2001/07/31 by A. Bianchini, Bianchini, A., C. Tappert +7
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0107583
9 pages 11 figures, submitted to MNRAS
arxiv created 2001/07/31 · arxiv updated 2009/12/01
From photometric observations of the old nova RW UMi (1956) we have discovered the presence of five sub-orbital periodicities. The longest period, P1 = 54.4 min, always observed, could be the beat period between the orbital period and the white dwarf (WD) spin period that we assume to be P2 = 33.4 min. The other suborbital periods could be orbital sidebands with respect to P2 and/or correspond to Keplerian resonance radii. We suggest that in its post-outburst state, characterized by higher mass transfer rate, RW UMi is an asynchronous intermediate polar with a truncated accretion disc. If the magnetic momentum of the WD is μ34 ∼ 0.8, in its quiescent pre-outburst state, the nova would appear as a discless, synchronous intermediate polar.