Hydromagnetic Instabilities in Proto–Neutron Stars | Zendy

J. A. Miralles | Zendy; J. A. Pons | Zendy; V. Urpin | Zendy

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Hydromagnetic Instabilities in Proto–Neutron Stars

Author(s) -

J. A. Miralles,

J. A. Pons,

V. Urpin

Publication year - 2002

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/340899

Subject(s) - neutron star , magnetar , physics , pulsar , dissipative system , instability , magnetic field , astrophysics , stars , neutrino , nuclear physics , mechanics , thermodynamics , quantum mechanics

The stability properties of newly born neutron stars, or proto--neutronstars, are considered. We take into account dissipative processes, such asneutrino transport and viscosity, in the presence of a magnetic field. In orderto find the regions of the star subject to different sorts of instability, wederive the general instability criteria and apply it to evolutionary models ofPNSs. The influence of the magnetic field on instabilities is analyzed and thecritical magnetic field stabilizing the star is obtained. In the light of ourresults, we estimate of the maximum poloidal magnetic field that might bepresent in young pulsars or magnetars.Comment: 18 pages, 4 figures, to appear in Astrophysical Journa

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