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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-12746" class="post-12746 post type-post status-publish format-standard has-post-thumbnail category-features category-highlights tag-astrochemistry tag-comets tag-planet-formation tag-protoplanetary-disks 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"> Icy Insights from Comets and Planet-Forming Disks </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="2024-09-23T12:00:55-04:00" title="2024-09-23" itemprop="datePublished">23 September 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%2F09%2F23%2Ficy-insights-from-comets-and-planet-forming-disks%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%2F09%2F23%2Ficy-insights-from-comets-and-planet-forming-disks%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%2F09%2F23%2Ficy-insights-from-comets-and-planet-forming-disks%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%2F09%2F23%2Ficy-insights-from-comets-and-planet-forming-disks%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%2F09%2F23%2Ficy-insights-from-comets-and-planet-forming-disks%2F" class="fa fa-reddit" title="Share on Reddit"> <span class="visuallyhidden">Reddit</span></a> <a href="mailto:?subject=Icy%20Insights%20from%20Comets%20and%20Planet-Forming%20Disks&body=https%3A%2F%2Faasnova.org%2F2024%2F09%2F23%2Ficy-insights-from-comets-and-planet-forming-disks%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/2024/09/STScI-01EVVCJMYFQSEJVKSTYQ4AHTXE.jpg" title="Icy Insights from Comets and Planet-Forming Disks" itemprop="image"> <img width="702" height="336" src="https://aasnova.org/wp-content/uploads/2024/09/STScI-01EVVCJMYFQSEJVKSTYQ4AHTXE-702x336.jpg" class="attachment-main-slider size-main-slider wp-post-image" alt="Enhanced Hubble image of Comet ISON" title="Icy Insights from Comets and Planet-Forming Disks" decoding="async" fetchpriority="high" /> </a> <div class="caption">A digitally enhanced view of the comet C/2012 S1 (ISON) as seen by the Hubble Space Telescope. [<a href="https://hubblesite.org/contents/media/images/2013/14/3174-Image.html">NASA, ESA, J.-Y. Li (Planetary Science Institute), and the Hubble Comet ISON Imaging Science Team</a>]</div> </div> </header> <div class="post-container cf"> <div class="post-content-right"> <div class="post-content description " itemprop="articleBody"> <p>Are the icy objects that inhabit the outer solar system truly pristine remnants of the early solar system, or have they been altered by the chaotic process of planet formation? Recent research that compares the chemistry of solar system comets and planet-forming systems may provide an answer to this key question.</p> <h4>Time Capsules from the Early Solar System(?)</h4> <div id="attachment_12750" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-scaled.jpg" data-rel="lightbox-image-0" data-rl_title="Diagram showing the locations of the Kuiper Belt and Oort Cloud. Click to enlarge. [Adapted from ESA (Acknowledgement: work performed by ATG under contract to ESA); CC BY-SA IGO 3.0]" data-rl_caption="Diagram showing the locations of the Kuiper Belt and Oort Cloud. Click to enlarge. [Adapted from ESA (Acknowledgement: work performed by ATG under contract to ESA); CC BY-SA IGO 3.0]" title="Diagram showing the locations of the Kuiper Belt and Oort Cloud. Click to enlarge. [Adapted from ESA (Acknowledgement: work performed by ATG under contract to ESA); CC BY-SA IGO 3.0]"><img decoding="async" aria-describedby="caption-attachment-12750" class="size-thumbnail wp-image-12750" src="https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-260x140.jpg" alt="Diagram showing the locations of the Kuiper Belt and Oort Cloud" width="260" height="140" srcset="https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-260x140.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-702x378.jpg 702w, https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-768x414.jpg 768w, https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-600x323.