http://solar.gmu.edu/heliophysics/index.php?action=history&feed=atom&title=Additional_Resources 2026-06-01T09:59:44Z Revision history for this page on the wiki MediaWiki 1.31.0 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1985&oldid=prev 2013-11-07T21:11:19Z

<p>‎<span dir="auto"><span class="autocomment">2011</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:11, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l27" >Line 27:</td> <td colspan="2" class="diff-lineno">Line 27:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. doi: [http://dx.doi.org/10.1088/0004-637X/732/2/117 10.1088/0004-637X/732/2/117] http://http://iopscience.iop.org/0004-637X/<del class="diffchange diffchange-inline">732</del>/2/<del class="diffchange diffchange-inline">117</del>/</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. doi: [http://dx.doi.org/10.1088/0004-637X/732/2/117 10.1088/0004-637X/732/2/117] http://<ins class="diffchange diffchange-inline">iopscience.iop.org/0004-637X/732/2/117/</ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins class="diffchange diffchange-inline">*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. I. Geometrical Analysis,&#160; 731, 2, 109, 2011. doi: [http://dx.doi.org/10.1088/0004-637X/731/2/109 10.1088/0004-637X/731/2/109] </ins>http://iopscience.iop.org/0004-637X/<ins class="diffchange diffchange-inline">731</ins>/2/<ins class="diffchange diffchange-inline">109</ins>/</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1984&oldid=prev 2013-11-07T21:08:45Z

<p>‎<span dir="auto"><span class="autocomment">2011</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:08, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l27" >Line 27:</td> <td colspan="2" class="diff-lineno">Line 27:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. doi: [http://dx.doi.org/<del class="diffchange diffchange-inline">110</del>.1088/0004-637X/732/2/117 10.1088/0004-637X/732/2/117] http://http://iopscience.iop.org/0004-637X/732/2/117/</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. doi: [http://dx.doi.org/<ins class="diffchange diffchange-inline">10</ins>.1088/0004-637X/732/2/117 10.1088/0004-637X/732/2/117] http://http://iopscience.iop.org/0004-637X/732/2/117/</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1983&oldid=prev 2013-11-07T21:06:42Z

<p>‎<span dir="auto"><span class="autocomment">2012</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:06, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l16" >Line 16:</td> <td colspan="2" class="diff-lineno">Line 16:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Savani, N. P.; Shiota, D.; Kusano, K.; Vourlidas, A.; Lugaz, N.: A Study of the Heliocentric Dependence of Shock Standoff Distance and Geometry using 2.5D Magnetohydrodynamic Simulations of Coronal Mass Ejection Driven Shocks, 759, 2, 103, 2012. doi: [<del class="diffchange diffchange-inline">http://</del>http://dx.doi.org/10.1088/0004-637X/759/2/103 10.1088/0004-637X/759/2/103] http://iopscience.iop.org/0004-637X/759/2/103/</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Savani, N. P.; Shiota, D.; Kusano, K.; Vourlidas, A.; Lugaz, N.: A Study of the Heliocentric Dependence of Shock Standoff Distance and Geometry using 2.5D Magnetohydrodynamic Simulations of Coronal Mass Ejection Driven Shocks, 759, 2, 103, 2012. doi: [http://dx.doi.org/10.1088/0004-637X/759/2/103 10.1088/0004-637X/759/2/103] http://iopscience.iop.org/0004-637X/759/2/103/</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Savani, N. P.; Davies, J. A.; Davis, C. J.; Shiota, D.; Rouillard, A. P.; Owens, M. J.; Kusano, K.; Bothmer, V.; Bamford, S. P.; Lintott, C. J.; Smith, A.: Observational Tracking of the 2D Structure of Coronal Mass Ejections Between the Sun and 1 AU, 279, 2, pp. 517-535, 2012. doi: [<del class="diffchange diffchange-inline">http://</del>http://dx.doi.org/10.1007/s11207-012-0041-6 10.1007/s11207-012-0041-6] http://link.springer.com/article/10.1007%2Fs11207-012-0041-6</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Savani, N. P.; Davies, J. A.; Davis, C. J.; Shiota, D.; Rouillard, A. P.; Owens, M. J.; Kusano, K.; Bothmer, V.; Bamford, S. P.; Lintott, C. J.; Smith, A.: Observational Tracking of the 2D Structure of Coronal Mass Ejections Between the Sun and 1 AU, 279, 2, pp. 517-535, 2012. doi: [http://dx.doi.org/10.1007/s11207-012-0041-6 10.1007/s11207-012-0041-6] http://link.springer.com/article/10.1007%2Fs11207-012-0041-6</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 2. Main Phase of Storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 28–36. 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 31–40.)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 2. Main Phase of Storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 28–36. 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 31–40.)</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1982&oldid=prev 2013-11-07T21:06:13Z

