Convective Instability in Proto–Neutron Stars | Zendy

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

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Convective Instability in Proto–Neutron Stars

Author(s) -

J. A. Miralles,

J. A. Pons,

V. Urpin

Publication year - 2000

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 - 10.1086/317163

Subject(s) - instability , dissipative system , physics , neutron star , convection , convective instability , stars , stability (learning theory) , mechanics , neutrino , viscosity , classical mechanics , astrophysics , nuclear physics , thermodynamics , computer science , machine learning

The linear hydrodynamic stability of proto-neutron stars (PNSs) is consideredtaking into account dissipative processes such as neutrino transport andviscosity. We obtain the general instability criteria which differ essentiallyfrom the well-known Ledoux criterion used in previous studies. We apply thecriteria to evolutive models of PNSs that, in general, can be subject to thevarious known regimes such as neutron fingers and convective instabilities. Ourresults indicate that the fingers instability arises in a more extended regionof the stellar volume and lasts a longer time than expected.Comment: 17 pages, 3 figures. Accepted for publication in Astrophysical Journa

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