# Modelling of an eclipsing RS CVn-binary: V405 And

Source: [Modelling of an eclipsing RS CVn-binary: V405 And](<https://www.sota2.com/research/paper/68fa2b491e209131ce845522>)

Collection index: [llms.txt](<https://www.sota2.com/research/llms.txt>)

Data updated: 2025-10-24T14:05:28.049Z

Authors: K. Vida, K. Ol\\'ah, Zs. K\\H{o}v\\'ari

Published: 2012-05-29T15:06:47.000Z

## Abstract

V405 And is an ultrafast-rotating (P\_rot ~ 0.46 days) eclipsing binary. The system consists of a primary star with radiative core and convective envelope, and a fully convective secondary. Theories have shown, that stellar structure can depend on magnetic activity, i.e., magnetically active M-dwarfs should have larger radii. Earlier light curve modelling of V405 And indeed showed this behaviour: we found that the radius of the primary is significantly larger than the theoretically predicted value for inactive main sequence stars (the discrepancy is the largest of all known objects), while the secondary fits well to the mass-radius relation. By modelling our recently obtained light curves, which show significant changes of the spotted surface of the primary, we can find further proof for this phenomenon.

## Recorded benchmark results

A research result applies to its stated dataset, split, metric and evaluation configuration. Compare like-for-like settings, preserve the metric's unit and direction, and distinguish paper-reported results from independent reproduction. The best result recorded here is not a claim of exhaustive, current global coverage.

## Original sources and implementation

[Original paper](<https://arxiv.org/abs/1205.6384>)

[PDF](<https://arxiv.org/pdf/1205.6384.pdf>)