Tilted Disk Precession and Negative Superhumps in HS 2325+8205: A Multi-Window Analysis

TL;DR

This study uses TESS data to analyze tilted disk precession and negative superhumps in the dwarf nova HS 2325+8205, revealing complex variability patterns and their correlations, advancing understanding of accretion disk dynamics in cataclysmic variables.

Contribution

First comprehensive multi-window analysis of tilted disk precession and negative superhumps in HS 2325+8205, linking observed variability to disk and accretion processes.

Findings

Identified negative superhump period of 0.185671 days.

Detected a precession period of approximately 3.943 days.

Observed bi-periodic eclipse depth variations at ~4.131 and ~2.065 days.

Abstract

Tilted disk precession exists in different objects. Negative superhumps (NSHs) in cataclysmic variable stars (CVs) are believed to arise from the interaction between the reverse precession of a tilted disk and the streams from the secondary star.Utilizing TESS photometry, we present a comprehensive investigation into the tilted disk precession and NSHs in the dwarf nova (DN) HS 2325+8205, employing eclipse minima, eclipse depths, NSH frequencies, and NSH amplitudes and the correlation between them as the windows. We identified NSHs with a period of 0.185671(17) days in HS 2325+8205. The NSH frequency exhibits variability with a period of 3.943(9) days, akin to the tilted disk precession period validated in novae-like stars (NLs, SDSS J0812) and intermediate polars (IPs, TV Col).The O-C of eclipse minima were similarly found to vary cyclically in period 4.135(5) days, characterized by a faster rise than fall. Furthermore, the NSH amplitude exhibits complex and diverse variations, which may be linked to changes in the disk radius, mass transfer rate, and the apparent area of the hot spot. For the first time in DNe, we observe bi-periodic variations in eclipse depth (P1= 4.131(4) d and P2= 2.065(2) d ~ Pprec/2), resembling those seen in IPs, suggesting that variations with P2 are not attributable to an accretion curtain, as previously suspected. Moreover, NSH amplitude and eclipse depth decrease with increasing NSH frequency, while NSH amplitude correlates positively with eclipse depth.These complex variations observed across multiple observational windows provide substantial evidence for understanding of tilted disk precession and NSHs.