The He-shell flash in action: T Ursae Minoris revisited

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dc.creatorSzatmary, K.
dc.creatorKiss, L. L.
dc.creatorBebesi, Zs.
dc.date2002-11-13
dc.date.accessioned2026-07-07T12:49:56Z
dc.date.available2026-07-07T12:49:56Z
dc.descriptionWe present an updated and improved description of the light curve behaviour of T Ursae Minoris, which is a Mira star with the strongest period change (the present rate is an amazing -3.8+/-0.4 days/year corresponding to a relative decrease of about 1% per cycle). Ninety years of visual data were collected from all available databases and the resulting, almost uninterrupted light curve was analysed with the O-C diagram, Fourier analysis and various time-frequency methods. The Choi-Williams and Zhao-Atlas-Marks distributions gave the clearest image of frequency and light curve shape variations. A decrease of the intensity average of the light curve was also found, which is in accordance with a period-luminosity relation for Mira stars. We predict the star will finish its period decrease in the meaningfully near future (c.c. 5 to 30 years) and strongly suggest to closely follow the star's variations (photometric, as well as spectroscopic) during this period.
dc.description6 pages, 7 figures, accepted for publication in A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/0211284
dc.identifierhttp://arxiv.org/abs/astro-ph/0211284
dc.identifierAstron.Astrophys.398:277-282,2003
dc.identifierdoi:10.1051/0004-6361:20021646
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/222541
dc.subjectAstrophysics
dc.titleThe He-shell flash in action: T Ursae Minoris revisited
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