Constucting an accretion disk around an RG and AGB star

For my masters level thesis, I plan complete and analyze MHD simulations of an accretion disk around the center of a RG and AGB star to investigate the stability and magnetic field generation . This is in an attempt to computationally verify the suggestion that High Field Magnetic White Dwarfs are the result of a Common Envelope, Nordhaus et al. 2011:

Link:​https://arxiv.org/abs/1010.1529

To do this I have looked to Ohlmann’s thesis and previous blog posts made by Luke:

1.) Run The Mesa Stellar Evolution to Generate density, pressure, and temperature profiles at different points in time.

2.) The idea in Nordhaus et al. 2011 is that magnetic field is built up by the engulfment and the accretion of a companion. This is most likely when the radius is at a maximum, So I identified these maximum. (Radius (log[R/Rsun]) vs Time (years) for a 2 solar mass star)

3.) Modify those profiles with the modified-lane-emdan equations in accordance with Ohlmanns thesis (Link:​https://archiv.ub.uni-heidelberg.de/volltextserver/21513/1/thesis-sohlmann.pdf) (Lukes Code)

Link:​http://www.pas.rochester.edu/~lchamandy/Presentations/profile_blog1.pdf

4.) Set the central mass by hand such that the mass contained within the smoothing radius is the same as before modification. Place onto grid with at least 10 cells across smoothing radius

5.) If the central density is stable then I can move on to adding an accretion disk to the central region of the simulation.

Disk parameters: R ~ 10e10 cm

H ~ 10e9 cm M ~10 Jupiter Masses

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