Chemistry in T Tauri winds

Details Chemistry in T Tauri winds Chemistry in T Tauri winds

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.230..695r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 230, Feb. 15, 1988, p. 695-704.

Astronomy and Astrophysics

Astronomy

24

Abundance, Cosmochemistry, Interstellar Chemistry, Stellar Winds, T Tauri Stars, Carbon Monoxide, Hydrogen, Interstellar Matter

Scientific paper

The chemistry occurring in the winds of T Tauri stars is investigated. On the assumption that the wind is dust-free, routes to H2 are inhibited under the conditions in the wind, and subsequent chemistry does not produce substantial molecular abundances. The major losses to the chemical network lie in the geometrical dilution and collisional dissociation rather than in chemical destruction and photodissociation. Mass loading of the wind with dust and H2 may, however, occur. This stimulates the chemistry and may in some circumstances lead to a conversion of about 1-10 percent of carbon into CO. This gives a column density of CO which is marginally detectable. A positive detection of CO at high wind velocities would imply that the winds must be cool and that mixing of molecular material from a disk, which may play a role in collimating the wind, or the remnants of a disk, must occur.

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