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Observation and modelling of main-sequence star chromospheres - XVI. Rotation of dK5 stars
Using two different spectrographs, High Accuracy Radial velocity PlanetSearch (HARPS) (European Southern Observatory) and SOPHIE (Observatoirede Haute Provence), we have measured v sin i for a sample of dK5 stars.These are the first measurements of v sin i for most of the starsstudied here.We measured v sin i to an accuracy of 0.3 km s-1 and adetection limit of about 0.5-1 km s-1. All our targets havesimilar (R - I)c colour. This is an advantage and facilitatesthe determination of the narrowest line profiles for v sin i ˜ 0.In our total sample, we detected rotation for 22 stars (three dK5e and19 dK5 stars), and we did not detect rotation in a further 22 stars.This result shows that there are many dK5 slow rotators, and many morethan for dM1 stars. We also report on a newly discovered dK5e star, McC522, which is also the fastest rotator in our sample.We determine radii and effective temperatures for all our target stars.The effective temperatures were derived using the (R - I)ccolour and empirical far-red colour-effective temperature correlations,and the radii were derived from the standard formulae relatingMbol, bolometric correction and Teff.We find that the distribution of P/sin i (the projected rotation period)is rather homogeneous, i.e. the distribution of the 22 detected stars asa function of P/sin i is approximately flat and does not show anymaximum, unlike for dM1 stars, a close spectral type. We find that thedistribution in v sin i is bimodal, as in dM1 stars, with fast dK5erotators and slower dK5 rotators. Based on observations available atObservatoire de Haute Provence and the European Southern Observatorydata bases and on Hipparcos parallax measurements.
| Space Motions of Low-Mass Stars. III.
Radial velocity observations are presented for 149 stars taken from theMcCormick lists of dwarf K and M stars in a continuing program of radialvelocities of faint nearby stars. The data will serve to derive a totalstellar density of these kinds of stars in the solar neighborhood. Thesedata were obtained with the spectrometer of the Vilnius UniversityObservatory mounted on the 1.6 m Kuiper Telescope of the StewardObservatory.
| Photometry of dwarf K and M stars
An observational program using UBVRI photometry is presented for 688stars from among the dwarf K and M stars already found spectroscopicallyby Vyssotsky (1958). Of these, 211 have not been observedphotometrically. These observations were obtained over a period ofseveral years at the Kitt Peak National Observatory using a GaAsphotomultiplier with an 0.9 m reflector. Based on night-to-nightvariations in the measures of individual stars, the internal errors maybe estimated to be roughly 0.01 mag for the colors and 0.015 for the Vmagnitudes. The photometric parallaxes reported for each star werecomputed in the manner discussed by Weis (1986).
| Dwarf M stars found spectrophotometrically .
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1956AJ.....61..201V&db_key=AST
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Membre dels grups següents:
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Dades d'Observació i Astrometria
| Constel·lació: | Ursa Major |
| Ascensió Recta: | 10h22m07.41s |
| Declinació: | +39°26'54.6" |
| Magnitud Aparent: | 10.989 |
| Moviment propi RA: | 108.2 |
| Moviment propi Dec: | -97.8 |
| B-T magnitude: | 12.018 |
| V-T magnitude: | 11.074 |
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