Numerical Relativity in Spherical Coordinates - Revision history

129.21.16.204 at 14:12, 20 March 2018

2018-03-20T14:12:33Z

129.21.16.204 at 17:58, 19 March 2018

2018-03-19T17:58:46Z

129.21.16.204 at 17:58, 19 March 2018

2018-03-19T17:58:02Z

Noncct yosef zlochower at 17:28, 19 March 2018

2018-03-19T17:28:24Z

New page

Numerical Relativity in Spherical Coordinates Working Group

'''Team''':
Lead: Manuela Campanelli (RIT)

* Vassilios Mewes (RIT)
* Yosef Zlochower (RIT)
* Zach Etienne (WVU)
* Ian Ruchlin (WVU)
* Thomas Baumgarte (Bowdoin)

'''Funding''':

* NSF 1550436 (Einstein Toolkit)
* etc

'''Background''':

'''Development''':

* Parity boundary conditions completed.
* Implementation of BSSN equations in Spherical coordinates completed.
* Interface to AHFinderDirect completed.
* Interface to QuasiLocal measures completed.
* Radiation extraction code completed.

'''Activities'''

* Submitted Paper "Numerical Relativity in Spherical Coordinates with the Einstein Toolkit", bu Mewes, Zlochower, Campanelli, Ruchlin, Etienne, and Baumgarte [https://arxiv.org/abs/1802.09625]

* Implementation of Hydro in Spherical Coordinates ... Begun.

←Older revision		Revision as of 17:58, 19 March 2018
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	'''Background''':		'''Background''':
		+
	Numerical relativity codes that do not make assumptions on spatial symmetries most commonly adopt Cartesian coordinates. While these coordinates have many attractive features, spherical coordinates are much better suited to take advantage of approximate symmetries in a number of astrophysical objects, including single stars, black holes and accretion disks. While the appearance of coordinate singularities often spoils numerical relativity simulations in spherical coordinates, especially in the absence of any symmetry assumptions, it has recently been demonstrated that these problems can be avoided if the coordinate singularities are handled analytically. This is possible with the help of a reference-metric version of the Baumgarte-Shapiro-Shibata-Nakamura formulation together with a proper rescaling of tensorial quantities.		Numerical relativity codes that do not make assumptions on spatial symmetries most commonly adopt Cartesian coordinates. While these coordinates have many attractive features, spherical coordinates are much better suited to take advantage of approximate symmetries in a number of astrophysical objects, including single stars, black holes and accretion disks. While the appearance of coordinate singularities often spoils numerical relativity simulations in spherical coordinates, especially in the absence of any symmetry assumptions, it has recently been demonstrated that these problems can be avoided if the coordinate singularities are handled analytically. This is possible with the help of a reference-metric version of the Baumgarte-Shapiro-Shibata-Nakamura formulation together with a proper rescaling of tensorial quantities.

@@ Line 30: / Line 30: @@
 * Interface to AHFinderDirect completed.
 * Interface to QuasiLocalMeasures completed.
 * Radiation extraction code completed.

@@ Line 19: / Line 19: @@
 '''Background''':
 '''Development''':
@@ Line 26: / Line 28: @@
 * Implementation of BSSN equations in Spherical coordinates completed.
 * Interface to AHFinderDirect completed.
-* Interface to QuasiLocal measures completed.
+* Interface to QuasiLocalMeasures completed.
 * Radiation extraction code completed.
 '''Activities'''
-* Submitted Paper "Numerical Relativity in Spherical Coordinates with the Einstein Toolkit", bu Mewes, Zlochower, Campanelli, Ruchlin, Etienne, and Baumgarte [https://arxiv.org/abs/1802.09625]
+* Submitted Paper "Numerical Relativity in Spherical Coordinates with the Einstein Toolkit", by Mewes, Zlochower, Campanelli, Ruchlin, Etienne, and Baumgarte [https://arxiv.org/abs/1802.09625]
 * Implementation of Hydro in Spherical Coordinates ... Begun.