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Inside computer-made gas disks, outer regions around paired stars produced clusters of young planet-sized bodies.<\/p>\n
At the University of Lancashire<\/a>, astrophysicist Dr. Matthew Teasdale traced those bodies to disk fragments collapsing under gravity.<\/p>\n In the single-star and paired-star tests, wider stellar pairs stirred their disks sooner, and cooler realistic disks produced more young planet-forming bodies.<\/p>\n That pattern turns an old worry on its head for planet hunters, but only beyond the region where two stars pull too hard.<\/p>\n Why paired stars matter<\/p>\n About half of sun-like stars live with stellar partners, a long-running survey<\/a> of nearby systems found.<\/p>\n Astronomers call these systems binary stars, meaning two stars locked in orbit around a shared center.<\/p>\n Their gravity does not simply stir the gas; it can also help dense patches collapse faster.<\/p>\n For planet formation, the same tug that destroys order near the middle can organize material farther out in the disk.<\/p>\n Planets with two suns<\/strong><\/p>\n Worlds that circle both stars are circumbinary planets, a term for planets orbiting a stellar pair.<\/p>\n When astronomers confirmed Kepler-16b<\/a> in 2011, a Saturn-sized world orbiting two stars, the idea became real.<\/p>\n The NASA Exoplanet Archive<\/a>, which gathers confirmed worlds from NASA missions and research teams, now tracks thousands of planets around other stars.<\/p>\n Against that backdrop, finding more than 50 two-star planets no longer looks like a cosmic fluke, especially on wide orbits.<\/p>\n The forbidden center<\/p>\n Close-in orbits around a binary system have a well-known stability limit.<\/p>\n Gravity from two stars changes direction as they orbit, pulling nearby dust and gas into crossings that stop steady growth.<\/p>\n \u201cClose to a binary star it\u2019s simply too violent for planets to form,\u201d said Teasdale.<\/p>\n Beyond roughly 50 astronomical units \u2013 about 4.6 billion miles from the stars \u2013 the modeled disks calmed enough for gravity to split them.<\/p>\n How giant planets grow<\/p>\n Farther from the paired stars, gravitational instability<\/a> \u2013 gas becoming heavy enough to collapse under its own pull \u2013 took over.<\/p>\n Dense patches broke away from the disk, forming protoplanets \u2013 young bodies still feeding on nearby gas.<\/p>\n Because the outer disk stayed cooler, many starting masses fell near one to four times Jupiter\u2019s mass.<\/p>\n Continued feeding can still push some bodies toward brown dwarfs<\/a>, failed-star objects too heavy for planets but too small for star-like fusion.<\/p>\n The numbers tell a story<\/p>\n Across all simulations, the team produced 341 protoplanets in disks around single stars and stellar pairs.<\/p>\n Realistic paired-star disks made about nine protoplanets per disk, compared with 7.5 in single-star disks.<\/p>\n By final mass, about 71% of the realistic paired-star objects stayed in the planetary range.<\/p>\n Those figures matter because more starting bodies leave less gas for each one, making planet-sized endings more likely before they grow too massive.<\/p>\n Some worlds escape<\/p>\n Crowded young systems also threw some bodies away, creating free-floating planets \u2013 worlds that are no longer orbiting stars<\/a>.<\/p>\n Out of 341 protoplanets, 13 escaped the modeled systems, an overall ejection rate near 4%.<\/p>\n Tighter and more stretched-out stellar pairs caused more close encounters, which gave small bodies escape speed.<\/p>\n Those castoffs left at roughly 1 to 4 miles per second, fast enough to drift between stars for millions of years.<\/p>\n Limits of the planet simulations<\/p>\n Most simulated survivors ended up near 100 astronomical units, or about 9.3 billion miles from their stars.<\/p>\n Observed two-star planets cluster both close to their stars and far away, partly because planet-hunting methods are better at spotting certain orbits. <\/p>\n The model did not produce close-in planets because it tested stellar pairs separated by 465 million to 930 million miles.<\/p>\n That boundary keeps the result useful, but it shows close-in circumbinary planets likely need tighter stellar pairs or later migration.<\/p>\n Future research directions <\/p>\n Computer models simplify real systems, even when they track gas, gravity, heating, and repeated close encounters.<\/p>\n The simulations ended after 70% of each disk\u2019s material fell onto stars or young bodies.<\/p>\n Later movement after formation through gas or gravity could move planets inward, outward, or out of the system after the model stopped.<\/p>\n Future observations of young paired-star disks can test whether the brief bright phase appears where the simulations predict during observing campaigns.<\/p>\n Instead of blocking planet birth, paired stars can carve a violent center while helping outer gas make giant worlds.<\/p>\n Future searches will test how often that pathway works, especially for planets that orbit far from both stars.<\/p>\n The study is published in the journal Monthly Notices of the Royal Astronomical Society<\/a>.<\/p>\n Image Credit: Center for Astrophysics | Harvard & Smithsonian<\/p>\n \u2014\u2013<\/p>\n Like what you read? Subscribe to our newsletter<\/a> for engaging articles, exclusive content, and the latest updates.<\/p>\n Check us out on EarthSnap<\/a>, a free app brought to you by Eric Ralls<\/a> and Earth.com.<\/p>\n \u2014\u2013<\/p>\n","protected":false},"excerpt":{"rendered":"A new study has found that giant planets can form more easily around two young stars than around…\n","protected":false},"author":2,"featured_media":945369,"comment_status":"","ping_status":"","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[3844],"tags":[70,413,16,15],"class_list":{"0":"post-945368","1":"post","2":"type-post","3":"status-publish","4":"format-standard","5":"has-post-thumbnail","7":"category-space","8":"tag-science","9":"tag-space","10":"tag-uk","11":"tag-united-kingdom"},"share_on_mastodon":{"url":"https:\/\/pubeurope.com\/@uk\/116537254330176230","error":""},"_links":{"self":[{"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/posts\/945368","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/users\/2"}],"replies":[{"embeddable":true,"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/comments?post=945368"}],"version-history":[{"count":0,"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/posts\/945368\/revisions"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/media\/945369"}],"wp:attachment":[{"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/media?parent=945368"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/categories?post=945368"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/www.europesays.com\/uk\/wp-json\/wp\/v2\/tags?post=945368"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}