Patterns of Gravitational Cooling in Schr”odinger Newton System. (arXiv:1811.09694v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Bak_D/0/1/0/all/0/1">Dongsu Bak</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Kim_S/0/1/0/all/0/1">Seulgi Kim</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Min_H/0/1/0/all/0/1">Hyunsoo Min</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Song_J/0/1/0/all/0/1">Jeong-Pil Song</a>
We study time evolution of Schr”odinger-Newton system using the
self-consistent Crank-Nicolson method to understand the dynamical
characteristics of nonlinear systems. Compactifying the radial coordinate by a
new one, which brings the spatial infinity to a finite value, we are able to
impose the boundary condition at infinity allowing for a numerically exact
treatment of the Schr”odinger-Newton equation. We study patterns of
gravitational cooling starting from exponentially localized initial states.
When the gravitational attraction is strong enough, we find that a small-sized
oscillatory solitonic core is forming quickly, which is surrounded by a growing
number of temporary halo states. In addition a significant fraction of
particles escape to asymptotic regions. The system eventually settles down to a
stable solitonic core state while all the excess kinetic energy is carried away
by the escaping particles, which is a phenomenon of gravitational cooling.
We study time evolution of Schr”odinger-Newton system using the
self-consistent Crank-Nicolson method to understand the dynamical
characteristics of nonlinear systems. Compactifying the radial coordinate by a
new one, which brings the spatial infinity to a finite value, we are able to
impose the boundary condition at infinity allowing for a numerically exact
treatment of the Schr”odinger-Newton equation. We study patterns of
gravitational cooling starting from exponentially localized initial states.
When the gravitational attraction is strong enough, we find that a small-sized
oscillatory solitonic core is forming quickly, which is surrounded by a growing
number of temporary halo states. In addition a significant fraction of
particles escape to asymptotic regions. The system eventually settles down to a
stable solitonic core state while all the excess kinetic energy is carried away
by the escaping particles, which is a phenomenon of gravitational cooling.
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