https://gssc.esa.int/navipedia/index.php?action=history&feed=atom&title=Satellite_Eclipses
Satellite Eclipses - Revision history
2026-10-15T17:24:55Z
Revision history for this page on the wiki
MediaWiki 1.43.1
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=14045&oldid=prev
Claudia.Prajanu at 19:15, 8 July 2018
2018-07-08T19:15:31Z
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>}}</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>High-precision GNSS positioning degrades during the GNSS satellites eclipse seasons. Indeed, once the satellite goes into the shadow, the radiation pressure vanishes. This effect introduces errors in the satellite dynamics due to the difficulty to properly modelling the solar radiation pressure. On the other hand, the satellite solar sensors lose sight of the sun and the attitude control (trying to keep the panels facing the sun) is degraded. The yaw attitude of GPS satellites is essentially random during an eclipse and for up to <math>30</math> minutes past exiting from shadow <ref name="Bar_Sever"> [Bar-Sever, Y.E., 1994] Bar-Sever, Y.E., 1994. Improvement to the GPS attitude control subsystem enables predictable attitude during eclipse seasons. <del style="font-weight: bold; text-decoration: none;">http://igscb.jpl.nasa.gov/mail/igsmail/1994/msg00166.html. </del></ref>.Each GPS satellite has two eclipse seasons per year, each lasting for about seven weeks <ref name="Mervat"> [Mervat, 1995] Mervat, L., 1995. Ambiguity Resolution Techniques in Geodetic and Geodynamic Applications of the Global Positioning System. PhD. University of Bern, Philosophisch-naturwissenschftichen Fakultat. </ref>.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>High-precision GNSS positioning degrades during the GNSS satellites eclipse seasons. Indeed, once the satellite goes into the shadow, the radiation pressure vanishes. This effect introduces errors in the satellite dynamics due to the difficulty to properly modelling the solar radiation pressure. On the other hand, the satellite solar sensors lose sight of the sun and the attitude control (trying to keep the panels facing the sun) is degraded. The yaw attitude of GPS satellites is essentially random during an eclipse and for up to <math>30</math> minutes past exiting from shadow <ref name="Bar_Sever"> [Bar-Sever, Y.E., 1994] Bar-Sever, Y.E., 1994. Improvement to the GPS attitude control subsystem enables predictable attitude during eclipse seasons. <ins style="font-weight: bold; text-decoration: none;"> </ins></ref>.Each GPS satellite has two eclipse seasons per year, each lasting for about seven weeks <ref name="Mervat"> [Mervat, 1995] Mervat, L., 1995. Ambiguity Resolution Techniques in Geodetic and Geodynamic Applications of the Global Positioning System. PhD. University of Bern, Philosophisch-naturwissenschftichen Fakultat. </ref>.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>As a consequence, the orbit during shadow and eclipse periods may be considerably degraded and the removal of satellites under such conditions can improve the high-precision positioning results.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>As a consequence, the orbit during shadow and eclipse periods may be considerably degraded and the removal of satellites under such conditions can improve the high-precision positioning results.</div></td></tr>
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Claudia.Prajanu
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=12733&oldid=prev
Filipe.Pelica at 13:41, 13 May 2014
2014-05-13T13:41:50Z
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun <del style="font-weight: bold; text-decoration: none;">( </del>and <del style="font-weight: bold; text-decoration: none;"> </del><math>\displaystyle {r}_{sun}</math> is its magnitude<del style="font-weight: bold; text-decoration: none;">)</del>, <del style="font-weight: bold; text-decoration: none;">and </del><math>\displaystyle a_e</math> is the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector<ins style="font-weight: bold; text-decoration: none;">, respectively</ins>. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun and <math>\displaystyle {r}_{sun}</math> is its magnitude, <ins style="font-weight: bold; text-decoration: none;">while </ins><math>\displaystyle a_e</math> is the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be removed during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be removed during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td></tr>
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Filipe.Pelica
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=12713&oldid=prev
Lorenzo.Ferrario at 15:10, 7 May 2014
2014-05-07T15:10:14Z
