Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009mnras.395..234f&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 395, Issue 1, pp. 234-239.
Astronomy and Astrophysics
Astronomy
5
Radiative Transfer, Shock Waves, Ism: Jets And Outflows, Ism: Molecules, Infrared: Ism, Radio Lines: Ism
Scientific paper
We have calculated emission by CO molecules from interstellar shock waves. Two approximations have been used to determine the population densities, nJ, of the rotational levels, J: steady state (∂/∂t ≡ 0) and statistical equilibrium (d/dt ≡ 0). A large-velocity-gradient approximation to the line-transfer problem was adopted in both cases. We find that there can be substantial differences between the values of the integrated rotational line intensities calculated in steady state and in the limit of statistical equilibrium. On the other hand, although CO can be the dominant coolant towards the rear of the cooling flow which follows the dynamical heating of the gas, the rate of cooling computed assuming statistical equilibrium is likely to be reasonably accurate, given that the limit of statistical equilibrium is approached in this region.
Flower David R.
Gusdorf Antoine
No associations
LandOfFree
Emission and cooling by CO in interstellar shock waves 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 Emission and cooling by CO in interstellar shock waves, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Emission and cooling by CO in interstellar shock waves will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-814487