ACCURATE LOW-MASS STELLAR MODELS OF KOI-126

被引：54

作者：

Feiden, Gregory A. ^{[1
]}

Chaboyer, Brian ^{[1
]}

Dotter, Aaron ^{[2
]}

机构：

[1] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA

[2] Space Telescope Sci Inst, Baltimore, MD 21218 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 740卷 / 01期

基金：

美国国家科学基金会;

关键词：

binaries: eclipsing; stars: evolution; stars: low-mass; starspots; EVOLUTIONARY MODELS; ELEMENT DIFFUSION; GLOBULAR-CLUSTERS; MAIN-SEQUENCE; STARS; ISOCHRONES; OPACITIES; ABUNDANCE; EQUATION; RADII;

D O I：

10.1088/2041-8205/740/1/L25

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The recent discovery of an eclipsing hierarchical triple system with two low-mass stars in a close orbit (KOI-126) by Carter et al. appeared to reinforce the evidence that theoretical stellar evolution models are not able to reproduce the observational mass-radius relation for low-mass stars. We present a set of stellar models for the three stars in the KOI-126 system that show excellent agreement with the observed radii. This agreement appears to be due to the equation of state implemented by our code. A significant dispersion in the observed mass-radius relation for fully convective stars is demonstrated; indicative of the influence of physics currently not incorporated in standard stellar evolution models. We also predict apsidal motion constants for the two M dwarf companions. These values should be observationally determined to within 1% by the end of the Kepler mission.

引用

页数：5

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