Adding viscous shear heating to Ae disk models makes Hα emission much easier to produce for spectral types A2 and cooler, and this dependence is proposed as a new way to measure the disk viscosity parameter α, though the current data give inconsistent values.
Linear line polarimetry modelling of pre-main sequence stars
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abstract
We present emission line polarimetry data and modelling relevant to the circumstellar geometry and kinematics around pre-main sequence stars. For a sample of both Herbig Ae/Be stars and T Tauri stars, we find that most show polarization changes across Halpha, implying that flattened structures are common on the smallest scales -- and over a range of stellar masses. We also present Monte Carlo calculations of spectral line profiles scattered in rotating accretion disks. We consider both the case of a central star that emits line photons uniformly, as well as via hot spots. Intriguingly, the switch between a uniform point source and a finite-sized star results in a marked difference in the position angle variation across the line. Our models demonstrate the diagnostic potential of line polarimetry in determining the disk inclination and the size of the inner hole -- a spatial scale no other technique currently accesses.
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Using the Coolest Ae Stars to Constrain Circumstellar Disk Viscosity
Adding viscous shear heating to Ae disk models makes Hα emission much easier to produce for spectral types A2 and cooler, and this dependence is proposed as a new way to measure the disk viscosity parameter α, though the current data give inconsistent values.