Changes between Version 29 and Version 30 of u/erica/UniformCollapse

Timestamp:

06/29/15 16:45:12 (10 years ago)

Author:

Erica Kaminski

Comment:

—

u/erica/UniformCollapse

@@ -76 +76 @@
 
 [[Image(density.png, 40%)]]
-[[br]]'''''Density of collapsing sphere over time.''''' '''Shown here are 2 overlaid spheres, one with initial radius [[latex($r=r_0=10$)]] and one with [[latex($r=r_0/2=5$)]]. They are exactly the same, so you only see one line. That is, the density is constant throughout a collapsing uniform density sphere.
+[[br]]'''''Density of collapsing sphere over time.''''' '''Shown here are 2 overlaid spheres, one with initial radius [[latex($r=r_0=10$)]] and one with [[latex($r=r_0/2=5$)]]. They are exactly the same, so you only see one line. That is, the density grows uniformly everywhere inside a collapsing uniform density sphere, and the average density is the exact density at any radius.
 
 This plot shows that the entire interior of the sphere experiences a homologous (uniform) increase in density. The density increases everywhere exactly the same! Furthermore, the density increases by many orders of magnitude over the period of collapse. Assuming the collapse is isothermal (which is a good approximation over much of the collapse of protostars), implies that the Jeans mass decreases drastically over the period of collapse. This means that local regions of the collapsing sphere themselves will begin collapsing, and the whole cloud can be expected to fragment.
@@ -86 +86 @@
 [[Image(collapse.png, 40%)]]
 [[br]]'''Blue = acceleration, gold = velocity, green = position, red = density'''
+
+'''Ram pressure'''
+
+With the density over time, and the velocity profiles over time, I can get a ram pressure radial profile over time of a collapsing uniform sphere. This is what I was after all along, as I want to match this to the outward ram pressure of the splashed region in the MHD colliding flows runs.
+
+Here she is:
+
+[[Image(rampressure.png, 40%)]]