Skip to main content
OSTI.GOVU.S. Department of Energy Office of Scientific and Technical Information
U.S. Department of Energy
Office of Scientific and Technical Information
 

Search for optical coronal line emission from the x-ray sources epsilon Orionis (B0 Ia) and kappa Orionis (B0. 5 Ia)

Journal Article · · Astrophys. J.; (United States)
DOI:https://doi.org/10.1086/159192· OSTI ID:5883805
; ;
High signal-to-noise observations have been made at the wavelengths of the lines of (Fe X) 6574 A and (Fe XIV) 5303 A to search for evidence of a coronal region at the base of the winds of epsilon Ori (B0 Ia) and kappa Ori (B0.5 Ia). These two stars have been detected as soft X-ray sources with the Imaging Proportional Counter (IPC) detector on board the Einstein X-Ray Observatory, and both stars also show anomalously strong O VI lines in the UV spectra, which has been explained as a product of Auger ionization in cool stellar wind. From the total X-ray flux and Auger-enhanced ionization, large coronal emission measures of a base corona were expected. The nondetection of the iron coronal lines places new upper limits on the emission measure if the coronal temperature is in the range 0.7 x 10/sup 6/1 x 10/sup 6/ for kappa Ori and T/sub c/>2 x 10/sup 6/ for epsilon Ori. For epsilon Ori the contraints are then no longer compatible with the energy distribution measured with the IPC. It is suggested that at least some of the X-rays arise not from the base corona, but from source regions farther out in the wind.
Research Organization:
Washburn Observatory, University of Wisconsin: Madison
OSTI ID:
5883805
Journal Information:
Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 248:2; ISSN ASJOA
Country of Publication:
United States
Language:
English

Similar Records

Detection of the Fe XIV 5303 A coronal line in the supernova remnant Vela X
Journal Article · Mon Sep 15 00:00:00 EDT 1975 · Astrophys. J., v. 200, no. 3, pp. 715-718 · OSTI ID:4123898
Fe XIV solar corona at 5303 angstroms: an atlas of synoptic charts from the Sacramento Peak Coronal Photometer, May 1973-December 1985. Technical note
Technical Report · Sat Jan 31 23:00:00 EST 1987 · OSTI ID:6269707
The latitudinal structure of solar wind streams from radio scintillation observations
Technical Report · Fri Jun 02 00:00:00 EDT 1978 · OSTI ID:6181997

Related Subjects

640103* -- Astrophysics & Cosmology-- Quasi-Stellar
Radio
& X-Ray Sources-- (-1987)
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
AUGER EFFECT
CHARGED PARTICLES
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
ELECTROMAGNETIC RADIATION
EMISSION
GIANT STARS
IONIZING RADIATIONS
IONS
IRON IONS
MAIN SEQUENCE STARS
OXYGEN IONS
RADIATION FLUX
RADIATIONS
SPECTRA
STARS
STELLAR ATMOSPHERES
STELLAR WINDS
SUPERGIANT STARS
VISIBLE SPECTRA
X RADIATION