X-RAY AND ULTRAVIOLET EMISSION FROM THE RECURRENT NOVA RS OPHIUCHI IN QUIESCENCE: SIGNATURES OF ACCRETION AND SHOCKED GAS

Journal Article · Wed Aug 10 00:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/737/1/7· OSTI ID:21580003

Nelson, T; Mukai, K ^[1]; Orio, M ^[2]; Luna, G J. M. ^[3]

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1. CRESST and X-ray Astrophysics Laboratory NASA/GSFC, Greenbelt, MD 20771 (United States)
2. INAF-Osservatorio Astronomico di Padova, vicolo Osservatorio, 5, I-35122 Padova (Italy)
3. Harvard-Smithsonian Center for Astrophysics, 60 Garden St. MS15, Cambridge, MS 02138 (United States)

RS Ophiuchi is a recurrent nova system that experiences outbursts every {approx}20 years, implying accretion at a high rate onto a massive white dwarf. However, previous X-ray observations of the system in quiescence have detected only faint emission that is difficult to reconcile with the high accretion rate (>2 x 10{sup -8} M{sub sun} yr{sup -1}) predicted by nova theory for such frequent outbursts. Here, we use new Chandra and XMM-Newton observations obtained 537 and 744 days after the 2006 outburst to constrain both the accretion rate onto the white dwarf and the properties of the nova ejecta at these times. We detect low level UV variability with the XMM-Newton Optical Monitor on day 744 that is consistent with accretion disk flickering, and use this to place a lower limit on the accretion rate at this epoch. The X-ray spectra in both observations are well described by a two component thermal plasma model. We identify the first component as the nova shell, which can emit X-rays for up to a decade after the outburst. The other component likely arises in the accretion disk boundary layer, and can be equally well fit by a single temperature plasma or a cooling flow model. Although the flux of the single temperature model implies an accretion rate that is 40 times too low to power the observed nova outburst rate (assuming that half of the accretion luminosity is emitted as X-rays in the boundary layer), the best-fit cooling flow model implies M-dot < 1.2 x 10{sup -8} M{sub sun} yr{sup -1} 537 days after the outburst, which is within a factor of two of the theoretical accretion rate required to power an outburst every 20 years. Furthermore, we place an upper limit on the accretion rate through an optically thick region of the boundary layer of 2.0 x 10{sup -8} M{sub sun} yr{sup -1}. Thus, these new quiescence data are consistent with the accretion rate expectations of nova theory. Finally, we discuss the possible origins of the low temperature associated with the accretion component, which is a factor of 10 lower than in T CrB, an otherwise similar recurrent nova.

• OSTI ID: 21580003
• Journal Information: Astrophysical Journal, Vol. 737, Issue 1; Other Information: DOI: 10.1088/0004-637X/737/1/7; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
BOUNDARY LAYERS
EMISSION
FLOW MODELS
NOVAE
STAR ACCRETION
ULTRAVIOLET RADIATION
WHITE DWARF STARS
X RADIATION
BINARY STARS
DWARF STARS
ELECTROMAGNETIC RADIATION
ERUPTIVE VARIABLE STARS
EVOLUTION
IONIZING RADIATIONS
LAYERS
MATHEMATICAL MODELS
RADIATIONS
STAR EVOLUTION
STARS
VARIABLE STARS