Interferometric observations of RS ophiuchi and the origin of the near-infrared emission

B. F. Lane; J. L. Sokoloski; R. K. Barry; W. A. Traub; A. Retter; M. W. Muterspaugh; R. R. Thompson; J. A. Eisner; E. Serabyn; B. Mennesson

doi:10.1086/511414

Interferometric observations of RS ophiuchi and the origin of the near-infrared emission

B. F. Lane, J. L. Sokoloski, R. K. Barry, W. A. Traub, A. Retter, M. W. Muterspaugh, R. R. Thompson, J. A. Eisner, E. Serabyn, B. Mennesson

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19 Scopus citations

Abstract

We 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 2006 February outburst. The near-IR source initially expands to a size of ∼5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching ∼2 mas 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.

Original language	English (US)
Pages (from-to)	520-524
Number of pages	5
Journal	Astrophysical Journal
Volume	658
Issue number	1 I
DOIs	https://doi.org/10.1086/511414
State	Published - Mar 20 2007
Externally published	Yes

Keywords

Techniques: interferometric

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/511414

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title = "Interferometric observations of RS ophiuchi and the origin of the near-infrared emission",

abstract = "We 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 2006 February outburst. The near-IR source initially expands to a size of ∼5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching ∼2 mas 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.",

keywords = "Techniques: interferometric",

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T1 - Interferometric observations of RS ophiuchi and the origin of the near-infrared emission

AU - Lane, B. F.

AU - Sokoloski, J. L.

AU - Barry, R. K.

AU - Traub, W. A.

AU - Retter, A.

AU - Muterspaugh, M. W.

AU - Thompson, R. R.

AU - Eisner, J. A.

AU - Serabyn, E.

AU - Mennesson, B.

PY - 2007/3/20

Y1 - 2007/3/20

N2 - We 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 2006 February outburst. The near-IR source initially expands to a size of ∼5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching ∼2 mas 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.

AB - We 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 2006 February outburst. The near-IR source initially expands to a size of ∼5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching ∼2 mas 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.

KW - Techniques: interferometric

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JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

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Interferometric observations of RS ophiuchi and the origin of the near-infrared emission

Abstract

Keywords

ASJC Scopus subject areas

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