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	~~! Quantity~~
	~~! Expression~~
	~~\|- align="left"~~
	~~\| [[Length]] (R)~~
	\| <~~math~~>~~\frac{1}{R} = \frac{2}{M^2} \sum_{i,j \ne i}^{N} \frac{m_i m_j}{\left\| \vec{r_j}-\vec{r_i} \right\| }~~<~~/math~~>
	\|-
	~~\| [[Mass]] (M)~~
	\| <~~math~~>~~M = \sum_{i=1}^{N} m_i~~<~~/math~~>
	\|}
	~~<!--~~
	:~~<math> M~~ = ~~G = R = 1 \ </math>~~
	-->
	~~'''N-body units''' are~~ a ~~completely self-contained~~ [~~[Systems of measurement\|system of units~~]~~] used for [[N-body simulation]]s of self gravitating systems~~ in ~~astrophysics~~. ~~In this system, the base physical units are chosen so that the total mass, ''M'',~~ the [~~[gravitational constant~~]~~], ''G''~~, and ~~the [[Virial theorem#Virial radius\|virial radius]]~~, ~~''R''~~, ~~are normalised~~. ~~The underlying assumption is~~ that the ~~system of N objects (stars) satisfies the [[virial theorem]]~~. ~~The consequence of standard N-body units is that the velocity dispersion of the system is~~ <~~math~~>~~\scriptstyle v = 1/\sqrt{2}~~ <~~/math~~> and ~~that~~ the ~~dynamical -crossing- time scales as~~ <~~math~~>~~\scriptstyle t = 2\sqrt{2}~~ <~~/math~~>.
	~~The first mention~~ of ~~standard N-body units was by Michel Hénon (1971).<ref>~~http://~~adsabs~~.~~harvard~~.~~edu~~/~~cgi-bin~~/~~nph-bib_query?bibcode=1971Ap%26SS~~..14..~~151H&db_key=AST&data_type=HTML&format=&high=45c123dad007642~~<~~/ref~~>
	~~They were taken up by Haldan Cohn (1979)~~<~~ref~~>http://~~adsabs~~.~~harvard~~.~~edu/cgi-bin/nph-bib_query~~?~~bibcode=1979ApJ~~...~~234~~.~~1036C&db_key=AST&data_type=HTML&format=&high=439859188922689~~<~~/ref~~>
	~~and later widely advertised and generalized by Douglas Heggie and Robert Mathieu (1986)~~.<~~ref~~>~~http://adsabs~~.~~harvard~~.~~edu/cgi-bin/nph-bib_query?bibcode=1986LNP~~...~~267~~.~~.233H&db_key=AST&data_type=HTML&format=&high=439859188922689~~<~~/ref~~>

	~~==References==~~
	~~{{Reflist}}~~

	~~{{systems~~ of ~~measurement}}~~

	~~[[Category:Physical cosmology]]~~

en>Steve Quinn: Fixing links to disambiguation pages, using AWB

2010-02-11T03:53:07Z

Fixing links to disambiguation pages, using AWB

New page

{| class="wikitable" align="right" style="margin-left: 1em; background-color: #ffffff"
! Quantity
! Expression
|- align="left"
| [[Length]] (R)
| <math>\frac{1}{R} = \frac{2}{M^2} \sum_{i,j \ne i}^{N} \frac{m_i m_j}{\left| \vec{r_j}-\vec{r_i} \right| }</math>
|-
| [[Mass]] (M)
| <math>M = \sum_{i=1}^{N} m_i</math>
|}

'''N-body units''' are a completely self-contained [[Systems of measurement|system of units]] used for [[N-body simulation]]s of self gravitating systems in astrophysics. In this system, the base physical units are chosen so that the total mass, ''M'', the [[gravitational constant]], ''G'', and the [[Virial theorem#Virial radius|virial radius]], ''R'', are normalised. The underlying assumption is that the system of N objects (stars) satisfies the [[virial theorem]]. The consequence of standard N-body units is that the velocity dispersion of the system is <math>\scriptstyle v = 1/\sqrt{2} </math> and that the dynamical -crossing- time scales as <math>\scriptstyle t = 2\sqrt{2} </math>.
The first mention of standard N-body units was by Michel Hénon (1971).<ref>http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1971Ap%26SS..14..151H&db_key=AST&data_type=HTML&format=&high=45c123dad007642</ref>
They were taken up by Haldan Cohn (1979)<ref>http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1979ApJ...234.1036C&db_key=AST&data_type=HTML&format=&high=439859188922689</ref>
and later widely advertised and generalized by Douglas Heggie and Robert Mathieu (1986).<ref>http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1986LNP...267..233H&db_key=AST&data_type=HTML&format=&high=439859188922689</ref>

==References==
{{Reflist}}

{{systems of measurement}}

[[Category:Physical cosmology]]

Group delay dispersion - Revision history

134.34.139.56 at 18:04, 12 November 2014

en>Steve Quinn: Fixing links to disambiguation pages, using AWB