Energy release in the solar corona from spatially resolved magnetic braids

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The Sun's outer atmosphere, or corona, is millions of degrees hotter than its surface. The search for mechanisms capable of transferring energy from the Sun's interior to the periphery on such a scale has identified two strong candidates: wave heating is thought to heat the corona to 1.5 million K, and the reconnection and unravelling of magnetic braids has been proposed as the means of boosting the temperature towards 4 million K. New evidence to support that latter mechanism is provided by a five-minute series of images obtained by a high-resolution camera on-board a sounding rocket. The images reveal fine-scale braiding to a resolution of about 150 km in a coronal active region, and the images are consistent with energy production sufficient for the observed heating. It is now apparent that there are at least two heating mechanisms in the Sun’s outer atmosphere, or corona1,2,3,4,5. Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000 K (refs 1, 2, 3). The active corona needs additional heating to reach 2,000,000–4,000,000 K; this heat has been theoretically proposed6,7,8,9,10,11,12 to come from the reconnection and unravelling of magnetic ‘braids’. Evidence favouring that process has been inferred13,14, but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought1,2,3,15,16,17 to have an angular width of about 0.2 arc seconds have not been resolved10,18,19,20. Fine-scale braiding has been seen21,22 in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000 K. Although our 5-minute observations cannot unambiguously identify the field reconnection and subsequent relaxation as the dominant heating mechanism throughout active regions, the energy available from the observed field relaxation in our example is ample for the observed heating.","datePublished":"2013-01-23T00:00:00Z","dateModified":"2013-01-23T00:00:00Z","pageStart":"501","pageEnd":"503","sameAs":"https://doi.org/10.1038/nature11772","keywords":["Space physics","Stars","Science","Humanities and Social Sciences","multidisciplinary"],"image":["https://media.springernature.com/lw1200/springer-static/image/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_Article_BFnature11772_Fig1_HTML.jpg","https://media.springernature.com/lw1200/springer-static/image/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_Article_BFnature11772_Fig2_HTML.jpg","https://media.springernature.com/lw1200/springer-static/image/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_Article_BFnature11772_Fig3_HTML.jpg","https://media.springernature.com/lw1200/springer-static/image/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_Article_BFnature11772_Fig4_HTML.jpg"],"isPartOf":{"name":"Nature","issn":["1476-4687","0028-0836"],"volumeNumber":"493","@type":["Periodical","PublicationVolume"]},"publisher":{"name":"Nature Publishing Group UK","logo":{"url":"https://www.springernature.com/app-sn/public/images/logo-springernature.png","@type":"ImageObject"},"@type":"Organization"},"author":[{"name":"J. 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DeForest","affiliation":[{"name":"Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA","address":{"name":"Instrumentation and Space Research Division, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA, ","@type":"PostalAddress"},"@type":"Organization"}],"@type":"Person"}],"isAccessibleForFree":false,"hasPart":{"isAccessibleForFree":false,"cssSelector":".main-content","@type":"WebPageElement"},"@type":"ScholarlyArticle"},"@context":"https://schema.org","@type":"WebPage"}</script> <link rel="canonical" href="https://www.nature.com/articles/nature11772"> <meta name="journal_id" content="41586"/> <meta name="dc.title" content="Energy release in the solar corona from spatially resolved magnetic braids"/> <meta name="dc.source" content="Nature 2013 493:7433"/> <meta name="dc.format" content="text/html"/> <meta name="dc.publisher" content="Nature Publishing Group"/> <meta name="dc.date" content="2013-01-23"/> <meta name="dc.type" content="OriginalPaper"/> <meta name="dc.language" content="En"/> <meta name="dc.copyright" content="2013 Springer Nature Limited"/> <meta name="dc.rights" content="2013 Springer Nature