Doctoral thesis for the University of Texas at Austin.
|Statement||George Thomas O"Brien, Jr.|
Spectra of the He I line have been obtained for 23 metal-poor stars, the majority of which are dwarfs ranging in metallicity from [Fe/H] = to The Angstrom Helium Line Among Evolved Stars in the Globular Cluster M4 We have obtained spectra of the chromospheric He I A line in 16 red horizontal branch, red giant branch, and Here we present a spectroscopic study of helium in the nearby globular cluster M4. We have obtained spectra of the chromospheric He I A line in 16 red horizontal branch, red giant branch, and asymptotic giant branch stars. Clear He I absorption or emission is present in most of the :// The new spectra show that nine of the ten stars observed have P-Cygni or asymmetric blue-shifted profiles in the He I $\lambda$ line. In all cases, the He I line indicates a mass outflow
Proc. SPIE , Optical Spectroscopic Techniques and Instrumentation for Atmospheric and Space Research, pg 2 (30 September ); doi: / The un-normalized spectrum of β Peg around cm −1. One full order and parts of two neighbouring orders on either side are presented. Three distinct water lines can be seen in the middle :// The line profiles (on 1st August, ) in the helium-rich white dwarf, L Note the enormous strength of these lines, the broad and often asymmetrical wings, and the relatively sharp cores. For comparison I give the He I line ;t in a helium-rich subdwarf HZ A modeling study involving the spreading of the incident particles in a proton aurora has been reported by Jasperse (). Helium emissions. 10, Å emissions from metastable state of orthohelium (2 3 S) in sunlit aurora was reported by Mironov
UNITS. e traditional and fundamental unit of wavelength Th in optical spectroscopy is the angstrom, symbol A, now defined as exactly lo meter. By adoption of a resolution, the 11th General Conference of Weights and Measures (October, ) has defined the meter as equal to wavelengths in vacuum of the orange line of ] krypton Abstract. This report has been prepared by the President in collaboration with the Secretary of the Commission. It is based on (1) material supplied by those members and associates of the Commission who responded to requests made in our circulars, (2) a bibliographical search intended to supplement the above material, (3) discussions with other interested persons, and (4) our own knowledge and The considered Stark broadening data have been entered into a spectrum synthesis program for binary stars and have been used for the helium surface mapping and spectrum variability considerations of ET Andromedae [23,26], for the investigation of the He λ Å spectral line formation mechanism in classical cepheides, for the consideration Abstract. In Sect. we describe methods for determining the opacity for atomic mixtures. This implies absence of chemical bonding, i.e., temperatures and densities are such that molecules are dissociated. It also implies that ion–ion interactions, such as their effects on line broadening, are ://