Update 7/20

  • Looked again at the Parker wind differential equation:

If we assume spherically symmetric outflow in an isothermal corona, then by conservation of momentum, continuity, and the ideal gas law, we have

Continuity shows that , where C is a constant. If we substitute for p and rho into the momentum equation, we get a differential equation in u and r:

Define so that (i.e., sonic radius); substitute and rearrange to find

Integrate both sides to find the Parker wind equation,

  • Modified the domain on a couple of simulations to better resolve the planet/capture sonic radius. Also plotted contour of sonic radius.
Value Mdot (g/s)
lambda=5 5.6x1011 (unchanged)
Mp = 0.25MJ > 1.67x109 (not well resolved) 3.7x108
Tp = 5x104 K Negative throughout (not resolved) 3.4x108

For lambda=5, may not reach quasi-steady state.

Tp = 5x104 K:

Mp = 0.25 MJ:

Sonic radii:

  • Continuing to work my way through Zel'dovich.

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