Limited"/> <meta name="dc.rightsAgent" content="journalpermissions@springernature.com"/> <meta name="dc.description" content="Solar observations at a resolution of 0.2 arc seconds show the reconnection and relaxation of magnetic braids in a coronal active region, leading to the dissipation of sufficient energy to heat the structures to about 4,000,000 K. The Sun's outer atmosphere, or corona, is millions of degrees hotter than its surface. The search for mechanisms capable of transferring energy from the Sun's interior to the periphery on such a scale has identified two strong candidates: wave heating is thought to heat the corona to 1.5 million K, and the reconnection and unravelling of magnetic braids has been proposed as the means of boosting the temperature towards 4 million K. New evidence to support that latter mechanism is provided by a five-minute series of images obtained by a high-resolution camera on-board a sounding rocket. The images reveal fine-scale braiding to a resolution of about 150 km in a coronal active region, and the images are consistent with energy production sufficient for the observed heating. It is now apparent that there are at least two heating mechanisms in the Sun’s outer atmosphere, or corona1,2,3,4,5. Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000 K (refs 1, 2, 3). The active corona needs additional heating to reach 2,000,000–4,000,000 K; this heat has been theoretically proposed6,7,8,9,10,11,12 to come from the reconnection and unravelling of magnetic ‘braids’. Evidence favouring that process has been inferred13,14, but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought1,2,3,15,16,17 to have an angular width of about 0.2 arc seconds have not been resolved10,18,19,20. Fine-scale braiding has been seen21,22 in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000 K. Although our 5-minute observations cannot unambiguously identify the field reconnection and subsequent relaxation as the dominant heating mechanism throughout active regions, the energy available from the observed field relaxation in our example is ample for the observed heating."/> <meta name="prism.issn" content="1476-4687"/> <meta name="prism.publicationName" content="Nature"/> <meta name="prism.publicationDate" content="2013-01-23"/> <meta name="prism.volume" content="493"/> <meta name="prism.number" content="7433"/> <meta name="prism.section" content="OriginalPaper"/> <meta name="prism.startingPage" content="501"/> <meta name="prism.endingPage" content="503"/> <meta name="prism.copyright" content="2013 Springer Nature Limited"/> <meta name="prism.rightsAgent" content="journalpermissions@springernature.com"/> <meta name="prism.url" content="https://www.nature.com/articles/nature11772"/> <meta name="prism.doi" content="doi:10.1038/nature11772"/> <meta name="citation_pdf_url" content="https://www.nature.com/articles/nature11772.pdf"/> <meta name="citation_fulltext_html_url" content="https://www.nature.com/articles/nature11772"/> <meta name="citation_journal_title" content="Nature"/> <meta name="citation_journal_abbrev" content="Nature"/> <meta name="citation_publisher" content="Nature Publishing Group"/> <meta name="citation_issn" content="1476-4687"/> <meta name="citation_title" content="Energy release in the solar corona from spatially resolved magnetic braids"/> <meta name="citation_volume" content="493"/> <meta name="citation_issue" content="7433"/> <meta name="citation_publication_date" content="2013/01"/> <meta name="citation_online_date" content="2013/01/23"/> <meta name="citation_firstpage" content="501"/> <meta name="citation_lastpage" content="503"/> <meta name="citation_article_type" content="Article"/> <meta name="citation_language" content="en"/> <meta name="dc.identifier" content="doi:10.1038/nature11772"/> <meta name="DOI" content="10.1038/nature11772"/> <meta name="size" content="72191"/> <meta name="citation_doi" content="10.1038/nature11772"/> <meta name="citation_springer_api_url" content="http://api.springer.com/xmldata/jats?q=doi:10.1038/nature11772&api_key="/> <meta name="description" content="Solar observations at a resolution of 0.2 arc seconds show the reconnection and relaxation of magnetic braids in a coronal active region, leading to the dissipation of sufficient energy to heat the structures to about 4,000,000 K. 