Kinematics and Ionization of the Proplyd M42 177-341

Details Kinematics and Ionization of the Proplyd M42 177-341 Kinematics and Ionization of the Proplyd M42 177-341

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmxac...9..198h&link_type=abstract

"Astrophysical Plasmas: Codes, Models, and Observations, Proceedings of the conference held in Mexico City, October 25-29, 1999,

Astronomy and Astrophysics

Astrophysics

4

Scientific paper

The bright proplyds in the Orion nebula (M42) are the result of accretion disks around low-mass stars in the Trapezium cluster being photoevaporated by the ultraviolet radiation from the O stars in the cluster. Henney & O'Dell (1999) presented high resolution optical emission line spectroscopy of four proplyds and demonstrated a correlation between line width and ionization potential, indicative of acceleration in an ionization-stratified photoevaporating flow. Here I present previously unpublished supplementary material concerning 177-341, one of the proplyds in the Henney & O'Dell study.

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