{"id":2184,"date":"2026-10-04T18:22:56","date_gmt":"2026-10-04T16:22:56","guid":{"rendered":"https:\/\/latelierastro.com\/?p=2184"},"modified":"2026-10-05T15:07:18","modified_gmt":"2026-10-05T13:07:18","slug":"perseides","status":"publish","type":"post","link":"https:\/\/latelierastro.com\/?p=2184","title":{"rendered":"PERSEIDES"},"content":{"rendered":"\n<article class=\"article-ifn\">\n<header>\n<p class=\"ifn-category\">D\u00e9cryptage \u00b7 Pers\u00e9ides<\/p>\n<h1>Que sont les \u00e9toiles filantes ?<\/h1>\n<p class=\"ifn-subtitle\">D\u2019o\u00f9 viennent leurs couleurs ?<\/p>\n<p class=\"ifn-author\">Par Beno\u00eet Saintot<\/p>\n<\/header>\n<section id=\"introduction\">\n<p>Au-del\u00e0 de la premi\u00e8re impression \u00ab Vitesse lumi\u00e8re, Chewbacca ! \u00bb, sur cette image, les Pers\u00e9ides semblent toutes converger vers un m\u00eame point : leur <strong>radiant<\/strong>, situ\u00e9 dans la constellation de Pers\u00e9e. Mais derri\u00e8re ces traits lumineux se cache une physique bien plus complexe qu\u2019un simple \u00ab caillou qui br\u00fble \u00bb.<\/p>\n<p>Une \u00e9toile filante appara\u00eet lorsqu\u2019un <strong>m\u00e9t\u00e9oro\u00efde<\/strong> p\u00e9n\u00e8tre dans la haute atmosph\u00e8re \u00e0 tr\u00e8s grande vitesse. Les Pers\u00e9ides arrivent \u00e0 environ <strong>59 km\/s<\/strong>.<\/p>\n<\/section>\n<nav aria-label=\"Sommaire de l\u2019article\">\n<p><strong>Dans cet article<\/strong><\/p>\n<ul>\n<li><a href=\"#compression\">Compression, plasma et vaporisation<\/a><\/li>\n<li><a href=\"#excitation\">Excitation : l\u2019origine des raies color\u00e9es<\/a><\/li>\n<li><a href=\"#ionisation\">Puis vient l\u2019ionisation<\/a><\/li>\n<li><a href=\"#atmosphere\">L\u2019atmosph\u00e8re participe elle aussi<\/a><\/li>\n<li><a href=\"#recombinaison\">Apr\u00e8s le passage : la recombinaison<\/a><\/li>\n<li><a href=\"#vitesse\">Une question de vitesse<\/a><\/li>\n<\/ul>\n<\/nav>\n<section id=\"compression\">\n<h2>1 \u2014 Compression, plasma et vaporisation<\/h2>\n<p>\u00c0 cette vitesse, le m\u00e9t\u00e9oro\u00efde comprime brutalement l\u2019air devant lui. Le gaz est port\u00e9 \u00e0 plusieurs milliers de degr\u00e9s et devient partiellement ionis\u00e9 : un <strong>plasma<\/strong> se forme autour du corps.<\/p>\n<p>Cette \u00e9nergie provoque l\u2019<strong>ablation<\/strong> du m\u00e9t\u00e9oro\u00efde : sa surface chauffe et se vaporise, lib\u00e9rant des atomes de sodium, magn\u00e9sium, fer, calcium\u2026<\/p>\n<\/section>\n<section id=\"excitation\">\n<h2>2 \u2014 Excitation : l\u2019origine des raies color\u00e9es<\/h2>\n<p>Les collisions excitent les \u00e9lectrons de ces atomes. Lorsqu\u2019ils reviennent vers un niveau d\u2019\u00e9nergie inf\u00e9rieur, ils \u00e9mettent des photons \u00e0 des longueurs d\u2019onde bien pr\u00e9cises.<\/p>\n<p>Chaque \u00e9l\u00e9ment poss\u00e8de donc sa propre signature spectrale :<\/p>\n<ul>\n<li><strong>Sodium \u2248 589 nm<\/strong> : jaune-orang\u00e9 ;<\/li>\n<li><strong>Magn\u00e9sium \u2248 518 nm<\/strong> : vert ;<\/li>\n<li><strong>Fer<\/strong> : nombreuses raies r\u00e9parties dans le visible, contribuant notamment aux zones blanch\u00e2tres ;<\/li>\n<li>D\u2019autres \u00e9l\u00e9ments compl\u00e8tent le spectre.