Rr-Lyrae Delta-Scuti Sx-Phoenicis Stars and Baade-Wesselink Method - Part Four - Physical Parameters and Distances of Bs-Aquarii and Dy-Pegasi and the Period / Radius Relations for Pulsating Stars

Details Rr-Lyrae Delta-Scuti Sx-Phoenicis Stars and Baade-Wesselink Method - Part Four - Physical Parameters and Distances of Bs-Aquarii and Dy-Pegasi and the Period / Radius Relations for Pulsating Stars Rr-Lyrae Delta-Scuti Sx-Phoenicis Stars and Baade-Wesselink Method - Part Four - Physical Parameters and Distances of Bs-Aquarii and Dy-Pegasi and the Period / Radius Relations for Pulsating Stars

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...159..261b&link_type=abstract

Astronomy and Astrophysics, Vol.159, NO.1&2:APRII, P. 261, 1986

Astronomy and Astrophysics

Astrophysics

21

Scientific paper

The observations of the Scuti star BS Aqr and of the SX Phoenicis star DY Peg in Geneva photometry and radial velocity with CORAVEL are analysed. Three different versions of the Baade-Wesselink method are applied and the following values of the physical parameters and distance are derived: It is shown that DY Peg has an evolutionary status probably similar to that of the three known variable blue straggler stars in the globular cluster ω Centauri. A general log R vs. log P diagram is constructed, collecting the Baade-Wesselink radii for seventy stars in six classes of pulsating variables: the classical cepheids and the W Virginis, BL Herculis, RR Lyrae, δ Scuti, and SX Phoenicis stars. This observational diagram is discussed on the basis of theoretical predictions from models of pulsating stars.

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