Accretion Processes in Star Formation, 2nd Edition by Lee Hartmann

By Lee Hartmann

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Extra info for Accretion Processes in Star Formation, 2nd Edition (Cambridge Astrophysics)

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11. Comparison of the SEDs (normalized to the stellar photospheres) of AB Aur, a Herbig Ae/Be star (intermediate-mass equivalent of a T Tauri star), with HR 4796, a debrisdisk system – that is, a system whose dust is thought to be the product of collisions between large bodies rather than being “primordial” dust. HR 4796 (currently) has the largest known ratio of infrared excess luminosity to stellar luminosity (most other debris-disk systems have an order of magnitude or more fainter infrared excesses).

1995). 6 μG and a random component of 5 μG; then the system is allowed to evolve. When a threshhold density is reached, an energy source is introduced locally to simulate the energy input of massive stars. After several tens of Myr, large-scale flows have been set up, mostly in the direction of galactic rotation. The magnetic field similarly gets more ordered in the direction of rotation, though with significant distortions. There are relatively few cloud structures in this region. , de Avillez & Mac Low 2001; Wada & Norman 2001).

Turbulent motions may either promote star formation by collecting additional mass into limited regions 24 Beginnings: molecular clouds which can then become gravitationally unstable and collapse, or inhibit star formation in principle by providing a “pressure” which resists gravitational collapse. Recent reviews of turbulence and issues related to star formation can be found in Mac Low and Klessen (2004) and Ballesteros-Paredes et al. (2007). Older models of molecular clouds envisioned a sort of equilibrium or average steadystate condition, partly due to the then limitations of computing power which precluded detailed time-dependent simulations.

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