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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-12806" class="post-12806 post type-post status-publish format-standard has-post-thumbnail category-astrobites category-highlights tag-exoplanets tag-planet-formation tag-variable-stars 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"> Star Alignment and a Planet’s Origin: The Case of HIP 65426 </h1>  </div> <div class="post-meta cf"> <span class="posted-by">By <span class="reviewer" itemprop="author"><a href="https://aasnova.org/person/astrobites/" title="Astrobites">Astrobites</a></span> </span> <span class="posted-on">on <span class="dtreviewed"> <time class="value-title" datetime="2024-10-22T12:00:19-04:00" title="2024-10-22" itemprop="datePublished">22 October 2024</time> </span> </span> <span class="subcat">Astrobites</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%2F10%2F22%2Fstar-alignment-and-a-planets-origin-the-case-of-hip-65426%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%2F10%2F22%2Fstar-alignment-and-a-planets-origin-the-case-of-hip-65426%2F" class="fa fa-facebook" title="Share on Facebook"> <span class="visuallyhidden">Facebook</span></a> <a 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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/2024/09/HIP65426.png" title="Star Alignment and a Planet’s Origin: The Case of HIP 65426" itemprop="image"> <img width="702" height="336" src="https://aasnova.org/wp-content/uploads/2024/09/HIP65426-702x336.png" class="attachment-main-slider size-main-slider wp-post-image" alt="Infrared images of the exoplanet HIP 65426 b from JWST" title="Star Alignment and a Planet’s Origin: The Case of HIP 65426" decoding="async" fetchpriority="high" srcset="https://aasnova.org/wp-content/uploads/2024/09/HIP65426-702x336.png 702w, https://aasnova.org/wp-content/uploads/2024/09/HIP65426-260x124.png 260w, https://aasnova.org/wp-content/uploads/2024/09/HIP65426-768x367.png 768w, https://aasnova.org/wp-content/uploads/2024/09/HIP65426-600x287.png 600w, https://aasnova.org/wp-content/uploads/2024/09/HIP65426-1078x516.png 1078w, https://aasnova.org/wp-content/uploads/2024/09/HIP65426.png 1250w" sizes="(max-width: 702px) 100vw, 702px" /> </a> <div class="caption">Infrared images of the exoplanet HIP 65426 b from JWST. [<a href="https://webbtelescope.org/contents/media/images/01GBT1E93YV7YND5MFS1603FWJ">NASA, ESA, CSA, Alyssa Pagan (STScI)</a>]</div> </div> </header> <div class="post-container cf"> <div class="post-content-right"> <div class="post-content description " itemprop="articleBody"> <blockquote><p><em>Editor’s Note:</em> <a href="http://astrobites.org" target="_blank" rel="noopener noreferrer">Astrobites</a> is a graduate-student-run organization that digests astrophysical literature for undergraduate students. As part of the <a href="https://aas.org/posts/news/2016/06/aas-and-astrobites-formalize-partnership" target="_blank" rel="noopener noreferrer">partnership</a> between the AAS and astrobites, we occasionally repost astrobites content here at AAS Nova. We hope you enjoy this post from astrobites; the original can be viewed at <a href="http://astrobites.org" target="_blank" rel="noopener noreferrer">astrobites.org</a>.</p></blockquote> <p><strong>Title: </strong><a href="https://doi.org/10.3847/1538-3881/ad4964">HIP 65426 Is a High-Frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with Its Directly Imaged Exoplanet</a><br /> <strong>Authors:</strong> Aldo G. Sepulveda et al.<strong><br /> First Author’s Institution:</strong> University of Hawaiʻi at Mānoa<strong><br /> Status: </strong>Published in <em>AJ</em></p> <h4 class="wp-block-heading">What Is HIP 65426?</h4> <p>HIP 65426 is a star relatively close to Earth, and it has a giant planet called <a href="https://en.wikipedia.org/wiki/HIP_65426_b">HIP 65426b</a> orbiting around it that has been directly imaged. You might recall HIP 65426b from a <a href="https://webbtelescope.org/contents/media/images/01GBT1E93YV7YND5MFS1603FWJ">JWST early science release</a>, as it was the first exoplanet directly imaged by JWST.</p> <p>The star itself is part of a group of young stars called the Lower Centaurus–Crux (LCC) moving group, which is around 10–23 million years old, but scientists estimate HIP 65426 to be around 14 million years old using different methods. This star rotates very quickly and shows signs of potential pulsations in its brightness. Confirming these pulsations, known as <a href="https://en.wikipedia.org/wiki/Delta_Scuti_variable">δ Scuti pulsations</a>, could help determine the star’s age more precisely. Determining ages of stars is actually surprisingly difficult, so any method that can accurately predict ages is very intriguing to astronomers.</p> <p>Now switching gears briefly, planet HIP 65426b is located relatively far from the star, between 62 and 120 times the distance between Earth and the Sun. Its orbit is tilted at a significant angle relative to our line of sight. This is particularly interesting because the alignment between a star and its orbiting companions, like planets or brown dwarfs, can tell us more about how these systems formed and evolved.</p> <p>A recent work revealed that misalignments are common with brown dwarfs, but the orbits of giant planets tended to be aligned or nearly aligned with the spins of their host stars. Understanding whether planets like HIP 65426b are aligned with their stars helps us understand planet formation and the history of these systems.