Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations
In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a func...
Gespeichert in:
| Veröffentlicht in: | The Astrophysical journal 2010-03, Vol.711 (1), p.75-98 |
|---|---|
| Hauptverfasser: | , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext bestellen |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | 98 |
|---|---|
| container_issue | 1 |
| container_start_page | 75 |
| container_title | The Astrophysical journal |
| container_volume | 711 |
| creator | Landi, E Raymond, J. C Miralles, M. P Hara, H |
| description | In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration. |
| doi_str_mv | 10.1088/0004-637X/711/1/75 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_O3W</sourceid><recordid>TN_cdi_osti_scitechconnect_21394394</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>849473832</sourcerecordid><originalsourceid>FETCH-LOGICAL-c379t-963e6d81ab5af6697c73e31f818632ef48c1259dce333ede00a74ae27778e3</originalsourceid><addsrcrecordid>eNp9kNFLwzAQxoMoOKf_gE8BH0RYbdO0TfooYzphUnE-6FPI0ivL6JKadML-e1srexkIB8fd_b6P40PomkT3JOI8jKIoCTLKPkJGSEhClp6gEUkpDxKaslM0OgDn6ML7TT_GeT5Cn6_rvddK1nhqTalbbY3H2mDZzc6abv8ivcezDaj-hitnt3iujS1hgpctOLATLE2Jl8W8wMXKg_uWvy6X6KyStYervz5Gb4-z9-k8WBRPz9OHRaAoy9sgzyhkJSdylcoqy3KmGAVKKk54RmOoEq5InOalAkoplBBFkiUSYsYYBzpGN4Op9a0WXukW1FpZY7p3RUxonvQ1RrcD1Tj7tQPfiq32CupaGrA7L3iSJ4xyGndkPJDKWe8dVKJxeivdXpBI9EmLPjnRBym6pAURLO1Ed4NI2-bAH3OiKauODY7Zf7x_AEWtioM</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>849473832</pqid></control><display><type>article</type><title>Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations</title><source>IOP Publishing Free Content</source><creator>Landi, E ; Raymond, J. C ; Miralles, M. P ; Hara, H</creator><creatorcontrib>Landi, E ; Raymond, J. C ; Miralles, M. P ; Hara, H</creatorcontrib><description>In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/711/1/75</identifier><language>eng</language><publisher>United States: IOP Publishing</publisher><subject>ACCELERATION ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; ATMOSPHERES ; BRIGHTNESS ; ELECTROMAGNETIC RADIATION ; ENERGY ; HEATING ; HEATING RATE ; HOT PLASMA ; KINETIC ENERGY ; MAIN SEQUENCE STARS ; MASS ; OPTICAL PROPERTIES ; PHYSICAL PROPERTIES ; PLASMA ; PLASMA HEATING ; RADIATIONS ; SOLAR ACTIVITY ; SOLAR ATMOSPHERE ; SOLAR CORONA ; SPECTRA ; STARS ; STELLAR ACTIVITY ; STELLAR ATMOSPHERES ; STELLAR CORONAE ; SUN ; TIME DEPENDENCE ; ULTRAVIOLET RADIATION</subject><ispartof>The Astrophysical journal, 2010-03, Vol.711 (1), p.75-98</ispartof><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c379t-963e6d81ab5af6697c73e31f818632ef48c1259dce333ede00a74ae27778e3</citedby><cites>FETCH-LOGICAL-c379t-963e6d81ab5af6697c73e31f818632ef48c1259dce333ede00a74ae27778e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.1088/0004-637X/711/1/75/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27605,27901,27902,53906</link.rule.ids><linktorsrc>$$Uhttp://iopscience.iop.org/0004-637X/711/1/75$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://www.osti.gov/biblio/21394394$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Landi, E</creatorcontrib><creatorcontrib>Raymond, J. C</creatorcontrib><creatorcontrib>Miralles, M. P</creatorcontrib><creatorcontrib>Hara, H</creatorcontrib><title>Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations</title><title>The Astrophysical journal</title><description>In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration.</description><subject>ACCELERATION</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>ATMOSPHERES</subject><subject>BRIGHTNESS</subject><subject>ELECTROMAGNETIC RADIATION</subject><subject>ENERGY</subject><subject>HEATING</subject><subject>HEATING RATE</subject><subject>HOT PLASMA</subject><subject>KINETIC ENERGY</subject><subject>MAIN SEQUENCE STARS</subject><subject>MASS</subject><subject>OPTICAL PROPERTIES</subject><subject>PHYSICAL PROPERTIES</subject><subject>PLASMA</subject><subject>PLASMA HEATING</subject><subject>RADIATIONS</subject><subject>SOLAR ACTIVITY</subject><subject>SOLAR ATMOSPHERE</subject><subject>SOLAR CORONA</subject><subject>SPECTRA</subject><subject>STARS</subject><subject>STELLAR