Influence of Active Regions on Solar Wind Characteristics at the Cycle Maximum
Active regions (ARs) on the Sun are discussed as a possible source of the slow solar wind (SW) whose origin is still a subject of debates. In this paper we present experimental evidence for the possible influence of ARs on the SW speed and temperature near the maximum of solar cycle 23 (2000–2002)....
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| Veröffentlicht in: | Astronomy letters 2022-07, Vol.48 (7), p.406-415 |
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| creator | Bogachev, S. A. Reva, A. A. Kirichenko, A. S. Ulyanov, A. S. Loboda, I. P. |
| description | Active regions (ARs) on the Sun are discussed as a possible source of the slow solar wind (SW) whose origin is still a subject of debates. In this paper we present experimental evidence for the possible influence of ARs on the SW speed and temperature near the maximum of solar cycle 23 (2000–2002). We have studied separately the characteristics of the SW formed in the periods when ARs were on the central meridian (CM) of the Sun (
of the entire observing time) and the characteristics of the SW formed in the absence of ARs on the CM (
of the observing time). The SW speed in the former case (in the presence of ARs), on average, have turned out to be lower than the speed of the SW formed in the absence of ARs approximately by 1
(434.06 versus 438.09 km s
with a measurement error
km s
). For the SW temperature the corresponding difference is about 6
(
K versus
K with an error
K). This result confirms, on average, a lower speed and temperature of the SW forming in ARs in comparison with the SW component forming in coronal holes. |
| doi_str_mv | 10.1134/S1063773722070039 |
| format | Article |
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of the entire observing time) and the characteristics of the SW formed in the absence of ARs on the CM (
of the observing time). The SW speed in the former case (in the presence of ARs), on average, have turned out to be lower than the speed of the SW formed in the absence of ARs approximately by 1
(434.06 versus 438.09 km s
with a measurement error
km s
). For the SW temperature the corresponding difference is about 6
(
K versus
K with an error
K). This result confirms, on average, a lower speed and temperature of the SW forming in ARs in comparison with the SW component forming in coronal holes.</description><identifier>ISSN: 1063-7737</identifier><identifier>EISSN: 1562-6873</identifier><identifier>DOI: 10.1134/S1063773722070039</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Astronomy ; Astrophysics and Astroparticles ; Coronal holes ; Error analysis ; Observations and Techniques ; Physics ; Physics and Astronomy ; Solar cycle ; Solar wind</subject><ispartof>Astronomy letters, 2022-07, Vol.48 (7), p.406-415</ispartof><rights>Pleiades Publishing, Inc. 2022</rights><rights>Pleiades Publishing, Inc. 2022.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c246t-df9e666796586fcaad80b6fa543e7e14d9463f3c47a88c3aab638c9fbe5a008b3</citedby><cites>FETCH-LOGICAL-c246t-df9e666796586fcaad80b6fa543e7e14d9463f3c47a88c3aab638c9fbe5a008b3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1134/S1063773722070039$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1134/S1063773722070039$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,777,781,27905,27906,41469,42538,51300</link.rule.ids></links><search><creatorcontrib>Bogachev, S. A.</creatorcontrib><creatorcontrib>Reva, A. A.</creatorcontrib><creatorcontrib>Kirichenko, A. S.</creatorcontrib><creatorcontrib>Ulyanov, A. S.</creatorcontrib><creatorcontrib>Loboda, I. P.</creatorcontrib><title>Influence of Active Regions on Solar Wind Characteristics at the Cycle Maximum</title><title>Astronomy letters</title><addtitle>Astron. Lett</addtitle><description>Active regions (ARs) on the Sun are discussed as a possible source of the slow solar wind (SW) whose origin is still a subject of debates. In this paper we present experimental evidence for the possible influence of ARs on the SW speed and temperature near the maximum of solar cycle 23 (2000–2002). We have studied separately the characteristics of the SW formed in the periods when ARs were on the central meridian (CM) of the Sun (
of the entire observing time) and the characteristics of the SW formed in the absence of ARs on the CM (
of the observing time). The SW speed in the former case (in the presence of ARs), on average, have turned out to be lower than the speed of the SW formed in the absence of ARs approximately by 1
