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fa-facebook" title="Facebook"><span class="visuallyhidden">Facebook</span></a></li> <li><a href="/?feed=rss2" class="icon fa fa-rss" title="RSS"><span class="visuallyhidden">RSS</span></a></li> <li><a href="https://bsky.app/profile/aasnova.bsky.social" class="icon fa fa-bluesky" title="Bluesky"><span class="visuallyhidden">Bluesky</span></a></li> </ul></div> </nav> </div> </div> <div class="main wrap cf"> <div class="row"> <div class="col-8 main-content"> <article id="post-10534" class="post-10534 post type-post status-publish format-standard has-post-thumbnail category-features category-highlights tag-eclipses tag-magnetic-fields tag-plasma-physics tag-solar-corona title-above" itemscope itemtype="http://schema.org/Article"> <header class="post-header cf"> <div class="heading cf"> <h1 class="post-title item fn" itemprop="name"> A Simple New Way to Determine Magnetic Fields in the Solar Corona </h1>  </div> <div class="post-meta cf"> <span class="posted-by">By <span class="reviewer" itemprop="author"><a href="https://aasnova.org/person/kerry-hensley/" title="Kerry Hensley">Kerry Hensley</a></span> </span> <span class="posted-on">on <span class="dtreviewed"> <time class="value-title" datetime="2023-04-05T12:00:41-04:00" title="2023-04-05" itemprop="datePublished">5 April 2023</time> </span> </span> <span class="subcat">Features</span> <span class="cats"> <div class="post-share"> <span class="text">Share:</span> <span class="share-links">  <a href="https://twitter.com/intent/tweet?url=https%3A%2F%2Faasnova.org%2F2023%2F04%2F05%2Fa-simple-new-way-to-determine-magnetic-fields-in-the-solar-corona%2F" class="fa fa-twitter" title="Tweet It"> <span class="visuallyhidden">Twitter</span></a> <a href="http://www.facebook.com/sharer.php?u=https%3A%2F%2Faasnova.org%2F2023%2F04%2F05%2Fa-simple-new-way-to-determine-magnetic-fields-in-the-solar-corona%2F" class="fa fa-facebook" title="Share on Facebook"> <span class="visuallyhidden">Facebook</span></a> <a 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href="mailto:?subject=A%20Simple%20New%20Way%20to%20Determine%20Magnetic%20Fields%20in%20the%20Solar%20Corona&body=https%3A%2F%2Faasnova.org%2F2023%2F04%2F05%2Fa-simple-new-way-to-determine-magnetic-fields-in-the-solar-corona%2F" class="fa fa-envelope-o" title="Share via Email"> <span class="visuallyhidden">Email</span></a> </span> </div> </span> </div> <div class="featured"> <a href="https://aasnova.org/wp-content/uploads/2023/04/36329608000_2e0f627e4b_o.jpg" title="A Simple New Way to Determine Magnetic Fields in the Solar Corona" itemprop="image"> <img width="702" height="336" src="https://aasnova.org/wp-content/uploads/2023/04/36329608000_2e0f627e4b_o-702x336.jpg" class="attachment-main-slider size-main-slider wp-post-image" alt="a photograph of a total solar eclipse with the solar corona showing" title="A Simple New Way to Determine Magnetic Fields in the Solar Corona" decoding="async" fetchpriority="high" srcset="https://aasnova.org/wp-content/uploads/2023/04/36329608000_2e0f627e4b_o-702x336.jpg 702w, https://aasnova.org/wp-content/uploads/2023/04/36329608000_2e0f627e4b_o-1078x516.jpg 1078w" sizes="(max-width: 702px) 100vw, 702px" /> </a> <div class="caption">The solar corona peeks out from behind the Moon's disk during a total solar eclipse in August 2017. [<a href="https://www.nasa.gov/image-feature/suns-corona-seen-during-the-2017-solar-eclipse">NASA/Carla Thomas</a>]</div> </div> </header> <div class="post-container cf"> <div class="post-content-right"> <div class="post-content description " itemprop="articleBody"> <p>A recent research article describes a new way to measure the magnetic field of the Sun’s tenuous upper atmosphere, or corona, from images taken during total solar eclipses.