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Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000 K (refs 1, 2, 3). The active corona needs additional heating to reach 2,000,000–4,000,000 K; this heat has been theoretically proposed6,7,8,9,10,11,12 to come from the reconnection and unravelling of magnetic ‘braids’. Evidence favouring that process has been inferred13,14, but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought1,2,3,15,16,17 to have an angular width of about 0.2 arc seconds have not been resolved10,18,19,20. Fine-scale braiding has been seen21,22 in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000 K. 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data-test="article-identifier"> <li class="c-article-identifiers__item" data-test="article-category">Letter</li> <li class="c-article-identifiers__item">Published: <time datetime="2013-01-23">23 January 2013</time></li> </ul> <h1 class="c-article-title" data-test="article-title" data-article-title="">Energy release in the solar corona from spatially resolved magnetic braids</h1> <ul class="c-article-author-list c-article-author-list--short" data-test="authors-list" data-component-authors-activator="authors-list"><li class="c-article-author-list__item"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-J__W_-Cirtain-Aff1" data-author-popup="auth-J__W_-Cirtain-Aff1" data-author-search="Cirtain, J. W." data-corresp-id="c1">J. W. Cirtain<svg width="16" height="16" focusable="false" role="img" aria-hidden="true" class="u-icon"><use xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="#icon-eds-i-mail-medium"></use></svg></a><sup class="u-js-hide"><a href="#Aff1">1</a></sup>, </li><li class="c-article-author-list__item"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-L_-Golub-Aff2" data-author-popup="auth-L_-Golub-Aff2" data-author-search="Golub, L.">L. Golub</a><sup class="u-js-hide"><a href="#Aff2">2</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-A__R_-Winebarger-Aff1" data-author-popup="auth-A__R_-Winebarger-Aff1" data-author-search="Winebarger, A. R.">A. R. Winebarger</a><sup class="u-js-hide"><a href="#Aff1">1</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-B_-De_Pontieu-Aff3" data-author-popup="auth-B_-De_Pontieu-Aff3" data-author-search="De Pontieu, B.">B. De Pontieu</a><sup class="u-js-hide"><a href="#Aff3">3</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-K_-Kobayashi-Aff4" data-author-popup="auth-K_-Kobayashi-Aff4" data-author-search="Kobayashi, K.">K. Kobayashi</a><sup class="u-js-hide"><a href="#Aff4">4</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-R__L_-Moore-Aff1" data-author-popup="auth-R__L_-Moore-Aff1" data-author-search="Moore, R. L.">R. L. Moore</a><sup class="u-js-hide"><a href="#Aff1">1</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-R__W_-Walsh-Aff5" data-author-popup="auth-R__W_-Walsh-Aff5" data-author-search="Walsh, R. W.">R. W. Walsh</a><sup class="u-js-hide"><a href="#Aff5">5</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-K__E_-Korreck-Aff2" data-author-popup="auth-K__E_-Korreck-Aff2" data-author-search="Korreck, K. E.">K. E. Korreck</a><sup class="u-js-hide"><a href="#Aff2">2</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-M_-Weber-Aff2" data-author-popup="auth-M_-Weber-Aff2" data-author-search="Weber, M.">M. Weber</a><sup class="u-js-hide"><a href="#Aff2">2</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-P_-McCauley-Aff2" data-author-popup="auth-P_-McCauley-Aff2" data-author-search="McCauley, P.">P. McCauley</a><sup class="u-js-hide"><a href="#Aff2">2</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-A_-Title-Aff3" data-author-popup="auth-A_-Title-Aff3" data-author-search="Title, A.">A. Title</a><sup class="u-js-hide"><a href="#Aff3">3</a></sup>, </li><li class="c-article-author-list__item c-article-author-list__item--hide-small-screen"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-S_-Kuzin-Aff6" data-author-popup="auth-S_-Kuzin-Aff6" data-author-search="Kuzin, S.">S. Kuzin</a><sup class="u-js-hide"><a href="#Aff6">6</a></sup> & </li><li class="c-article-author-list__show-more" aria-label="Show all 13 authors for this article" title="Show all 13 authors for this article">…</li><li class="c-article-author-list__item"><a data-test="author-name" data-track="click" data-track-action="open author" data-track-label="link" href="#auth-C__E_-DeForest-Aff7" data-author-popup="auth-C__E_-DeForest-Aff7" data-author-search="DeForest, C. E.">C. E. 