The Long-Term H$α$ Emission Line Variation in $α$ Eri

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dc.creatorVinicius, M. M. F.
dc.creatorLeister, Nelson Vani
dc.creatorZorec, Juan
dc.creatorLevenhagen, Ronaldo
dc.date2005-09-07
dc.date.accessioned2026-07-07T02:18:36Z
dc.date.available2026-07-07T02:18:36Z
dc.descriptionThe long-term variation of the H$α$ line in $α$ Eri has 14-15 years cyclic \bbe phase transitions. The disc formation time scales, interpreted as the periods during which the H$α$ line emission increases from zero to its maximum, agree with the viscous decretion model. On the other hand, the time required for the disc dissipation ranges from 6 to 12 years which questions the viscous disc model predictions.
dc.identifierhttps://arxiv.org/abs/astro-ph/0509180
dc.identifierhttp://arxiv.org/abs/astro-ph/0509180
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/9546
dc.subjectAstrophysics
dc.titleThe Long-Term H$α$ Emission Line Variation in $α$ Eri
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