Tidal Disruption of Stars

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For in-depth information, please read the paper:

Three-Dimensional Simulations of Tidally Disrupted Solar-Type Stars and the Observational Signatures of Shock Breakout
James Guillochon, Enrico Ramirez-Ruiz. 2009, ApJ, 705, 844.

Here are some movies from the run featured in the paper. t = 0 is defined as the time when the star’s center of mass crosses pericenter.

Density
Variable: $\log_{10} \rho$
Times Shown: -200 to 500 seconds (700s duration)
Slice Plane: Orbital Plane (x-y plane through z = 0)
Viewpoint: Shows the log of density in the orbital plane, subject to a cut of 1e-3 grams/cc.
Box dimensions: $8 \times 10^{11}$ cm per side.
Surface temperature
Variable: $\log_{10} T$

Times Shown: 0 to 100 seconds (100s duration)
Viewpoint: Shows the log of photon temperature at the surface, where the surface is defined by where $\partial_z (\rho) / \rho$ is at a maximum. Surface elements where radiation pressure is larger than gas pressure are omitted since we did not use an EOS that included radiation pressure. This surface is flattened into a 2D projection.
Box dimensions: $4 \times 10^{11}$ cm per side.
Density along the minor axis
Variable: $\log_{10} \rho$
Times Shown: -44 to 130 seconds (174s duration)
Viewpoint: Shows the log of density in the plane perpendicular to the orbital plane and containing the minor axis of the remnant, subject to a cut of 0.1 grams/cc.
Box dimensions: $10^{11}$ by $4 \times 10^{10}$ cm.
Density along the major axis
Variable: $\log_{10} \rho$
Times Shown: -44 to 130 seconds (174s duration)
Viewpoint: Shows the log of density in the plane perpendicular to the orbital plane and containing the major axis of the remnant, subject to a cut of 0.1 grams/cc.
Box dimensions: $4 \times 10^{11}$ by $4 \times 10^{10}$ cm.