of the SN, E_URCA is the energy of the late X-ray emission URCA (see Fig. 3), R_NS is the radius of the neutron star, and z is the redshift of the event.

^(a)

See Kaneko et al. (2007);

^(b)

Mazzali (priv. comm. at MG11 meeting in Berlin, July 2006), Iwamoto et al. (1998);

^(c)

evaluated fitting the URCAs with a power law followed by an exponentially decaying part;

^(d)

evaluated assuming a mass of the neutron star M = 1.5 M_⊙ and T ~ 5–7 keV in the source rest frame;

^(e)

see Galama et al. (1998); Greiner et al. (2003); Prochaska et al. (2004); Mirabal et al. (2006).

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