Interferometric Observations of RS Ophiuchi and the Origin of the Near-IR Emission

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dc.creatorLane, B. F.
dc.creatorSokoloski, J. L.
dc.creatorBarry, R. K.
dc.creatorTraub, W. A.
dc.creatorRetter, A.
dc.creatorMuterspaugh, M. W.
dc.creatorThompson, R. R.
dc.creatorEisner, J. A.
dc.creatorSerabyn, E.
dc.creatorMennesson, B.
dc.date2006-12-04
dc.date.accessioned2026-07-07T12:31:14Z
dc.date.available2026-07-07T12:31:14Z
dc.descriptionWe report observations of the recurrent nova RS Oph using long-baseline near-IR interferometry. We are able to resolve emission from the nova for several weeks after the February 2006 outburst. The near-IR source initially expands to a size of approximately 5 milli-arcseconds. However, beginning around day 10 the IR source appears to begin to shrink, reaching approximately 2 milli-arcseconds by day 100. We combine our measured angular diameters with previously available interferometric and photometric data to derive an emission measure for the source, and hence are able to determine the mass-loss rate of the nova in the days following the outburst.
dc.description17 pages, 4 figures. Accepted for publication in ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0612099
dc.identifierhttp://arxiv.org/abs/astro-ph/0612099
dc.identifierAstrophys.J.658:520-524,2007
dc.identifierdoi:10.1086/511414
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/216381
dc.subjectAstrophysics
dc.titleInterferometric Observations of RS Ophiuchi and the Origin of the Near-IR Emission
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