</p> <h4>Illuminating the Solar Corona</h4> <div id="attachment_9671" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full.jpg" data-rel="lightbox-image-0" data-rl_title="An illustration of the regions of the Sun's atmosphere and interior. Click to enlarge. [NASA/Goddard]" data-rl_caption="An illustration of the regions of the Sun's atmosphere and interior. Click to enlarge. [NASA/Goddard]" title="An illustration of the regions of the Sun's atmosphere and interior. Click to enlarge. [NASA/Goddard]"><img decoding="async" aria-describedby="caption-attachment-9671" class="size-thumbnail wp-image-9671" src="https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-260x195.jpg" alt="An illustration of the regions of the Sun's atmosphere and interior." width="260" height="195" srcset="https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-260x195.jpg 260w, https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-702x527.jpg 702w, https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-768x576.jpg 768w, https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-600x450.jpg 600w, https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-1536x1152.jpg 1536w, https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full-1320x990.jpg 1320w, https://aasnova.org/wp-content/uploads/2022/07/462977main_sun_layers_full.jpg 1680w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-9671" class="wp-caption-text">An illustration of the regions of the Sun’s atmosphere and interior. Click to enlarge. [<a href="https://www.nasa.gov/mission_pages/sunearth/science/Sunlayers.html">NASA/Goddard</a>]</p></div>The outermost layer of the Sun’s atmosphere is normally hidden from view, but a total solar eclipse reveals ghostly tendrils flowing out from the Sun: the corona. The solar corona is exceptionally hot, sparse, and dynamic, and it’s the source of a variety of exciting space weather phenomena. It’s this last point that makes understanding the properties of the corona important, especially the strength and direction of its magnetic field.</p> <p>Because direct measurements of the coronal magnetic field are hard to come by — the only spacecraft yet designed to travel into the harsh coronal environment, the Parker Solar Probe, has barely dipped a toe into the region — researchers must use complex models to reproduce measurements made from a distance to understand this important region of the Sun.</p> <div id="attachment_10561" style="width: 270px" class="wp-caption alignleft"><a href="https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr.jpg" data-rel="lightbox-image-1" data-rl_title="A projection of the magnetic field strength derived using the total solar eclipse (TSE) method and the magnetohydrodynamic (MHD) modeling method. Click to enlarge. [Bemporad 2023]" data-rl_caption="A projection of the magnetic field strength derived using the total solar eclipse (TSE) method and the magnetohydrodynamic (MHD) modeling method. Click to enlarge. [Bemporad 2023]" title="A projection of the magnetic field strength derived using the total solar eclipse (TSE) method and the magnetohydrodynamic (MHD) modeling method. Click to enlarge. [Bemporad 2023]"><img decoding="async" aria-describedby="caption-attachment-10561" class="size-thumbnail wp-image-10561" src="https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr-260x173.jpg" alt="comparison of output from the two methods" width="260" height="173" srcset="https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr-260x173.jpg 260w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr-702x468.jpg 702w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr-768x512.jpg 768w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr-600x400.jpg 600w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f8_hr.jpg 1250w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-10561" class="wp-caption-text">A projection of the magnetic field strength derived using the total solar eclipse (TSE) method and the magnetohydrodynamic (MHD) modeling method. Click to enlarge. [Bemporad 2023]</p></div> <h4>A Simpler Solution?</h4> <p>Alessandro Bemporad (National Institute for Astrophysics, Italy; Purple Mountain Observatory) explored a simpler way. Bemporad’s analysis method starts with polarized-light images of the corona from the 21 August 2017 total solar eclipse. The author first used an established technique to calibrate the images and convert the brightness of each pixel to an important physical quantity: how densely packed or rarefied the plasma is within the corona.