Z Cam Stars in the Twenty-First Century

ABSTRACT: Z Cam stars are a small subset of dwarf novae that exhibit standstills in their light curves. Most modern literature and catalogs of cataclysmic variables quote the number of known Z Cams to be on the order of 30 or so systems. After a four-year observing campaign and an exhaustive examination of the data in the AAVSO International Database we have trimmed that number by a third. One of the reasons for the misclassification of some systems is the fact that the definition of what a Z Cam is has changed over the last 85 years to what it is today. This has caused many stars formerly assumed to be Z Cams or rumored to be Z Cams to be eliminated from the final list. In this paper we present the results of our investigation into 65 stars listed at one time or another in the literature as Z Cams or possible Z Cams. 1-INTRODUCTION: Dwarf novae (DNe), or U Geminorum (UG) systems, are a subclass of cataclysmic variable stars (CVs); semi-detached close binary systems in which a white dwarf (WD) accretes material from a Roche-lobe-filling secondary via an accretion disk (Warner 1995). They are called “dwarf novae” because DNe outbursts are smaller in amplitude and higher in frequency than classical novae eruptions. DNe outbursts result from a temporary increase in the rate of accretion onto the WD. According to the thermal-viscous disc instability model, over time, the mass of accreted material grows and the temperature of the disk rises, until it becomes sufficiently high to switch into a hot, highly viscous state. The disk becomes unstable and mass is dumped onto the surface of the WD after plowing through a violent transition region just above the surface of the WD called the "boundary layer", releasing copious amounts of energy, from optical to x-rays. DNe are classified into sub-groups based primarily on their light curves. SS Cygni stars (UGSS), brighten dramatically by 2-6 magnitudes in 1-2 days, and return to their original brightness after a period of several days to a week or more. Cycle times between outbursts range from 10 days to years. Orbital periods are usually longer than 3 hours. SU Ursae Majoris stars (UGSU), exhibit normal outbursts, but also have brighter and longer "super-outbursts." The cycle times of superoutbursts (super-cycle) are usually several times the length of time between normal outbursts and can be years or decades long. In general, the shorter the orbital period, the longer the super-cycle. Orbital periods are usually in the range of 75 minutes to 2 hours. Z Camelopardalis stars (UGZ) are DNe that exhibit normal UG-type outbursts, as well as random standstills. A standstill usually starts at the end of an outburst and consists of a period of relatively constant brightness, 1 to 1.5 magnitudes below maximum light that may last from a few days to 1,000 days. The orbital periods of UGZ are all longer than 3 hours. This classification system has evolved over time as our understanding of the physical processes behind the observed behaviors has grown. However, the changing definition of UGZ stars has created confusion in the literature and many stars that used to fit the definition no longer meet the requirements of membership in the Z Cam classification.