Hubble Space Telescope observations of the environments of young stars

Details Hubble Space Telescope observations of the environments of young stars Hubble Space Telescope observations of the environments of young stars

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..393..143h&link_type=abstract

The seventh astrophysical conference: Star formation, near and far. AIP Conference Proceedings, Volume 393, pp. 143-152 (1997).

Astronomy and Astrophysics

Astrophysics

4

Star Formation, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Mass Loss And Stellar Winds, Masses

Scientific paper

Since the installation of the WFPC2 in the Hubble Space Telescope in late 1993, the HST has proven itself to be a powerful tool for the study of the immediate environments of young stellar objects. In regions of low mass star formation, HST images of objects such as HH30 and HL Tau have effectively replaced the classical textbook ``artist's rendition'' of disks, jets, and outflow cavities with images that clearly show the structure of this environment. Together, these images support a view in which the young stars themselves are responsible for limiting infall and clearing away the dense molecular material from which they formed. In short, these stars determine their own masses. Regions in which high mass stars are forming show a very different picture. HST images still show disks and dense envelopes surrounding young stars, but in regions such as M16 and M42 these objects are immersed within the evacuated interiors of the H II regions. Intense UV and winds from massive stars have disrupted the environment of star formation, cutting these objects off from the material from which they formed or were forming. The timing of this event has nothing to do with the young stellar object itself, and can happen at any arbitrary stage in the growth of the YSO, effectively ``freezing'' the mass of the object at that point. The HST images provide strong circumstantial evidence that the masses of many low mass stars may be determined, not by the process of star formation itself, but instead by the effects of nearby massive stars.

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