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Magnetic tornadoes as energy channels into the solar corona. Nature 486, 505–508 (2012)" href="/articles/nature11772#ref-CR1" id="ref-link-section-d259248322e503">1</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 2" title="McIntosh, S. et al. Alfvenic waves with sufficient energy to power the quiet solar corona and fast solar wind. Nature 475, 477–480 (2011)" href="/articles/nature11772#ref-CR2" id="ref-link-section-d259248322e506">2</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 3" title="De Pontieu, B. et al. Chromospheric Alfevic waves strong enough to power the solar wind. Science 318, 1574–1577 (2007)" href="/articles/nature11772#ref-CR3" id="ref-link-section-d259248322e509">3</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 4" title="Cirtain, J. et al. Evidence for Alfven waves in solar X-ray jets. Science 318, 1580–1582 (2007)" href="/articles/nature11772#ref-CR4" id="ref-link-section-d259248322e512">4</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 5" title="Priest, E. et al. Nature of the heating mechanism for the diffuse solar corona. Nature 393, 545–547 (1998)" href="/articles/nature11772#ref-CR5" id="ref-link-section-d259248322e515">5</a></sup>. Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000 K (refs <a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 1" title="Wedemeyer-Böhm, S. et al. Magnetic tornadoes as energy channels into the solar corona. Nature 486, 505–508 (2012)" href="/articles/nature11772#ref-CR1" id="ref-link-section-d259248322e518">1</a>, <a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 2" title="McIntosh, S. et al. Alfvenic waves with sufficient energy to power the quiet solar corona and fast solar wind. Nature 475, 477–480 (2011)" href="/articles/nature11772#ref-CR2" id="ref-link-section-d259248322e521">2</a>, <a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 3" title="De Pontieu, B. et al. Chromospheric Alfevic waves strong enough to power the solar wind. Science 318, 1574–1577 (2007)" href="/articles/nature11772#ref-CR3" id="ref-link-section-d259248322e524">3</a>). The active corona needs additional heating to reach 2,000,000–4,000,000 K; this heat has been theoretically proposed<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 6" title="Parker, E. Magnetic neutral sheets in evolving fields. I. General Theory. Astrophys. J. 264, 635–641 (1983)" href="/articles/nature11772#ref-CR6" id="ref-link-section-d259248322e528">6</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 7" title="Parker, E. Magnetic neutral sheets in evolving fields. II. Formation of the solar corona. Astrophys. J. 264, 642–647 (1983)" href="/articles/nature11772#ref-CR7" id="ref-link-section-d259248322e531">7</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 8" title="Schrijver, K. Braiding-induced interchange reconnection of the magnetic field and the width of solar coronal loops. Astrophys. J. 662, L119–L122 (2007)" href="/articles/nature11772#ref-CR8" id="ref-link-section-d259248322e534">8</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 9" title="Gudiksen, B. V. & Nordlund, Å. An ab initio approach to the solar coronal heating problem. Astrophys. J. 618, 1020–1030 (2005)" href="/articles/nature11772#ref-CR9" id="ref-link-section-d259248322e537">9</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 10" title="Klimchuk, J. On solving the coronal heating problem. Sol. Phys. 234, 41–77 (2006)" href="/articles/nature11772#ref-CR10" id="ref-link-section-d259248322e540">10</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 11" title="Gold, T. in Stellar and Solar Magnetic Fields (ed. Lüst, R. ) 390–398 (Proc. IAU Symp. 22, International Astronomical Union, 1965)" href="/articles/nature11772#ref-CR11" id="ref-link-section-d259248322e543">11</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 12" title="Warren, H. P., Winebarger, A. R. & Hamilton, P. S. Hydrodynamic modeling of active region loops. Astrophys. J. 579, L41–L44 (2002)" href="/articles/nature11772#ref-CR12" id="ref-link-section-d259248322e547">12</a></sup> to come from the reconnection and unravelling of magnetic ‘braids’. Evidence favouring that process has been inferred<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 13" title="Schrijver, K. et al. Large-scale coronal heating by the small-scale magnetic field of the Sun. Nature 394, 152–154 (1998)" href="/articles/nature11772#ref-CR13" id="ref-link-section-d259248322e552">13</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 14" title="Lee, J. et al. Coronal currents, magnetic fields, and heating in a solar active region. Astrophys. J. 501, 853–865 (1998)" href="/articles/nature11772#ref-CR14" id="ref-link-section-d259248322e555">14</a></sup>, but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 1" title="Wedemeyer-Böhm, S. et al. Magnetic tornadoes as energy channels into the solar corona. Nature 486, 505–508 (2012)" href="/articles/nature11772#ref-CR1" id="ref-link-section-d259248322e559">1</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 2" title="McIntosh, S. et al. Alfvenic waves with sufficient energy to power the quiet solar corona and fast solar wind. Nature 475, 477–480 (2011)" href="/articles/nature11772#ref-CR2" id="ref-link-section-d259248322e562">2</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 3" title="De Pontieu, B. et al. Chromospheric Alfevic waves strong enough to power the solar wind. Science 318, 1574–1577 (2007)" href="/articles/nature11772#ref-CR3" id="ref-link-section-d259248322e565">3</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 15" title="De Pontieu, B. et al. Observing solar coronal heating-in the chromosphere. Astrophys. J. 701, L1–L6 (2009)" href="/articles/nature11772#ref-CR15" id="ref-link-section-d259248322e568">15</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 16" title="De Pontieu, B. et al. The origins of hot plasma in the solar corona. Science 331, 55–58 (2011)" href="/articles/nature11772#ref-CR16" id="ref-link-section-d259248322e571">16</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 17" title="DeForest, C. E. On the size of structures in the corona. Astrophys. J. 661, 532–542 (2007)" href="/articles/nature11772#ref-CR17" id="ref-link-section-d259248322e574">17</a></sup> to have an angular width of about 0.2 arc seconds have not been resolved<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 10" title="Klimchuk, J. On solving the coronal heating problem. Sol. Phys. 234, 41–77 (2006)" href="/articles/nature11772#ref-CR10" id="ref-link-section-d259248322e578">10</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 18" title="Berger, M. &. Asgari-Targhi, M. Self-organized braiding and the structure of coronal loops. Astrophys. J. 705, 347–355 (2009)" href="/articles/nature11772#ref-CR18" id="ref-link-section-d259248322e581">18</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 19" title="van Ballegooijen, A. Heating of the solar chromosphere and corona by Alfven wave turbulence. Astrophys. J. 736, 3–9 (2011)" href="/articles/nature11772#ref-CR19" id="ref-link-section-d259248322e584">19</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 20" title="Malanushenko, A., Yusuf, M. H. & Longcope, D. Direct measurements of magnetic twist in the solar corona. Astrophys. J. 736, 97–109 (2011)" href="/articles/nature11772#ref-CR20" id="ref-link-section-d259248322e587">20</a></sup>. Fine-scale braiding has been seen<sup><a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 21" title="Rutten, R. Hα as chromospheric diagnostic. ASP Conf. Ser. 397, 54–58 (2008)" href="/articles/nature11772#ref-CR21" id="ref-link-section-d259248322e591">21</a>,<a data-track="click" data-track-action="reference anchor" data-track-label="link" data-test="citation-ref" aria-label="Reference 22" title="Martin, S. Conditions for the formation and maintenance of filaments. Sol. Phys. 182, 107–137 (1998)" href="/articles/nature11772#ref-CR22" id="ref-link-section-d259248322e594">22</a></sup> in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000 K. Although our 5-minute observations cannot unambiguously identify the field reconnection and subsequent relaxation as the dominant heating mechanism throughout active regions, the energy available from the observed field relaxation in our example is ample for the observed heating.