Water Abundance and Velocity Structure in S140, ρ Oph A, and B335

Details Water Abundance and Velocity Structure in S140, ρ Oph A, and B335 Water Abundance and Velocity Structure in S140, ρ Oph A, and B335

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...539l.119a&link_type=abstract

The Astrophysical Journal, Volume 539, Issue 2, pp. L119-L122.

Astronomy and Astrophysics

Astronomy

21

Ism: Abundances, Ism: Clouds, Ism: Molecules, Radio Lines: Ism, Stars: Formation

Scientific paper

We present Monte Carlo radiative transfer models for B335, S140, and ρ Ophiuchi A that simulate the emission line arising from the 557 GHz 110-->101 ground-state transition of ortho-H216O. These models reproduce the line profiles with a combination of turbulent and macroscopic motions, and are consistent with gravitational infall in ρ Oph A. We cannot, however, discriminate infall from outflow for S140. Our models are consistent with ortho-H2O abundances relative to H2 of 2×10-8 and 4.5×10-9 in S140 and ρ Oph A, respectively, and an upper limit of 4×10-6 (3 σ) in B335, assuming the ratio ortho-H2/para-H2 = 0.1. We quantify the impact of dust continuum emission on the derived abundances.

Affiliated with

Also associated with

No associations

Rating

Water Abundance and Velocity Structure in S140, ρ Oph A, and B335 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 Water Abundance and Velocity Structure in S140, ρ Oph A, and B335, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Water Abundance and Velocity Structure in S140, ρ Oph A, and B335 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-736148