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Histoire De La Cosmologie

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Histoire De La Cosmologie Histoire de la cosmologie Un cours offert aux étudiants de la Faculté des Lettres, de la Faculté de Biologie et de médecine, de la Faculté des Hautes études commerciales, de la Faculté de Géosciences et environnement, de la Faculté des Sciences sociales et politiques et de la Faculté de Théologie et de sciences des religions de l’Université de Lausanne dans le cadre de « Sciences au carré » Histoire de la cosmologie Histoire de la cosmologie le vendredi 19 mai 2017 le cours aura lieu Prof. Georges Meylan de 13h00 à 15h10 Laboratoire d’astrophysique Ecole Polytechnique Fédérale de Lausanne dans l’auditoire I du Cubotron = BSP Site web du laboratoire et du cours : http://lastro.epfl.ch Site web du cours : http://lastro.epfl.ch Histoire de la cosmologie le vendredi 19 mai 2017 le cours aura lieu de 13h00 à 15h10 Histoire de la cosmologie le dernier cours aura lieu le vendredi 26 mai 2017 de 13h00 à 15h10 dans la salle 2097 de l’Anthropole avec la présence de la Radio Télévision Suisse dans l’auditoire I du Cubotron = BSP Site web du cours : http://lastro.epfl.ch Histoire de la cosmologie 10 – Etoiles et galaxies Histoire de la cosmologie 10.1 Etoiles et amas d’étoiles 10.2 Naissance des étoiles examen écrit portant sur la matière du cours 10.3 Diagrammes H-R et C-M vendredi 9 juin 2017 10.4 Mort des étoiles 10.5 Nébuleuse ou galaxie de 13h15 à 15h00 10.6 La Voie lactée, notre Galaxie 10.7 Classification morphologique des galaxies 10.8 Groupes et amas de galaxies dans l’auditoire Internef # 263 Site web du cours : http://lastro.epfl.ch Voir le fichier 10-EtoilesetGalaxies.pdf sur le site web du laboratoire et du cours : http://lastro.epfl.ch Histoire de la cosmologie 10.1 10 – Etoiles et galaxies Bibliographie succincte Etoiles et amas d’étoiles • CELNIKIER, Ludwik M. Find a Hotter Place ! A History of Nuclear Astrophysics. London : World Scientific, 2006. • CHABERLOT, Frédéric. La Voie Lactée : Histoire des conceptions et des modèles de notre Galaxie des temps anciens aux années 1930. Paris : CNRS Editions, 2003. • COLLIN-ZAHN, Suzy. Des quasars aux trous noirs. Paris : EDP, 2009. • LEQUEUX, James. Naissance, évolution et mort des étoiles. Paris: EDP, 2011 • LUMINET, Jean-Pierre. Le destin de l’Univers. Paris : Fayard, 2006. APOD APOD 2010 April 18 2010 April 18 Grande Grande éruption éruption solaire solaire Satellite Stereo Satellite Stereo NASA NASA Notre Soleil est une étoile isolée rayon = 700’000 km rayon = 700’000 km à 150’000’000 km de la Terre à 150’000’000 km de la Terre FonctionPoint Spread Func0on = PSF d’étalement du point : PSF Point Spread Function Amas ouvert h et Per Un amas ouvert tel que les Pléiades χ contient quelques centaines d’étoiles L’amas globulaire 47 Tucanae Un amas globulaire contient quelques millions d’étoiles Un amas globulaire tel que ω Centauri Un amas globulaire tel que ω Centauri contient quelques millions d’étoiles contient quelques millions d’étoiles WFI camera at the 2.2-m MPG-ESO telescope at La Silla Observatory WFI camera at the 2.2-m MPG-ESO telescope at La Silla Observatory Un amas globulaire tel que ω Centauri Un amas globulaire tel que ω Centauri contient quelques millions d’étoiles contient quelques millions d’étoiles WFI camera at the 2.2-m MPG-ESO telescope at La Silla Observatory l’amas globulaire géant Omega Centauri VST ESO Paranal Chili l’amas globulaire géant Omega Centauri VST ESO Paranal Chili June 2011 June 2011 l’amas globulaire géant Omega Centauri VST ESO Paranal Chili Visible/infrared comparison views of the newly discovered globular cluster VVV CL001 June 2011 ESO VISTA October 2011 Problème à N corps Les trois lois de la mécanique newtonienne • Lex prima : de Newton Let a number, N, of particles interact classically through Newton's Laws of Motion and Newton's inverse square Law of Gravitation. The resulting equations of motion provide Tout corps persévère dans l’état de repos ou de mouvement rectiligne an approximate mathematical model with numerous applications in astrophysics, uniforme à moins que quelque force n’agisse sur lui et ne le contraigne à including the motion of the moon and other bodies in the Solar System (planets, changer d’état » asteroids, comets and meteor particles); stars in stellar systems ranging from binary and other multiple stars to star clusters and galaxies; and the motion of dark matter particles in cosmology. For N=1 and N=2 the equations can be solved analytically. The case N=3 • Lex secunda : de Newton provides one of the richest of all unsolved dynamical problems -- the general three-body Les changements qui arrivent dans le mvt sont proportionnels à la force problem. For problems