</p></div></div></section> <noscript> <div class="c-nature-box c-nature-box--side " data-component="entitlement-box"> <div class="js-access-button"> <a href="https://wayf.springernature.com?redirect_uri=https%3A%2F%2Fwww.nature.com%2Farticles%2Fnature11772" class="c-article__button" data-test="ra21"> <svg class="u-icon" width="18" height="18" aria-hidden="true" focusable="false"><use href="#icon-institution"></use></svg> <span class="c-article__button-text">Access through your institution</span> </a> </div> <div class="js-buy-button"> <a href="#access-options" class="c-article__button c-article__button--inverted" data-test="ra21"> <span>Buy or subscribe</span> </a> </div> </div> </noscript> <div 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This LPI work was supported in part by the Russian Foundation for Basic Research (project 11–02–01079-a), Program No. 22 of the Presidium of the Russian Academy of Sciences.</p></div></div></section><section aria-labelledby="author-information" data-title="Author information"><div class="c-article-section" id="author-information-section"><h2 class="c-article-section__title js-section-title js-c-reading-companion-sections-item" id="author-information">Author information</h2><div class="c-article-section__content" id="author-information-content"><h3 class="c-article__sub-heading" id="affiliations">Authors and Affiliations</h3><ol class="c-article-author-affiliation__list"><li id="Aff1"><p class="c-article-author-affiliation__address">Marshall Space Flight Center, NASA, Mail Code ZP13, MSFC, Alabama 36812, USA, </p><p class="c-article-author-affiliation__authors-list">J. W. Cirtain, A. R. Winebarger & R. L. Moore</p></li><li id="Aff2"><p class="c-article-author-affiliation__address">Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, 01238, Massachusetts, USA</p><p class="c-article-author-affiliation__authors-list">L. Golub, K. E. Korreck, M. Weber & P. McCauley</p></li><li id="Aff3"><p class="c-article-author-affiliation__address">Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Palo Alto, 94304, California, USA</p><p class="c-article-author-affiliation__authors-list">B. De Pontieu & A. Title</p></li><li id="Aff4"><p class="c-article-author-affiliation__address">Center for Space and Aeronautic Research, University of Alabama-Huntsville, 320 Sparkman Avenue, Huntsville, Alabama 35812, USA, </p><p class="c-article-author-affiliation__authors-list">K. Kobayashi</p></li><li id="Aff5"><p class="c-article-author-affiliation__address">University of Central Lancashire, Preston, Lancashire PR1 2HE, UK, </p><p class="c-article-author-affiliation__authors-list">R. W. Walsh</p></li><li id="Aff6"><p class="c-article-author-affiliation__address">Lebedev Physical Institute, 53 Leninski Prospekt, 119991 Moscow, Russia, </p><p class="c-article-author-affiliation__authors-list">S. Kuzin</p></li><li id="Aff7"><p class="c-article-author-affiliation__address">Instrumentation and Space Research Division, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA, </p><p class="c-article-author-affiliation__authors-list">C. E. DeForest</p></li></ol><div class="u-js-hide u-hide-print" data-test="author-info"><span class="c-article__sub-heading">Authors</span><ol class="c-article-authors-search u-list-reset"><li id="auth-J__W_-Cirtain-Aff1"><span class="c-article-authors-search__title u-h3 js-search-name">J. W. Cirtain</span><div class="c-article-authors-search__list"><div class="c-article-authors-search__item c-article-authors-search__list-item--left"><a href="/search?author=J.%20W.%20Cirtain" class="c-article-button" data-track="click" data-track-action="author link - publication" data-track-label="link" rel="nofollow">View author publications</a></div><div class="c-article-authors-search__item c-article-authors-search__list-item--right"><p class="search-in-title-js c-article-authors-search__text">You can also search for this author in <span class="c-article-identifiers"><a class="c-article-identifiers__item" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?cmd=search&term=J.%20W.%20Cirtain" data-track="click" data-track-action="author link - pubmed" data-track-label="link" rel="nofollow">PubMed</a><span class="u-hide"> </span><a class="c-article-identifiers__item" href="http://scholar.google.co.uk/scholar?as_q=&num=10&btnG=Search+Scholar&as_epq=&as_oq=&as_eq=&as_occt=any&as_sauthors=%22J.