Two-horn quiescent prominence observed in H-alpha and MgII h&k lines with THEMIS and IRIS
Prominences are large magnetic structures in the corona filled by cool plasma with fast evolving fine structure. We aim to better understand the plasma conditions in the fine structure of a quiescent prominence including two transient horns observed at the bottom of the cavity using the high-resolut...
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| creator | Barczynski, Krzysztof Schmieder, Brigitte Gelly, Bernard Peat, Aaron W Labrosse, Nicolas |
| description | Prominences are large magnetic structures in the corona filled by cool plasma with fast evolving fine structure. We aim to better understand the plasma conditions in the fine structure of a quiescent prominence including two transient horns observed at the bottom of the cavity using the high-resolution spectrograph IRIS and the MulTi-Raies (MTR) spectrograph of the THEMIS in the Canary Islands. We analysed the spectra obtained in H-alpha by THEMIS and MgII by IRIS and compare them with a grid of 23940 1D radiative transfer models which include a prominence-to-corona transition region (PCTR). The full observed profiles of MgII in each pixel are fitted completely by synthesised profiles with xRMS (Cross RMS; an improved version of the rolling root mean square (rRMS) method). When the RMS is below a certain threshold value, we recover the plasma conditions from the parameters of the model best fitting the observed line profile. This criterion is met in two regions (the horns and edge of the prominence) where the line profiles can generally be described as single peaked. The 1D models suggest that two different kinds of model atmospheres correspond to these two regions. The region at the edge is found to be fitted mainly with isothermal and isobaric models, while the other area (the horns) is seen to be fitted with models with a PCTR that have optical thicknesses |
| doi_str_mv | 10.48550/arxiv.2309.13776 |
| format | Article |
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We aim to better understand the plasma conditions in the fine structure of a quiescent prominence including two transient horns observed at the bottom of the cavity using the high-resolution spectrograph IRIS and the MulTi-Raies (MTR) spectrograph of the THEMIS in the Canary Islands. We analysed the spectra obtained in H-alpha by THEMIS and MgII by IRIS and compare them with a grid of 23940 1D radiative transfer models which include a prominence-to-corona transition region (PCTR). The full observed profiles of MgII in each pixel are fitted completely by synthesised profiles with xRMS (Cross RMS; an improved version of the rolling root mean square (rRMS) method). When the RMS is below a certain threshold value, we recover the plasma conditions from the parameters of the model best fitting the observed line profile. This criterion is met in two regions (the horns and edge of the prominence) where the line profiles can generally be described as single peaked. The 1D models suggest that two different kinds of model atmospheres correspond to these two regions. The region at the edge is found to be fitted mainly with isothermal and isobaric models, while the other area (the horns) is seen to be fitted with models with a PCTR that have optical thicknesses <5. In the prominence edge, the theoretical relationship between the integrated intensities in H-alpha and MgII is verified and corresponds to low emission measure values. In these regions the electron density is ~10^10 cm^{-3}, while it is one order of magnitude less in the horn regions. In the horns, we find some profiles are best fitted with models with high mean temperatures. This suggests that the hot PCTR found in the horns could be interpreted as prominence plasma in condensation phase at the bottom of the coronal cavity.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 2331-8422</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.48550/arxiv.2309.13776</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Atmospheric models ; Electron density ; Fine structure ; K lines ; One dimensional models ; Physics ; Physics - Solar and Stellar Astrophysics ; Plasma ; Prominences ; Radiative transfer</subject><ispartof>Astronomy and astrophysics (Berlin), 2023-09</ispartof><rights>2023. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,314,777,781,882,27905,27906</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2309.13776$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1051/0004-6361/202345970$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://hal.science/hal-04309200$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Barczynski, Krzysztof</creatorcontrib><creatorcontrib>Schmieder, Brigitte</creatorcontrib><creatorcontrib>Gelly, Bernard</creatorcontrib><creatorcontrib>Peat, Aaron W</creatorcontrib><creatorcontrib>Labrosse, Nicolas</creatorcontrib><title>Two-horn quiescent prominence observed in H-alpha and MgII h&k lines with THEMIS and IRIS</title><title>Astronomy and astrophysics (Berlin)</title><description>Prominences are large magnetic structures in the corona filled by cool plasma with fast evolving fine structure. We aim to better understand the plasma conditions in the fine structure of a quiescent prominence including two transient horns observed at the bottom of the cavity using the high-resolution spectrograph IRIS and the MulTi-Raies (MTR) spectrograph of the THEMIS in the Canary Islands. We analysed the spectra obtained in H-alpha by THEMIS and MgII by IRIS and compare them with a grid of 23940 1D radiative transfer models which include a prominence-to-corona transition region (PCTR). The full observed profiles of MgII in each pixel are fitted completely by synthesised profiles with xRMS (Cross RMS; an improved version of the rolling root mean square (rRMS) method). When the RMS is below a certain threshold value, we recover the plasma conditions from the parameters of the model best fitting the observed line profile. This criterion is met