<p>‎<span dir="auto"><span class="autocomment">2011</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:06, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l27" >Line 27:</td> <td colspan="2" class="diff-lineno">Line 27:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. &#160;</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. <ins class="diffchange diffchange-inline">doi: [http://dx.doi.org/110.1088/0004-637X/732/2/117 10.1088/0004-637X/732/2/117] http://http://iopscience.iop.org/0004-637X/732/2/117/</ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1981&oldid=prev 2013-11-07T21:04:27Z

<p>‎<span dir="auto"><span class="autocomment">2011</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:04, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l27" >Line 27:</td> <td colspan="2" class="diff-lineno">Line 27:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;">*Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth, R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.: Evolution of Coronal Mass Ejection Morphology with Increasing Heliocentric Distance. II. In Situ Observations,&#160; 732, 2, 117, 2011. </ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev Yu. I., Lodkina I. G., Nikolaeva N. S., and Yermolaev M. Yu., Statistical Study of Interplanetary Condition Effect on Geomagnetic Storms: 2. Variations of Parameters, Cosmic Research, 2011, Vol. 49, No. 1, pp. 21-34, 2011. (Original Russian Text: Yu.I. Yermolaev, I.G. Lodkina, N.S. Nikolaeva, M.Yu. Yermolaev, published in Kosmicheskie Issledovaniya, 2011, Vol. 49, No.1, pp. 24-37)</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Nikolaeva N. S., Yermolaev Yu. I., and Lodkina I. G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams, Geomagnetism and Aeronomy, 2011, Vol. 51, No. 1, pp. 49-65. 2011. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2011, published in Geomagnetizm i Aeronomiya, 2011, Vol. 51, No. 1, pp. 51-67) &#160;</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Nikolaeva N. S., Yermolaev Yu. I., and Lodkina I. G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams, Geomagnetism and Aeronomy, 2011, Vol. 51, No. 1, pp. 49-65. 2011. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2011, published in Geomagnetizm i Aeronomiya, 2011, Vol. 51, No. 1, pp. 51-67)</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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>&#160;</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2010 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2010 ===</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Poomvises, Watanachak; Zhang, Jie; Olmedo, Oscar:&quot; Coronal Mass Ejection Propagation and Expansion in Three-dimensional Space in the Heliosphere Based on Stereo/SECCHI Observations&quot;, The Astrophysical Journal Letters, Volume 717, Issue 2, pp. L159-L163, 07/2010</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Poomvises, Watanachak; Zhang, Jie; Olmedo, Oscar:&quot; Coronal Mass Ejection Propagation and Expansion in Three-dimensional Space in the Heliosphere Based on Stereo/SECCHI Observations&quot;, The Astrophysical Journal Letters, Volume 717, Issue 2, pp. L159-L163, 07/2010</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1980&oldid=prev 2013-11-07T21:02:30Z