<\/li>\n<\/ul>\n<\/section>\n<section id=\"ionisation\">\n<h2>3 \u2014 Puis vient l\u2019ionisation<\/h2>\n<p>Lorsque les collisions deviennent suffisamment \u00e9nerg\u00e9tiques, elles peuvent arracher des \u00e9lectrons aux atomes : ils deviennent des <strong>ions<\/strong>, qui poss\u00e8dent \u00e0 leur tour leurs propres raies d\u2019\u00e9mission.<\/p>\n<ul>\n<li><strong>Ca II \u2014 393,4 et 396,8 nm<\/strong> : calcium ionis\u00e9, dans le <strong>violet profond<\/strong>, \u00e0 la limite du proche ultraviolet ;<\/li>\n<li><strong>Mg II \u2014 448,1 nm<\/strong> : magn\u00e9sium ionis\u00e9, dans le <strong>bleu<\/strong>, donc bien dans le spectre visible ;<\/li>\n<li><strong>Si II \u2014 notamment vers 634,7 nm<\/strong> : silicium ionis\u00e9, dans le <strong>rouge<\/strong>.<\/li>\n<\/ul>\n<p>Excitation et ionisation ne sont pas deux r\u00e9gimes s\u00e9par\u00e9s : elles coexistent, leur importance \u00e9voluant progressivement avec l\u2019\u00e9nergie disponible.<\/p>\n<\/section>\n<section id=\"atmosphere\">\n<h2>4 \u2014 L\u2019atmosph\u00e8re participe elle aussi<\/h2>\n<p>La lumi\u00e8re ne provient pas uniquement du m\u00e9t\u00e9oro\u00efde. L\u2019<strong>azote et l\u2019oxyg\u00e8ne atmosph\u00e9riques<\/strong> sont eux aussi excit\u00e9s et ionis\u00e9s et ajoutent leurs \u00e9missions \u00e0 celles de la mati\u00e8re vaporis\u00e9e.<\/p>\n<p>La couleur observ\u00e9e est donc le r\u00e9sultat d\u2019un m\u00e9lange entre les \u00e9missions du m\u00e9t\u00e9oro\u00efde et celles de l\u2019atmosph\u00e8re.<\/p>\n<figure>\n<img src=\"https:\/\/latelierastro.com\/wp-content\/uploads\/2026\/10\/fb39750d-d50b-4fd2-b52e-c0cf3a91d3bd-scaled.png\" alt=\"Illustration annot\u00e9e des \u00e9missions lumineuses et des couleurs d\u2019une Pers\u00e9ide\" loading=\"lazy\" decoding=\"async\">\n<figcaption>D\u00e9cryptage des couleurs d\u2019une Pers\u00e9ide.<\/figcaption>\n<\/figure>\n<\/section>\n<section id=\"recombinaison\">\n<h2>5 \u2014 Et apr\u00e8s le passage : la recombinaison<\/h2>\n<p>Dans le sillage subsiste bri\u00e8vement une colonne de gaz ionis\u00e9. En se refroidissant, ions et \u00e9lectrons se <strong>recombinent<\/strong>, produisant encore de la lumi\u00e8re. Sur les m\u00e9t\u00e9ores les plus brillants, ce ph\u00e9nom\u00e8ne participe aux <strong>tra\u00een\u00e9es persistantes<\/strong> observables apr\u00e8s leur passage.<\/p>\n<\/section>\n<section id=\"vitesse\">\n<h2>Une question de vitesse<\/h2>\n<p>Il n\u2019existe pas de seuil parfaitement net, mais on peut retenir quelques ordres de grandeur :<\/p>\n<ul>\n<li><strong>11\u201320 km\/s<\/strong> : excitation largement dominante ;<\/li>\n<li><strong>20\u201330 km\/s<\/strong> : ionisation de plus en plus importante ;<\/li>\n<li><strong>&gt; 30\u201340 km\/s<\/strong> : excitation et ionisation deviennent toutes deux tr\u00e8s fortes.<\/li>\n<\/ul>\n<p>\u00c0 <strong>59 km\/s<\/strong>, les Pers\u00e9ides appartiennent donc clairement aux m\u00e9t\u00e9ores rapides, capables d\u2019ioniser fortement leur propre mati\u00e8re comme l\u2019atmosph\u00e8re.<\/p>\n<p>Sur cette image, les variations du jaune-orang\u00e9 au blanc puis au vert t\u00e9moignent ainsi de l\u2019\u00e9volution de l\u2019ablation, de la composition des mat\u00e9riaux vaporis\u00e9s, de leur excitation et de leur ionisation, mais aussi de la contribution de l\u2019atmosph\u00e8re.