Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999arep...43..209l&link_type=abstract
Astronomy Reports, Volume 43, Issue 4, April 1999, pp.209-215
Astronomy and Astrophysics
Astronomy
2
Scientific paper
Long-term monitoring of the H2O maser emission of a number of sources has shown that the radial-velocity deviations from the mean drift value are characterized by a short-period chaotic velocity component. This enables determination of the main parameters of turbulent motions in the maser condensations u_0, tau_0, and R_0-the characteristic velocity, lifetime, and scale size for the turbulent motions. The values found for these quantities correspond to Strouhal numbers xi_0 = u_0 tau_0/R_0 << 1, so that it is possible to estimate the coefficient of turbulent diffusion as D_T ~= u_0^2 tau_0/3. Turbulence with xi_0 << 1 can be caused by either noncompressible gas motions or motions that involve a mixture of chaotically propagating shock waves. In the latter case, the parameter xi_0 also determines the mean relative compression of the gas delta V/V ~= xi_0. The determination of the coefficient of turbulent diffusion D_T and the viscosity nu_T ~= D_T for various types of turbulence is discussed in detail.
Lekht E. E.
Mendoza-Torres Jose E.
Silant'ev N. A.
No associations
LandOfFree
Main parameters of turbulence in star-forming regions from observations of H2O maser emission 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 Main parameters of turbulence in star-forming regions from observations of H2O maser emission, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Main parameters of turbulence in star-forming regions from observations of H2O maser emission will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1429927