Monthly climatology from 2002 to 2010 • Forecast from 0 to 44

We also see a lot of envelope material hitting the outer parts of the disk in our semi-analytical collapse model, but there is still a fair amount (up to 50%) that makes its way to

Figure 2.3 – Dust temperature due to the accretion shock (vertical axis) and stellar radiation (hor- izontal axis) at the point of entry into the disk for 0.1-µm grains in a sample

For example, it was already known that the collapse-phase chemistry is dominated by a few key chemical processes and that the collapsing core never attains chemical equilibrium

The 2D treatment of the accretion results in material accreting at larger radii, so a smaller fraction comes close enough to the star for amorphous silicates to be thermally

Figure 5.7 – Histogram of the absolute relative difference between the approximate method (see text for details) and the full computation for the absolute photodissociation rates

A disk around a Herbig Ae/Be star containing PAHs of 50 or 96 carbon atoms shows strong PAH features, but the 24-C spectrum contains only thermal dust emission.. The goal

Daarmee kan prima de chemische evolutie in de instortende kern worden gevolgd, maar voor een goede beschrijving van de circumstellaire schijf zijn tweedimensionale modellen nodig..

1932, in Annual Report of the Board of Regents of the Smithsonian Institution (Washington: Smithsonian Inst.), 133.. 1988, in Rate Coefficients in