ICRF to CEP - Revision history

Gema.Cueto at 10:58, 3 September 2025

2025-09-03T10:58:43Z

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 \\
 \\
-=\left[  \begin{array}{ccc} \cos \Delta \psi  & -\cos \varepsilon \; \sin \Delta \psi  & -\sin \varepsilon \; \sin \Delta \psi  \\  -\cos (\varepsilon +\Delta \varepsilon )\; \sin \Delta \psi  &  \begin{array}{c} \cos (\varepsilon +\Delta \varepsilon )\; \cos \varepsilon \; \cos \Delta \psi - \\  -\sin (\varepsilon +\Delta \varepsilon )\; \sin \varepsilon  \end{array} &  \begin{array}{c} \cos (\varepsilon +\Delta \varepsilon )\; \sin \varepsilon \; \cos \Delta \psi + \\  +\sin (\varepsilon +\Delta \varepsilon )\; \cos \varepsilon  \end{array} \\  \sin (\varepsilon +\Delta \varepsilon )\; \sin \Delta \psi  &  \begin{array}{c} -\sin (\varepsilon +\Delta \varepsilon )\; \cos \varepsilon \; \cos \Delta \psi + \\  +\cos (\varepsilon +\Delta \varepsilon )\; \sin \varepsilon  \end{array} &  \begin{array}{c} -\sin (\varepsilon +\Delta \varepsilon )\; \sin \varepsilon \; \cos \Delta \psi + \\  +\cos (\varepsilon +\Delta \varepsilon )\; \cos \varepsilon  \end{array} \end{array} \right]
+=\left[
 \\
 \end{array}

2012-02-23T11:33:37Z

2012-01-23T08:32:51Z

2012-01-19T08:05:46Z

← Older revision		Revision as of 08:05, 19 January 2012
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	</math>		</math>

	:: Table 1: Earth rotation variations due to zonal tides [Yoder et al., 1981]<ref> [Yoder et al., 1981] Yoder, C., Williams, J. and Parke, M., 1981. Tidal Variations of Earth Rotation. Journal of Geophysical Research. pp. 881-891.</ref> (see IERS 96 Conventions). Components with period under 35 days. See also http://hpiers.obspm.fr/eop-pc/models/UT1/~~UT1R\_tab~~.html		:: Table 1: Earth rotation variations due to zonal tides [Yoder et al., 1981]<ref> [Yoder et al., 1981] Yoder, C., Williams, J. and Parke, M., 1981. Tidal Variations of Earth Rotation. Journal of Geophysical Research. pp. 881-891.</ref> (see IERS 96 Conventions). Components with period under 35 days. See also http://hpiers.obspm.fr/eop-pc/models/UT1/UT1R_tab.html


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	\end{array}		\end{array}
	</math>		</math>
	:::Table 2: IAU1980 Theory of Nutation model (http://hpiers.obspm.fr/~~eoppc~~/models/nutations/~~nut\_IAU1980~~.dat).		:::Table 2: IAU1980 Theory of Nutation model (http://hpiers.obspm.fr/eop-pc/models/nutations/nut_IAU1980.dat).

	==Notes==		==Notes==

2012-01-19T07:55:26Z

← Older revision		Revision as of 07:55, 19 January 2012
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	* '''Nutation Matrix:''' <math>{\mathbf N}</math>		* '''Nutation Matrix:''' <math>{\mathbf N}</math>

	:This matrix is similar to that studied in the previous case. In Figure ~~\ref{nutation}~~ are described the steps to perform the Nutation correction. The objective of this rotation is to match the mean coordinates (labelled with "<math>m</math>") with the true coordinates (labelled with "<math>t</math>"), this operation is made through the ecliptic plane as showed in this graphic.		:This matrix is similar to that studied in the previous case. In Figure 2 are described the steps to perform the Nutation correction. The objective of this rotation is to match the mean coordinates (labelled with "<math>m</math>") with the true coordinates (labelled with "<math>t</math>"), this operation is made through the ecliptic plane as showed in this graphic.

