Observational astrophysics from rockets. stellar spectra
Ultraviolet aurora with north-south asymmetry and stellar spectra taken from aerobee rocket flight
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Ultraviolet aurora with north-south asymmetry and stellar spectra taken from aerobee rocket flight
Ultraviolet rocket spectrometer for measuring stellar spectra
Line blanketing attenuation of stellar UV RADIATION from rocket observation, noting B-star atmosphere
Interstellar extinction in middle UV, deriving normalized curve from photoelectric photometry data
Theoretical line profiles in UV spectra of two early B stars from 911.6 to 3000 angstroms
B1 V star model atmosphere calculated and iterated for flux constancy, considering blanketing by strongest lines in UV
Sky survey in two IR spectral ranges, obtaining unbiased census of objects emitting in atmospheric window
Lithium/calcium ratio of five F giant and six G giant stars
Stellar spectroscopy in UV region using f/2 Schmidt camera onboard Aerobee rockets
Visible spectrum of radiation release from type I supernova outburst
Slitless absolute spectral photometry method for atmospheric entry and astronomical radiation measurements
Continuous spectra of hot white dwarfs, and color indexes of such stars with hydrogen and helium atmospheres
Lithium content in spectra of T Taurus type stars and in cosmic rays
Abnormal low helium abundance in atmospheres of old halo B star based on weak absorption lines in helium spectra
Classification of slit spectrograms of 185 bright stars in Morgan-Keenan system
Far UV spectra of brighter stars in vicinity of epsilon Orionis photographed with objective spectrograph carried by rocket
Spectra of the radio-quiet quasar PHL 957 were obtained at a 200-in. telescope with a Cassegrain image tube, a Cassegrain multichannel spectrometer, and an integrating television camera on the spectrograph. The image-tube spectra revealed 64 absorption lines between 3200 and 6800 A. The absolute energy distribution indicates that this quasar is one of the most luminous known. The absorption line redshifts and line profiles observed are discussed.