Accurate masses and radii of normal stars

Andersen, J.

doi:10.1007/bf00873538

Cited by 665 publications

(658 citation statements)

References 80 publications

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“…Raising Z to 0.02 would increase M 1 and M 1 by 4 per cent, so uncertainties of ±0.1 M are appropriate. The value of 2.05 M for M 2 is fully in accordance with Andersen (1991), whose plot of mass against (B − V ) suggests that an A3 dwarf such as 12 Com B is likely to have a mass in the range 1.9-2.3 M . By substituting the values for M 1 and M 2 in the orbit solution (Table 5) …”

Section: Masses Of the Component Starssupporting

confidence: 79%

Composite spectra: XVII. 12 Comae, a member of the Coma open cluster

Griffin

Griffin²

2011

Astron Nachr

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The components of binary stars offer the potential to examine the predictions of stellar-evolution theory with particularly tight constraints. Those constraints are further tightened when the binary belongs to a cluster whose properties have been well determined independently. 12 Comae presents both advantages, belonging as it does to the Coma Cluster, Melotte 111. The orbit of 12 Comae has an eccentricity of nearly 0.6 and a period of 13 months. By a process of subtraction we separate the spectra of the component stars, derive a precise double-lined orbit solution, and by modelling the photometry we extract the individual stellar photometric and physical properties, ages and rotation. By fitting theoretical evolutionary tracks to the positions of the stars in the H-R diagram we confirm their individual masses, and derive a ZAMS of ∼0.65 Gyr, which accords well with measurements published for the cluster itself. We show that the primary of 12 Comae is an evolving giant of spectral type ∼G7 and mass 2.6 M , while its secondary (whose spectrum could be isolated particularly cleanly) is an A3 dwarf which has a mass of 2.05 M and has commenced its evolution away from the main sequence. There is evidence that both stars are slightly metal-weak (−0.25 < [Fe/H] < 0.0), well in keeping with analyses of other members of this cluster.

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Section: Masses Of the Component Starssupporting

confidence: 79%

Composite spectra: XVII. 12 Comae, a member of the Coma open cluster

Griffin

Griffin²

2011

Astron Nachr

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“…If the metallicity is known, and if the surface brightness of each component is well determined (through spectroscopic or photometric estimate of effective temperature), tests of evolutionary models of single stars can be made, provided the components are sufficiently far apart ("detached" systems). Such tests have been discussed by, e.g., Andersen (1991).…”

Section: Introductionmentioning

confidence: 99%

New distance and depth estimates from observations of eclipsing binaries in the SMC

2008

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Abstract.A sample of 33 eclipsing binaries observed in a field of the SMC with FLAMES@VLT is presented. The radial velocity curves obtained, together with existing OGLE light curves, allowed the determination of all stellar and orbital parameters of these binary systems. The mean distance modulus of the observed part of the SMC is 19.05 mag, based on the 26 most reliable systems. Assuming an average error of 0.1 mag on the distance modulus to an individual system, and a gaussian distribution of the distance moduli, we obtain a 2-σ depth of 0.36 mag or 10.6 kpc. Some results on the kinematics of the binary stars and of the H ii gas are also given.

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“…Such M-dwarf eclipsing binaries are straightforward to detect from MEarth data, and it should be possible to characterise them extremely well due to their brightness, allowing model-independent mass and radius estimates with uncertainties of only a few percent to be made (e.g. Andersen 1991). …”

Section: Statusmentioning

confidence: 99%

The MEarth project: searching for transiting habitable super-Earths around nearby M dwarfs

et al. 2008

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Abstract. Due to their small radii, M dwarfs are very promising targets to search for transiting super-Earths, with a planet of 2 Earth radii orbiting an M5 dwarf in the habitable zone giving rise to a 0.5% photometric signal, with a period of two weeks. This can be detected from the ground using modest-aperture telescopes by targeting samples of nearby M dwarfs. Such planets would be very amenable to follow-up studies due to the brightness of the parent stars, and the favourable planet-star flux ratio. MEarth is such a transit survey of ∼ 2000 nearby M dwarfs. Since the targets are distributed over the entire (Northern) sky, it is necessary to observe them individually, which will be done by using 8 independent 0.4m robotic telescopes, two of which have been in operation since December 2007 at the Fred Lawrence Whipple Observatory (FLWO) located on Mount Hopkins, Arizona. We discuss the survey design and hardware, and report on the current status of the survey, and preliminary results obtained from the commissioning data.

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Accurate masses and radii of normal stars

Cited by 665 publications

References 80 publications

Composite spectra: XVII. 12 Comae, a member of the Coma open cluster

Composite spectra: XVII. 12 Comae, a member of the Coma open cluster

New distance and depth estimates from observations of eclipsing binaries in the SMC

The MEarth project: searching for transiting habitable super-Earths around nearby M dwarfs

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