</p> <h4 class="wp-block-heading">Observing with and Using Data from TESS</h4> <p><a href="https://irsa.ipac.caltech.edu/data/SPITZER/docs/irac/iracinstrumenthandbook/47/#:~:text=The%20goal%20of%20time%20series,curve%20of%20an%20astronomical%20source.">Time-series photometry</a> from the <a href="https://science.nasa.gov/mission/tess">Transiting Exoplanet Survey Satellite</a> (TESS) has provided a lot of data about the rotation of stars and any variations in brightness caused by features on their surfaces or by orbiting objects passing in front of them. Time-series photometry also probes for other phenomena, including stellar pulsations and transit events. In this article, the authors use this data, along with some data from direct imaging of the HIP 65426 system, to investigate the orbital inclination of the exoplanet HIP 65426b. They aim to determine whether there is evidence for misalignment between the planet and its host star.</p> <p>The star was observed by TESS in three different time periods called sectors (Figure 1). These sectors spanned from April 2019 to May 2019, April 2021 to May 2021, and April 2023 to May 2023. Data was collected from the star every 2 minutes during these time periods. The data was analyzed using a software called <a href="https://www.youtube.com/watch?v=K90fk6DxIMY">lightkurve</a>, which helps process and analyze the light curves of stars. To ensure the data are clean and free from contamination, the authors first removed any unusual or outlier data points from the light curves. Then, they examined a region around the star within a radius of 80 arcseconds to see if any nearby objects were affecting the measurements. This is important because contamination from other sources can affect the accuracy of the analysis.</p> <div id="attachment_12810" style="width: 712px" class="wp-caption aligncenter"><a href="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr.jpg" data-rel="lightbox-image-0" data-rl_title="Figure 1: TESS time-series photometry of HIP 65426 for Sectors (a) 11, (b) 38, and (c) 64. [Adapted from Sepulveda et al. 2024]" data-rl_caption="Figure 1: TESS time-series photometry of HIP 65426 for Sectors (a) 11, (b) 38, and (c) 64. [Adapted from Sepulveda et al. 2024]" title="Figure 1: TESS time-series photometry of HIP 65426 for Sectors (a) 11, (b) 38, and (c) 64. [Adapted from Sepulveda et al. 2024]"><img decoding="async" aria-describedby="caption-attachment-12810" class="size-medium wp-image-12810" src="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr-702x501.jpg" alt="TESS time-series photometry of HIP 65426" width="702" height="501" srcset="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr-702x501.jpg 702w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr-260x186.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr-768x548.jpg 768w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr-600x428.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f1_hr.jpg 1000w" sizes="(max-width: 702px) 100vw, 702px" /></a><p id="caption-attachment-12810" class="wp-caption-text">Figure 1: TESS time-series photometry of HIP 65426 for Sectors (a) 11, (b) 38, and (c) 64. [Adapted from Sepulveda et al. 2024]</p></div> <h4 class="wp-block-heading">Identification of the δ Scuti pulsations for Mass and Age Estimations</h4> <p>Several pulsation modes, spanning 28–131 cycles per day, were identified in the star. This is consistent with a high-frequency Scuti pulsator. The presence of these high-frequency Scuti pulsations confirms the young age of HIP 65426 and may even provide an opportunity to estimate its age through detailed asteroseismic modeling, which is beyond the scope of the article.</p> <p>The authors also investigated the possibility of pulsation timing variations caused by mutual gravitation with an orbital companion. This is typically measurable only for sufficiently massive planets with long enough periods. No such variations were detected, which places an upper limit of 12.8 Jupiter masses on the mass of HIP 65426b.</p> <h4 class="wp-block-heading">Stellar Inclination of the Host Star</h4> <p>Using a known relation between the star’s rotation period, its radius, and a measure of its rotational velocity, one can constrain the angle between the star’s rotational axis and our line of sight, also known as stellar inclination. This article uses a <a href="https://en.wikipedia.org/wiki/Bayesian_inference">Bayesian framework</a> that properly computes the inclination using these parameters. Based on their analysis using values of these parameters from literature (radius from <a href="https://en.m.wikipedia.org/wiki/Stellar_isochrone">isochrones</a> and rotational velocity from spectroscopy) and TESS measurements (rotation period), the authors place statistical limits on the inclination difference between the star and the planet, the median value being 105 (+7/-9) degrees.