In Situ Observations of Solar Wind Stream Interface Evolution
The heliocentric orbits of the two STEREO satellites are similar in radius and ecliptic latitude, with separation in longitude increasing by about 45° per year. This arrangement provides a unique opportunity to study the evolution of stream interfaces near 1 AU over time scales of hours to a few day...
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| Veröffentlicht in: | Solar physics 2009-10, Vol.259 (1-2), p.323-344 |
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| creator | Simunac, K. D. C. Kistler, L. M. Galvin, A. B. Lee, M. A. Popecki, M. A. Farrugia, C. Moebius, E. Blush, L. M. Bochsler, P. Wurz, P. Klecker, B. Wimmer-Schweingruber, R. F. Thompson, B. Luhmann, J. G. Russell, C. T. Howard, R. A. |
| description | The heliocentric orbits of the two STEREO satellites are similar in radius and ecliptic latitude, with separation in longitude increasing by about 45° per year. This arrangement provides a unique opportunity to study the evolution of stream interfaces near 1 AU over time scales of hours to a few days, much less than the period of a Carrington rotation. Assuming nonevolving solar wind sources that corotate with the Sun, we calculated the expected time and longitude of arrival of stream interfaces at the Ahead observatory based on the
in situ
solar wind speeds measured at the Behind observatory. We find agreement to within 5° between the expected and actual arrival longitude until the spacecraft are separated by more than 20° in heliocentric inertial longitude. This corresponds to about one day between the measurement times. Much larger deviations, up to 25° in longitude, are observed after 20° separation. Some of the deviations can be explained by a latitude difference between the spacecraft, but other deviations most likely result from evolution of the source region. Both remote and
in situ
measurements show that changes at the source boundary can occur on a time scale much shorter than one solar rotation. In 32 of 41 cases, the interface was observed earlier than expected at STEREO/Ahead. |
| doi_str_mv | 10.1007/s11207-009-9393-y |
| format | Article |
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in situ
solar wind speeds measured at the Behind observatory. We find agreement to within 5° between the expected and actual arrival longitude until the spacecraft are separated by more than 20° in heliocentric inertial longitude. This corresponds to about one day between the measurement times. Much larger deviations, up to 25° in longitude, are observed after 20° separation. Some of the deviations can be explained by a latitude difference between the spacecraft, but other deviations most likely result from evolution of the source region. Both remote and
in situ
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in situ
solar wind speeds measured at the Behind observatory. We find agreement to within 5° between the expected and actual arrival longitude until the spacecraft are separated by more than 20° in heliocentric inertial longitude. This corresponds to about one day between the measurement times. Much larger deviations, up to 25° in longitude, are observed after 20° separation. Some of the deviations can be explained by a latitude difference between the spacecraft, but other deviations most likely result from evolution of the source region. Both remote and
in situ
measurements show that changes at the source boundary can occur on a time scale much shorter than one solar rotation. In 32 of 41 cases, the interface was observed earlier than expected at STEREO/Ahead.</description><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Atmospheric Sciences</subject><subject>In situ measurement</subject><subject>Latitude</subject><subject>Longitude</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Solar physics</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Spacecraft</subject><subject>STEREO Science Results at Solar Minimum</subject><subject>Sun</subject><subject>Wind speed</subject><issn>0038-0938</issn><issn>1573-093X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2009</creationdate><recordtype>article</recordtype><sourceid>C6C</sourceid><sourceid>BENPR</sourceid><recordid>eNqN0U9LwzAYBvAgCs7pB_BWPOip-iZp_h08iEwdDHaYoreQZol0dO1M2sG-vS0VBEHdKTn8njfkfRA6x3CNAcRNxJiASAFUqqii6e4AjTATNAVF3w7RCIDK_i6P0UmMK4A-xUbodloli6Jpk3keXdiapqirmNQ-WdSlCclrUS2TRROcWSfTqnHBG-uSybYu216eoiNvyujOvs4xenmYPN8_pbP54_T-bpZahlmTGtk9zHKfLUVuOTfSecaWRhLDeSZAKsklp2LpAVvP8jzzQoAFa01GciUFHaOrYe4m1B-ti41eF9G6sjSVq9uoJQgiug-pf6XIKMcYZ728_FMSTInKQOwBiehktgcESRmnHbz4AVd1G6pug1oKIonCtEd4QDbUMQbn9SYUaxN2GoPu29ND57rrXPed612XIUMmdrZ6d-F78O-hT_oLrKc</recordid><startdate>20091001</startdate><enddate>20091001</enddate><creator>Simunac, K. 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D. C.</au><au>Kistler, L. M.</au><au>Galvin, A. B.</au><au>Lee, M. A.</au><au>Popecki, M. A.</au><au>Farrugia, C.</au><au>Moebius, E.</au><au>Blush, L. M.</au><au>Bochsler, P.</au><au>Wurz, P.</au><au>Klecker, B.</au><au>Wimmer-Schweingruber, R. F.</au><au>Thompson, B.</au><au>Luhmann, J. G.</au><au>Russell, C. T.</au><au>Howard, R. A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>In Situ Observations of Solar Wind Stream Interface Evolution</atitle><jtitle>Solar physics</jtitle><stitle>Sol Phys</stitle><date>2009-10-01</date><risdate>2009</risdate><volume>259</volume><issue>1-2</issue><spage>323</spage><epage>344</epage><pages>323-344</pages><issn>0038-0938</issn><eissn>1573-093X</eissn><abstract>The heliocentric orbits of the two STEREO satellites are similar in radius and ecliptic latitude, with separation in longitude increasing by about 45° per year. This arrangement provides a unique opportunity to study the evolution of stream interfaces near 1 AU over time scales of hours to a few days, much less than the period of a Carrington rotation. Assuming nonevolving solar wind sources that corotate with the Sun, we calculated the expected time and longitude of arrival of stream interfaces at the Ahead observatory based on the
in situ
solar wind speeds measured at the Behind observatory. We find agreement to within 5° between the expected and actual arrival longitude until the spacecraft are separated by more than 20° in heliocentric inertial longitude. This corresponds to about one day between the measurement times. Much larger deviations, up to 25° in longitude, are observed after 20° separation. Some of the deviations can be explained by a latitude difference between the spacecraft, but other deviations most likely result from evolution of the source region. Both remote and
in situ
measurements show that changes at the source boundary can occur on a time scale much shorter than one solar rotation. In 32 of 41 cases, the interface was observed earlier than expected at STEREO/Ahead.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s11207-009-9393-y</doi><tpages>22</tpages><oa>free_for_read</oa></addata></record> |
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| source | Springer Nature - Complete Springer Journals |
| subjects | Astrophysics Astrophysics and Astroparticles Atmospheric Sciences In situ measurement Latitude Longitude Physics Physics and Astronomy Solar physics Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Spacecraft STEREO Science Results at Solar Minimum Sun Wind speed |
| title | In Situ Observations of Solar Wind Stream Interface Evolution |
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