Spectral Energy Distributions Of High-Mass Protostellar Objects - Evidence For High Accretion Rates

Details Spectral Energy Distributions Of High-Mass Protostellar Objects - Evidence For High Accretion Rates Spectral Energy Distributions Of High-Mass Protostellar Objects - Evidence For High Accretion Rates

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.8905f&link_type=abstract

American Astronomical Society, AAS Meeting #211, #89.05; Bulletin of the American Astronomical Society, Vol. 39, p.878

Astronomy and Astrophysics

Astronomy

Scientific paper

The spectral energy distributions (SEDs) spanning the mid-infrared to millimeter wavelengths of a sample of 13 high-mass protostellar objects (HMPOs) were studied in conjunction with a large archive of 2-D axisymmetric radiative transfer models. Measurements from the Spitzer GLIMPSE and MIPSGAL surveys (infrared), and the MSX survey (infrared) were used in addition to our own surveys at millimeter and submillimeter wavelengths using the IRAM 30m (millimeter) and JCMT (submillimeter) telescopes to construct the SEDs, which were then fit to the archive of models. These models assumed that stars of all masses form via accretion, and allowed us to make estimates for the masses, luminosities and envelope accretion rates of the HMPOs. The models fit the observed SEDs well, supporting the accretion-based scenario of massive star formation. The envelope accretion rates were found to be M'env ≈ 10-2 - 10-3 M&sun;/yr. Such high accretion rates, indirectly indicated by past outflow observations, are required for massive star-formation, which our results confirm independently. With the derived accretion rates, and with mass estimates of up to 20 M&sun; for these objects, it appears likely that stars with stellar masses M* > 20 M&sun; can form via accretion. We are also able to make the first observational estimate of the fraction of the infalling material that is lost to the outflow and study the dependence of the accretion rate on stellar mass.

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