Infrared Observations of AR Ursae Majoris: Modeling the Ellipsoidal Variations
Abstract
We have obtained time-series infrared photometry for the highly magnetic cataclysmic variable AR UMa. Our J and K' band observations occurred during a low state and they show a distinctive double-humped structure. Using detailed models for the expected ellipsoidal variations in the infrared due to the non-spherical secondary star, we find that the most likely value for the system inclination is 70 degrees. We also model low state V band photometry and find that its observed double-humped structure is not caused by ellipsoidal variations, as they have been ascribed to, but are due to beamed cyclotron radiation. We use this result to estimate the magnetic field strength of the active southern accretion region (B <= 190 MG) and its magnetic longitude (330 degrees).
Keywords
Cite
@article{arxiv.astro-ph/0008520,
title = {Infrared Observations of AR Ursae Majoris: Modeling the Ellipsoidal Variations},
author = {Steve B. Howell and Dawn M. Gelino and Thomas E. Harrison},
journal= {arXiv preprint arXiv:astro-ph/0008520},
year = {2009}
}
Comments
Accepted to AJ, to appear Jan 2001 issue