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>::<math></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>::<math></div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>\cos \phi =\displaystyle \frac{{\mathbf r}^{sat}\cdot {\mathbf r}_{sun}}{<del style="font-weight: bold; text-decoration: none;">|</del>{<del style="font-weight: bold; text-decoration: none;">\mathbf </del>r}^{sat}<del style="font-weight: bold; text-decoration: none;">\cdot </del>{<del style="font-weight: bold; text-decoration: none;">\mathbf </del>r}_{sun}<del style="font-weight: bold; text-decoration: none;">|</del>} < 0 </math> and <math>r^{sat} \sqrt{1-\cos^2 \phi}\, < a_e</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>\cos \phi =\displaystyle \frac{{\mathbf r}^{sat}\cdot {\mathbf r}_{sun}}{ {r}^{sat} {r}_{sun}} < 0 </math> and <math>r^{sat} \sqrt{1-\cos^2 \phi}\, < a_e</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>\qquad \mbox{(1)}</math></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>\qquad \mbox{(1)}</math></div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>\displaystyle a_e</math> is the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun <ins style="font-weight: bold; text-decoration: none;">( and <math>\displaystyle {r}_{sun}</math> is its magnitude)</ins>, and <math>\displaystyle a_e</math> is the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be removed during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be removed during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td></tr>
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Lorenzo.Ferrario
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=11650&oldid=prev
Carlos.Lopez at 11:41, 23 February 2012
2012-02-23T11:41:25Z
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Carlos.Lopez
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=10861&oldid=prev
Jaume.Sanz at 12:34, 30 January 2012
2012-01-30T12:34:55Z
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>\displaystyle a_e</math> <del style="font-weight: bold; text-decoration: none;">in </del>the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>\displaystyle a_e</math> <ins style="font-weight: bold; text-decoration: none;">is </ins>the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be removed during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be removed during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td></tr>
</table>
Jaume.Sanz
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=10860&oldid=prev
Jaume.Sanz at 12:19, 30 January 2012
2012-01-30T12:19:45Z
<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 12:19, 30 January 2012</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|Title={{PAGENAME}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|Title={{PAGENAME}}</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>}}</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>High-precision GNSS positioning degrades during the GNSS satellites eclipse seasons. Indeed, once the satellite goes into the shadow, the radiation pressure vanishes. This effect introduces errors in the satellite dynamics due to the difficulty to properly modelling the solar radiation pressure. On the other hand, the satellite solar sensors lose sight of the sun and the attitude control (trying to keep the panels facing the sun) is degraded. The yaw attitude of GPS satellites is essentially random during an eclipse and for up to <math>30</math> minutes past exiting from shadow <ref name="Bar_Sever"> [Bar-Sever, Y.E., 1994] Bar-Sever, Y.E., 1994. Improvement to the GPS attitude control subsystem enables predictable attitude during eclipse seasons. http://igscb.jpl.nasa.gov/mail/igsmail/1994/msg00166.html. </ref>.Each GPS satellite has two eclipse seasons per year, each lasting for about seven weeks <ref name="Mervat"> [Mervat, 1995] Mervat, L., 1995. Ambiguity Resolution Techniques in Geodetic and Geodynamic Applications of the Global <del style="font-weight: bold; text-decoration: none;">positioning </del>System. PhD. University of Bern, Philosophisch-naturwissenschftichen Fakultat. </ref>.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>High-precision GNSS positioning degrades during the GNSS satellites eclipse seasons. Indeed, once the satellite goes into the shadow, the radiation pressure vanishes. This effect introduces errors in the satellite dynamics due to the difficulty to properly modelling the solar radiation pressure. On the other hand, the satellite solar sensors lose sight of the sun and the attitude control (trying to keep the panels facing the sun) is degraded. The yaw attitude of GPS satellites is essentially random during an eclipse and for up to <math>30</math> minutes past exiting from shadow <ref name="Bar_Sever"> [Bar-Sever, Y.E., 1994] Bar-Sever, Y.E., 1994. Improvement to the GPS attitude control subsystem enables predictable attitude during eclipse seasons. http://igscb.jpl.nasa.gov/mail/igsmail/1994/msg00166.html. </ref>.Each GPS satellite has two eclipse seasons per year, each lasting for about seven weeks <ref name="Mervat"> [Mervat, 1995] Mervat, L., 1995. Ambiguity Resolution Techniques in Geodetic and Geodynamic Applications of the Global <ins style="font-weight: bold; text-decoration: none;">Positioning </ins>System. PhD. University of Bern, Philosophisch-naturwissenschftichen Fakultat. </ref>.