{"id":1590,"date":"2020-06-10T04:11:40","date_gmt":"2020-06-10T02:11:40","guid":{"rendered":"http:\/\/spectro-uvex.tech\/?p=1590"},"modified":"2022-12-03T18:41:52","modified_gmt":"2022-12-03T17:41:52","slug":"rr-lyrae","status":"publish","type":"post","link":"https:\/\/spectro-uvex.tech\/?p=1590","title":{"rendered":"RR Lyrae"},"content":{"rendered":"\t\t
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Les \u00e9toiles RR lyrae<\/a>\u00a0sont des \u00e9toiles massives qui arrivant en fin de vie passe par une phase d’instabilit\u00e9. Ce sont des \u00e9toiles pulsantes avec une p\u00e9riode de l’ordre de la journ\u00e9e. Leur p\u00e9riode est une fonction simple de leur luminosit\u00e9 intrins\u00e8que ce qui en fait des chandelles standard pour la mesure des distances dans l’univers. On les trouvent en nombre dans les amas globulaires ce qui permis par exemple \u00e0 Walter Baade de calculer la distance de l’amas globulaire NGC 6522 en 1951<\/a>.<\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t

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Voici un exemple d’\u00e9tude faite gr\u00e2ce \u00e0 l’UVEX3, l’\u00e9toile variable RR lyrae, arch\u00e9type des \u00e9toiles du m\u00eame nom, qui est suffisamment brillante pour r\u00e9aliser des spectres \u00e0 haute fr\u00e9quences temporelles. Sa magnitude varie entre 7 et 8 sur une p\u00e9riode de 13 heures et 36 min, son type spectral varie entre A5 et F7 dans le m\u00eame temps. Pendant sa p\u00e9riode, l’enveloppe ext\u00e9rieure gonfle et se refroidit sa couleur rougie, pour ensuite se r\u00e9tracter et se r\u00e9chauffer, sa couleur bleuie. Au d\u00e9but de la phase de contraction lorsque les couches sup\u00e9rieures s’effondrent sur les couches internes de l’\u00e9toile, il se forme une onde de choc qui se traduit par un minimum d\u2019absorption dans les raies de Balmer. Le moment de ce choc constitue le maximum spectroscopique.<\/span><\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t

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Animation de l'\u00e9volution du spectre de RR Lyr. Lorsque l'onde de choc appara\u00eet, la raie H alpha dispara\u00eet presque, H b\u00e9ta et les autres raies sont r\u00e9duites dans une moindre mesure.<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t
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Spectre 2D de la s\u00e9quence, d\u00e9but de la s\u00e9quence 22h45 le 5 juin 2020 fin au lever de soleil \u00e0 5h07 HL. On remarque autour de la date 2459006,464 le passage de l'onde de choc et autour de 2459006.514 le maximum de temp\u00e9rature, qui correspond au maximum photom\u00e9trique.<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t
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H B\u00e9ta - 300s<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t
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<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t
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Le pr\u00e9traitement des images de RR lyr commence de facon standard comme si on cherchait a additionner toutes les poses pour avoir un spectre unique de la time s\u00e9rie.<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t
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Les fichiers temporaires @rr*.fits sont ensuite normalis\u00e9s par la commande L_Norm entre 5000 et 5200A (Au pr\u00e9alable ne pas oublier de d\u00e9sactiver la supression des fichiers temporaires dans configuration)<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t
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L'onglet Animation dans ISIS permet de cr\u00e9er une animation du profil de raies @anim-c.gif et une image 2D color\u00e9e @anim-c.fits ainsi que tous les profils de raies au format png.<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t
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Pendant l'acquisition - Prism dans le sens horaire, RR lyr autoguidage Asi ZWO 178 MM 1s de pose (gain \u00e0 400), controle de la lampe de calibration, resp. panneaux de contr\u00f4le de la ZWO 178MM, DMK 41, ATIK 314L, Histogramme, prise de vue chercheur electronique (DMK41 + chercheur Geoptik 10x50), Spectre de RR Lyrae ATIK 314L. Au centre carte de champ.<\/figcaption>\n\t\t\t\t\t\t\t\t\t\t<\/figure>\n\t\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t
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R\u00e9f\u00e9rences<\/h2>\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t
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Comment animer une s\u00e9quence de spectres: http:\/\/www.astrosurf.com\/buil\/isis\/animation\/animation_fr.htm<\/a><\/span><\/p>\n

Comment faire une animation et un spectre 2D d’une s\u00e9quence de spectres C.BUIL:\u00a0http:\/\/www.astrosurf.com\/buil\/isis\/isis_tuto\/tuto4.htm<\/a><\/span><\/p>\n

Eph\u00e9m\u00e9rides de RR Lyrae, maximums photom\u00e9triques et maximums spectroscopiques:http:\/\/wsdiscovery.free.fr\/rrlyr\/index.php<\/a><\/span><\/p>\n

Suivi spectroscopique de RR lyrae en 2013 C.BUIL: https:\/\/fr.wikipedia.org\/wiki\/RR_Lyrae<\/a><\/span><\/p>\n

Une vid\u00e9o de l’ESO montrant des RR Lyrae dans la voie lact\u00e9e:\u00a0https:\/\/www.eso.org\/public\/france\/videos\/eso1636a\/<\/a><\/span><\/p>\n

\u00a0<\/p>\t\t\t\t\t\t\t\t<\/div>\n\t\t\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/div>\n\t\t\t\t\t<\/div>\n\t\t<\/section>\n\t\t\t\t<\/div>\n\t\t","protected":false},"excerpt":{"rendered":"

Les \u00e9toiles RR lyrae sont des \u00e9toiles massives qui arrivant en fin de vie passe par une phase d’instabilit\u00e9. Ce sont des \u00e9toiles pulsantes avec une p\u00e9riode de l’ordre de la journ\u00e9e. Leur p\u00e9riode est une fonction simple de leur luminosit\u00e9 intrins\u00e8que ce qui en fait des chandelles standard pour la mesure des distances dans l’univers. 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