A close-up view of the S87 molecular outflow

Details A close-up view of the S87 molecular outflow A close-up view of the S87 molecular outflow

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345..268b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 1, 1989, p. 268-281.

Astronomy and Astrophysics

Astronomy

20

Astronomical Spectroscopy, H Ii Regions, Molecular Clouds, Nebulae, Pre-Main Sequence Stars, Charge Coupled Devices, Infrared Astronomy Satellite, Molecular Spectra, Stellar Winds, Very Large Array (Vla)

Scientific paper

Observations of the S87 star-forming region have been made at optical, far-infrared, centimeter, and millimeter wavelengths in order to explain the origin of the previously discovered supersonic molecular gas in this source. S87/IRS 1 is a massive, pre-main-sequence object still embedded in its parent molecular cloud, but disrupting its surroundings through the action of its powerful stellar wind. The shocked wind gas provides the force required to accelerate the surrounding molecular gas to supersonic velocities. An ordered, large-scale magnetic field is postulated to set up an initially anisotropic pressure distribution which channels the flow into two oppositely directed lobes and provides some further acceleration to the already supersonic molecular gas. Only 5 percent of the molecular gas actually reaches escape velocity.

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