2012-01-19T07:52:30Z

← Older revision		Revision as of 07:52, 19 January 2012
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	where <math>T</math> is the time expressed in Julian centuries (see [[Transformations between Time Systems]]) between the reference epoch J2000.0 and the epoch <math>t</math> of observation. An important note to point out is that the time <math>t</math> must be expressed in TDB scale because, as said in previous sections, all computations related to solar system planet orbits and mechanics must be expressed in this scale.		where <math>T</math> is the time expressed in Julian centuries (see equation (17) in [[Transformations between Time Systems]]) between the reference epoch J2000.0 and the epoch <math>t</math> of observation. An important note to point out is that the time <math>t</math> must be expressed in TDB scale because, as said in previous sections, all computations related to solar system planet orbits and mechanics must be expressed in this scale.

2012-01-18T09:20:56Z

← Older revision		Revision as of 09:20, 18 January 2012
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	{{Article Infobox2		{{Article Infobox2
	\|Category=Fundamentals		\|Category=Fundamentals
	~~\|Title={{PAGENAME}}~~		\|Authors=J. Sanz Subirana, J.M. Juan Zornoza and M. Hernández-Pajares, Technical University of Catalonia, Spain.
	\|Authors=J. Sanz Subirana, JM. Juan Zornoza and M. ~~Hernandez~~-Pajares, University of ~~Catalunia~~, Spain.
	\|Level=Advanced		\|Level=Advanced
	\|YearOfPublication=2011		\|YearOfPublication=2011
			\|Title={{PAGENAME}}
	}}		}}
			To transform coordinates from ICRF to the CEP it is necessary to correct the Precession and Nutation effects. This transformation is performed by a composite of rotations that can done by two orthogonal matrices <math>{\mathbf P}</math> and <math>{\mathbf N}</math> as follows:
	To transform coordinates ~~form~~ ICRF to the CEP it is necessary to correct the Precession and Nutation effects. This transformation is performed by a composite of rotations that can done by two orthogonal matrices <math>{\mathbf P}</math> and <math>{\mathbf N}</math> as follows:

2011-10-28T10:10:24Z

← Older revision		Revision as of 10:10, 28 October 2011
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	\|Title={{PAGENAME}}		\|Title={{PAGENAME}}
	\|Authors=J. Sanz Subirana, JM. Juan Zornoza and M. Hernandez-Pajares, University of Catalunia, Spain.		\|Authors=J. Sanz Subirana, JM. Juan Zornoza and M. Hernandez-Pajares, University of Catalunia, Spain.
	\|Level=~~Basic~~		\|Level=Advanced
	\|YearOfPublication=2011		\|YearOfPublication=2011
	}}		}}

2011-08-09T08:47:42Z

← Older revision		Revision as of 08:47, 9 August 2011
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	[[Category:Fundamentals]]		[[Category:Fundamentals]]
			[[Category:GNSS Time Reference, Coordinate Frames and Orbits]]
			[[Category:Coordinate Systems]]

2011-08-08T12:51:04Z

← Older revision		Revision as of 12:51, 8 August 2011
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	:::<math>		:::<math>
	\alpha_5=\Omega =450\,160_{\cdot}^{\prime \prime}280-(5^r+482\,890_{\cdot}^{\prime \prime}539)\; T+7_{\cdot}^{\prime \prime}455\; T^2+0_{\cdot}^{\prime \prime}008\; T^3		\alpha_5=\Omega =450\,160_{\cdot}^{\prime \prime}280-(5^r+482\,890_{\cdot}^{\prime \prime}539)\; T+7_{\cdot}^{\prime \prime}455\; T^2+0_{\cdot}^{\prime \prime}008\; T^3
	\qquad \mbox{(9)}		\qquad \mbox{(10)}
	</math>		</math>