Is the old nova RW UMi (1956) an intermediate polar?
| dc.creator | Bianchini, A. | |
| dc.creator | Tappert, C. | |
| dc.creator | Osborne, H. | |
| dc.creator | Canterna, Ronald | |
| dc.creator | Tamburini, F. | |
| dc.date | 2001-07-31 | |
| dc.date.accessioned | 2026-07-07T01:59:29Z | |
| dc.date.available | 2026-07-07T01:59:29Z | |
| dc.description | 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 $μ_{34} \sim 0.8$, in its quiescent pre-outburst state, the nova would appear as a discless, synchronous intermediate polar. | |
| dc.description | 9 pages 11 figures, submitted to MNRAS | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0107583 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0107583 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/3134 | |
| dc.subject | Astrophysics | |
| dc.title | Is the old nova RW UMi (1956) an intermediate polar? | |
| dc.type | text |