ACTIVITY</subject><subject>STELLAR ATMOSPHERES</subject><subject>STELLAR CORONAE</subject><subject>SUN</subject><subject>TIME DEPENDENCE</subject><subject>ULTRAVIOLET RADIATION</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2010</creationdate><recordtype>article</recordtype><recordid>eNp9kNFLwzAQxoMoOKf_gE8BH0RYbdO0TfooYzphUnE-6FPI0ivL6JKadML-e1srexkIB8fd_b6P40PomkT3JOI8jKIoCTLKPkJGSEhClp6gEUkpDxKaslM0OgDn6ML7TT_GeT5Cn6_rvddK1nhqTalbbY3H2mDZzc6abv8ivcezDaj-hitnt3iujS1hgpctOLATLE2Jl8W8wMXKg_uWvy6X6KyStYervz5Gb4-z9-k8WBRPz9OHRaAoy9sgzyhkJSdylcoqy3KmGAVKKk54RmOoEq5InOalAkoplBBFkiUSYsYYBzpGN4Op9a0WXukW1FpZY7p3RUxonvQ1RrcD1Tj7tQPfiq32CupaGrA7L3iSJ4xyGndkPJDKWe8dVKJxeivdXpBI9EmLPjnRBym6pAURLO1Ed4NI2-bAH3OiKauODY7Zf7x_AEWtioM</recordid><startdate>20100301</startdate><enddate>20100301</enddate><creator>Landi, E</creator><creator>Raymond, J. C</creator><creator>Miralles, M. P</creator><creator>Hara, H</creator><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>OTOTI</scope></search><sort><creationdate>20100301</creationdate><title>Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations</title><author>Landi, E ; Raymond, J. C ; Miralles, M. P ; Hara, H</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c379t-963e6d81ab5af6697c73e31f818632ef48c1259dce333ede00a74ae27778e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2010</creationdate><topic>ACCELERATION</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>ATMOSPHERES</topic><topic>BRIGHTNESS</topic><topic>ELECTROMAGNETIC RADIATION</topic><topic>ENERGY</topic><topic>HEATING</topic><topic>HEATING RATE</topic><topic>HOT PLASMA</topic><topic>KINETIC ENERGY</topic><topic>MAIN SEQUENCE STARS</topic><topic>MASS</topic><topic>OPTICAL PROPERTIES</topic><topic>PHYSICAL PROPERTIES</topic><topic>PLASMA</topic><topic>PLASMA HEATING</topic><topic>RADIATIONS</topic><topic>SOLAR ACTIVITY</topic><topic>SOLAR ATMOSPHERE</topic><topic>SOLAR CORONA</topic><topic>SPECTRA</topic><topic>STARS</topic><topic>STELLAR ACTIVITY</topic><topic>STELLAR ATMOSPHERES</topic><topic>STELLAR CORONAE</topic><topic>SUN</topic><topic>TIME DEPENDENCE</topic><topic>ULTRAVIOLET RADIATION</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Landi, E</creatorcontrib><creatorcontrib>Raymond, J. C</creatorcontrib><creatorcontrib>Miralles, M. P</creatorcontrib><creatorcontrib>Hara, H</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Landi, E</au><au>Raymond, J. C</au><au>Miralles, M. P</au><au>Hara, H</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations</atitle><jtitle>The Astrophysical journal</jtitle><date>2010-03-01</date><risdate>2010</risdate><volume>711</volume><issue>1</issue><spage>75</spage><epage>98</epage><pages>75-98</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration.</abstract><cop>United States</cop><pub>IOP Publishing</pub><doi>10.1088/0004-637X/711/1/75</doi><tpages>24</tpages></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2010-03, Vol.711 (1), p.75-98 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_osti_scitechconnect_21394394 |
| source | IOP Publishing Free Content |
| subjects | ACCELERATION ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ATMOSPHERES BRIGHTNESS ELECTROMAGNETIC RADIATION ENERGY HEATING HEATING RATE HOT PLASMA KINETIC ENERGY MAIN SEQUENCE STARS MASS OPTICAL PROPERTIES PHYSICAL PROPERTIES PLASMA PLASMA HEATING RADIATIONS SOLAR ACTIVITY SOLAR ATMOSPHERE SOLAR CORONA SPECTRA STARS STELLAR ACTIVITY STELLAR ATMOSPHERES STELLAR CORONAE SUN TIME DEPENDENCE ULTRAVIOLET RADIATION |
| title | Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-16T06%3A32%3A18IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_O3W&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Physical%20Conditions%20in%20a%20Coronal%20Mass%20Ejection%20from%20Hinode,%20Stereo,%20and%20SOHO%20Observations&rft.jtitle=The%20Astrophysical%20journal&rft.au=Landi,%20E&rft.date=2010-03-01&rft.volume=711&rft.issue=1&rft.spage=75&rft.epage=98&rft.pages=75-98&rft.issn=0004-637X&rft.eissn=1538-4357&rft_id=info:doi/10.1088/0004-637X/711/1/75&rft_dat=%3Cproquest_O3W%3E849473832%3C/proquest_O3W%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=849473832&rft_id=info:pmid/&rfr_iscdi=true |