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>As a consequence, the orbit during shadow and eclipse periods may be considerably degraded and the removal of satellites under such conditions can improve the high-precision positioning results.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>As a consequence, the orbit during shadow and eclipse periods may be considerably degraded and the removal of satellites under such conditions can improve the high-precision positioning results.</div></td></tr>
</table>
Jaume.Sanz
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=10801&oldid=prev
Jaume.Sanz at 12:53, 27 January 2012
2012-01-27T12:53:10Z
<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 12:53, 27 January 2012</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>::[[File:Geom_Range_Modell_Sat_Eclipses_Eclipse.png|none|thumb|400px|frameless| '''''Figure 1:''''' Simple cylinder model for the shadow of the Earth]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>::[[File:Geom_Range_Modell_Sat_Eclipses_Eclipse.png|none|thumb|400px|frameless| '''''Figure 1:''''' Simple cylinder model for the shadow of the Earth<ins style="font-weight: bold; text-decoration: none;">.</ins>]]</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
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</table>
Jaume.Sanz
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=10800&oldid=prev
Jaume.Sanz at 12:52, 27 January 2012
2012-01-27T12:52:49Z
<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 12:52, 27 January 2012</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|Title={{PAGENAME}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>|Title={{PAGENAME}}</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>}}</div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>High-precision GNSS positioning degrades during the GNSS satellites eclipse seasons. Indeed, once the satellite goes into the shadow, the radiation pressure vanishes. This effect introduces errors in the satellite dynamics due to the difficulty to properly modelling the solar radiation pressure. On the other hand, the satellite solar sensors lose sight of the sun and the attitude control (trying to keep the panels facing the sun) is degraded. The yaw attitude of GPS satellites is essentially random during an eclipse and for up to <math>30</math> minutes past exiting from shadow <ref name="Bar_Sever"> [Bar-Sever, Y.E., 1994] Bar-Sever, Y.E., 1994. Improvement to the GPS attitude control <del style="font-weight: bold; text-decoration: none;">subsystemenables </del>predictable attitude during eclipse seasons. http://igscb.jpl.nasa.gov/mail/igsmail/1994/msg00166.html. </ref>.Each GPS satellite has two eclipse seasons per year, each lasting for about seven weeks <ref name="Mervat"> [Mervat, 1995] Mervat, L., 1995. Ambiguity Resolution Techniques in Geodetic and Geodynamic Applications of the Global positioning System. PhD. University of Bern, Philosophisch-naturwissenschftichen Fakultat. </ref>.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>High-precision GNSS positioning degrades during the GNSS satellites eclipse seasons. Indeed, once the satellite goes into the shadow, the radiation pressure vanishes. This effect introduces errors in the satellite dynamics due to the difficulty to properly modelling the solar radiation pressure. On the other hand, the satellite solar sensors lose sight of the sun and the attitude control (trying to keep the panels facing the sun) is degraded. The yaw attitude of GPS satellites is essentially random during an eclipse and for up to <math>30</math> minutes past exiting from shadow <ref name="Bar_Sever"> [Bar-Sever, Y.E., 1994] Bar-Sever, Y.E., 1994. Improvement to the GPS attitude control <ins style="font-weight: bold; text-decoration: none;">subsystem enables </ins>predictable attitude during eclipse seasons. http://igscb.jpl.nasa.gov/mail/igsmail/1994/msg00166.html. </ref>.Each GPS satellite has two eclipse seasons per year, each lasting for about seven weeks <ref name="Mervat"> [Mervat, 1995] Mervat, L., 1995. Ambiguity Resolution Techniques in Geodetic and Geodynamic Applications of the Global positioning System. PhD. University of Bern, Philosophisch-naturwissenschftichen Fakultat. </ref>.