ASASSN-14cc: Likely Helium Analog of RZ Leonis Minoris

TL;DR

ASASSN-14cc is a highly active helium dwarf nova exhibiting frequent long outbursts and superhumps, closely resembling RZ LMi but with a shorter superhump period, indicating a high mass transfer rate near the disk stability limit.

Contribution

This study identifies ASASSN-14cc as a helium analog of RZ LMi, providing detailed observational evidence of its outburst behavior and superhump characteristics, expanding understanding of AM CVn-type objects.

Findings

ASASSN-14cc shows long outbursts every 21-33 days with durations of 9-18 days.

Detected superhumps with a period of approximately 22.5 minutes during long outbursts.

The object exhibits the highest outburst activity among AM CVn-type systems.

Abstract

We identified that ASASSN-14cc is a very active dwarf nova spending approximately 60% of the time in outburst. Our long-term photometry revealed that the object shows long outbursts recurring with a period of 21-33 d and very brief short outbursts lasting less than 1 d. The maximum decline rate exceeds 2.8 mag/d. The duration of long outbursts is 9-18 d, comprising 50-60% of the recurrence time of long outbursts. We detected 0.01560-0.01562 d (22.5 min) modulations during long outbursts, which we identified to be superhumps. These features indicate that ASASSN-14cc has outburst parameters very similar to the extreme dwarf nova RZ LMi but with a much shorter superhump period. All the observations can be naturally understood considering that this object is a helium analog (AM CVn-type object) of RZ LMi. The highest outburst activity among AM CVn-type objects can be understood as the high-mass transfer rate expected for the orbital period giving a condition close to the stability limit of the accretion disk. In contrast to RZ LMi, this object shows little evidence for premature quenching of the superoutburst, which has been proposed to explain the unusual outburst parameters in RZ LMi.