<\/p>\n<p>Chaque Pers\u00e9ide est finalement, pendant une fraction de seconde, un v\u00e9ritable <strong>spectre naturel<\/strong> d\u2019un fragment de mati\u00e8re interplan\u00e9taire traversant notre atmosph\u00e8re.<\/p>\n<\/section>\n<\/article>\n\n","protected":false},"excerpt":{"rendered":"<p>D\u00e9cryptage \u00b7 Pers\u00e9ides Que sont les \u00e9toiles filantes ? D\u2019o\u00f9 viennent leurs couleurs ? Par Beno\u00eet Saintot Au-del\u00e0 de la premi\u00e8re impression \u00ab Vitesse lumi\u00e8re, Chewbacca ! \u00bb, sur cette image, les Pers\u00e9ides semblent toutes converger vers un m\u00eame point : leur radiant, situ\u00e9 dans la constellation de Pers\u00e9e. Mais derri\u00e8re ces traits lumineux se&hellip;&nbsp;<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_uag_custom_page_level_css":"","neve_meta_sidebar":"","neve_meta_container":"","neve_meta_enable_content_width":"","neve_meta_content_width":0,"neve_meta_title_alignment":"","neve_meta_author_avatar":"","neve_post_elements_order":"[\"content\",\"comments\"]","neve_meta_disable_header":"","neve_meta_disable_footer":"","neve_meta_disable_title":"","neve_meta_reading_time":"","footnotes":""},"categories":[1],"tags":[],"class_list":["post-2184","post","type-post","status-publish","format-standard","hentry","category-non-classe"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v28.6 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>Pers\u00e9ides : comprendre les \u00e9toiles filantes \u2014 L\u2019Atelier Astro<\/title>\n<meta name=\"description\" content=\"Que sont les Pers\u00e9ides et d\u2019o\u00f9 viennent leurs couleurs ? 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D\u2019o\u00f9 viennent leurs couleurs ? Par Beno\u00eet Saintot Au-del\u00e0 de la premi\u00e8re impression \u00ab Vitesse lumi\u00e8re, Chewbacca ! \u00bb, sur cette image, les Pers\u00e9ides semblent toutes converger vers un m\u00eame point : leur radiant, situ\u00e9 dans la constellation de Pers\u00e9e. Mais derri\u00e8re ces traits lumineux se&hellip;&nbsp;","_links":{"self":[{"href":"https:\/\/latelierastro.com\/index.php?rest_route=\/wp\/v2\/posts\/2184","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/latelierastro.com\/index.php?rest_route=\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/latelierastro.com\/index.php?rest_route=\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/latelierastro.com\/index.php?rest_route=\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/latelierastro.com\/index.php?rest_route=%2Fwp%2Fv2%2Fcomments&post=2184"}],"version-history":[{"count":3,"href":"https:\/\/latelierastro.com\/index.php?rest_route=\/wp\/v2\/posts\/2184\/revisions"}],"predecessor-version":[{"id":2188,"href":"https:\/\/latelierastro.com\/index.php?rest_route=\/wp\/v2\/posts\/2184\/revisions\/2188"}],"wp:attachment":[{"href":"https:\/\/latelierastro.com\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=2184"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/latelierastro.com\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=2184"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/latelierastro.com\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=2184"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}