</p> <div id="attachment_12809" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr.jpg" data-rel="lightbox-image-1" data-rl_title="Figure 2: A sample of 100 sky-projected orbits used for fitting the orbit of HIP 65426b. The cyan star represents the position of HIP 65426 and the orange dots represent the relative astrometry of HIP 65426b. [Adapted from Sepulveda et al. 2024]" data-rl_caption="Figure 2: A sample of 100 sky-projected orbits used for fitting the orbit of HIP 65426b. The cyan star represents the position of HIP 65426 and the orange dots represent the relative astrometry of HIP 65426b. [Adapted from Sepulveda et al. 2024]" title="Figure 2: A sample of 100 sky-projected orbits used for fitting the orbit of HIP 65426b. The cyan star represents the position of HIP 65426 and the orange dots represent the relative astrometry of HIP 65426b. [Adapted from Sepulveda et al. 2024]"><img decoding="async" aria-describedby="caption-attachment-12809" class="size-thumbnail wp-image-12809" src="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr-260x198.jpg" alt="plot of sky-projected orbits for HIP 65426 b" width="260" height="198" srcset="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr-260x198.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr-702x534.jpg 702w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr-768x585.jpg 768w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr-600x457.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f6_hr.jpg 1168w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12809" class="wp-caption-text">Figure 2: A sample of 100 sky-projected orbits used for fitting the orbit of HIP 65426b. The cyan star represents the position of HIP 65426 and the orange dots represent the relative astrometry of HIP 65426b. [Adapted from Sepulveda et al. 2024]</p></div> <h4 class="wp-block-heading">Orbital Inclination of the Giant Planet</h4> <p>The orbit of the planet was measured out using astrometric measurements from various sources, including high-precision measurements from <a href="https://www.eso.org/public/teles-instr/paranal-observatory/vlt/vlt-instr/gravity/">VLTI/GRAVITY</a>. From MCMC fitting of Keplerian orbits using the Python package <a href="https://astrobites.org/2022/09/16/learning-more-about-exoplanet-orbits-using-orbitize/">orbitize</a>, the median orbital inclination is estimated to be 108 (+6/-3) degrees, consistent with recent studies of the system although different input measurements were used in this work. Orbits drawn from the fitting process are shown in Figure 2.</p> <h4 class="wp-block-heading">Is There a Misalignment?</h4> <p>Figure 3 says no! Here the authors compared the inclination of HIP 65426b with the inclination of its host star. As the plot shows, the stellar and planetary orbital inclinations line up within their uncertainties, and hence there’s a lack of evidence for a misalignment, just a small star–planet obliquity as suggested by the roughly 3-degree difference in inclination.</p> <div id="attachment_12808" style="width: 712px" class="wp-caption aligncenter"><a href="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr.jpg" data-rel="lightbox-image-2" data-rl_title="Figure 3: The normalized orbital and stellar inclination posteriors for the HIP 65426 system. The purple histogram corresponds to the orbital inclination of the planet and the gray plot represents the stellar inclination of the host star. [Sepulveda et al. 2024]" data-rl_caption="Figure 3: The normalized orbital and stellar inclination posteriors for the HIP 65426 system. The purple histogram corresponds to the orbital inclination of the planet and the gray plot represents the stellar inclination of the host star. [Sepulveda et al. 2024]" title="Figure 3: The normalized orbital and stellar inclination posteriors for the HIP 65426 system. The purple histogram corresponds to the orbital inclination of the planet and the gray plot represents the stellar inclination of the host star. [Sepulveda et al. 2024]"><img loading="lazy" decoding="async" aria-describedby="caption-attachment-12808" class="size-medium wp-image-12808" src="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-702x332.jpg" alt="plot of normalized probability density as a function of inclination angle" width="702" height="332" srcset="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-702x332.jpg 702w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-260x123.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-768x363.jpg 768w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-600x283.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-1536x726.jpg 1536w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr-1320x624.jpg 1320w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f5_hr.jpg 1996w" sizes="(max-width: 702px) 100vw, 702px" /></a><p id="caption-attachment-12808" class="wp-caption-text">Figure 3: The normalized orbital and stellar inclination posteriors for the HIP 65426 system. The purple histogram corresponds to the orbital inclination of the planet and the gray plot represents the stellar inclination of the host star. [Sepulveda et al. 2024]</p></div>This seems to be in line with the general trend of alignment where directly imaged long-period giant planets appear aligned with their host stars, as shown by the plot in Figure 4, where the orbital and host-star inclinations for six directly imaged exoplanet systems are being compared. This type of perfect alignment also extends to <a href="https://public.nrao.edu/blogs/what-is-a-debris-disk/">debris disks</a>, which are analogous to our solar system’s Kuiper Belt.