Changes between Version 53 and Version 54 of u/erica/CoreCollapseBlog
- Timestamp:
- 04/17/18 16:03:24 (7 years ago)
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u/erica/CoreCollapseBlog
v53 v54 35 35 As shown below (post from 3/15), the profiles generated by AstroBEAR's HSE module closely match the input progenitor profiles, which are in HSE. How well the simulation data matches the input progenitor profile following Interpolation onto the mesh then depends on the resolution. The following line plot shows that increasing the resolution by a factor of 8 (blue curve) improves the accuracy of the HSE solver -- the sphere reaches HSE over much smaller region in the higher resolution case rather than the lower resolution run. It seems HSE is achieved by about 30 grid cells on the finest mesh -- thus, want to minimize the physical distance these cells take up within the sphere. 36 36 37 [[Image( )]]37 [[Image(HSE_octant_resolutionStudy.png, 35%)]] 38 38 39 39 At an effective resolution of ~$dx = .0019$, the sphere is very close to HSE within .1 of its radius. … … 70 70 Running the same setup but at 8x higher resolution gives profiles that more closely match the input progenitor density: 71 71 72 [[Image(density_2D_higheres.png, 50%)]]72 [[Image(density_2D_higheres.png, 35%)]] 73 73 74 74 and a zoom-in: 75 75 76 [[Image(density_2D_higheres_zoomin.png, 50%)]]76 [[Image(density_2D_higheres_zoomin.png, 35%)]] 77 77 78 78 Am moving onto 3D now and exploring if the code can handle this setup over a couple of freefall times. However, need to adjust the refinement criteria as currently, the entire domain is being resolved to the maximum level. … … 80 80 Here are pressure, density, and temperature color plots: 81 81 82 [[Image(highres_2D_pressColor.png, 50%)]]82 [[Image(highres_2D_pressColor.png, 35%)]] 83 83 84 [[Image(highres_2D_rhoColor.png, 50%)]]84 [[Image(highres_2D_rhoColor.png, 35%)]] 85 85 86 [[Image(highres_2D_tempColor.png, 50%)]]86 [[Image(highres_2D_tempColor.png, 35%)]] 87 87 88 88 I think the rings in the above image may be plotting artifacts, as the difference in color bands isn't that great compared to those in density and pressure... … … 96 96 As shown in Figure 1, Astrobear interpolates the progenitor density profile (red diamonds, Fig. 1) onto arbitrary positions of the mesh (i.e. cell centers, blue curve). 97 97 98 [[Image(rho_2D_lowres.png, 50%)]][[br]]98 [[Image(rho_2D_lowres.png, 35%)]][[br]] 99 99 '''Figure 1.''' A comparison of the interpolated density profile from the HSE self gravity module in Astrobear (blue) to the supplied progenitor density profile (red). 100 100 … … 102 102 103 103 104 [[Image(press_2D_lowres.png, 50%)]][[br]]104 [[Image(press_2D_lowres.png, 35%)]][[br]] 105 105 '''Figure 2.''' A comparison of the interpolated pressure profile from the HSE self gravity module in Astrobear (blue) to the supplied progenitor pressure profile (red). 106 106 … … 109 109 Figures 3 & 4 are zoom-ins of the density and pressure profiles between the innermost zone (located at dx=5.6e+7 cm) and the radius at which the profiles begin to noticeably deviate. Note the progenitor profile has data sampling down to radius of r=7.84e+5 cm, so about 2 orders of magnitude finer resolution than in this example simulation. 110 110 111 [[Image(2D_rho_zoomin.png, 50%)]][[br]]111 [[Image(2D_rho_zoomin.png, 35%)]][[br]] 112 112 '''Figure 3.''' Zoom-in of density profiles described in text. 113 113 114 [[Image(2D_press_zoomin.png, 50%)]][[br]]114 [[Image(2D_press_zoomin.png, 35%)]][[br]] 115 115 '''Figure 4.''' Zoom-in of pressure profiles described in text. 116 116 … … 132 132 An initial run was producing weird results near the boundary between the clump and the ambient medium, and this had to do with commenting out the smoothing of the profiles in clump.f90 (should not comment these out if you want no smoothing of the clump outer boundary into the ambient medium!! instead you should set your smoothing length to 0 in the clumpdef). 133 133 134 [[Image(Screen Shot 2018-03-01 at 9.50.04 AM.png, 50%)]]134 [[Image(Screen Shot 2018-03-01 at 9.50.04 AM.png,35%)]] 135 135 136 136 = 2/28/18 = … … 159 159 Fryer sent progenitor data. The density, pressure, temperature, and velocity profiles of this progenitor look like: 160 160 161 [[Image(progenitor_profiles.png, 50%)]]161 [[Image(progenitor_profiles.png, 35%)]] 162 162 163 163 The goal is to get these profiles initialized on an Eulerian grid in astrobear and to make sure the solution can be numerically stable over multiple dynamical times. The question of stability is interesting and something we will turn to next.
