HS 2325+8205 - an ideal laboratory for accretion disk physics

TL;DR

HS 2325+8205 is an eclipsing dwarf nova with frequent outbursts, making it an ideal system for studying accretion disc physics in real-time through spectroscopic and photometric observations.

Contribution

This paper identifies HS 2325+8205 as an ideal laboratory for accretion disc physics due to its eclipsing nature, frequent outbursts, and well-characterized orbital parameters.

Findings

Orbital period of 279.84 minutes.

Radial velocity measurements of the secondary star and accretion disc.

Outburst recurrence time of 12-14 days.

Abstract

We identify HS 2325+8205 as an eclipsing, frequently outbursting dwarf nova with an orbital period of 279.841731(5) min. Spectroscopic observations are used to derive the radial velocity curve of the secondary star from absorption features and also from the H-alpha emission lines, originating from the accretion disc, yielding K_secondary = K_abs = 237 +- 28 km/s and K_emn = 145 +- 9 km/s respectively. The distance to the system is calculated to be 400 (+200, -140) pc. A photometric monitoring campaign reveals an outburst recurrence time of 12-14 d, The combination of magnitude range (17-14 mag), high declination, eclipsing nature and frequency of outbursts makes HS 2325+8205 the ideal system for "real-time" studies of the accretion disc evolution and behavior in dwarf nova outbursts.