RZ Leonis Minoris, PG 0943+521, and V1159 Orionis: Three Cataclysmic Variables with Similar and Unusual Outburst Behavior

Abstract

We call attention to a small group of cataclysmic variable stars (whose prototype might be considered RZ LMi) that have complex light curves of similar shape which repeat with typical periods of a few weeks. The predictability of the time of each superoutburst and the stability of the shape of the light curve is unexpectedly high for cataclysmic variables, which are well-known for erratic variations in both the timing and the shape of their outbursts. The phenomenon appears to be closely related to SU Ursae Majoris-type superoutbursts, especially since superhumps appear in these stars. The similarities and differences between these RZ LMi stars and SU UMa systems are summarized and discussed in the context of extant models for the superoutbursts of SU UMa-type dwarf novae.

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

“…In our periodogram (Fig. 10), we detect a clear peak (and its harmonics) at P = 44.3±0.1 d, which is agreement with, or may improve or complement, previous determinations at 44.2-46.8 d (Robertson et al 1995;Richter 1995;Kato 2001;Pitts et al 2002). 11.7 and 12.4 mag (No.…”

“…V1159 Ori was discovered by Wolf & Wolf (1906), who gave it the name "Var.,Orionis 36.1906", and first investigated by Kippenhahn (1953) and Jablonski & Cieslinski (1992). Afterwards, its very short outburst cycle, superhumps, orbital periods, and high energy (X-ray, ultraviolet) emission have been studied by a number of authors (Nogami et al 1995;Robertson et al 1995;Patterson et al 1995;Thorstensen et al 1997;Szkody et al 1999). We can add little to the knowledge on V1159 Ori except for its supercycle period.…”

IUE and Optical Spectra of RZ LMI and ER UMa Throughout their 19 and 43 Day Cycles

“…(95 m for ER UMa and 85.6 m for RZ LMi; Robertson et al 1995), and are close to those expected from the superhump-orbital period relationships of SU UMa stars in general (Howell & Hurst 1994), it is reasonable to assume that these are the observed orbital periods.…”

“…In the past year, it has become apparent that the 3 CVs RZ LMi, ER UMa and VI159 Ori exhibit a unique pattern of behavior similar to the normal SU UMa stars, but at extreme minima of time-scale and amplitude (Robertson, Honeycutt & Turner 1995). These 3 objects show very short (19...45 day) supercycles, have very low P (10 -3 ) and very low amplitude (3 mag) superoutbursts.…”

The Reflares and Outburst Evolution in the Accreting Millisecond Pulsar Sax J1808.4–3658: A Disk Truncated Near Co-Rotation?

“…Reflares (also known in the literature as "rebrightenings," "echo-outbursts," "mini-outbursts" and "flaring-tail") have been observed in a number of different systems, including dwarf novae (WZ Sge, Patterson et al 2002;EG Cnc, Osaki et al 2001; ER UMA Robertson et al 1995;Patterson et al 2013, AL Com Howell et al 1996, UZ Boo, Kuulkers et al 1996; BK Lyn Patterson et al 2013), neutron stars (e.g., KS 1731-260, Šimon 2010, SAX J1750.8-2900 Allen et al 2015 and possibly IGR J00291+5934, Lewis et al 2010) and black hole low-mass X-ray binaries (LMXBs) (e.g., XTE J1650-500, Tomsick et al 2004; GRO J0422+32, Kuulkers et al 1996;GRS 1009-45, Bailyn & Orosz 1995XTE J1859+226, Zurita et al 20024U 15434U -47, Li et al 1976. The ubiquity of the phenomenon among different types of accreting compact objects suggests that reflares are related to specific properties of the accretion disk itself rather than properties of the compact object.…”