By Lee Hartmann
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Additional resources for Accretion Processes in Star Formation, 2nd Edition (Cambridge Astrophysics)
The dramatic reduction in dust emission in HR 4796A is evident, especially at short wavelengths, where the infrared excess is very low if not absent. 10), which shows a ring structure. It is plausible that this structure indicates the presence of massive bodies (planets) which shepherd this ring, just as small moons shepherd the rings of Saturn. What happens to disk gas, which originally constituted the bulk of the mass, is not clear. , Hollenbach et al. 2000; Alexander et al. 2006a,b). This process seems to be occuring in the central regions of the Orion Nebula, due to the intense radiation field of O7 star θ 1 Ori C.
A major factor in limiting cloud lifetimes is stellar energy input, especially when massive stars are formed. For example, in the nearest B association, Scorpius-Centaurus, 26 Beginnings: molecular clouds which consists of stars with ages of ∼5–15 Myr, molecular gas is not present in the older population; the large H I shells surround the three subconcentrations – Lower CentaurusCrux, Upper Centaurus-Lupus, and Upper Scorpius – which are probably the result of the dispersal of association molecular gas by stellar winds and supernovae (de Geus 1992).
9. Gravitational acceleration toward the center of a thin sheet (solid curve) or filament (dotted curve) as a function of position in units of the sheet radius R or filament length 2l (measured from the filament center). From Burkert and Hartmann (2004). 33) and thus tc = δr = v R πG 1/2 . 34) This estimate reproduces the numerical results for of the time it takes for the edge of the circular sheet to fall to the center. The important feature is that tc is independent of the size of the region δr ; this means that larger scales must be moving at larger velocities, which makes it difficult to fragment on small scales.
Accretion Processes in Star Formation, 2nd Edition (Cambridge Astrophysics) by Lee Hartmann