Update 4/30 (Radiation Pressure)

WASP-12b paper accepted - will be posting to ArXiv today.

Radiation pressure:

All of the following are in computational units:

For and , white is .

http://www.pas.rochester.edu/~adebrech/PlanetIonization/alpha_top.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/alpha_side.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/alpha_cross.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/beta_top.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/beta_side.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/beta_cross.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/delta_top.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/delta_side.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/delta_cross.png

Cross-cut

http://www.pas.rochester.edu/~adebrech/PlanetIonization/2d14_cross.png

Ly- flux for HD209458b

From ​here (Bourrier & Lecavalier des Etangs 2013), flux peaks at J = ~28x10-14 erg cm-2 s-1 AU-1.

Converting to photons cm-2 s-1,

Which is 3 orders of magnitude less than the maximum flux in our simulation. If instead it should be scaled to the orbital radius (0.04747 AU, not 1 AU), that reduces it to 1.2x1010.

Timescale for blowoff vs. replenshiment

Assume torus of axis AU, radius of cm, and uniform density g/cm3. Given the mass loss rate of the planet, the timescale for replenishment is:

s

The timescale for blowoff is dependent upon the gravitational binding energy and the energy deposited by photons on the edge of the torus per unit time:

erg

erg/s

s

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