</p> <p>To convert from plasma density to magnetic field strength, Bemporad made a bit of a leap. In many physical systems, energy is distributed fairly equally among different types — like thermal, kinetic, magnetic, or potential energy. For a system like the solar corona, the dominant forms of energy are magnetic and gravitational potential. By making the assumption that these forms of energy are balanced, Bemporad estimated the magnetic field strength without needing complex modeling.</p> <h4>Looking Forward, Looking Back</h4> <div id="attachment_10562" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr.jpg" data-rel="lightbox-image-2" data-rl_title="Left: Relative difference between the magnetic field strength derived using the total solar eclipse method and the fluid modeling. Right: Cumulative distribution of relative differences between pixel values. Click to enlarge. [Bemporad 2023]" data-rl_caption="Left: Relative difference between the magnetic field strength derived using the total solar eclipse method and the fluid modeling. Right: Cumulative distribution of relative differences between pixel values. Click to enlarge. [Bemporad 2023]" title="Left: Relative difference between the magnetic field strength derived using the total solar eclipse method and the fluid modeling. Right: Cumulative distribution of relative differences between pixel values. Click to enlarge. [Bemporad 2023]"><img loading="lazy" decoding="async" aria-describedby="caption-attachment-10562" class="size-thumbnail wp-image-10562" src="https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr-260x111.jpg" alt="comparison of output from the new method and the more complex fluid dynamics modeling" width="260" height="111" srcset="https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr-260x111.jpg 260w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr-702x300.jpg 702w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr-768x329.jpg 768w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr-600x257.jpg 600w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr-1320x565.jpg 1320w, https://aasnova.org/wp-content/uploads/2023/04/apjacb8b8f11_hr.jpg 1500w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-10562" class="wp-caption-text">Left: Relative difference between the magnetic field strength derived using the total solar eclipse method and the fluid modeling. Right: Cumulative distribution of relative differences between pixel values. Click to enlarge. [Bemporad 2023]</p></div>To test the validity of the new method, Bemporad compared his results against those from fluid dynamics models. In general, the output from the two methods differed by less than 50%. Given that the results from the more complicated fluid models aren’t ground truth, Bemporad considers these discrepancies small.</p> <p>Bemporad notes that the new method can be applied to any white-light images of the solar corona, not just those taken during total solar eclipses. This means that any ground- or space-based images made using a coronagraph (an instrument that blocks the light from the Sun’s bright disk so that the fainter corona can be photographed) are ripe for further exploration, including images taken decades ago — opening a new window into the magnetic conditions of past solar cycles.</p> <h4>Citation</h4> <p>“Coronal Magnetic Fields Derived with Images Acquired during the 2017 August 21 Total Solar Eclipse,” A. Bemporad 2023 <em>ApJ</em> <b>946</b> 14. <a href="https://doi.org/10.3847/1538-4357/acb8b8">doi:10.3847/1538-4357/acb8b8</a></p> <div class="tagcloud"><a href="https://aasnova.org/tag/eclipses/" rel="tag">eclipses</a> <a href="https://aasnova.org/tag/magnetic-fields/" rel="tag">magnetic fields</a> <a href="https://aasnova.org/tag/plasma-physics/" rel="tag">plasma physics</a> <a href="https://aasnova.org/tag/solar-corona/" rel="tag">solar corona</a></div> </div> </div> </div> </article> <div class="comments"> <div id="comments"> <p class="nocomments"></p> </div> </div> </div> <aside class="col-4 sidebar"> <ul> <li id="bunyad-related-posts-widget-2" class="widget related-posts"> <h3 class="widgettitle">RELATED HIGHLIGHTS</h3> <ul class="posts-list"> <li> <a href="https://aasnova.org/2024/07/24/tailor-made-turbulence-for-all-your-modeling-needs/"><img width="110" height="96" src="https://aasnova.org/wp-content/uploads/2024/07/hubble_ngc2024_flame1_wfc3_ir_display-jpg-110x96.webp" 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