Spectropolarimetry of V1315 Aql

Abstract

Recent years have seen the emergence of a group of nova-like variables which exhibit remarkably similar behaviour. To date, there exist five such well-studied systems: V1315 Aql (Downes et al. 1986; Dhillon, Marsh and Jones 1991), SW Sex (Penning et al. 1984; Honeycutt, Schlegel and Kaitchuck 1986), DW UMa (Shafter, Hessman and Zhang 1988; Dhillon, Jones and Marsh 1994), BH Lyn (Thorstensen, Davis and Ringwald 1991; Dhillon et al. 1992) and PX And (Thorstensen et al. 1991; Still, Dhillon and Jones 1994). All five objects are eclipsing systems with orbital periods lying in the narrow range of 3.24 to 3.74 hr; all five objects exhibit single-peaked Balmer and HeI emission lines which remain largely unobscured during primary eclipse and which show strong absorption features around the inferior conjunction of the emission-line source; all five objects show single-peaked high-excitation emission lines which are eclipsed by the secondary; and all five objects show radial velocity curves with significant phase shifts relative to photometric conjunction. In addition, a number of systems are believed to be related to these five, exhibiting some, but not all, of the above features: WX Ari (Beuermann et al. 1992), UU Aqr (Diaz and Steiner 1991) and LB1800 (Buckley et al. 1990).KeywordsOrbital PeriodAccretion DiscBalmer LineRadial Velocity CurveRoyal Greenwich ObservatoryThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.