6533b85afe1ef96bd12b986f
RESEARCH PRODUCT
Evolution of the surface magnetic field of rotating proto-neutron stars
Miguel-ángel AloyMartin Obergaulingersubject
High Energy Astrophysical Phenomena (astro-ph.HE)PhysicsHistory010308 nuclear & particles physicsTurbulenceAstrophysics::High Energy Astrophysical PhenomenaFOS: Physical sciencesAstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysics01 natural sciencesMagnetic fluxAccretion (astrophysics)Spectral lineComputer Science ApplicationsEducationMagnetic fieldMagnetizationStarsNeutron star0103 physical sciencesAstrophysics::Solar and Stellar AstrophysicsAstrophysics::Earth and Planetary AstrophysicsAstrophysics - High Energy Astrophysical Phenomena010303 astronomy & astrophysicsAstrophysics::Galaxy Astrophysicsdescription
We study the evolution of the field on the surface of proto-neutron stars in the immediate aftermath of stellar core collapse by analyzing the results of self-consistent, axisymmetric simulations of the cores of rapidly rotating high-mass stars. To this end, we compare the field topology and the angular spectra of the poloidal and toroidal field components over a time of about one seconds for cores. Both components are characterized by a complex geometry with high power at intermediate angular scales. The structure is mostly the result of the accretion of magnetic flux embedded in the matter falling through the turbulent post-shock layer onto the PNS. Our results may help to guide further studies of the long-term magnetothermal evolution of proto-neutron stars. We find that the accretion of stellar progenitor layers endowed with low or null magnetization bury the magnetic field on the PNS surface very effectively.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2017-11-21 |