# A tale of three cataclysmic variables with distinct superhumps

## TL;DR

This study analyzes TESS data of three cataclysmic variables, revealing superhump behaviors, disc precession, and potential classification of one as a high-mass transfer CV, contributing new insights into their accretion disc dynamics.

## Contribution

It provides detailed observations of superhump period variations and disc precession in three CVs, including the first detection of certain periods and a proposed reclassification of one system.

## Key findings

- Superhump period variations in CRTS J110014.7+131552
- Discovery of new orbital and superhump periods in SDSS J093537.46+161950.8
- Identification of negative superhump and disc-precession periods in [PK2008] HalphaJ130559

## Abstract

We present the TESS observations of CRTS J110014.7+131552, SDSS J093537.46+161950.8, and [PK2008] HalphaJ130559. Among them, a superoutburst is observed in CRTS J110014.7+131552 which is associated with the precursor outburst, where prominent superhumps are observed during maximum of the outburst with a mean period of 0.06786(1) d. We have observed variations in the superhump period, along with changes in the shape of the light curve profile and the amplitude of the superhumps during different phases of the outburst, indicating disc-radius variation as well as periodically variable dissipation at the accretion stream's bright spot. The data on SDSS J093537.46+161950.8 reveal previously unknown variations modulated with periods 0.06584(2) d and 2.36(2) d, related to the positive superhump and the disc-precession periods, respectively, which can reasonably be interpreted as a result of the prograde rotation of an eccentric accretion disc. Despite its short orbital period, the lack of outburst activity, along with its stable long-term brightness, discovery spectrum, and absolute magnitude suggests that the object might not be an SU UMa type dwarf nova. Instead, it may belong to the group of high mass-transfer CVs below the period gap, either to a rare class of nova-like variables or to the class of high-luminosity IPs, a subclass of magnetic CVs. For [PK2008] HalphaJ130559, a new average orbital period of 0.15092(1) d has been identified. Additionally, this system displays previously undetected average periods of 0.14517(3) d and 3.83(1) d, which can be provisionally identified as negative superhump and disc-precession periods, respectively. If the identified simultaneous signals do indeed reflect negative superhump and disc-precession period variations then their origin may be associated with the retrograde precession of a tilted disc and its interaction with the secondary stream.