RR Lyrae, Delta Scuti, SX Phoenicis stars and Baade-Wesselink method. III - Physical parameters and distance of DX Del, and the problem of the mean absolute magnitude of RR Lyrae stars. IV - Physical parameters and distances of BS AQR and DY Peg, and the p

Details RR Lyrae, Delta Scuti, SX Phoenicis stars and Baade-Wesselink method. III - Physical parameters and distance of DX Del, and the problem of the mean absolute magnitude of RR Lyrae stars. IV - Physical parameters and distances of BS AQR and DY Peg, and the p RR Lyrae, Delta Scuti, SX Phoenicis stars and Baade-Wesselink method. III - Physical parameters and distance of DX Del, and the problem of the mean absolute magnitude of RR Lyrae stars. IV - Physical parameters and distances of BS AQR and DY Peg, and the p

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...159..255b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 159, no. 1-2, April 1986, p. 255-268.

Astronomy and Astrophysics

Astrophysics

28

Astronomical Photometry, Radial Velocity, Stellar Magnitude, Variable Stars, Distance, Electrophotometry, Metallicity

Scientific paper

The observations of the RR Lyrae star DX Del in Geneva photometry and radial velocity with CORAVEL are analysed. Three different versions of the Baade-Wesselink method are applied to derive the mean radius. The physical parameters are determined, in particular R0 = 5.5 ± O.2 Rsun and Mv =0.49 ± 0.16. The distance to the sun is 75O ± 45 pc. The total uncertainties on these quantities are roughly twice as large as the mathematical values given here. The various determinations of the mean absolute magnitude of the RR Lyrae stars are compared. A mean value < Mv > =0.57 ± 0.09 can be derived from the 7 stars for which the Baade-Wesselink method has been successfully applied. However, the RR Lyrae stars of intermediate metallicity ([Fe/H] ≅ -1.2) could be brighter, by about 0.2, than either the very deficient ones ([Fe/H] ≅ -2.0) or those with [Fe/H] ≅ 0.

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