An Atmospheric Model for the Ion Cyclotron Line of Geminga

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dc.creatorJacchia, A.
dc.creatorDe Luca, F.
dc.creatorLazzaro, E.
dc.creatorCaraveo, P. A.
dc.creatorMignani, R. P.
dc.creatorBignami, G. F.
dc.date1999-04-29
dc.date.accessioned2026-07-07T02:31:27Z
dc.date.available2026-07-07T02:31:27Z
dc.descriptionRecent optical/UV data of Geminga (Mignani et al. 1998) have strengthen the significance of the emission feature present over the thermal continuum best fitting the EUV/soft X-ray data. Here we present a phenomenological model interpreting the data in terms of an ion cyclotron feature, arising from a thin outer layer of hot plasma covering Geminga's polar caps. The width of the feature favours for Geminga the strongly oblique rotator configuration, as already deduced from the soft X-ray data (Halpern & Ruderman 1993). Our interpretation implies a magnetic field of 3 - 5 10d11 G, consistent with the value deduced from the dynamical parameters of the pulsar. This would represent the first case of an independent measurement of the surface magnetic field of an isolated neutron star. The expected time modulation of Geminga's feature is also discussed.
dc.description7 pages, LaTex, 7 Postscript figures. Astronomy&Astrophysics-in press
dc.identifierhttps://arxiv.org/abs/astro-ph/9904412
dc.identifierhttp://arxiv.org/abs/astro-ph/9904412
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/14155
dc.subjectAstrophysics
dc.titleAn Atmospheric Model for the Ion Cyclotron Line of Geminga
dc.typetext

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