<p>‎<span dir="auto"><span class="autocomment">2012</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 21:02, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l15" >Line 15:</td> <td colspan="2" class="diff-lineno">Line 15:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;">*Savani, N. P.; Shiota, D.; Kusano, K.; Vourlidas, A.; Lugaz, N.: A Study of the Heliocentric Dependence of Shock Standoff Distance and Geometry using 2.5D Magnetohydrodynamic Simulations of Coronal Mass Ejection Driven Shocks, 759, 2, 103, 2012. doi: [http://http://dx.doi.org/10.1088/0004-637X/759/2/103 10.1088/0004-637X/759/2/103] http://iopscience.iop.org/0004-637X/759/2/103/</ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;">*Savani, N. P.; Davies, J. A.; Davis, C. J.; Shiota, D.; Rouillard, A. P.; Owens, M. J.; Kusano, K.; Bothmer, V.; Bamford, S. P.; Lintott, C. J.; Smith, A.: Observational Tracking of the 2D Structure of Coronal Mass Ejections Between the Sun and 1 AU, 279, 2, pp. 517-535, 2012. doi: [http://http://dx.doi.org/10.1007/s11207-012-0041-6 10.1007/s11207-012-0041-6] http://link.springer.com/article/10.1007%2Fs11207-012-0041-6</ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 2. Main Phase of Storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 28–36. 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 31–40.)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 2. Main Phase of Storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 28–36. 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 31–40.)</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1979&oldid=prev 2013-11-07T20:53:10Z

<p>‎<span dir="auto"><span class="autocomment">2013</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 20:53, 7 November 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l8" >Line 8:</td> <td colspan="2" class="diff-lineno">Line 8:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>== Relevant Papers ==</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>== Relevant Papers ==</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;">*Savani, N. P.; Vourlidas, A.; Pulkkinen, A.; Nieves-Chinchilla, T.; Lavraud, B.; Owens, M. J.: Tracking the momentum flux of a CME and quantifying its influence on geomagnetically induced currents at Earth, Space Weather, 11, 5, pp 245-261, [http://dx.doi.org/10.1002/swe.20038 doi: 10.1002/swe.20038] http://onlinelibrary.wiley.com/doi/10.1002/swe.20038/abstract;jsessionid=0DD02C59D5E6E7CAC107973D50D6C212.f04t01</ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45 http://iopscience.iop.org/0004-637X/769/1/45/</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45 http://iopscience.iop.org/0004-637X/769/1/45/</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Al-Haddad, N.; Nieves-Chinchilla, T.; Savani, N.P.; Möstl, C.; Marubashi, K.; Hidalgo, M.A.; Roussev, I.; Poedts, S.; Farrugia, C.J.: Magnetic Field Configuration Models and Reconstruction Methods: a comparative study, Solar Physics, Topical Issue “Flux-rope structure of coronal mass ejections”, 284, 1, pp 129-149, 2013. doi: 10.1007/s11207-013-0244-5 http://link.springer.com/article/10.1007%2Fs11207-013-0244-5</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Al-Haddad, N.; Nieves-Chinchilla, T.; Savani, N.P.; Möstl, C.; Marubashi, K.; Hidalgo, M.A.; Roussev, I.; Poedts, S.; Farrugia, C.J.: Magnetic Field Configuration Models and Reconstruction Methods: a comparative study, Solar Physics, Topical Issue “Flux-rope structure of coronal mass ejections”, 284, 1, pp 129-149, 2013. doi: 10.1007/s11207-013-0244-5 http://link.springer.com/article/10.1007%2Fs11207-013-0244-5</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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><del style="font-weight: bold; text-decoration: none;"></del></div></td><td colspan="2">&#160;</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td></tr> </table>

Ns902 http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1296&oldid=prev 2013-06-12T11:14:07Z