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>As a consequence, the orbit during shadow and eclipse periods may be considerably degraded and the removal of satellites under such conditions can improve the high-precision positioning results.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>As a consequence, the orbit during shadow and eclipse periods may be considerably degraded and the removal of satellites under such conditions can improve the high-precision positioning results.</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>\displaystyle a_e</math> in the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>\displaystyle a_e</math> in the mean equatorial radius of the Earth (see table (1) or (2) in [[Reference Frames in GNSS]]).</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be <del style="font-weight: bold; text-decoration: none;">remove </del>during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be <ins style="font-weight: bold; text-decoration: none;">removed </ins>during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
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</table>
Jaume.Sanz
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=10799&oldid=prev
Jaume.Sanz at 12:50, 27 January 2012
2012-01-27T12:50:03Z
<p></p>
<table style="background-color: #fff; color: #202122;" data-mw="interface">
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 12:50, 27 January 2012</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>a_e</math> in the mean equatorial radius of the Earth (see [[Reference Frames in GNSS]]).</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> are the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math><ins style="font-weight: bold; text-decoration: none;">\displaystyle </ins>a_e</math> in the mean equatorial radius of the Earth (see <ins style="font-weight: bold; text-decoration: none;">table (1) or (2) in </ins>[[Reference Frames in GNSS]]).</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be remove during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be remove during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td></tr>
</table>
Jaume.Sanz
https://gssc.esa.int/navipedia/index.php?title=Satellite_Eclipses&diff=10798&oldid=prev
Jaume.Sanz at 12:46, 27 January 2012
2012-01-27T12:46:50Z
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<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td>
<td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 12:46, 27 January 2012</td>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>::<math></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>::<math></div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>\cos \phi =\displaystyle \frac{{\mathbf r}<del style="font-weight: bold; text-decoration: none;">_</del>{sat}\cdot {\mathbf r}_{sun}}{|{\mathbf r}<del style="font-weight: bold; text-decoration: none;">_</del>{sat}\cdot {\mathbf r}_{sun}|} < 0 </math> and <math><del style="font-weight: bold; text-decoration: none;">r_</del>{sat} \sqrt{1-\cos^2 \phi}\, < a_e</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>\cos \phi =\displaystyle \frac{{\mathbf r}<ins style="font-weight: bold; text-decoration: none;">^</ins>{sat}\cdot {\mathbf r}_{sun}}{|{\mathbf r}<ins style="font-weight: bold; text-decoration: none;">^</ins>{sat}\cdot {\mathbf r}_{sun}|} < 0 </math> and <math><ins style="font-weight: bold; text-decoration: none;">r^</ins>{sat} \sqrt{1-\cos^2 \phi}\, < a_e</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>\qquad \mbox{(1)}</math></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>\qquad \mbox{(1)}</math></div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> <del style="font-weight: bold; text-decoration: none;">is </del>the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>a_e</math> in the mean equatorial radius of the Earth (see [[Reference Frames in GNSS]]).</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Where <math>{\mathbf r}^{sat}</math> and <math>\displaystyle r^{sat}</math> <ins style="font-weight: bold; text-decoration: none;">are </ins>the vector from the geocentre to the satellite and the magnitude of that vector. Vector <math>{\mathbf r}_{sun}</math> is the geocentre vector to sun, and <math>a_e</math> in the mean equatorial radius of the Earth (see [[Reference Frames in GNSS]]).</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be remove during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Notice that, as commented before, the satellites should be remove during the eclipse condition and also during the first <math>30</math> minutes, at least, after exiting from eclipse.</div></td></tr>
</table>
Jaume.Sanz