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Modeling Radiatively Confined Clouds Around
Celestial Objects
Deval Mehta
August 28, 2015
1
I spent the past summer working with Dr. Stanley Owocki of the Bartol
Research Institute and Department of Physics and Astronomy at the Uni-
versity of Delaware on modeling the behavior of gas clouds on around radi-
ation sources, with specific application to quasi-stellar objects, also known
as quasars.
I started the summer working with another Undergraduate named Robert
Jaquette on a simple scattering toy-problem as a learning exercise and back-
ground for the cloud modeling project. We wrote a simple Monte Carlo
method that would track the evolution of a large number of photons through
a one-dimensional, planar cloud. After successfully completing this one-
dimensional model, we set out to work on a preliminary problem set to
derive an analytic solution for the gas pressure in the cloud as a function of
optical depth. The results of this calculation set the initial condition in my
radiation-hydrodynamic models.
The code that I am using is called Virginia Hydrodynamics One and
was originally developed at North Carolina State University. VH1 is a hy-
drodynamics code coupled with a radiative solver, which allows us to model
systems impacted by a light source. This is key in modeling these gas clouds.
In particular, I have been modeling a one-dimensional planar gas cloud
that is confined by gas pressure on one side (due to a source of radiation
which is farther away than the cloud is long) and by a radiation force on the
other. I am working in the frame of reference of an observer to whom the
cloud itself is moving in steady state. In other words, the time-derivative of
the velocity of the cloud is 0. I am assuming a length of nearly 0.5 pc for
the cloud, with a quasar 1 pc away. The goal of the one-dimensional model
is to ensure that it remains in hydrostatic equilibrium.
So far the cloud is almost hydrostatic in one-dimension. Once this is
completed, I will be extending the model to two dimensions, wherein I will
introduce a small perturbation in density along the second dimension. We
will then monitor the data and analyze the effects of these density pertur-
bations on the behavior of the gas within the cloud. If all goes well, this
will be done within the next month, after which we will continue to make
adjustments to model until we have a viable two-dimensional approximation.

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DeSGC_Summary_2015

  • 1. Modeling Radiatively Confined Clouds Around Celestial Objects Deval Mehta August 28, 2015
  • 2. 1 I spent the past summer working with Dr. Stanley Owocki of the Bartol Research Institute and Department of Physics and Astronomy at the Uni- versity of Delaware on modeling the behavior of gas clouds on around radi- ation sources, with specific application to quasi-stellar objects, also known as quasars. I started the summer working with another Undergraduate named Robert Jaquette on a simple scattering toy-problem as a learning exercise and back- ground for the cloud modeling project. We wrote a simple Monte Carlo method that would track the evolution of a large number of photons through a one-dimensional, planar cloud. After successfully completing this one- dimensional model, we set out to work on a preliminary problem set to derive an analytic solution for the gas pressure in the cloud as a function of optical depth. The results of this calculation set the initial condition in my radiation-hydrodynamic models. The code that I am using is called Virginia Hydrodynamics One and was originally developed at North Carolina State University. VH1 is a hy- drodynamics code coupled with a radiative solver, which allows us to model systems impacted by a light source. This is key in modeling these gas clouds. In particular, I have been modeling a one-dimensional planar gas cloud that is confined by gas pressure on one side (due to a source of radiation which is farther away than the cloud is long) and by a radiation force on the other. I am working in the frame of reference of an observer to whom the cloud itself is moving in steady state. In other words, the time-derivative of the velocity of the cloud is 0. I am assuming a length of nearly 0.5 pc for the cloud, with a quasar 1 pc away. The goal of the one-dimensional model is to ensure that it remains in hydrostatic equilibrium. So far the cloud is almost hydrostatic in one-dimension. Once this is completed, I will be extending the model to two dimensions, wherein I will introduce a small perturbation in density along the second dimension. We will then monitor the data and analyze the effects of these density pertur- bations on the behavior of the gas within the cloud. If all goes well, this will be done within the next month, after which we will continue to make adjustments to model until we have a viable two-dimensional approximation.