Observations of interstellar helium with a gas absorption cell - Implications for the structure of the local interstellar medium

Details Observations of interstellar helium with a gas absorption cell - Implications for the structure of the local interstellar medium Observations of interstellar helium with a gas absorption cell - Implications for the structure of the local interstellar medium

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....83...58f&link_type=abstract

Astronomy and Astrophysics, vol. 83, no. 1-2, Mar. 1980, p. 58-64.

Astronomy and Astrophysics

Astrophysics

9

Helium Atoms, Interstellar Gas, Line Spectra, Ultraviolet Spectra, Apollo Soyuz Test Project, Astronomical Photometry, Data Processing, Gas Heating

Scientific paper

A photometer sensitive at the 584 A line of He 1, incorporating a helium gas resonance absorption cell, was flown on the Apollo-Soyuz Test Project in July 1975. The instrument observed much of the night-time sky, and returned 42 min of usable data. The data were analyzed by fitting to a model of resonant scattering of solar 584 A flux from nearby interstellar helium. Good model fits were obtained for an interstellar gas bulk velocity vector pointing toward alpha = 72 deg, delta = +15 deg, with speed 20 km/s, with interstellar medium temperatures from 5000 to 20,000 K and with neutral interstellar helium density (8.9 plus or minus 10 to the -3rd/cu cm). In the context of theoretical studies of the interstellar medium by McKee and Ostriker (1977), the results may indicate that the sun lies in the warm, partially ionized periphery of a cold interstellar cloud, surrounded by a high-temperature gas heated by old supernova remnants.

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