Journal
ASTROPHYSICAL JOURNAL
Volume 678, Issue 1, Pages 376-384Publisher
IOP Publishing Ltd
DOI: 10.1086/587043
Keywords
accretion, accretion disks; novae, cataclysmic variables; stars : dwarf novae; stars : individual (EI UMa)
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We present optical and X-ray time series photometry of EI UMa that reveal modulation at 746 and 770 s, which we interpret as the white dwarf spin and spin-orbit sidebands. These detections, combined with previous X-ray studies, establish EI UMa as an intermediate polar. We estimate the mass accretion rate to be similar to 3.6 x 10(17) g s(-1), which is close to, and likely greater than, the critical rate above which dwarf nova instabilities are suppressed. We also estimate the white dwarf to have a large magnetic moment mu > (3.4 +/- 0.2); 10(33) G cm(3). The high mass accretion rate and magnetic moment imply the existence of an accretion ring rather than a disk, and along with the relatively long orbital period, these suggest that EI UMa is a rare example of a prepolar cataclysmic variable.
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