Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21560645b&link_type=abstract
American Astronomical Society, AAS Meeting #215, #606.45; Bulletin of the American Astronomical Society, Vol. 36, p.1137
Astronomy and Astrophysics
Astronomy
Scientific paper
Herbig-Haro (HH) flows are thought to be an extremely important part of the star formation process. They are the result of high-velocity outflows emanating from young accreting stars. They are seen at optical wavelengths as nebulous knots of shock-excited line emission resulting from the impact of ejected gas on either ambient molecular cloud material or gas/dust released in previous outburst events. HH flows appear episodic in nature and are postulated to occur throughout a stars’ early formation history. The stars responsible for HH flows, which have been designated Herbig-Haro energy sources (HHens), are often embedded in dense circumstellar envelopes and disks and/or located deep within molecular clouds making them optically faint and hence, less well-studied than their optical counterparts. Some HHens are optically visible and yet have still been studied sparingly. Several outstanding questions remain as to the nature of HHens and the processes leading to the ejection of HH flows.
We present the results of an infrared survey of 66 HHens in an effort to provide more reliable data on these objects. Photometric analysis of the HHens was made from data taken with IRAC and MIPS cameras onboard the Spitzer Space Telescope. We present all available infrared photometry along with colors. Using this we will classify these young objects using color-color diagrams based on data from Allen et al. (2004) and Muzerolle et al. (2007). This work was conducted by a Research Experience for Undergraduates (REU) position at the University of Hawai'i's Institute for Astronomy and funded by the NSF.
Aspin Colin
Battisti Andrew
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