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Evolutionary sequences of rotating protoneutron stars

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Evolutionary sequences of rotating protoneutron stars

dc.contributor.author	Villain, Loic
dc.contributor.author	Pons, J.A.
dc.contributor.author	Cerdá Durán, Pablo
dc.contributor.author	Gourgoulhon, E.
dc.date.accessioned	2010-06-29T11:11:09Z
dc.date.available	2010-06-29T11:11:09Z
dc.date.issued	2004
dc.identifier.citation	VILLAIN, Loic ; Pons, J.A. ; Cerda Duran, Pablo ; Gourgoulhon, E., 2004, Evolutionary sequences of rotating protoneutron stars, Astronomy and Astrophysics, vol. 418, no. 1, p. 283-294	en
dc.identifier.uri	http://hdl.handle.net/10550/14022
dc.description.abstract	We investigate the evolution of rigidly and differentially rotating protoneutron stars during the first twenty seconds of their life. We solve the equations describing stationary axisymmetric configurations in general relativity coupled to a finite temperature, relativistic equation of state, to obtain a sequence of quasi-equilibrium configurations describing the evolution of newly born neutron stars. The initial rotation profiles have been taken to mimic the situation found immediately following the gravitational collapse of rotating stellar cores. By analyzing the output of several models, we estimate that the scale of variation of the angular velocity in a newly born neutron star is of the order of 7−10 km.We obtain the maximum rotation frequency that can be reached as the protoneutron stars deleptonizes and cools down, as well as other relevant parameters such as total angular momentum or the instability parameter \|T/W\|. Our study shows that imposing physical constraints (conservation of baryonic mass and angular momentum) and choosing reasonable thermodynamical profiles as the star evolves gives results consistent with the energetics of more complex simulations of non-rotating protoneutron stars. It appears to be unlikely that newly born protoneutron stars formed in nearly axisymmetric core collapses reach the critical angular velocity to undergo the bar mode instability. They could, however, undergo secular or low \|T/W\| rotational instabilities a few seconds after birth, resulting in a strong emission of gravitational waves retarded with respect to the neutrino luminosity peak. We also found that the geometry of strongly differentially rotating protoneutron stars can become toroidal-like for large values of the angular velocity, before reaching the mass shedding limit.	en
dc.language.iso	en	en
dc.subject	Neutron ; Stars ; Rotation ; Evolution	en
dc.title	Evolutionary sequences of rotating protoneutron stars	en
dc.type	journal article	es_ES
dc.subject.unesco	UNESCO::ASTRONOMÍA Y ASTROFÍSICA	en
dc.subject.unesco	UNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia	en
dc.identifier.doi	10.1051/0004-6361:20035619	en
dc.identifier.idgrec	006140	en
dc.type.hasVersion	VoR	es_ES
dc.identifier.url	http://www.aanda.org/articles/aa/pdf/2004/16/aa0619.pdf	en