Interactions between pre-main-sequence objects and molecular clouds. II - PV Cephei

Details Interactions between pre-main-sequence objects and molecular clouds. II - PV Cephei Interactions between pre-main-sequence objects and molecular clouds. II - PV Cephei

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...277..634l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 15, 1984, p. 634-639.

Astronomy and Astrophysics

Astrophysics

47

Interstellar Matter, Molecular Clouds, Pre-Main Sequence Stars, Stellar Mass Ejection, Astronomical Models, Carbon Monoxide, Nebulae, Stellar Winds

Scientific paper

CO observations reveal a bipolar flow associated with the peculiar pre-main-sequence object PV Cephei. The axis of this flow is roughly aligned with the symmetry axis of GM 29, the cometary nebula illuminated by PV Cephei. The total mass in high-velocity gas is 0.8-2.6 solar masses; its expansion age is (0.5-1.5) x 10 to the 5th years. If driven by a 400 km/s stellar wind, a mass loss rate of (0.4-2.0) x 10 to the -6th solar mass/yr is required to drive this flow. The optical morphology of GM 29 provides strict constraints on the size of any collimating disk in the PV Cephei system. Implications of these observations for models of cometary nebulae and bipolar flows are discussed.

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