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Is the old nova RW UMi (1956) an intermediate polar? | | A. Bianchini
; C. Tappert
; H. Osborne
; Ronald Canterna
; F. Tamburini
; | | Date: |
31 Jul 2001 | | Subject: | astro-ph | | Affiliation: | 1 and 2), C. Tappert (2 and 3), H. Osborne (1 and 4), Ronald Canterna , and F. Tamburini ( Dept. of Physics and Astronomy University of Wyoming USA, Department of Astronomy University of Padova Italy, Departamento de Fisica Universidad de Concepcion | | Abstract: | 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 $mu_{34} sim 0.8$, in its quiescent pre-outburst state, the nova would appear as a discless, synchronous intermediate polar. | | Source: | arXiv, astro-ph/0107583 | | Services: | Forum | Review | PDF | Favorites | |
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