%20W.%20Cirtain%22&as_publication=&as_ylo=&as_yhi=&as_allsubj=all&hl=en" data-track="click" data-track-action="author link - scholar" data-track-label="link" rel="nofollow">Google Scholar</a></span></p></div></div></li><li id="auth-L_-Golub-Aff2"><span class="c-article-authors-search__title u-h3 js-search-name">L. 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E. DeForest</span><div class="c-article-authors-search__list"><div class="c-article-authors-search__item c-article-authors-search__list-item--left"><a href="/search?author=C.%20E.%20DeForest" class="c-article-button" data-track="click" data-track-action="author link - publication" data-track-label="link" rel="nofollow">View author publications</a></div><div class="c-article-authors-search__item c-article-authors-search__list-item--right"><p class="search-in-title-js c-article-authors-search__text">You can also search for this author in <span class="c-article-identifiers"><a class="c-article-identifiers__item" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?cmd=search&term=C.%20E.%20DeForest" data-track="click" data-track-action="author link - pubmed" data-track-label="link" rel="nofollow">PubMed</a><span class="u-hide"> </span><a class="c-article-identifiers__item" href="http://scholar.google.co.uk/scholar?as_q=&num=10&btnG=Search+Scholar&as_epq=&as_oq=&as_eq=&as_occt=any&as_sauthors=%22C.%20E.%20DeForest%22&as_publication=&as_ylo=&as_yhi=&as_allsubj=all&hl=en" data-track="click" data-track-action="author link - scholar" data-track-label="link" rel="nofollow">Google Scholar</a></span></p></div></div></li></ol></div><h3 class="c-article__sub-heading" id="contributions">Contributions</h3><p>J.W.C., A.R.W., B.D.P., P.M. and C.E.D. performed image processing and analysis of observations. M.W., K.K., B.D.P., C.E.D. and A.R.W. all contributed to the calibration and alignment of the instrument and science data. J.W.C., L.G., K.K. and K.E.K. managed the design, construction and testing of the experiment. J.W.C. and A.R.W. determined velocities and J.W.C and R.L.M. calculated the stored energy. A.T., R.W.W. and S.K. contributed to the instrumentation.</p><h3 class="c-article__sub-heading" id="corresponding-author">Corresponding author</h3><p id="corresponding-author-list">Correspondence to <a id="corresp-c1" href="mailto:jonathan.w.cirtain@nasa.gov">J. W. Cirtain</a>.</p></div></div></section><section data-title="Ethics declarations"><div class="c-article-section" id="ethics-section"><h2 class="c-article-section__title js-section-title js-c-reading-companion-sections-item" id="ethics">Ethics declarations</h2><div class="c-article-section__content" id="ethics-content"> <h3 class="c-article__sub-heading">Competing interests</h3> <p>The authors declare no competing financial interests.</p> </div></div></section><section data-title="Supplementary information"><div class="c-article-section" id="Sec2-section"><h2 class="c-article-section__title js-section-title js-c-reading-companion-sections-item" id="Sec2">Supplementary information</h2><div class="c-article-section__content" id="Sec2-content"><div data-test="supplementary-info"><div id="figshareContainer" class="c-article-figshare-container" data-test="figshare-container"></div><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM70"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" data-track="click" data-track-action="view supplementary info" data-test="supp-info-link" data-track-label="supplementary info" href="https://static-content.springer.com/esm/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_BFnature11772_MOESM70_ESM.pdf" data-supp-info-image="">Supplementary Info</a></h3><div class="c-article-supplementary__description" data-component="thumbnail-container"><p>DESCRIPTION (PDF 2220 kb)</p></div></div><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM71"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" data-track="click" data-track-action="view supplementary info" data-test="supp-info-link" data-track-label="experiment regions of interest" href="https://static-content.springer.com/esm/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_BFnature11772_MOESM71_ESM.mov" data-supp-info-image="">Experiment