Radio observations of OH toward Zeta Ophiuchi - Evidence for an interstellar shock

Details Radio observations of OH toward Zeta Ophiuchi - Evidence for an interstellar shock Radio observations of OH toward Zeta Ophiuchi - Evidence for an interstellar shock

Aug 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...231l.151c&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 231, Aug. 1, 1979, p. L151-L153.

Astronomy and Astrophysics

Astronomy

29

Hydroxyl Emission, Interstellar Matter, O Stars, Radio Astronomy, Shock Waves, Electromagnetic Absorption, H Ii Regions, Interstellar Gas, Line Spectra

Scientific paper

The 1667-MHz line of OH has been observed toward Zeta Ophiuchi and toward several dusty patches seen projected on the H II region. The column density of OH from radio and that from optical data agree. The OH is in two velocity components, at about -0.5 km/s and 5 km/s. The more negative velocity is that of the strongest atomic and molecular lines observed both at optical and radio wavelengths toward Zeta Ophiuchi, with the notable exception of CH(+). The more positive velocity is that of the dust seen in projection. The OH data, together with information about the distance of the material from the star, provide strong support for the theory of Elitzur and Watson (1978) that CH(+) is formed by a shock produced by Zeta Ophiuchi.

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