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Far-ultraviolet intensities of Orion stars

Published online by Cambridge University Press:  14 August 2015

George R. Carruthers
George R. Carruthers*
Affiliation:
E. O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, D.C., U.S.A.

Abstract

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Photometric data in the 1050–1180 Å and 1230–1350 Å wavelength ranges, and electronographic spectra in the 1000–1600 Å wavelength range, were obtained in an Aerobee rocket flight on January 30, 1969. The spectral intensities derived from these data for main-sequence stars are in good agreement with the model atmospheres of Morton and co-workers. Giant and supergiant stars, however, appear to be up to one magnitude weaker, at 1115 Å, than main-sequence stars of the same spectral class.

The correction for interstellar reddening appears to be not inconsistent with a 1/λ extrapolation of earlier determinations of Smith (1967) and Stecher (1965), except in the case of θ Ori, in which the predicted color excess appears to be much too great, confirming the existence of a peculiar reddening law in the Orion Nebula region.

Type
Part I: Stellar Fluxes
Information
Symposium - International Astronomical Union , Volume 36: Ultraviolet Stellar Spectra and Related Ground-Based Observations , 1970 , pp. 100 - 108
Copyright
Copyright © Reidel 1970 

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