Modeling the Dust and Ammonia Emission in the G 31.41+0.31 Hot Molecular Core

Details Modeling the Dust and Ammonia Emission in the G 31.41+0.31 Hot Molecular Core Modeling the Dust and Ammonia Emission in the G 31.41+0.31 Hot Molecular Core

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15..204o&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Astronomy and Astrophysics

Astronomy

H Ii Regions, Ism: Molecules, Radiative Transfer, Radio Lines: Ism, Stars: Formation

Scientific paper

Hot Molecular Cores (HMCs) are dense molecular clumps with T gtrsim 100 K, found in the proximity of ultracompact H II (UCHII) regions. It is believed that HMCs are envelopes infalling onto a central high-mass protostar. Osorio, Lizano, & D'Alessio (1999) modeled in detail their spectral energy distribution (SED) from dust emission, and obtained their physical parameters.

Affiliated with

Also associated with

No associations

Rating

Modeling the Dust and Ammonia Emission in the G 31.41+0.31 Hot Molecular Core does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Modeling the Dust and Ammonia Emission in the G 31.41+0.31 Hot Molecular Core, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Modeling the Dust and Ammonia Emission in the G 31.41+0.31 Hot Molecular Core will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1321715