The Spectroscopic Orbit and Pulsation Mode of the Cepheid Polaris

Details The Spectroscopic Orbit and Pulsation Mode of the Cepheid Polaris The Spectroscopic Orbit and Pulsation Mode of the Cepheid Polaris

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4401t&link_type=abstract

American Astronomical Society Meeting 208, #44.01; Bulletin of the American Astronomical Society, Vol. 38, p.118

Astronomy and Astrophysics

Astronomy

2

Scientific paper

The spectroscopic subsystem of the bright Cepheid Polaris has undergone four complete orbits since the beginning of spectroscopic coverage in the 1880s. The recent detection of the unresolved companion by Evans et al. (2006) with the Hubble Space Telescope raises the possibility of constraining the distance to Polaris using the spectroscopic orbit. To that end, the existing radial velocity data, including previously unpublished observations from the past two decades, have been collected, reanalyzed, and examined, with the aim of providing improved orbital parameters for the spectroscopic binary. Small anomalies exist in some of the radial velocity data, perhaps a consequence of different sets of spectral lines and wavelength coverage used to infer the photospheric motion, or to the inevitable problems of establishing reliable systemic velocities for a pulsating star. The new orbital parameters for Polaris do not differ greatly from those established by Kamper (1996), yet they imply a maximum distance to the star of about 100 pc, well below the value inferred from its Hipparcos parallax. The results directly affect how we interpret the pulsation mode of the Cepheid.

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