Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b)

A. Ibarra; E. Kuulkers; J. P. Osborne; K. Page; J. U. Ness; R. D. Saxton; W. Baumgartner; V. Beckmann; M. F. Bode; M. Hernanz; K. Mukai; M. Orio; G. Sala; Sumner Starrfield; G. A. Wynn

doi:10.1051/0004-6361/200911710

Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b)

A. Ibarra, E. Kuulkers, J. P. Osborne, K. Page, J. U. Ness, R. D. Saxton, W. Baumgartner, V. Beckmann, M. F. Bode, M. Hernanz, K. Mukai, M. Orio, G. Sala, Sumner Starrfield, G. A. Wynn

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20 Scopus citations

Abstract

Classical novae are phenomena caused by explosive hydrogen burning onto an accreting white dwarf. Only one classical nova had been identified in X-rays before the actual optical outburst occurred (V2487 Oph). The recently discovered nova, V2491 Cyg, is one of the fastest (He/N) novae observed to date. Using archival ROSAT, XMM-Newton, and Swift data, we show that V2491 Cyg was a persistent X-ray source during its quiescent time before the optical outburst. We present the X-ray spectral characteristics and derive X-ray fluxes. The pre-outburst X-ray emission is variable, and, at least in one observation, it exhibits a soft X-ray source.

Original language	English (US)
Pages (from-to)	L5-L8
Journal	Astronomy and Astrophysics
Volume	497
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361/200911710
State	Published - Apr 2009

Keywords

Novae, cataclysmic variables
X-rays: Binaries

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/200911710

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title = "Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b)",

abstract = "Classical novae are phenomena caused by explosive hydrogen burning onto an accreting white dwarf. Only one classical nova had been identified in X-rays before the actual optical outburst occurred (V2487 Oph). The recently discovered nova, V2491 Cyg, is one of the fastest (He/N) novae observed to date. Using archival ROSAT, XMM-Newton, and Swift data, we show that V2491 Cyg was a persistent X-ray source during its quiescent time before the optical outburst. We present the X-ray spectral characteristics and derive X-ray fluxes. The pre-outburst X-ray emission is variable, and, at least in one observation, it exhibits a soft X-ray source.",

keywords = "Novae, cataclysmic variables, X-rays: Binaries",

author = "A. Ibarra and E. Kuulkers and Osborne, {J. P.} and K. Page and Ness, {J. U.} and Saxton, {R. D.} and W. Baumgartner and V. Beckmann and Bode, {M. F.} and M. Hernanz and K. Mukai and M. Orio and G. Sala and Sumner Starrfield and Wynn, {G. A.}",

year = "2009",

month = apr,

doi = "10.1051/0004-6361/200911710",

language = "English (US)",

volume = "497",

pages = "L5--L8",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

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TY - JOUR

T1 - Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b)

AU - Ibarra, A.

AU - Kuulkers, E.

AU - Osborne, J. P.

AU - Page, K.

AU - Ness, J. U.

AU - Saxton, R. D.

AU - Baumgartner, W.

AU - Beckmann, V.

AU - Bode, M. F.

AU - Hernanz, M.

AU - Mukai, K.

AU - Orio, M.

AU - Sala, G.

AU - Starrfield, Sumner

AU - Wynn, G. A.

PY - 2009/4

Y1 - 2009/4

N2 - Classical novae are phenomena caused by explosive hydrogen burning onto an accreting white dwarf. Only one classical nova had been identified in X-rays before the actual optical outburst occurred (V2487 Oph). The recently discovered nova, V2491 Cyg, is one of the fastest (He/N) novae observed to date. Using archival ROSAT, XMM-Newton, and Swift data, we show that V2491 Cyg was a persistent X-ray source during its quiescent time before the optical outburst. We present the X-ray spectral characteristics and derive X-ray fluxes. The pre-outburst X-ray emission is variable, and, at least in one observation, it exhibits a soft X-ray source.

AB - Classical novae are phenomena caused by explosive hydrogen burning onto an accreting white dwarf. Only one classical nova had been identified in X-rays before the actual optical outburst occurred (V2487 Oph). The recently discovered nova, V2491 Cyg, is one of the fastest (He/N) novae observed to date. Using archival ROSAT, XMM-Newton, and Swift data, we show that V2491 Cyg was a persistent X-ray source during its quiescent time before the optical outburst. We present the X-ray spectral characteristics and derive X-ray fluxes. The pre-outburst X-ray emission is variable, and, at least in one observation, it exhibits a soft X-ray source.

KW - Novae, cataclysmic variables

KW - X-rays: Binaries

UR - http://www.scopus.com/inward/record.url?scp=63849167963&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=63849167963&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/200911710

DO - 10.1051/0004-6361/200911710

M3 - Article

AN - SCOPUS:63849167963

SN - 0004-6361

VL - 497

SP - L5-L8

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

ER -

Pre-nova X-ray observations of V2491 Cygni (Nova Cyg 2008b)

Abstract

Keywords

ASJC Scopus subject areas

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