Research Highlights | High Altitude Observatory

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data-drupal-messages-fallback class="hidden"></div><div id="block-pagetitle" class="block block-core block-page-title-block"> <h2 class="mb-md-2">Research Highlights</h2> <h1 class="page-title">Research Highlights</h1> </div> <div id="block-unity-main-page-content" class="block block-system block-system-main-block"> <div class="views-element-container"><div class="col-12 component view view-article-view view-id-article_view view-display-id-page_2 js-view-dom-id-1f7054d91fcb287fd6b6aa02f4eeac8838168bdde035aa0b5fef10583cfc4f87"> <div class="view-header"> <p>A selection of highlights culled from publications by HAO staff.</p> </div> <div class="view-content"> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/spectra-solar-shallow-water-waves-bright-point-observations" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-11/Raphaldini_Hov30.png?itok=v3-jvkev" width="480" height="240" alt="Hovmoller (time × longitude) diagram at 30◦ latitudes" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/spectra-solar-shallow-water-waves-bright-point-observations" hreflang="en">Spectra of solar shallow-water waves from bright point observations</a></h3> <div class="card-date"><time datetime="2024-11-05T12:00:00Z" class="datetime">Nov 5, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>Breno Raphaldini</strong>, <strong>Mausumi Dikpati</strong>, Scott W. McIntosh, and Andre S. W. Teruya, utilize 3 years of global, synchronous observations of coronal bright point densities to obtain empirical signatures of dispersion relations that can be attributed to the simulated waves in tachocline. By tracking the bright point densities at selected latitudes, they compute their wave-number X frequency spectra. </p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/data-driven-mhd-simulation-2011-02-15-coronal-mass-ejection-active" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-05/Fan_MHD%20simulation%20coronal%20mass%20ejection%20%28CME%29.png?itok=cLFpYdXL" width="346" height="480" alt="MHD simulation of the 2011-02-15 coronal mass ejection (CME)" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/data-driven-mhd-simulation-2011-02-15-coronal-mass-ejection-active" hreflang="en">A data-driven MHD simulation of the 2011-02-15 coronal mass ejection from Active Region NOAA 11158</a></h3> <div class="card-date"><time datetime="2024-10-01T12:00:00Z" class="datetime">Oct 1, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>Yuhong Fan</strong>, Maria Kazachenko, Andrei Afanasev, and George Fisher present a boundary data-driven magneto-hydrodynamic (MHD) simulation of the 2011-02-15 coronal mass ejection (CME) event of Active Region (AR) NOAA 11158. The simulation is driven at the lower boundary with an electric field derived from the normal magnetic field and the vertical electric current measured from the Solar Dynamics Observatory (SDO) Helioseismic Magnetic Imager (HMI) vector magnetograms. </p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/observing-evolution-suns-global-coronal-magnetic-field" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-05/Gibson_CoronalActivity.jpg?itok=vqe4PEYJ" width="480" height="372" alt="Gibson Coronal Activity" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/observing-evolution-suns-global-coronal-magnetic-field" hreflang="en">Observing the evolution of the Sun’s global coronal magnetic field</a></h3> <div class="card-date"><time datetime="2024-09-17T12:00:00Z" class="datetime">Sep 17, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p>Zihao Yang, Hui Tian, Steven Tomczyk, Xianyu Liu, <strong>Sarah Gibson</strong>, Richard Morton, Cooper Downs, using the Upgraded Coronal Multi-channel Polarimeter, have obtained magnetograms of the global corona above the solar limb over approximately eight months.</p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/global-and-local-dynamics-x-flare-producing-active-regions-during-solar" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-09/Ralphaldini_21st%20February%202024%20synopticMap.png?itok=50nrZwj3" width="480" height="177" alt="21st February 2024 synoptic map" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/global-and-local-dynamics-x-flare-producing-active-regions-during-solar" hreflang="en">Global and Local Dynamics of X-flare Producing Active Regions During Solar Cycle 25 Peak-Phase</a></h3> <div class="card-date"><time datetime="2024-09-15T12:00:00Z" class="datetime">Sep 15, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>Breno Raphaldini</strong>, <strong>Mausumi Dikpati</strong>, Andre S. W. Teruya , Kiran Jain, Aimee A. Norton , and <strong>Scott W. McIntosh</strong> investigate the circumstances under which two of the most flare-prolific active regions of solar cycle 25, namely ARs 13590 and 13514, flared. </p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/subauroral-red-arcs-generated-inner-magnetospheric-heat-flux-and" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-09/Lin_HeatFlux-SAPSimpacts.SARarcs.png?itok=nIqffwmg" width="431" height="480" alt="Heat flux/SAPS impacts on SAR arcs" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/subauroral-red-arcs-generated-inner-magnetospheric-heat-flux-and" hreflang="en">SubAuroral Red Arcs Generated by Inner Magnetospheric Heat Flux and by SubAuroral Polarization Streams</a></h3> <div class="card-date"><time datetime="2024-09-06T12:00:00Z" class="datetime">Sep 6, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>Dong Lin</strong>, <strong>Wenbin Wang</strong>, Mei-Ching Fok, <strong>Kevin Pham</strong>, Jia Yue, and <strong>Haonan Wu</strong>, <span>utilize first-principles inner magnetosphere model and ionosphere-thermosphere model to illustrate the thermodynamic coupling effects between the topside ionosphere and the magnetosphere, and compare the relative significance between the heat flux and plasma convection due to electrodynamic coupling. </span></p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/euv-polarimetric-diagnostics-solar-corona-hanle-effect-ne-viii-770" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-04/Gibson_diagnosticPotentialCoronalEmissionLines.jpg?itok=5NtfYx_C" width="480" height="385" alt="Diagnostic Potential of a Coronal Emission Line" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/euv-polarimetric-diagnostics-solar-corona-hanle-effect-ne-viii-770" hreflang="en">EUV polarimetric diagnostics of the solar corona: the Hanle effect of Ne viii 770 A</a></h3> <div class="card-date"><time datetime="2024-08-31T12:00:00Z" class="datetime">Aug 31, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>Raveena Khan</strong>, <strong>Sarah Gibson</strong>, <strong>Roberto Casini</strong>, and K. Nagaraju utilize 3D 'Magneto-hydrodynamic Algorithm outside a Sphere' (MAS) models as input to the FORWARD code to model polarization in Ne viii line produced due to resonance scattering, and interpret its modification due to collisions and the magnetic fields through the Hanle effect. </p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/intermittency-hot-plasma-loops-solar-corona" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-08/Judge_SDOandDKISTdate.png?itok=fZkAyX7I" width="321" height="239" alt="SDO and DKIS data" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/intermittency-hot-plasma-loops-solar-corona" hreflang="en">On the intermittency of hot plasma loops in the solar corona</a></h3> <div class="card-date"><time datetime="2024-08-20T12:00:00Z" class="datetime">Aug 20, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>P. Judge</strong> and N.P.M. Kuin ask why and how are entire hydromagnetic structures only intermittently loaded with bright coronal plasma in the Sun? Their findings consolidate the claim that unobserved physical processes are at work which govern the heating of long-lived coronal loops.</p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/erratum-analysis-seeing-induced-polarization-cross-talk-and-modulation" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-07/Casini_Graph-polarimetricErrors.png?itok=0ID_z_a5" width="480" height="368" alt="Graph of polarimetric errors" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/erratum-analysis-seeing-induced-polarization-cross-talk-and-modulation" hreflang="en">Erratum: Analysis of Seeing-Induced Polarization Cross-Talk and Modulation Scheme Performance</a></h3> <div class="card-date"><time datetime="2024-08-01T12:00:00Z" class="datetime">Aug 1, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>R. Casini, A. G. de Wijn, P. G. Judge</strong> analyze <em>(Published 2012 September 4) </em>the generation of polarization cross-talk in Stokes polarimeters by atmospheric seeing, and its effects on the noise statistics of spectropolarimetric measurements for both single-beam and dual-beam instruments.</p> </div> </div> </div> </div></div> <div><div class="card h-100"> <figure class="card__image"> <a href="/news/publication-highlight/magnetohydrodynamic-turbulence-simulations-testing-ground-punch" hreflang="en"><img loading="lazy" src="/sites/default/files/styles/large/public/2024-04/Gibson_magnetohydrodynamicSimulationsOfTurbulence.jpg?itok=y7GI0m5S" width="480" height="151" alt="Magnetohydrodynamic Simulations of Turbulence" class="image-style-large img-fluid" /> </a> </figure> <div class="card-body"> <h3 class="card-title"><a href="/news/publication-highlight/magnetohydrodynamic-turbulence-simulations-testing-ground-punch" hreflang="en">Magnetohydrodynamic turbulence simulations as a testing ground for PUNCH</a></h3> <div class="card-date"><time datetime="2024-08-01T12:00:00Z" class="datetime">Aug 1, 2024</time> </div> <div class="card__summary"> <div class="clearfix"><p><strong>Sarah Gibson</strong> et. al. present a numerical study that combines magnetohydrodynamic simulations of turbulence together with forward-modeling synthesis of white- light data via the FORWARD code. Their study is a first step in the process of analyzing and understanding the unprecedented information that The Polarimeter to UNify the Corona and Heliosphere (PUNCH) will provide.</p> </div> </div> </div> </div></div> </div> <nav class="pager" role="navigation" aria-labelledby="pagination-heading"> <h4 id="pagination-heading" class="visually-hidden">Pagination</h4> <ul class="pagination"> <li class="page-item is-active active"> <a href="?page=0" title="Current page" aria-current="page" class="page-link" aria-current="true" > <span class="visually-hidden"> Current page </span>1</a> </li> <li class="page-item "> <a href="?page=1" title="Go to page 2" class="page-link" > <span class="visually-hidden"> Page </span>2</a> </li> <li class="page-item "> <a href="?page=2" title="Go to page 3" class="page-link" > <span class="visually-hidden"> Page </span>3</a> </li> <li class="page-item "> <a href="?page=3" title="Go to page 4" class="page-link" > <span class="visually-hidden"> Page 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