</p> <div id="attachment_12807" style="width: 270px" class="wp-caption alignleft"><a href="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr.jpg" data-rel="lightbox-image-3" data-rl_title="Figure 4: Comparison of orbital inclinations and host-star inclinations for six directly imaged exoplanet systems comprising 11 total companions. [Sepulveda et al. 2024]" data-rl_caption="Figure 4: Comparison of orbital inclinations and host-star inclinations for six directly imaged exoplanet systems comprising 11 total companions. [Sepulveda et al. 2024]" title="Figure 4: Comparison of orbital inclinations and host-star inclinations for six directly imaged exoplanet systems comprising 11 total companions. [Sepulveda et al. 2024]"><img loading="lazy" decoding="async" aria-describedby="caption-attachment-12807" class="size-thumbnail wp-image-12807" src="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr-260x251.jpg" alt="plot of host star inclination versus orbital inclination" width="260" height="251" srcset="https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr-260x251.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr-702x678.jpg 702w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr-768x742.jpg 768w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr-600x580.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/ajad4964f7_hr.jpg 999w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12807" class="wp-caption-text">Figure 4: Comparison of orbital inclinations and host-star inclinations for six directly imaged exoplanet systems comprising 11 total companions. [Sepulveda et al. 2024]</p></div>If the observed trend of relatively aligned orbits between stars and their imaged giant planets continues, it goes against recent understanding from a 2023 work that suggests misalignments are common in brown-dwarf systems. These differences between giant planets and brown dwarfs could extend to other key characteristics, like their orbital shapes, which might indicate that they form through different processes.</p> <h4 class="wp-block-heading">Now, What Can We Tell About the Formation of HIP 65426b?</h4> <p>There are two key models that explain how planets could form: core accretion and disk instability. Core accretion does not really explain how this planet is born because it is farther away from the host star than the region where core accretion would take place. The lack of evidence for misalignment also disfavors the core-accretion scenario. Given the large orbital eccentricity, planet–planet scattering could be a possible mechanism. This scenario suggests that the planet formed closer to its star via core accretion and was then scattered to its current position by the gravitational interactions with other planets in the system. However, planet–planet scattering typically results in orbits being tilted relative to each other, which isn’t the case here, so the lack of significant misalignment between the HIP 65426b’s orbit and its star’s rotation axis doesn’t strongly support this idea.</p> <p>It is important to note that these theories are not conclusive. The current data don’t provide complete information about the system’s geometry, so it’s still possible that the star’s actual tilt might be larger than what’s currently estimated. Additionally, the orbital eccentricity is not yet concretely determined, so further astrometric measurements can change our current geometric understanding of the system.</p> <h4 class="wp-block-heading">The Big Picture</h4> <p>This article describes yet another work that combined space-based brightness data and direct imaging data to understand other planetary systems well after they have formed and understand the implications of their obliquity. With new missions and exoplanet surveys, new systems will be discovered that will also usher in more similar studies of inclinations and orbital architecture.</p> <p><em>Original astrobite edited by Amaya Sinha.<br /> </em></p> <blockquote> <h4 class="wpautbox-name">About the author, Maria Vincent:</h4> <p>Maria is a PhD candidate in astronomy at the Institute for Astronomy, University of Hawai’i at Manoa. Her research focuses on adaptive optics and high-contrast imaging science and instrumentation with ground-based telescopes. Driven by a fascination with planet formation and the intricate processes shaping our solar system, she uses the Subaru Coronagraphic Extreme Adaptive Optics suite to observe and study morphological features of protoplanetary disks in near-infrared wavelengths, aiming to understand disk structure and processes governing planet formation. On the instrumentation side, she is working on designing and constructing an optical testbed to test and characterize a new deformable mirror as part of the upcoming High-order Advanced Keck Adaptive Optics upgrade. Outside of work, she enjoys blogging, mystery, historical and science fiction literature and cinemedia, photography, hiking, and travel.</p></blockquote> <div class="tagcloud"><a href="https://aasnova.org/tag/exoplanets/" rel="tag">exoplanets</a> <a href="https://aasnova.org/tag/planet-formation/" rel="tag">planet formation</a> <a href="https://aasnova.org/tag/variable-stars/" rel="tag">variable stars</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/2024/11/20/charting-the-cosmic-shoreline-which-planets-have-atmospheres-gl-486b/"><img width="110" height="96" src="https://aasnova.org/wp-content/uploads/2024/11/jpegPIA21473-110x96.jpg" class="attachment-post-thumbnail size-post-thumbnail 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