regions of interest</a></h3><div class="c-article-supplementary__description" data-component="thumbnail-container"><p>This video shows the full sun AIA images taken during the Hi-C flight. It zooms into the Hi-C field of full field of view and extracts the two examples from the paper, and shows comparison movies for AIA and Hi-C. The first comparison is for example 1 shown in Fig 2 and Supplementary Fig. 2 and Supplementary Video 2. The second comparison is for example 2 and goes with Fig. 3 and Supplementary Videos 3 & 4. (MOV 4672 kb)</p></div></div><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM72"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" data-track="click" data-track-action="view supplementary info" data-test="supp-info-link" data-track-label="evolution of loops during component reconnection" href="https://static-content.springer.com/esm/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_BFnature11772_MOESM72_ESM.mov" data-supp-info-image="">Evolution of loops during component reconnection</a></h3><div class="c-article-supplementary__description" data-component="thumbnail-container"><p>This video presents the evolution of a set of loops that are interacting and wrapped together. As the structures evolve, reconnection allows the loops to relax into a less curved and thus more potential geometry. (MOV 4160 kb)</p></div></div><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM73"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" data-track="click" data-track-action="view supplementary info" data-test="supp-info-link" data-track-label="evolution in a braided loop ensemble" href="https://static-content.springer.com/esm/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_BFnature11772_MOESM73_ESM.mov" data-supp-info-image="">Evolution in a Braided Loop Ensemble</a></h3><div class="c-article-supplementary__description" data-component="thumbnail-container"><p>This braided loop has several loops near the 'base' that appear to be unwinding with significant apparent outflow. This is evidence of untwisting, and the braided structure also seeming to unwind with time. (MOV 5888 kb)</p></div></div><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM74"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" data-track="click" data-track-action="view supplementary info" data-test="supp-info-link" data-track-label="the temperature history of the braided structure" href="https://static-content.springer.com/esm/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_BFnature11772_MOESM74_ESM.mov" data-supp-info-image="">The Temperature history of the Braided Structure</a></h3><div class="c-article-supplementary__description" data-component="thumbnail-container"><p>Within the braided bundle, several episodic intensity increases are observed in many of the AIA passbands. This is direct evidence of impulsive energy release likely the result of reconnection. The process is observed many times in the AIA data over a long period of observations leading to the conclusion that the region is constantly being sheared, thus storing energy, and frequently releases some of this energy in these localized heating events. (MOV 1664 kb)</p></div></div></div></div></div></section><section data-title="PowerPoint slides"><div class="c-article-section" id="Sec3-section"><h2 class="c-article-section__title js-section-title js-c-reading-companion-sections-item" id="Sec3">PowerPoint slides</h2><div class="c-article-section__content" id="Sec3-content"><div data-test="supplementary-info"><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM66"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" data-track="click" data-track-action="view supplementary info" data-test="supp-info-link" data-track-label="powerpoint slide for fig. 1" href="https://static-content.springer.com/esm/art%3A10.1038%2Fnature11772/MediaObjects/41586_2013_BFnature11772_MOESM66_ESM.ppt" data-supp-info-image="">PowerPoint slide for Fig. 1</a></h3></div><div class="c-article-supplementary__item" data-test="supp-item" id="MOESM67"><h3 class="c-article-supplementary__title u-h3"><a class="print-link" 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Energy release in the solar corona from spatially resolved magnetic braids | Nature