(434.06 versus 438.09 km s
with a measurement error
km s
). For the SW temperature the corresponding difference is about 6
(
K versus
K with an error
K). This result confirms, on average, a lower speed and temperature of the SW forming in ARs in comparison with the SW component forming in coronal holes.</description><subject>Astronomy</subject><subject>Astrophysics and Astroparticles</subject><subject>Coronal holes</subject><subject>Error analysis</subject><subject>Observations and Techniques</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Solar cycle</subject><subject>Solar wind</subject><issn>1063-7737</issn><issn>1562-6873</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNp1kF9LwzAUxYMoOKcfwLeAz9WkaZP0cRT_DKaCU3wsaXqzdbTJTFJx396OCT6IT_fAOb9z4SB0Sck1pSy7WVLCmRBMpCkRhLDiCE1oztOES8GORz3ayd4_RWchbAghBWNkgp7m1nQDWA3YGTzTsf0E_AKr1tmAncVL1ymP31vb4HKtvNIRfBtiqwNWEcc14HKnO8CP6qvth_4cnRjVBbj4uVP0dnf7Wj4ki-f7eTlbJDrNeEwaUwDnXBQ8l9xopRpJam5UnjEQQLOmyDgzTGdCSamZUjVnUhemhlwRIms2RVeH3q13HwOEWG3c4O34skoFo0TmlGdjih5S2rsQPJhq69te-V1FSbWfrfoz28ikByaMWbsC_9v8P_QNK9VuLA</recordid><startdate>20220701</startdate><enddate>20220701</enddate><creator>Bogachev, S. A.</creator><creator>Reva, A. A.</creator><creator>Kirichenko, A. S.</creator><creator>Ulyanov, A. S.</creator><creator>Loboda, I. P.</creator><general>Pleiades Publishing</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope></search><sort><creationdate>20220701</creationdate><title>Influence of Active Regions on Solar Wind Characteristics at the Cycle Maximum</title><author>Bogachev, S. A. ; Reva, A. A. ; Kirichenko, A. S. ; Ulyanov, A. S. ; Loboda, I. P.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c246t-df9e666796586fcaad80b6fa543e7e14d9463f3c47a88c3aab638c9fbe5a008b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Astronomy</topic><topic>Astrophysics and Astroparticles</topic><topic>Coronal holes</topic><topic>Error analysis</topic><topic>Observations and Techniques</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Solar cycle</topic><topic>Solar wind</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bogachev, S. A.</creatorcontrib><creatorcontrib>Reva, A. A.</creatorcontrib><creatorcontrib>Kirichenko, A. S.</creatorcontrib><creatorcontrib>Ulyanov, A. S.</creatorcontrib><creatorcontrib>Loboda, I. P.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bogachev, S. A.</au><au>Reva, A. A.</au><au>Kirichenko, A. S.</au><au>Ulyanov, A. S.</au><au>Loboda, I. P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Influence of Active Regions on Solar Wind Characteristics at the Cycle Maximum</atitle><jtitle>Astronomy letters</jtitle><stitle>Astron. Lett</stitle><date>2022-07-01</date><risdate>2022</risdate><volume>48</volume><issue>7</issue><spage>406</spage><epage>415</epage><pages>406-415</pages><issn>1063-7737</issn><eissn>1562-6873</eissn><abstract>Active regions (ARs) on the Sun are discussed as a possible source of the slow solar wind (SW) whose origin is still a subject of debates. In this paper we present experimental evidence for the possible influence of ARs on the SW speed and temperature near the maximum of solar cycle 23 (2000–2002). We have studied separately the characteristics of the SW formed in the periods when ARs were on the central meridian (CM) of the Sun (
of the entire observing time) and the characteristics of the SW formed in the absence of ARs on the CM (
of the observing time). The SW speed in the former case (in the presence of ARs), on average, have turned out to be lower than the speed of the SW formed in the absence of ARs approximately by 1
(434.06 versus 438.09 km s
with a measurement error
km s
). For the SW temperature the corresponding difference is about 6
(
K versus
K with an error
K). This result confirms, on average, a lower speed and temperature of the SW forming in ARs in comparison with the SW component forming in coronal holes.</abstract><cop>Moscow</cop><pub>Pleiades Publishing</pub><doi>10.1134/S1063773722070039</doi><tpages>10</tpages></addata></record> |
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| language | eng |
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| source | Springer Nature - Complete Springer Journals |
| subjects | Astronomy Astrophysics and Astroparticles Coronal holes Error analysis Observations and Techniques Physics Physics and Astronomy Solar cycle Solar wind |
| title | Influence of Active Regions on Solar Wind Characteristics at the Cycle Maximum |
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