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Balman S. , Godon P., Sion E. M. , Ness J., Schlegel E., Barrett P. E. , ...Daha Fazla

ASTROPHYSICAL JOURNAL, cilt.741, sa.2, 2011 (SCI İndekslerine Giren Dergi) identifier identifier


We present an analysis of X-ray and UV data obtained with the XMM-Newton Observatory of the long-period dwarf nova RU Peg. RU Peg contains a massive white dwarf (WD), possibly the hottest WD in a dwarf nova (DN), it has a low inclination, thus optimally exposing its X-ray emitting boundary layer (BL), and has an excellent trigonometric parallax distance. We modeled the X-ray data using XSPEC assuming a multi-temperature plasma emission model built from the MEKAL code (i.e., CEVMKL). We obtained a maximum temperature of 31.7 keV, based on the European Photon Imaging Camera MOS1, 2 and pn data, indicating that RU Peg has an X-ray spectrum harder than most DNe, except U Gem. This result is consistent with and indirectly confirms the large mass of the WD in RU Peg. The X-ray luminosity we computed corresponds to a BL luminosity for a mass accretion rate of 2 x 10(-11) M-circle dot yr(-1) (assuming M-wd = 1.3 M-circle dot), in agreement with the expected quiescent accretion rate. The modeling of the O VIII emission line at 19 angstrom as observed by the Reflection Grating Spectrometer implies a projected stellar rotational velocity v(rot) sin i = 695 km s(-1), i.e., the line is emitted from material rotating at similar to 936-1245 km s(-1) (i similar to 34 degrees-48 degrees) or about 1/6 of the Keplerian speed; this velocity is much larger than the rotation speed of the WD inferred from the Far Ultraviolet Spectroscopic Explorer spectrum. Cross-correletion analysis yielded an undelayed (time lag similar to 0) component and a delayed component of 116 +/- 17 s where the X-ray variations/fluctuations lagged the UV variations. This indicates that the UV fluctuations in the inner disk are propagated into the X-ray emitting region in about 116 s. The undelayed component may be related to irradiation effects.