GU Bootis: A New 0.6 M☉ Detached Eclipsing Binary

By Mercedes López-Morales, I. Ribas. 2005

142 citations recorded by the source corpus.

We have found a new low-mass, double-lined, detached eclipsing binary, GU Boo, among a sample of new variables from the ROTSE-I database. The binary has an orbital period of 0.488728 ± 0.000002 days and estimated apparent magnitudes Vrotse ≃ 13.7 and I ≃ 11.8. Our analysis of the light and radial velocity curves of the system yields individual masses and radii of M1 = 0.610 ± 0.007 M☉, M2 = 0.599 ± 0.006 M☉, R1 = 0.623 ± 0.016 R☉, and R2 = 0.620 ± 0.020 R☉. The stars in GU Boo are therefore very similar to the components of the eclipsing binary YY Gem. For this study we have adopted a mean effective temperature for the binary of Teff = 3870 ± 130 K. Based on its space velocities we suggest that GU Boo is a main-sequence binary, possibly with an age of several Gyr. The metallicity of the binary is not well constrained at this point, but we speculate that it should not be very different from solar. We have compared the physical parameters of GU Boo with current low-mass stellar models, accounting for uncertainties in age and metallicity by considering a wide range of values for those parameters. Our comparisons reveal that all the models underestimate the radii of the components of GU Boo by at least 10%-15%. This result is in agreement with the recent studies of YY Gem and CU Cnc.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/488854984f37c6af0240b5552d332526bd1b6af0

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Citations in the corpus

The Stellar Populations of Praesepe and Coma Berenices (2007, result): “We have addressed this problem by increasing the masses of M1 stars by 5%, M2 stars by 10%, and later type stars by 20%; these adopted values are more consistent with the observations (e.g., Lacy 1977; Delfosse et al. 1999; Creevey et al. 2005; Lopez-Morales & Ribas 2005).”
Confirmation of the Electron Cyclotron Maser Instability as the Dominant Source of Radio Emission from Very Low Mass Stars and Brown Dwarfs (2008, background): “…eclipsing binary systems or interferometric studies of single stars, has been reported (Ribas 2006, and references therein), possibly due to the effects of activity (Mullan & McDonald 2001; López-Morales & Ribas 2005; López-Morales 2007; Morales et al. 2008) or metallicity (Berger et al. 2006).”
STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS (2012, background): “Additional evidence for this ongoing discrepancy can be found in the works of, e.g., López-Morales & Ribas (2005), von Braun et al. (2008), and Boyajian et al. (2008), providing motivation for adjustments to models in order to match the observations (Chabrier et al. 2007; Dotter et al. 2008) and…”
Accurate masses and radii of normal stars: modern results and applications (2009, background): “The effect is even more obvious for M stars (Torres & Ribas 2002; Ribas 2003; López-Morales & Ribas 2005).”
Masses and Radii of Low-Mass Stars: Theory Versus Observations (2005, unknown): “These are BW3 V38 (Maceroni & Montalbán 2004), TrES-Her0-07621 (Creevey et al. 2005), and GU Boo (López-Morales & Ribas 2005).”
M dwarfs: effective temperatures, radii and metallicities (2008, background): “Alternatively, it has also been suggested that the larger radii could simply be an effect of flux conservation in a magnetic spotcovered stellar surface (López-Morales & Ribas 2005).”
THE MASS–RADIUS(–ROTATION?) RELATION FOR LOW-MASS STARS (2010, background): “…low-mass eclipsing systems like GU Boo have found that the inferred radii can change by ∼1–2% depending on the details of spot modeling (e.g. Lopez-Morales & Ribas 2005 versus Morales et al. 2009); observations of other systems also find spots to be significant at this level (e.g. Irwin…”
Detection of carbon monoxide in the high-resolution day-side spectrum of the exoplanet HD 189733b (2013, background): “Precise dynamical measurements of the masses and radii of low-mass stars in DLEBs are not well-reproduced by stellar evolutions models and have radii that are up to 15% larger than predicted (López-Morales & Ribas 2005; Ribas 2006).”
On the Correlation between the Magnetic Activity Levels, Metallicities, and Radii of Low-Mass Stars (2007, methodology): “The distances to all the other bright binaries were compiled from Chabrier & Baraffe (1995), Torres & Ribas (2002), Ribas (2003), López-Morales & Ribas (2005), Lacy et al. (2005), and Torres et al. (2006).”