Interferometric survey of Be stars with the CHARA array
نویسندگان
چکیده
منابع مشابه
First Results from the Chara Array. Iv. the Interferometric Radii of Low-mass Stars
We have measured the angular diameters of six M dwarfs with the CHARA Array, a long-baseline optical interferometer located at Mount Wilson Observatory. Spectral types range from M1.0 V to M3.0 Vand linear radii from 0.38 to 0.69 R . These results are consistent with the seven other M dwarf radii measurements from optical interferometry and with those for 14 stars in eclipsing binary systems. W...
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We report the results of high-angular-resolution observations that search for exozodiacal light in a sample of main sequence stars and sub-giants. Using the “jouvence” of the fiber linked unit for optical recombination (JouFLU) at the center for high angular resolution astronomy (CHARA) telescope array, we have observed a total of 44 stars. Out of the 44 stars, 33 are new stars added to the ini...
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We present the results of long-baseline optical interferometry observations using the Precision Astronomical Visual Observations (PAVO) beam combiner at the Center for High Angular Resolution Astronomy (CHARA) Array to measure the angular sizes of three bright Kepler stars: θ Cygni, and both components of the binary system 16 Cygni. Supporting infrared observations were made with the Michigan I...
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Context. The radius of a star is a very important constraint to evolutionary models, particularly when combined with asteroseismology. Diameters can now be measured interferometrically with great precision (better than 1%), but the center-to-limb darkening (CLD) remains a potential source of bias. Measuring this bias is possible by completely resolving the star using long-baseline interferometr...
متن کاملStarspot Imaging with the CHARA Array
We present the first results of a starspot interferometric imaging program targeting the chromospherically active giant Lambda Andromedae. Our images are constructed using a new starspot model that incorporates a power limb darkening law and starspot foreshortening. The model solutions are determined through χ minimization of observed squared visibilities, triple amplitudes and closure phase. M...
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2010
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921311011665