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-1536x828.jpg 1536w, https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-2048x1104.jpg 2048w, https://aasnova.org/wp-content/uploads/2024/09/Small_objects_in_the_Solar_System-1320x712.jpg 1320w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12750" class="wp-caption-text">Diagram showing the locations of the Kuiper Belt and Oort Cloud. Click to enlarge. [Adapted from <a href="https://www.esa.int/ESA_Multimedia/Images/2023/11/Small_objects_in_the_Solar_System">ESA (Acknowledgement: work performed by ATG under contract to ESA)</a>; <a href="https://creativecommons.org/licenses/by-sa/3.0/igo/">CC BY-SA IGO 3.0</a>]</p></div>The Kuiper Belt and Oort Cloud contain unknown numbers of icy planetesimals left over from the formation of the solar system. One of the most pressing questions in planetary science today is whether these objects represent unaltered material from the dusty nebula from which the Sun and the planets formed, or if the process of planet formation and the intervening billions of years have changed their properties. The answer has profound implications for understanding the formation of our own solar system and planetary systems in general.</p> <p>There’s a good reason that this question poses such a challenge: these far-flung objects are difficult or impossible to observe directly. Luckily, they make occasional journeys into the inner solar system, transformed by warm sunlight into comets sporting twin tails of dust and ions. Now, a team led by Manuela Lippi (National Institute for Astrophysics, Italy) has amassed a sample of these icy interlopers to assess their chemistry and understand whether they’ve changed since their formation.</p> <div id="attachment_12749" style="width: 270px" class="wp-caption alignleft"><a href="https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr.jpg" data-rel="lightbox-image-1" data-rl_title="Abundances of methanol (CH3OH), formaldehyde (H2CO), and ammonia (NH3), expressed as mixing ratios with respect to water. From left to right, the sections separated by dotted lines show the overall abundances; the difference between comets inside and outside 1 au; differences between dynamically new (DN), long-period (LP), and Jupiter-family (JF) comets; pre- and post-perihelion (perihelion is the closest distance to the Sun reached on a comet's orbit); and pre- and post-perihelion for comet 67P. Click to enlarge. [Lippi et al. 2024]" data-rl_caption="Abundances of methanol (CH3OH), formaldehyde (H2CO), and ammonia (NH3), expressed as mixing ratios with respect to water. From left to right, the sections separated by dotted lines show the overall abundances; the difference between comets inside and outside 1 au; differences between dynamically new (DN), long-period (LP), and Jupiter-family (JF) comets; pre- and post-perihelion (perihelion is the closest distance to the Sun reached on a comet's orbit); and pre- and post-perihelion for comet 67P. Click to enlarge. [Lippi et al. 2024]" title="Abundances of methanol (CH3OH), formaldehyde (H2CO), and ammonia (NH3), expressed as mixing ratios with respect to water. From left to right, the sections separated by dotted lines show the overall abundances; the difference between comets inside and outside 1 au; differences between dynamically new (DN), long-period (LP), and Jupiter-family (JF) comets; pre- and post-perihelion (perihelion is the closest distance to the Sun reached on a comet's orbit); and pre- and post-perihelion for comet 67P. Click to enlarge. [Lippi et al. 2024]"><img decoding="async" aria-describedby="caption-attachment-12749" class="size-thumbnail wp-image-12749" src="https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-260x152.jpg" alt="calculated chemical abundances for the comets in the sample" width="260" height="152" srcset="https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-260x152.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-702x411.jpg 702w, https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-768x449.jpg 768w, https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-600x351.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-1536x899.jpg 1536w, https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-2048x1198.jpg 2048w, https://aasnova.org/wp-content/uploads/2024/09/apjlad5a6df1_hr-1320x772.jpg 1320w" sizes="(max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12749" class="wp-caption-text">Abundances of methanol (CH<sub>3</sub>OH), formaldehyde (H<sub>2</sub>CO), and ammonia (NH<sub>3</sub>), expressed as mixing ratios with respect to water. From left to right, the sections separated by dotted lines show the overall abundances; the difference between comets inside and outside 1 au; differences between dynamically new (DN), long-period (LP), and Jupiter-family (JF) comets; pre- and post-perihelion (perihelion is