The ionization of the very local interstellar gas

Details The ionization of the very local interstellar gas The ionization of the very local interstellar gas

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986aj.....92..653r&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 92, Sept. 1986, p. 653-657.

Astronomy and Astrophysics

Astronomy

21

Gas Ionization, Interstellar Gas, B Stars, Hot Stars, Solar Radiation, Spectrum Analysis, Ultraviolet Spectra, White Dwarf Stars

Scientific paper

Bertaux et al. (1985) have pointed out that the low ratio of atomic hydrogen to atomic helium densities (nH ≈ 0.05 cm-3, nHeI ≈ 0.02 cm-3) derived for the very local interstellar gas from interplanetary UV and EUV observations suggest that the local interstellar hydrogen is substantially ionized (nHII/nHI ≈ 3). In steady state this would imply an ionization rate ≡10-13s-1H-atom-1, which is much higher than that produced by cosmic rays or the diffuse X-ray background. An examination of available data on B stars and known hot white dwarf stars in the solar neighborhood reveals that the photon flux from these sources also is not capable of accounting for such a high ionization rate. The ionization appears to require either a local EUV flux of 104 - 105 photons cm-2s-1 in the 14 - 24 eV band or a transient event within the last (2 - 5)×105yr.

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