Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.201..527f&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 201, Nov. 1982, p. 527-549.
Astronomy and Astrophysics
Astronomy
16
Brightness Temperature, Energy Transfer, Hydroxyl Emission, Interstellar Gas, Interstellar Masers, Molecular Clouds, Background Radiation, Far Infrared Radiation, Interstellar Chemistry, Molecular Rotation, Turbulent Diffusion, Vortices
Scientific paper
The main purpose of this work is to make theoretical predictions of OH maser brightness temperatures in W3(OH) on the basis of a collisional pumping mechanism for Lambda-doublet inversion and a theory of maser amplification. The high observed values of brightness temperature (greater than 10 to the 12th K) are reproduced by conditions of molecular hydrogen number density of 10 to the 6th to 5 x 10 to the 7th/cu cm and temperature 50-150 K. Account is taken both of an external FIR radiation field and kinematic compression of the Doppler width consequent on gravitational accretion. An important conclusion is that a fully realistic evaluation of the physical conditions of the maser region must await experimental data on rate coefficients for rotationally inelastic collisions of H2 with OH2Pi. The dynamics of the maser region are investigated and it is suggested that a maser may consist of a turbulent eddy or group of eddies in the interstellar medium. From this model the temporal variability, linewidth and high associated magnetic fields follow and are shown to be naturally interdependent.
No associations
LandOfFree
An interpretation of OH maser observations in W3/OH/ 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 An interpretation of OH maser observations in W3/OH/, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and An interpretation of OH maser observations in W3/OH/ will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1758390