Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks

Free Access

Table 1:

Properties of gas components of the Milky Way.
Component	molecular gas	atomic gas
M (10⁹ $M_\odot)$ ^a	2	6
$L_{\rm d}$ (pc)^b	150	1000
$\sigma$ (km s^-1)^c	5	12
$E_{\rm kin}$ (10⁵⁵ erg s^-1)^d	0.5	8.6

Notes. ^(a) Total mass of the component. Values from Ferrière (2001) and Kalberla (2003). ^(b) We take twice the observed disk scale height as the true thickness to be considered. ^(c) The parameter $\sigma$ is the 3-dimensional velocity dispersion. We take the 1-dimensional velocity dispersion of the molecular gas to be 2.9 km s^-1 and of the HI gas to be 6.9 km s^-1. ^(d) Total kinetic energy of the component, $E_{\rm kin} = 1/2 ~ M \sigma^2$ .

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.