Modeling the Photometric Variability of Alpha\(^2\) CVn with a Dynamical Magnetosphere

Alpha\(^2\) Canum Venaticorum (AM CVn) is a strongly magnetic star with peculiar chemical signatures and periodic variability that have been long attributed to the diffusion of magnetic elements through the photosphere, leading to chemical spots across the stellar surface. However, recent studies of...

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Bibliographic Details
Published in:arXiv.org 2022-07
Main Authors: Pfeffer, Cameron M, McSwain, M Virginia
Format: Article
Language:English
Subjects:
Extrasolar planets
Hot stars
Magnetic dipoles
Magnetic stars
Magnetospheres
Modelling
Photosphere
Planet detection
Stellar surfaces
Transit
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Summary:Alpha\(^2\) Canum Venaticorum (AM CVn) is a strongly magnetic star with peculiar chemical signatures and periodic variability that have been long attributed to the diffusion of magnetic elements through the photosphere, leading to chemical spots across the stellar surface. However, recent studies of other magnetic hot stars are consistent with magnetospheric clouds above the surface. Here we take a renewed approach to modeling AM CVn with a simplified dynamical magnetosphere (DM) and a tilted, offset magnetic dipole to reproduce its Transiting Exoplanet Survey Satellite (TESS) variability. Our dipole model also reproduces well the magnetic surface map of AM CVn from Silvester, Kochukhov, & Wade (2014). Its ultraviolet variability, from IUE archival spectra, is also consistent with traditional reddening models. We further discuss the implications of a magnetosphere on other observable quantities from the system to conclude that it is unlikely to be present in AM CVn.
ISSN:2331-8422
DOI:10.48550/arxiv.2207.11151