Magnetar formation through a convective dynamo in protoneutron stars-Reference-Cited by-同舟云学术

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Magnetar formation through a convective dynamo in protoneutron stars

Published:2020-03-13 Issue:11 Volume:6 Page:
ISSN:2375-2548
Container-title:Science Advances
language:en
Short-container-title:Sci. Adv.

Author:

Raynaud Raphaël¹^ORCID,Guilet Jérôme¹^ORCID,Janka Hans-Thomas²^ORCID,Gastine Thomas³^ORCID

Affiliation:

1. AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, F-91191 Gif-sur-Yvette, France.

2. Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany.

3. Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris-Diderot, UMR7154 CNRS, 1 rue Jussieu, 75005 Paris, France.

Abstract

Strong field dynamos can explain magnetar formation consistently with the millisecond magnetar model for extreme explosions.

Funder

European Research Council

Deutsche Forschungsgemeinschaft

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference40 articles.

2. The source of magnetic fields in (neutron-) stars

3. The magnetic early B-type stars I: magnetometry and rotation

4. Numerical simulations of the magnetorotational instability in protoneutron stars – I. Influence of buoyancy

5. A large-scale dynamo and magnetoturbulence in rapidly rotating core-collapse supernovae

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