dominated by one massive body, as in many planetary problems, motrice et se font dans la ligne droite dans laquelle cette force a été approximate methods based on perturbation expansions have been developed. In stellar imprimée » dynamics, astrophysicists have developed numerous numerical and theoretical approaches to the problem for larger values of N, including treatments based on the Boltzmann equation and the Fokker-Planck equation; such N-body systems can also be • Lex tertia : de Newton modelled as self-gravitating gases, and thermodynamic insights underpin much of our L’action est toujours égale et opposée à la réaction, i.e., que les actions de qualitative understanding. deux corps l’un sur l’autre sont toujours égales et de direction opposées » Douglas Heggie http://fr.arxiv.org/abs/astro-ph/0503600v2 Problème à deux corps Problème à deux corps Problème à deux corps Problème à deux corps Problème à deux corps 10.2 IC 2948 / IC 2944 Running Chicken Naissance des étoiles Nebula Gum 39 & Gum 41 effondrement gravitationnel de nuages de gaz et de poussière Zoom into IC 2948 showing a group of thick clouds of dust known as the Thackeray globules la turbulence crée une hiérarchie de condensations comme la turbulence diminue localement, comme la turbulence diminue localement, la contraction s’amorce dans chacune des condensations la contraction s’amorce dans chacune des condensations tandis que des régions se contractent, tandis que des régions se contractent, des condensations individuelles s’effondrent et forme des étoiles des condensations individuelles s’effondrent et forme des étoiles tandis que des régions se contractent, tandis que des régions se contractent, des condensations individuelles s’effondrent et forme des étoiles des condensations individuelles s’effondrent et forme des étoiles dans les amas d’étoiles denses, des condensations peuvent fusionner dans les amas d’étoiles denses, des condensations peuvent fusionner lors de leur effondrement et donc contenir plusieurs proto-étoiles lors de leur effondrement et donc contenir plusieurs proto-étoiles dans les amas d’étoiles denses, des condensations peuvent fusionner dans les amas d’étoiles denses, des condensations peuvent fusionner lors de leur effondrement et donc contenir plusieurs proto-étoiles lors de leur effondrement et donc contenir plusieurs proto-étoiles dans les amas d’étoiles denses, des condensations peuvent fusionner dans les amas d’étoiles denses, lors de leur effondrement et donc contenir plusieurs proto-étoiles les effets dynamique à N-corps influencent la croissance des masses les rencontres gravitationnelles les vents stellaires mettent fin à la formation d’étoiles peuvent induire l’éjection d’étoiles il résulte un amas d’étoiles, parfois entouré d’une région HII NGC 602 in the LMC Hubble NASA/ESA 30 Doradus HST NASA/ESA M78 VISTA/ESO Equilibre hydrostatique Equilibre hydrostatique Durant la séquence principale, l'étoile est en équilibre hydrostatique, elle subit deux forces qui s'opposent et la maintiennent en équilibre : d'une part les réactions thermonucléaires qui ont lieu au cœur de l'étoile exercent une pression (gazeuse et radiative) qui tend à la faire augmenter de volume, ce qui entraîne une diminution de la température de l'étoile ; d'autre part les forces de gravité reprennent le dessus lorsque la pression (gazeuse et radiative) diminue, elles ont tendance à la faire se contracter et donc à augmenter la température de l'étoile, de sorte que les réactions nucléaires s'intensifient et que la pression (gazeuse et radiative) augmente à nouveau. en tout point, le gradient de pression équilibre la gravitation en tout point, le gradient de pression équilibre la gravitation La constellation d’Orion La constellation d’Orion contient une pouponnière d’étoiles La nébuleuse d’Orion vue par le Hubble Space Telescope Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA 1995 visible IR Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA 2015 Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA 2015 VISIBLE IR 2015 WFC3 1995 WFPC2 Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA 2015 Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA 1995 Gas in the Eagle Nebula (M16) : Pillars of Creation in a Star-Forming Region NASA/ESA 2015 HST NASA/ESA Carina HST NASA/ESA formation d’une étoile et d’un disque, lieu de futures planètes Illustration of disk evolution in relation to planet formation Herbig-Haro 110 is a geyser of hot gas from a newborn star that splashes up against and ricochets off the dense core of a cloud of molecular H. NASA/ESA 3 July 2012 Planet formation: this image illustrates a protoplanetary disk undergoing spiral wave instabilities as it would appear using a millimeter wave telescope.
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