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dc.contributor.authorDalla, Silvia C.
dc.contributor.authorBalogh, André
dc.contributor.authorKrucker, Säm Ä M.
dc.contributor.authorPosner, Arik
dc.contributor.authorMüller-Mellin, Reinhold
dc.contributor.authorAnglin, J. D.
dc.contributor.authorHofer, Mirjam Y.
dc.contributor.authorMarsden, Richard G.
dc.contributor.authorSanderson, T. R.
dc.contributor.authorZhang, Ming
dc.date.accessioned2018-01-09T18:03:26Z
dc.date.available2018-01-09T18:03:26Z
dc.date.issued2003-06-30
dc.identifier.citationDalla, S., Balogh, A., Krucker, S., Posner, A., Müller-Mellin, R., Anglin, J. D., . . . McKibben, R. B. (2003). Delay in solar energetic particle onsets at high heliographic latitudes. Annales Geophysicae, 21(6), 1367-1375.en_US
dc.identifier.urihttp://hdl.handle.net/11141/2267
dc.descriptionInterplanetary physics (energetic particles) – Solar physics, astrophysics and astronomy (energetic particles, flares and mass ejections)en_US
dc.description.abstractUlysses observations have shown that solar energetic particles (SEPs) can easily reach high heliographic latitudes. To obtain information on the release and propagation of SEPs prior to their arrival at Ulysses, we analyse the onsets of nine large high-latitude particle events. We measure the onset times in several energy channels, and plot them versus inverse particle speed. This allows us to derive an experimental path length and time of release from the solar atmosphere. We repeat the procedure for near-Earth observations by Wind and SOHO. We find that the derived path lengths at Ulysses are 1.06 to 2.45 times the length of a Parker spiral magnetic field line connecting the spacecraft to the Sun. The time of particle release from the Sun is between 100 and 350 min later than the release time derived from in-ecliptic measurements. We find no evidence of correlation between the delay in release and the inverse of the speed of the CME associated with the event, or the inverse of the speed of the corresponding interplanetary shock. The main parameter determining the magnitude of the delay appears to be the difference in latitude between the flare and the footpoint of the spacecraft.en_US
dc.language.isoen_USen_US
dc.rights© Dalla, Silvia C., Balogh, André, Krucker, Säm Ä M., Posner, Arik, Müller-Mellin, Reinhold, Anglin, J. D., Hofer, Mirjam Y., Marsden, Richard G., Sanderson, T. R., Zhang, Ming 2003. This work is distributed under the Creative Commons Attribution 3.0 License.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/3.0/en_US
dc.titleDelay in solar energetic particle onsets at high heliographic latitudesen_US
dc.typeArticleen_US
dc.identifier.doi10.5194/angeo-21-1367-2003
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©  Dalla, Silvia C., Balogh, André, Krucker, Säm Ä M., Posner, Arik, Müller-Mellin, Reinhold, Anglin, J. D., Hofer, Mirjam Y., Marsden, Richard G., Sanderson, T. R., Zhang, Ming 2003. This work is distributed under
the Creative Commons Attribution 3.0 License.
Except where otherwise noted, this item's license is described as © Dalla, Silvia C., Balogh, André, Krucker, Säm Ä M., Posner, Arik, Müller-Mellin, Reinhold, Anglin, J. D., Hofer, Mirjam Y., Marsden, Richard G., Sanderson, T. R., Zhang, Ming 2003. This work is distributed under the Creative Commons Attribution 3.0 License.