Post nova white dwarf cooling in V1500 Cygni

Simple item page
dc.creatorSomers, M. W.
dc.creatorNaylor, T.
dc.date1999-10-08
dc.date.accessioned2026-07-07T02:33:46Z
dc.date.available2026-07-07T02:33:46Z
dc.descriptionWe use the irradiated secondary star in the remnant of Nova Cyg 1975 as a probe of the cooling white dwarf. At superior conjunction the flux in the B band is dominated by the irradiated face of the secondary star. The heated face produces an orbital modulation which is dependent on the strength of the irradiating source. We demonstrate that the cooling rate of the white dwarf is consistent with the theoretical model of Prialnik (1986).
dc.description4 pages, 3 figures, A&A accepted
dc.identifierhttps://arxiv.org/abs/astro-ph/9910171
dc.identifierhttp://arxiv.org/abs/astro-ph/9910171
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/14976
dc.subjectAstrophysics
dc.titlePost nova white dwarf cooling in V1500 Cygni
dc.typetext

Files

Collections

arXiv