<p>‎<span dir="auto"><span class="autocomment">Relevant Papers</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 11:14, 12 June 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l9" >Line 9:</td> <td colspan="2" class="diff-lineno">Line 9:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45 http://iopscience.iop.org/0004-637X/769/1/45/</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45 http://iopscience.iop.org/0004-637X/769/1/45/</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;">*Al-Haddad, N.; Nieves-Chinchilla, T.; Savani, N.P.; Möstl, C.; Marubashi, K.; Hidalgo, M.A.; Roussev, I.; Poedts, S.; Farrugia, C.J.: Magnetic Field Configuration Models and Reconstruction Methods: a comparative study, Solar Physics, Topical Issue “Flux-rope structure of coronal mass ejections”, 284, 1, pp 129-149, 2013. doi: 10.1007/s11207-013-0244-5 http://link.springer.com/article/10.1007%2Fs11207-013-0244-5</ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 2. Main Phase of Storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 28–36. 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 31–40.)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 2. Main Phase of Storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 28–36. 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 31–40.)</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 3. Development of storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 37–48., 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. *Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 41–52.)</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Nikolaeva N.S., Yermolaev Yu.I., Lodkina I.G., Dependence of Geomagnetic Activity during Magnetic Storms on the Solar Wind Parameters for Different Types of Streams: 3. Development of storm, Geomagnetism and Aeronomy, 2012, Vol. 52, No. 1, pp. 37–48., 2012. (Original Russian Text: N.S. Nikolaeva, Yu.I. *Yermolaev, I.G. Lodkina, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 1, pp. 41–52.)</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev, Y. I., N. S. Nikolaeva, I. G. Lodkina, and M. Y. Yermolaev (2012), Geoeffectiveness and efficiency of CIR, sheath, and ICME in generation of magnetic storms, J. Geophys. Res., 117, A00L07, doi:10.1029/2011JA017139.</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev, Y. I., N. S. Nikolaeva, I. G. Lodkina, and M. Y. Yermolaev (2012), Geoeffectiveness and efficiency of CIR, sheath, and ICME in generation of magnetic storms, J. Geophys. Res., 117, A00L07, doi:10.1029/2011JA017139.</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev, Y. I., I. G. Lodkina, N. S. Nikolaeva, and M. Y. Yermolaev (2012), Recovery phase of magnetic storms induced by different interplanetary drivers, J. Geophys. Res., 117, A08207, doi:10.1029/2012JA017716</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>*Yermolaev, Y. I., I. G. Lodkina, N. S. Nikolaeva, and M. Y. Yermolaev (2012), Recovery phase of magnetic storms induced by different interplanetary drivers, J. Geophys. Res., 117, A08207, doi:10.1029/2012JA017716</div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2">&#160;</td><td class='diff-marker'>+</td><td style="color: #222; 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><ins style="font-weight: bold; text-decoration: none;">*Lugaz, N., P. Kintner, C. Möstl, L.K. Jian, C. Davis, C.J. Farrugia, Heliospheric observations of STEREO directed coronal mass ejections in 2008-2010: Lessons for future observations of Earth-directed CMEs, Solar Physics, 279, Issue 2, pp. 497-515, 2012. http://link.springer.com/article/10.1007%2Fs11207-012-0007-8</ins></div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2011 ===</div></td></tr> </table>

Moestlc http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1295&oldid=prev 2013-06-12T11:12:35Z

<p>‎<span dir="auto"><span class="autocomment">2013</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 11:12, 12 June 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l8" >Line 8:</td> <td colspan="2" class="diff-lineno">Line 8:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>== Relevant Papers ==</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>== Relevant Papers ==</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>*Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45</div></td><td class='diff-marker'>+</td><td style="color: #222; 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>*Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45 http://iopscience.iop.org/0004-637X/769/1/45/</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>http://iopscience.iop.org/0004-637X/769/1/45/</div></td><td colspan="2">&#160;</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2012 ===</div></td></tr> </table>

Moestlc http://solar.gmu.edu/heliophysics/index.php?title=Additional_Resources&diff=1294&oldid=prev 2013-06-12T11:12:28Z

<p>‎<span dir="auto"><span class="autocomment">2013</span></span></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 11:12, 12 June 2013</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l8" >Line 8:</td> <td colspan="2" class="diff-lineno">Line 8:</td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>== Relevant Papers ==</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>== Relevant Papers ==</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>=== 2013 ===</div></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; 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>Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45</div></td><td class='diff-marker'>+</td><td style="color: #222; 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><ins class="diffchange diffchange-inline">*</ins>Liu, Y., J.G. Luhmann, N. Lugaz, C. Möstl, J.A. Davies, S. D. Bale, R. P. Lin, On Sun-to-Earth propagation of coronal mass ejections, The Astrophysical Journal, 769, 45, 15 pp, 2013. doi:10.1088/0004-637X/769/1/45</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>http://iopscience.iop.org/0004-637X/769/1/45/</div></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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>http://iopscience.iop.org/0004-637X/769/1/45/</div></td></tr> <tr><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td><td class='diff-marker'>&#160;</td><td style="background-color: #f8f9fa; color: #222; 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;"></td></tr> </table>

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