Sizing Up the Stars

Details Sizing Up the Stars Sizing Up the Stars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21724203b&link_type=abstract

American Astronomical Society, AAS Meeting #217, #242.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

This work focuses on determining the fundamental properties of nearby, main sequence, A, F, G, K, and M-type stars. We present the results of angular diameters (average error 1.5%) obtained via interferometric observations made with the CHARA Array. These measurements combined with HIPPARCOS and ground-based parallaxes and bolometric fluxes provide an empirical determination of their effective temperatures, linear radii, and absolute luminosities. We derive empirically based relations for the stellar effective temperature for these types of stars, which are accurate to the 1% level.
Additionally, the masses and ages of the A, F, and G stars are determined by fitting the CHARA-determined temperatures, radii, and luminosities to Yonsei-Yale model isochrones, and we compare these results to those obtained by indirect methods. We show that for most cases the theoretical stellar radii for stars >1.3 Msun and <0.65 Msun are too small compared to observed radii by 5% and 15%, respectively (and temperatures too hot by 2% and 7%, respectively). For the early-type stars, these overestimated temperatures and underestimated radii appear to cause an additional offset in the star's surface gravity measurements, which consequently yield higher masses and younger ages. Furthermore, we elaborate on these discrepancies seen for the late-type stars where the onset of convection plays a significant role in determining the model radii for these stars.

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