A Model to Test the Internal Structure of the G31.41+0.31 Hot Molecular Core

Details A Model to Test the Internal Structure of the G31.41+0.31 Hot Molecular Core A Model to Test the Internal Structure of the G31.41+0.31 Hot Molecular Core

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.292..369o&link_type=abstract

Astrophysics and Space Science, v. 292, Issue 1, p. 369-374 (2004).

Astronomy and Astrophysics

Astrophysics

Radiative Transfer, Radio Lines: Ism, Stars: Formation, Ism: Individual (G31.41+0.31)

Scientific paper

We investigate the physical conditions of the material around massive protostars by modelling the so-called hot molecular cores. We present a model for the spectral energy distribution (SED) as well as the ammonia line emission of the G31.41+0.31 hot core. We find that the best fit to the SED is achieved by assuming a density distribution corresponding to the collapse of a magnetized logatropic sphere. On the other hand, the line emission is reproduced by adopting a gas phase ammonia abundance increasing towards the center of the core, as a result of the release of the ammonia molecules trapped in ice grain mantles.

Affiliated with

Also associated with

No associations

Rating

A Model to Test the Internal Structure of the G31.41+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 A Model to Test the Internal Structure of the G31.41+0.31 Hot Molecular Core, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A Model to Test the Internal Structure of the G31.41+0.31 Hot Molecular Core will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1857489