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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-12464" class="post-12464 post type-post status-publish format-standard has-post-thumbnail category-features category-highlights tag-magnetic-fields tag-magnetohydrodynamics tag-plasma-physics tag-simulations 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"> Tailor-Made Turbulence for All Your Modeling Needs </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="2024-07-24T12:00:49-04:00" title="2024-07-24" itemprop="datePublished">24 July 2024</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%2F2024%2F07%2F24%2Ftailor-made-turbulence-for-all-your-modeling-needs%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%2F2024%2F07%2F24%2Ftailor-made-turbulence-for-all-your-modeling-needs%2F" class="fa fa-facebook" title="Share on Facebook"> <span class="visuallyhidden">Facebook</span></a> <a href="http://www.linkedin.com/shareArticle?mini=true&url=https%3A%2F%2Faasnova.org%2F2024%2F07%2F24%2Ftailor-made-turbulence-for-all-your-modeling-needs%2F" class="fa fa-linkedin" title="Share on LinkedIn"> <span class="visuallyhidden">LinkedIn</span></a> <a href="https://plus.google.com/share?url=https%3A%2F%2Faasnova.org%2F2024%2F07%2F24%2Ftailor-made-turbulence-for-all-your-modeling-needs%2F" class="fa fa-google-plus" title="Share on Google+"> <span class="visuallyhidden">Google+</span></a> <a href="http://reddit.com/submit?url=https%3A%2F%2Faasnova.org%2F2024%2F07%2F24%2Ftailor-made-turbulence-for-all-your-modeling-needs%2F" class="fa fa-reddit" title="Share on Reddit"> <span class="visuallyhidden">Reddit</span></a> <a href="mailto:?subject=Tailor-Made%20Turbulence%20for%20All%20Your%20Modeling%20Needs&body=https%3A%2F%2Faasnova.org%2F2024%2F07%2F24%2Ftailor-made-turbulence-for-all-your-modeling-needs%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/2024/07/hubble_ngc2024_flame1_wfc3_ir_display-jpg.webp" title="Tailor-Made Turbulence for All Your Modeling Needs" itemprop="image"> <img width="702" height="336" src="https://aasnova.org/wp-content/uploads/2024/07/hubble_ngc2024_flame1_wfc3_ir_display-jpg-702x336.webp" class="attachment-main-slider size-main-slider wp-post-image" alt="Hubble image of the Flame Nebula" title="Tailor-Made Turbulence for All Your Modeling Needs" decoding="async" fetchpriority="high" srcset="https://aasnova.org/wp-content/uploads/2024/07/hubble_ngc2024_flame1_wfc3_ir_display-jpg-702x336.webp 702w, https://aasnova.org/wp-content/uploads/2024/07/hubble_ngc2024_flame1_wfc3_ir_display-jpg-1078x516.webp 1078w" sizes="(max-width: 702px) 100vw, 702px" /> </a> <div class="caption">The Flame Nebula, NGC 2024, is a star-forming region that's part of the Orion Molecular Cloud Complex. Turbulence is a common feature of molecular clouds. [<a href="https://science.nasa.gov/missions/hubble/hubble-spots-swirls-of-dust-in-the-flame-nebula/">NASA, ESA, and N. Da Rio (University of Virginia); Processing: Gladys Kober (NASA/Catholic University of America)</a>]</div> </div> </header> <div class="post-container cf"> <div class="post-content-right"> <div class="post-content description " itemprop="articleBody"> <div id="attachment_12487" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-scaled.jpg" data-rel="lightbox-image-0" data-rl_title="Visualization of the plume from a candle transitioning from a smooth flow near the wick to a turbulent flow higher up. [Gary Settles; CC BY-SA 3.0]" data-rl_caption="Visualization of the plume from a candle transitioning from a smooth flow near the wick to a turbulent flow higher up. [Gary Settles; CC BY-SA 3.0]" title="Visualization of the plume from a candle transitioning from a smooth flow near the wick to a turbulent flow higher up. [Gary Settles; CC BY-SA 3.0]"><img decoding="async" aria-describedby="caption-attachment-12487" class="size-thumbnail wp-image-12487" src="https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-260x335.jpg" alt="visualization of a turbulent flow" width="260" height="335" srcset="https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-260x335.jpg 260w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-702x905.jpg 702w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-768x990.jpg 768w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-600x773.jpg 600w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-1192x1536.jpg 1192w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-1589x2048.jpg 1589w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-1320x1701.jpg 1320w, https://aasnova.org/wp-content/uploads/2024/07/Laminar-turbulent_transition-scaled.jpg 1987w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12487" class="wp-caption-text">Visualization of the plume from a candle transitioning from a smooth flow near the wick to a turbulent flow higher up. [<a href="https://commons.wikimedia.org/wiki/File:Laminar-turbulent_transition.jpg#file">Gary Settles</a>; <a href="https://creativecommons.org/licenses/by-sa/3.0">CC BY-SA 3.0</a>]</p></div>Turbulence — the culprit behind bumpy airplane rides, breaking waves, and billowing clouds — happens throughout the universe. Modeling realistic turbulent plasmas is difficult and computationally expensive, but new methods make simulating turbulence easier, faster, and more flexible than ever before.</p> <h4>A Chaotic Challenge</h4> <p>In the accretion disks around supermassive black holes, the clouds of molecular gas where stars are born, and even the atmosphere of the Sun, turbulence plays an important role in transferring energy and mixing plasmas. Because turbulent plasmas are so common, researchers across astronomical fields must wrestle with the challenge of modeling these chaotic systems.</p> <p>The traditional way to model a turbulent system is to do so numerically: churning through sets of equations to track the behavior of a plasma across tiny time increments. But as models become more complex, this comes at a higher computational cost, requiring an increasingly large number of hours for computers to handle the math.