Shock Dissipation in Nearby Star Forming Regions

Details Shock Dissipation in Nearby Star Forming Regions Shock Dissipation in Nearby Star Forming Regions

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.3416b&link_type=abstract

Spitzer Proposal ID #3416

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Scientific paper

We propose to probe the line emission from nearby star forming regions in the 5 to 37 micron spectral range using the slit-scan mode of IRS. Our goals are: [1] Measure the fluxes produced by the pure rotational lines of molecular hydrogen and other spectral features in the 5 to 38 micrometer region from the surroundings of 4 well-studied and nearby outflow sources. [2] Trace the intermediate velocity (2 to 30 km/sec) shocks in outflow regions. Such emission is predicted by models in which high velocity motions traced by optical and near-IR emission lines (Herbig-Haro objects) accelerate molecular outflows and degrade into turbulent motions. We will obtain slit-scan maps in the LL and SL modes of IRS of arc-minute scale regions surrounding HH 211, HH212, L1448c and, NGC 2071. By observing these four sources, we will compare the mid-IR emission lines produced by regions supporting various levels of star formation activity ranging from the birth of isolated single stars, to small groups, to rich clusters containing over 100 YSOs and stars as massive as 8 to 10 Solar masses.

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