in two regions (the horns and edge of the prominence) where the line profiles can generally be described as single peaked. The 1D models suggest that two different kinds of model atmospheres correspond to these two regions. The region at the edge is found to be fitted mainly with isothermal and isobaric models, while the other area (the horns) is seen to be fitted with models with a PCTR that have optical thicknesses <5. In the prominence edge, the theoretical relationship between the integrated intensities in H-alpha and MgII is verified and corresponds to low emission measure values. In these regions the electron density is ~10^10 cm^{-3}, while it is one order of magnitude less in the horn regions. In the horns, we find some profiles are best fitted with models with high mean temperatures. This suggests that the hot PCTR found in the horns could be interpreted as prominence plasma in condensation phase at the bottom of the coronal cavity.</description><subject>Atmospheric models</subject><subject>Electron density</subject><subject>Fine structure</subject><subject>K lines</subject><subject>One dimensional models</subject><subject>Physics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Plasma</subject><subject>Prominences</subject><subject>Radiative transfer</subject><issn>0004-6361</issn><issn>2331-8422</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNo9kE1Lw0AQhhdRsNT-AE8uCIKH1NmP7CbHUqoJtAi2HjyF3ezWbE2TNmla_fduW_E0zLwPw8yD0C2BIY_CEJ5U8-32Q8ogHhImpbhAPcoYCSJO6SXqAQAPBBPkGg3aduVbKiQNQ9ZDH4tDHRR1U-Ft52yb22qHN029dpWtcotr3dpmbw12FU4CVW4KhVVl8OwzTXHx8IVLD7b44HYFXiSTWTo_xelbOr9BV0tVtnbwV_vo_XmyGCfB9PUlHY-mgSI0FkFuuDRKcxVbY2mstLRLLTk3YBRl0iw5cJsLGcWMeyLSOtccGIDWDASJWR89nvcWqsw2jVur5ierlcuS0TQ7zoB7LxRgTzx7d2ZPwv7po7jsJM4T92fCS9h2tt1lq7prKv9ARmPwF4OgnP0CbwRsVQ</recordid><startdate>20230924</startdate><enddate>20230924</enddate><creator>Barczynski, Krzysztof</creator><creator>Schmieder, Brigitte</creator><creator>Gelly, Bernard</creator><creator>Peat, Aaron W</creator><creator>Labrosse, Nicolas</creator><general>Cornell University Library, arXiv.org</general><general>EDP Sciences</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope><scope>1XC</scope><scope>VOOES</scope></search><sort><creationdate>20230924</creationdate><title>Two-horn quiescent prominence observed in H-alpha and MgII h&k lines with THEMIS and IRIS</title><author>Barczynski, Krzysztof ; Schmieder, Brigitte ; Gelly, Bernard ; Peat, Aaron W ; Labrosse, Nicolas</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a1296-cd47dab4a9ede29ab7efb744d0da237df404ec678934ede8bbcb40300bb306193</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Atmospheric models</topic><topic>Electron density</topic><topic>Fine structure</topic><topic>K lines</topic><topic>One dimensional models</topic><topic>Physics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Plasma</topic><topic>Prominences</topic><topic>Radiative transfer</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Barczynski, Krzysztof</creatorcontrib><creatorcontrib>Schmieder, Brigitte</creatorcontrib><creatorcontrib>Gelly, Bernard</creatorcontrib><creatorcontrib>Peat, Aaron W</creatorcontrib><creatorcontrib>Labrosse, Nicolas</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Barczynski, Krzysztof</au><au>Schmieder, Brigitte</au><au>Gelly, Bernard</au><au>Peat, Aaron W</au><au>Labrosse, Nicolas</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Two-horn quiescent prominence observed in H-alpha and MgII h&k lines with THEMIS and IRIS</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2023-09-24</date><risdate>2023</risdate><issn>0004-6361</issn><eissn>2331-8422</eissn><eissn>1432-0756</eissn><abstract>Prominences are large magnetic structures in the corona filled by cool plasma with fast evolving fine structure. We aim to better understand the plasma conditions in the fine structure of a quiescent prominence including two transient horns observed at the bottom of the cavity using the high-resolution spectrograph IRIS and the MulTi-Raies (MTR) spectrograph of the THEMIS in the Canary Islands. We analysed the spectra obtained in H-alpha by THEMIS and MgII by IRIS and compare them with a grid of 23940 1D radiative transfer models which include a prominence-to-corona transition region (PCTR). The full observed profiles of MgII in each pixel are fitted completely by synthesised profiles with xRMS (Cross RMS; an improved version of the rolling root mean square (rRMS) method). When the RMS is below a certain threshold value, we recover the plasma conditions from the parameters of the model best fitting the observed line profile. This criterion is met in two regions (the horns and edge of the prominence) where the line profiles can generally be described as single peaked. The 1D models suggest that two different kinds of model atmospheres correspond to these two regions. The region at the edge is found to be fitted mainly with isothermal and isobaric models, while the other area (the horns) is seen to be fitted with models with a PCTR that have optical thicknesses <5. In the prominence edge, the theoretical relationship between the integrated intensities in H-alpha and MgII is verified and corresponds to low emission measure values. In these regions the electron density is ~10^10 cm^{-3}, while it is one order of magnitude less in the horn regions. In the horns, we find some profiles are best fitted with models with high mean temperatures. This suggests that the hot PCTR found in the horns could be interpreted as prominence plasma in condensation phase at the bottom of the coronal cavity.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2309.13776</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Atmospheric models Electron density Fine structure K lines One dimensional models Physics Physics - Solar and Stellar Astrophysics Plasma Prominences Radiative transfer |
| title | Two-horn quiescent prominence observed in H-alpha and MgII h&k lines with THEMIS and IRIS |
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