Calibration of Luminosity of Hot Stars (Preliminary Results)

Details Calibration of Luminosity of Hot Stars (Preliminary Results) Calibration of Luminosity of Hot Stars (Preliminary Results)

Aug 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997esasp.402..307n&link_type=abstract

Proceedings of the ESA Symposium `Hipparcos - Venice '97', 13-16 May, Venice, Italy, ESA SP-402 (July 1997), p. 307-310

Physics

Scientific paper

For more than 15 years, Cramer and Maeder (1979) uses X, Y and Z parameters from the Geneva photometric system in order to estimate T_(eff), log(g) and chi for B3 to A3 stars. These methods are especially efficient for dwarf stars. The Cramer calibration will be refined thanks to the Hipparcos parallaxes. The photometric boxes (set of stars having almost the same colour indices) provide collection of stars often similar and allow the determination of very accurate statistical parallaxes. The criterium of the boxes can be more selective for hot stars having well-measured flux in the far UV by the TD-1 satellite for instance. With the Hipparcos parallaxes and the joint use of TD-1 and Geneva fluxes a calibration of hotter stars (B0.5 to B3 or so) seems realistic.

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