A reanalysis of the observed interplanetary hydrogen L. cap alpha. emission profiles and the derived local interstellar gas temperature and velocity

Journal Article · Tue Jul 01 00:00:00 EDT 1980 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/158119· OSTI ID:6757282

Wu, F M; Judge, D L

An improved model of the interplanetary emission profile is presented. In this model we utilize a new version of the modified Danby-Camm velocity distribution function to calculate emission profiles, and it appears to be very efficient. Using this model, the hydrogen L..cap alpha.. profiles are determined for various viewing directions, and at a solar distance of 1 AU. It is found that the linewidth of the emission profiles and their Doppler shifts depend strongly on the viewing direction, as well as the assumed interstellar temperature. Previous determinations of the interstellar temperature T/sub 0/ and the inflow velocity V/sub b/, using approximate theoretical hydrogen profiles, are found to be inadequate. These values are recalculated and are determined to be T/sub 0/=7000 +- 1200 K and V/sub b/=19 +- 3 km s/sup -1/.

• Research Organization: Space Sciences Institute and Department of Physics, University of Southern California
• OSTI ID: 6757282
• Journal Information: Astrophys. J.; (United States), Vol. 239:1
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC GASES
HYDROGEN
INTERPLANETARY SPACE
EMISSION
EMISSION SPECTRA
INTERSTELLAR SPACE
LINE WIDTHS
LYMAN LINES
RADIAL VELOCITY
SPECTRAL SHIFT
ULTRAVIOLET SPECTRA
ELEMENTS
FLUIDS
GASES
NONMETALS
SPACE
SPECTRA
VELOCITY
640107* - Astrophysics & Cosmology- Planetary Phenomena