</p> <div id="attachment_12485" style="width: 270px" class="wp-caption alignleft"><a href="https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr.jpg" data-rel="lightbox-image-1" data-rl_title="A representation of a typical three-dimensional turbulent magnetic field generated by BxC. [Adapted from Maci et al. 2024]" data-rl_caption="A representation of a typical three-dimensional turbulent magnetic field generated by BxC. [Adapted from Maci et al. 2024]" title="A representation of a typical three-dimensional turbulent magnetic field generated by BxC. [Adapted from Maci et al. 2024]"><img decoding="async" aria-describedby="caption-attachment-12485" class="size-thumbnail wp-image-12485" src="https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr-260x291.jpg" alt="representation of a simulated three-dimensional turbulent magnetic field" width="260" height="291" srcset="https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr-260x291.jpg 260w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr-702x786.jpg 702w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr-768x860.jpg 768w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr-600x672.jpg 600w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff1_hr.jpg 870w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12485" class="wp-caption-text">A representation of a typical three-dimensional turbulent magnetic field generated by BxC. [Adapted from Maci et al. 2024]</p></div> <h4>Synthetic Magnetic Fields</h4> <p><em>Synthetic models</em> that use relatively simple algorithms to generate realistic plasmas provide an alternative. Recently, Daniela Maci (KU Leuven) and collaborators introduced a new synthetic model of turbulent magnetic fields. The team’s model builds on an existing synthetic model called BxC, a Python-based code that speedily produces three-dimensional turbulent magnetic fields.</p> <p>To generate realistic turbulence, BxC starts with a random field of vectors based on white noise. From there, this vector field is tweaked and transformed to adjust its statistical properties. In practice, this means that not only do BxC’s synthetic fields <em>look</em> turbulent, they also reproduce the expected statistical properties of a turbulent field, setting BxC apart from other models. This makes BxC an excellent jumping-off platform for creating realistic turbulent magnetic fields, and Maci’s team showed how the statistical properties of the modeled field depend on the model’s inputs.<strong><br /> </strong></p> <h4>Paths Forward</h4> <div id="attachment_12486" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr.jpg" data-rel="lightbox-image-2" data-rl_title="Examples of simulated turbulence that develops on top of a background magnetic field. Click to enlarge. [Adapted from Maci et al. 2024]" data-rl_caption="Examples of simulated turbulence that develops on top of a background magnetic field. Click to enlarge. [Adapted from Maci et al. 2024]" title="Examples of simulated turbulence that develops on top of a background magnetic field. Click to enlarge. [Adapted from Maci et al. 2024]"><img loading="lazy" decoding="async" aria-describedby="caption-attachment-12486" class="size-thumbnail wp-image-12486" src="https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr-260x254.jpg" alt="simulation results showing turbulence that develops on top of a background magnetic field" width="260" height="254" srcset="https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr-260x254.jpg 260w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr-702x685.jpg 702w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr-768x749.jpg 768w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr-600x585.jpg 600w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr-1320x1288.jpg 1320w, https://aasnova.org/wp-content/uploads/2024/07/apjsad4bdff11_hr.jpg 1479w" sizes="auto, (max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12486" class="wp-caption-text">Examples of simulated turbulence that develops on top of a background magnetic field. Click to enlarge. [Adapted from Maci et al. 2024]</p></div>To make the synthetic fields more applicable to astrophysical plasmas, Maci’s team expanded upon the original code in a couple of key ways. First, they recognized that turbulence often develops on top of a background magnetic field, and they developed a way for turbulence to be applied while maintaining the underlying structure of the field. This applies to magnetic field structures like loops or flux tubes, both of which are seen in the atmosphere of the Sun. Second, they developed a way to incorporate anisotropy, or a difference in the strength of the turbulence with regard to direction.</p> <p>This work demonstrates the power and flexibility of synthetic models for representing turbulent magnetic fields — and all of these features are available orders of magnitude faster than they would be from a traditional numerical model. The team anticipates making future additions to their model, all of which would give the user more customization options and make the model applicable to more astrophysical scenarios.</p> <h4>Citation</h4> <p>“BxC Toolkit: Generating Tailored Turbulent 3D Magnetic Fields,” Daniela Maci et al 2024 <em>ApJS</em> <b>273</b> 11. <a href="https://doi.org/10.3847/1538-4365/ad4bdf">doi:10.3847/1538-4365/ad4bdf</a></p> <div class="tagcloud"><a href="https://aasnova.org/tag/magnetic-fields/" rel="tag">magnetic fields</a> <a href="https://aasnova.org/tag/magnetohydrodynamics/" rel="tag">magnetohydrodynamics</a> <a href="https://aasnova.org/tag/plasma-physics/" rel="tag">plasma physics</a> <a href="https://aasnova.org/tag/simulations/" rel="tag">simulations</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 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