the closest distance to the Sun reached on a comet’s orbit); and pre- and post-perihelion for comet 67P. Click to enlarge. [Lippi et al. 2024]</p></div> <h4>Comet Calculations</h4> <p>Using infrared and sub-millimeter observations, Lippi and collaborators studied the chemical compositions of 35 solar system comets. They found that the abundances of methanol, formaldehyde, and ammonia didn’t depend on the comet’s dynamical family. (A dynamical family is a group of comets with similar orbital characteristics.) For example, dynamically new comets — those making their first trek into the inner solar system — had similar chemistry to Jupiter-family comets whose orbits remain within the orbit of Jupiter and have visited the inner solar system many times.</p> <p>The similarity in chemical composition between comets in different dynamical families suggests that comets retain their chemical makeup after they form. If this is the case, comets in the solar system today should be chemically similar to the material surrounding young, planet-forming Sun-like stars.</p> <h4>Throwing Disks into the Mix</h4> <p>As a test of this theory, Lippi’s team compared the typical chemistry of solar system comets to that of 11 planet-forming systems. The systems in the comparison sample ranged in age from 10,000-year-old hot molecular cloud cores to million-year-old protoplanetary disks. Overall, the abundance ratios of solar system comets were similar to those of planet-forming systems. This is the first statistical evidence that planet-forming systems of all ages are chemically similar and that comets are indeed unaltered remnants of the early solar system.</p> <div id="attachment_12747" style="width: 270px" class="wp-caption alignright"><a href="https://aasnova.org/wp-content/uploads/2024/09/1567215847897-Rosetta_NavCam_comet_67P_20150314_enhanced_625.jpg" data-rel="lightbox-image-2" data-rl_title="Comet 67P/Churyumov–Gerasimenko as seen by the Rosetta spacecraft. [ESA/Rosetta/NAVCAM, CC BY-SA IGO 3.0]" data-rl_caption="Comet 67P/Churyumov–Gerasimenko as seen by the Rosetta spacecraft. [ESA/Rosetta/NAVCAM, CC BY-SA IGO 3.0]" title="Comet 67P/Churyumov–Gerasimenko as seen by the Rosetta spacecraft. [ESA/Rosetta/NAVCAM, CC BY-SA IGO 3.0]"><img loading="lazy" decoding="async" aria-describedby="caption-attachment-12747" class="size-thumbnail wp-image-12747" src="https://aasnova.org/wp-content/uploads/2024/09/1567215847897-Rosetta_NavCam_comet_67P_20150314_enhanced_625-260x255.jpg" alt="Comet 67P/Churyumov–Gerasimenko" width="260" height="255" srcset="https://aasnova.org/wp-content/uploads/2024/09/1567215847897-Rosetta_NavCam_comet_67P_20150314_enhanced_625-260x255.jpg 260w, https://aasnova.org/wp-content/uploads/2024/09/1567215847897-Rosetta_NavCam_comet_67P_20150314_enhanced_625-600x589.jpg 600w, https://aasnova.org/wp-content/uploads/2024/09/1567215847897-Rosetta_NavCam_comet_67P_20150314_enhanced_625.jpg 625w" sizes="auto, (max-width: 260px) 100vw, 260px" /></a><p id="caption-attachment-12747" class="wp-caption-text">Comet 67P/Churyumov–Gerasimenko as seen by the Rosetta spacecraft. [<a href="https://sci.esa.int/web/rosetta/-/55613-comet-67p-on-14-march-2015-navcam-enhanced">ESA/Rosetta/NAVCAM</a>, <a href="https://creativecommons.org/licenses/by-sa/3.0/igo/">CC BY-SA IGO 3.0</a>]</p></div>However, a note of caution: when Lippi and coauthors compared their solar system comet sample against measurements of the well-studied comet 67P/Churyumov–Gerasimenko, which hosted the Rosetta spacecraft in 2014–2016, they found substantial differences. If comet 67P stands apart from the average solar system comet, its use as a benchmark could bias studies of planet-forming systems.</p> <h4>Citation</h4> <p>“The Ice Chemistry in Comets and Planet-Forming Disks: Statistical Comparison of CH<sub>3</sub>OH, H<sub>2</sub>CO, and NH<sub>3</sub> Abundance Ratios,” Manuela Lippi et al 2024 <em>ApJL</em> <b>970</b> L5. <a href="https://doi.org/10.3847/2041-8213/ad5a6d">doi:10.3847/2041-8213/ad5a6d</a></p> <div class="tagcloud"><a href="https://aasnova.org/tag/astrochemistry/" rel="tag">astrochemistry</a> <a href="https://aasnova.org/tag/comets/" rel="tag">comets</a> <a href="https://aasnova.org/tag/planet-formation/" rel="tag">planet formation</a> <a href="https://aasnova.org/tag/protoplanetary-disks/" rel="tag">protoplanetary disks</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" 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