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Magneto–rotational and Thermal Evolution of Magnetars with Crustal Magnetic Fields

Published online by Cambridge University Press:  12 April 2016

U. Geppert ,
D. Page ,
M. Colpi  and
T. Zannias
U. Geppert
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, GERMANYe-mail:[email protected]
D. Page
Affiliation:
Institute de Astronomía, UNAM, 04510 Mexico D.F., MEXICOe-mail:[email protected]
M. Colpi
Affiliation:
Diparlimento di Fisica, Universitá degli Studi di Milano Bicocca, Via Emanueli 15, 20133 Milano, [email protected]
T. Zannias
Affiliation:
Instituto de Fásica y Matemáticas, Universidad Michoacana SNH, Morelia, Mich. 58040, MEXICOe-mail:[email protected]

Extract

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The interpretation of Soft–Gamma–Repeaters (SGRs) and Anomalous X–Ray Pulsars (AXPs) as Magnetars (Thompson & Duncan 1996) raises again the issue of the generation of the ultra–strong magnetic fields (MFs) in neutron stars (NSs) and the related question of where these fields are anchored: in the core, penetrating the whole star, or confined to the crust. Recently, Heyl & Kulkarni (1998) considered the magneto–thermal evolution of magnetars with a core field. Since the assumption of a crustal field is at least not in disagreement with the observations of isolated pulsars (Urpin & Konenkov 1997) and of NSs in binary systems (Urpin, Geppert & Konenkov 1998, Urpin, Konenkov & Geppert 1998), here we would like to address the question whether the observations of SGRs and AXPs can be interpreted as magnetars having a crustal MF. Given the strength of the MF in magnetars we take into account, in an approximate manner, the strongly non–linear Hall effect on its decay. We intend to provide a contribution to an unified picture of NS MF evolution based on the crustal field hypothesis.

Type
Part 10. Anomalous X-Ray Pulsars and Magnetars
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 681 - 684
Copyright
Copyright © Astronomical Society of the Pacific 2000

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