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Supernova Collision with
Interstellar Molecular Cloud
Researchers:
Shervin Bagheri
[email protected]
The Euler equations for a perfect
gas coupled with radiative transport
states the balance laws of mass,
momentum and energy, denoted .
Our simulation shows that
radiation is an important part of
the energy transport when an
exploding supernova collides
with an interstellar molecular
cloud.
Sven-Erik Ekström
[email protected]
The flux function, , describes the
flow of , and is the radiative
source term.
Advisor:
Per Andersson
[email protected]
Density after collision.
Contact:
Lina von Sydow
[email protected]
The short characteristic method
for a grey atmosphere is used to
solve the time independent
equation of radiative transfer,
resulting in the source term .
Shocks with and without radiative energy transfer,
denoted as HDRT and HD respectively.
The cloud is not totally
dispersed but compressed by
the shock, so that a star
formation might be possible.
Finite Volume Methods with
Godunov’s method, approximates
the homogenous Euler equations.
This is implemented with the
Clawpack library.
Energy after collision.
Finally operator splitting is used to
couple the two numerical methods.
Department of Information Technology
Box 337
SE-751 05 Uppsala
Sweden
Project in course ”Scientific Computing, Advanced course” May 2005 Further information: http://www.it.uu.se/edu/course/homepage/projektTDB/
Contact: [email protected]