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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-11342" class="post-11342 post type-post status-publish format-standard has-post-thumbnail category-astrobites category-highlights tag-exoplanets tag-planetary-systems 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"> What Shapes the Edge of a Planetary System? </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="2023-10-31T12:00:15-04:00" title="2023-10-31" itemprop="datePublished">31 October 2023</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%2F2023%2F10%2F31%2Fwhat-shapes-the-edge-of-a-planetary-system%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%2F10%2F31%2Fwhat-shapes-the-edge-of-a-planetary-system%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%2F2023%2F10%2F31%2Fwhat-shapes-the-edge-of-a-planetary-system%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%2F2023%2F10%2F31%2Fwhat-shapes-the-edge-of-a-planetary-system%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%2F2023%2F10%2F31%2Fwhat-shapes-the-edge-of-a-planetary-system%2F" class="fa fa-reddit" title="Share on Reddit"> <span class="visuallyhidden">Reddit</span></a> <a href="mailto:?subject=What%20Shapes%20the%20Edge%20of%20a%20Planetary%20System%3F&body=https%3A%2F%2Faasnova.org%2F2023%2F10%2F31%2Fwhat-shapes-the-edge-of-a-planetary-system%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/2023/10/PIA06939_fig1-scaled.jpg" title="What Shapes the Edge of a Planetary System?" itemprop="image"> <img width="702" height="336" src="https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-702x336.jpg" class="attachment-main-slider size-main-slider wp-post-image" alt="illustration of a planetary system" title="What Shapes the Edge of a Planetary System?" decoding="async" fetchpriority="high" srcset="https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-702x336.jpg 702w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-260x124.jpg 260w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-768x367.jpg 768w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-600x287.jpg 600w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-1536x735.jpg 1536w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-2048x980.jpg 2048w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-1078x516.jpg 1078w, https://aasnova.org/wp-content/uploads/2023/10/PIA06939_fig1-1320x631.jpg 1320w" sizes="(max-width: 702px) 100vw, 702px" /> </a> <div class="caption">An artist's impression of a planetary system containing planets and a ring of debris. [<a href="https://photojournal.jpl.nasa.gov/catalog/PIA06939">NASA/JPL-Caltech</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/10.3847/1538-4357/ace966">Can Cold Jupiters Sculpt the Edge-of-the-multis?</a><br /> <strong>Authors:</strong> Nicole Sobski and Sarah Millholland<br /> <strong>Authors’ Institutions: </strong>Wellesley College and Massachusetts Institute of Technology<br /> <strong>Status: </strong>Published in <em>ApJ</em></p> <p>The <a href="https://www.nasa.gov/mission_pages/kepler/overview/index.html">Kepler mission</a> revealed thousands of transiting exoplanets. Through this unique data set, we have come to understand much more about exoplanet demographics and the <a href="https://astrobites.org/2013/02/14/the-frequency-of-habitable-planets-around-m-dwarfs/">occurrence rates</a> of different kinds of planets. In particular, we now understand that the most common type of planetary system is what we refer to as a “compact multi-planetary system.” That is to say, a system of multiple small planets (less than 4 Earth radii each) where each planet orbits in similar, short timespans (usually less than about 50 days). Studies of the full Kepler data set show that these “compact multis” are ubiquitous across the galaxy. Furthermore, these systems are shown to have a high rate of intra-system uniformity, sometimes called <a href="https://astrobites.org/2019/07/15/peas-in-a-pod/#:~:text=A%20more%20intuitive%20way%20to,noise%20level%20of%20the%20star.">“peas-in-a-pod”</a> architecture. Planets within a compact multi often have similar radii and similar spacing in their orbital periods.</p> <p>But in a system of multiple transiting exoplanets of such uniformity, what causes the system to “end”? That is, what causes the pod to be filled up with peas? A new study looks into one possible force that may “sculpt” the edge of a compact multi-planet system: <a href="https://astrobites.org/2023/05/05/do-jupiters-hurt-small-planet-formation/">cold Jupiters</a>. A cold Jupiter is a planet that has the mass of our own solar system’s Jupiter and is widely separated from its host star. The authors explore if and how the existence of a cold Jupiter at wide separation from an inner compact multi arrangement might determine how the pod gets filled with peas.</p> <p>To test this, the authors needed a data set of known compact multis. They turned to the Kepler data set and selected the systems with at least four transiting planets. This left them with 279 planets in 64 systems. Next, they compiled the previously measured masses of these planets; only 60 of 279 had masses, so for the remainder they used a well-described mass–radius relationship to estimate planet masses. Planet mass is a crucial input for this study as mass is the primary parameter needed for dynamical studies, which inherently rely on gravitational forces.</p> <p>To determine if and how a cold Jupiter could sculpt the edge of the inner compact system, the authors devised a dynamical study. Dynamical studies test how planets interact with each other through their gravitational influence on one another; often a researcher will test to see if a certain configuration of planets is stable or if it is unstable. In an unstable system, some or all of the planets get gravitationally kicked out of the system. Using a simulation software called the <a href="https://github.com/dtamayo/spock">Stability of Planetary Orbital Configurations Klassifier (SPOCK)</a>, which takes in a list of planet masses and a few basic orbital parameters, the authors were able to compute the stability of the system over a specified time span. The authors added a simulated cold Jupiter (with parameters drawn from random distributions) to a planetary system with real planet masses and orbits and then determined the system’s stability over 1 billion years. For each of the 64 systems in the sample, they performed this test 10,000 times, noting the probability that the system was stable or not over that time span.