The binary system containing the classical Cepheid T MON

Details The binary system containing the classical Cepheid T MON The binary system containing the classical Cepheid T MON

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107.2164e&link_type=abstract

The Astronomical Journal (ISSN 0004-6256), vol. 107, no. 6, p. 2164-2171

Astronomy and Astrophysics

Astronomy

4

Binary Stars, Cepheid Variables, Companion Stars, Stellar Evolution, Stellar Luminosity, Stellar Spectra, Brightness Distribution, Iue, Radial Velocity, Velocity Distribution

Scientific paper

Several new results are presented for the binary system containing the 27d classical Cepheid T Mon. New radial velocities for the Cepheid have been obtained, which confirm the decreasing orbital motion at the current epoch. The spectral type of the companion (B9.8 V) has been determined from an International Ultraviolet Explorer (IUE) low resolution spectrum. An IUE high resolution spectrum has been measured to search for the velocity of the companion. A velocity signal at +36 km/s on JD 2,446,105.21 has been tentatively identified as the velocity of the companion, but confirmation of this velocity would be very valuable. Results based on this tentative identification of the velocity are that the companion does not have a high projected rotation velocity, that the companion is unlikely to be a short period binary, and that the gamma velocity of the system is between 20 and 36 km/s. The luminosity and temperature of both the Cepheid and the companion are well determined from the satellite and ground-based observations and the Cepheid PLC relation. However, the companion is above the ZAMS in the H-R diagram, which is inconsistent with the large luminosity difference between the two stars. High rotation for the companion (viewed pole-on) is a possible explanation. The lower limit to the mass function (from the lower limits to the orbital period and amplitude) requires a very high eccentricity for the system for reasonable estimates for the masses of the two stars.

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