The V471 Tauri System: A Multi-datatype Probe

TL;DR

This study uses a multi-datatype approach to analyze the V471 Tauri binary system, providing new insights into its potential third body, starspot activity, and stellar parameters, with implications for common envelope evolution.

Contribution

It introduces a unified algorithm that combines diverse datasets to derive comprehensive solutions for the V471 Tauri system, including refined stellar parameters and starspot behavior.

Findings

Possible detection of a brown dwarf companion near 12 AU.

Red dwarf mass larger than typical for K2V stars.

Starspot activity decreased then stabilized over decades.

Abstract

V471 Tauri, a white dwarf--red dwarf eclipsing binary in the Hyades, is well known for stimulating development of common envelope theory, whereby novae and other cataclysmic variables form from much wider binaries by catastrophic orbit shrinkage. Our evaluation of a recent imaging search that reported negative results for a much postulated third body shows that the object could have escaped detection or may have actually been seen. The balance of evidence continues to favor a brown dwarf companion about 12 AU from the eclipsing binary. A recently developed algorithm finds unified solutions from three datatypes. New radial velocities (RVs) of the red dwarf and BV RCIC light curves are solved simultaneously along with white dwarf and red dwarf RVs from the literature, uvby data, the MOST mission light curve, and 40 years of eclipse timings. Precision-based weighting is the key to proper information balance among the various datasets. Timewise variation of modeled starspots allows unified solution of multiple data eras. Light curve amplitudes strongly suggest decreasing spottedness from 1976 to about 1980, followed by approximately constant spot coverage from 1981 to 2005. An explanation is proposed for lack of noticeable variation in 1981 light curves, in terms of competition between spot and tidal variations. Photometric spectroscopic distance is estimated. The red dwarf mass comes out larger than normal for a K2V star, and even larger than adopted in several structure and evolution papers. An identified cause for this result is that much improved red dwarf RVs curves now exist.