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

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

Jul 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..389w&link_type=abstract

Astrophysical Journal, Part 1, vol. 239, July 1, 1980, p. 389-394.

Astronomy and Astrophysics

Astrophysics

15

Emission Spectra, Gas Temperature, H Lines, Interplanetary Medium, Interstellar Gas, Lyman Alpha Radiation, Distribution Functions, Doppler Effect, Ultrahigh Frequencies, Ultraviolet Spectra, Velocity Distribution

Scientific paper

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 Lα 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 T0 and the inflow velocity Vb, using approximate theoretical hydrogen profiles, are found to be inadequate. These values are recalculated and are determined to be T0 = 7000 ± 1200K and Vb = 19 ± 3 km s-1.

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