</p> <p>Each test resulted in one of three outcomes: unstable, fully stable, or metastable. Within the context of this study, metastable meant that the system was stable in about half of the simulations. Unstable simulations mean that the system will be ripped apart by gravitational interactions. The injected cold Jupiters that result in unstable configurations are not considered plausible edge-sculptors, then, because we <em>do</em> see planets in these systems; if the presence of a cold Jupiter made the system unstable, we wouldn’t see planets in the system. Next, the stable simulations represent injected cold Jupiters that had no effect on the inner system. These cold Jupiters exist at too wide a separation from the inner system for gravity to play a role in sculpting the edge of the pea pod. Therefore, these planets were also not considered plausible edge-sculptors. The metastable simulations, in which the odds of the system falling apart were between 30% and 70% (above 70% was considered fully stable), are the most interesting. These simulations correspond to systems in which the injected cold Jupiter had a real effect on the inner compact system and could potentially sculpt the edge of the inner compact system, as shown in Figure 1.</p> <div id="attachment_11344" style="width: 712px" class="wp-caption aligncenter"><a href="https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr.jpg" data-rel="lightbox-image-0" data-rl_title="Figure 1: An example of the results of the main dynamical experiment for one multi-planet system. Each point is one of the 10,000 simulations where a cold Jupiter with randomized orbital parameters (y axis) and mass (x axis) is injected into the dynamical simulation along with the real planets. The dots are color coded by the probability of a stable configuration after 1 billion years: purple is unlikely to be stable, yellow is very likely stable. The “meta-stable” region is defined by the shading and red line. Because this particular system has a very small meta-stable region, it is highly unlikely that any cold Jupiter, if it exists, would play the role of the “edge sculptor." [Adapted from Sobski & Millholland 2023]" data-rl_caption="Figure 1: An example of the results of the main dynamical experiment for one multi-planet system. Each point is one of the 10,000 simulations where a cold Jupiter with randomized orbital parameters (y axis) and mass (x axis) is injected into the dynamical simulation along with the real planets. The dots are color coded by the probability of a stable configuration after 1 billion years: purple is unlikely to be stable, yellow is very likely stable. The “meta-stable” region is defined by the shading and red line. Because this particular system has a very small meta-stable region, it is highly unlikely that any cold Jupiter, if it exists, would play the role of the “edge sculptor." [Adapted from Sobski & Millholland 2023]" title="Figure 1: An example of the results of the main dynamical experiment for one multi-planet system. Each point is one of the 10,000 simulations where a cold Jupiter with randomized orbital parameters (y axis) and mass (x axis) is injected into the dynamical simulation along with the real planets. The dots are color coded by the probability of a stable configuration after 1 billion years: purple is unlikely to be stable, yellow is very likely stable. The “meta-stable” region is defined by the shading and red line. Because this particular system has a very small meta-stable region, it is highly unlikely that any cold Jupiter, if it exists, would play the role of the “edge sculptor." [Adapted from Sobski & Millholland 2023]"><img decoding="async" aria-describedby="caption-attachment-11344" class="size-medium wp-image-11344" src="https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr-702x520.jpg" alt="Plot of probability of stability as a function of perturber orbital distance and perturber mass" width="702" height="520" srcset="https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr-702x520.jpg 702w, https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr-260x193.jpg 260w, https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr-768x569.jpg 768w, https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr-600x444.jpg 600w, https://aasnova.org/wp-content/uploads/2023/10/apjace966f4_hr.jpg 980w" sizes="(max-width: 702px) 100vw, 702px" /></a><p id="caption-attachment-11344" class="wp-caption-text">Figure 1: An example of the results of the main dynamical experiment for one multi-planet system. Each point is one of the 10,000 simulations where a cold Jupiter with randomized orbital parameters (<em>y</em> axis) and mass (<em>x</em> axis) is injected into the dynamical simulation along with the real planets. The dots are color coded by the probability of a stable configuration after 1 billion years: purple is unlikely to be stable, yellow is very likely stable. The metastable region is defined by the shading and red line. Because this particular system has a very small metastable region, it is highly unlikely that any cold Jupiter, if it exists, would play the role of the “edge sculptor.” [Adapted from Sobski & Millholland 2023]</p></div>However, looking at the mass and orbital parameters of the injected cold Jupiters that resulted in metastable simulations revealed a problem for the authors’ hypothesis: If these planets really existed in the Kepler systems tested, then observers should have been able to detect them in real data sets. These planets are large enough in radius that even accounting for transit probabilities, they likely would have been detected at appropriate rates in the Kepler data set. Similarly, they are massive enough and close enough to the inner system that <a href="https://www.planetary.org/articles/color-shifting-stars-the-radial-velocity-method">radial-velocity</a> surveys should easily detect them, but real radial-velocity data sets do not. (Radial-velocity surveys rely on measuring the Doppler shift of light due to a planet tugging on its host star.)</p> <p>Therefore, the authors conclude that cold Jupiters likely do not help sculpt the edge of compact multi-planet systems. If they could, we would have found them in real data; since we don’t find them in real data, they must not exist in the compact multis studied here. Even though this experiment led to the rejection of the original hypothesis, it is nevertheless a fascinating result that tells us a bit more about the way exoplanet systems may form and evolve.</p> <p><em>Original astrobite edited by Lindsay DeMarchi.<br /> </em></p> <blockquote> <h4 class="wpautbox-name">About the author, Jack Lubin:</h4> <p>Jack received his PhD in astrophysics from UC Irvine and is now a postdoc at UCLA. His research focuses on exoplanet detection and characterization, primarily using the radial-velocity method. 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