A gaseous metal disk around a white dwarf

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dc.creatorGaensicke, B. T.
dc.creatorMarsh, T. R.
dc.creatorSouthworth, J.
dc.creatorRebassa-Mansergas, A.
dc.date2006-12-22
dc.date2006-12-31
dc.date.accessioned2026-07-07T07:37:43Z
dc.date.available2026-07-07T07:37:43Z
dc.descriptionThe destiny of planetary systems through the late evolution of their host stars is very uncertain. We report a metal-rich gas disk around a moderately hot and young white dwarf. A dynamical model of the double-peaked emission lines constrains the outer disk radius to just 1.2 solar radii. The likely origin of the disk is a tidally disrupted asteroid, which has been destabilised from its initial orbit at a distance of more than 1000 solar radii by the interaction with a relatively massive planetesimal object or a planet. The white dwarf mass of 0.77 solar masses implies that planetary systems may form around high-mass stars.
dc.descriptionPublished 22 December in Science, added journal ref
dc.identifierhttps://arxiv.org/abs/astro-ph/0612697
dc.identifierhttp://arxiv.org/abs/astro-ph/0612697
dc.identifierVol. 314. no. 5807, pp. 1908 - 1910
dc.identifierdoi:10.1126/science.1135033
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/120866
dc.subjectAstrophysics
dc.titleA gaseous metal disk around a white dwarf
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