Two Long-Period Cataclysmic Variable Stars: ASASSN-14ho and V1062 Cyg

TL;DR

This study presents spectroscopic and photometric analysis of two long-period dwarf novae, ASASSN-14ho and V1062 Cyg, revealing their secondary star types, orbital periods, and unique emission features, contributing to understanding of cataclysmic variables.

Contribution

First detailed characterization of long-period cataclysmic variables ASASSN-14ho and V1062 Cyg, including secondary star classification and orbital parameters.

Findings

Secondary stars classified as K4 and M0.5.

Orbital periods nearly identical at ~350 minutes.

Unique H-alpha emission feature in V1062 Cyg.

Abstract

We report spectroscopy and photometry of the cataclysmic variable stars ASASSN-14ho and V1062 Cyg. Both are dwarf novae with spectra dominated by their secondary stars, which we classify as approxomately K4 and M0.5, respectively. Their orbital periods, determined mostly from the secondary stars' radial velociites, proved to be nearly identical, respectively 350.14 +- 0.15 and 348.25 +- 0.60 min. The H-alpha emission line in V1062 Cyg displays a relatively sharp emission component that tracks the secondary's motion, which may arise on the irradiated face of the secondary; tihs is not often seen and may indicate an unusually strong flux of ionizing radiation. Both systems exhibit double-peaked orbital modulation consistent with ellipsoidal variation from the changing aspect of the secondary. We model these variations to constrain the orbital inclination i, and estimate approximate component masses based oni and the secondary velocity amplitude K2.