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Toward Predictive Scenarios of Planetary Migration Clément Baruteau

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Toward Predictive Scenarios of Planetary Migration Clément Baruteau Toward predictive scenarios of planetary migration Clément Baruteau To cite this version: Clément Baruteau. Toward predictive scenarios of planetary migration. Astrophysics [astro-ph]. Observatoire de Paris, 2008. English. tel-00334456 HAL Id: tel-00334456 https://tel.archives-ouvertes.fr/tel-00334456 Submitted on 27 Oct 2008 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Ecole Doctorale d’Astronomie et d’Astrophysique d’Ile de France These` de Doctorat pr´esent´ee par Cl´ement Baruteau pour obtenir le grade de docteur de l’Observatoire de Paris en Astronomie et Astrophysique Vers des scenarios´ predictifs´ de la migration planetaire´ dirig´ee par Fr´ed´eric Masset et soutenue le 02 octobre 2008 devant la commission compos´ee de Dr. Gennaro D’Angelo ..............................rapporteur Prof. Jean-Marc Hure´ ..............................examinateur Prof. Wilhelm Kley ..................................rapporteur Prof. Douglas Lin ....................................rapporteur Dr. Fr´ed´eric Masset . directeur de th`ese Prof. Bruno Sicardy . .examinateur, pr´esident du jury Prof. Caroline Terquem ...........................examinatrice Service d’Astrophysique du CEA Saclay [email protected] Cl´ement Baruteau Toward predictive scenarios of planetary migration – CEA Saclay – Cover page : The perturbed surface density of a gaseous protoplanetary disc, obtained from a two-dimensional hydrodynamic calculation. The white circle at the center of the picture encloses the central star and the disc parts close to the star. The protoplanetary disc is perturbed by a low-mass planet (the brightest point on the right-hand side of the picture) that excites a spiral-shaped wake propagating in the disc. The planet induces an additional perturbation in a narrow annulus located close to the star-planet separation. Copyright – Cl´ement Baruteau 2008 Remerciements / Acknowledgments Je tiens d’abord `aremercier Pierre-Olivier Lagage pour m’avoir accueilli dans son service lors de ma th`ese. Je lui suis reconnaissant, ainsi qu’`ala direction de l’Irfu, de m’avoir permis de s´ejourner au Mexique, d’avoir assur´eles frais de trajet et de mission sur place. J’esp`ere que le pr´esent manuscrit, et le travail r´ealis´edurant ces trois ans de th`ese, auront ´et´e`ala hauteur de la confiance qui m’a ´et´eaccord´ee. Un grand merci aux personnes du service qui m’ont aid´e`aavancer au cours de ces trois ans. A Michel Tagger pour ses conseils sur l’auto-gravit´e. A Romain Teyssier et Thierry Foglizzo pour leurs explications et intuitions sur les discontinuit´es de contact. A Edouard Audit pour sa patience quant `amon utilisation surintensive de Godunov. Un remerciement plus particulier `aS´ebastien Fromang pour ses conseils pr´ecieux et avis´es sur des points aussi vari´es que la conception d’un poster, la r´edaction de dossiers pour les offres de postdocs ou la pr´eparation de la soutenance de th`ese. L’avanc´ee a aussi ´et´ehumaine, ainsi j’adresse aux ´etudiants (et assimil´es !) mes plus sinc`eres voeux de bonheur et de r´eussite : notre sp´ecialiste `es kouign amann Alain Gueguen, Ana Palacios, Matthias Gonzalez y el amigo Fabio Acero con los que fue un placer hablar espa˜nol, Ana¨elle Maury, Micka¨el Coriat, Lionel Prat, sans qui j’aurais eu du mal `aassister `a la conf´erence en Chine, J´erˆome Guilet, Benjamin Braconnier, mes super cobureaux Yohan Dubois et Benoˆıt Commer¸con, que je remercie d’avoir relu le premier chapitre de ce manuscrit, Estelle Deau, notre coureur Henri Triou, Ivan Debono, Savita Mathur, Julien Salmon, M´ed´eric Boquien, Laur`ene Jouve, Lilia Solovyeva, Guillaume Loisel, Pierrick Abrial, Jo¨el Berge´, Sandrine Pires, Vincent Duez, Nazirah Jetha, Arnaud Woiselle. Un petit mot enfin pour Jules Casoli, compagnon d’aventures mexicaines, `aqui je souhaite une th`ese brillante avec Fr´ed´eric. I wish to thank the following people for their help and comments on my research work. A special thank to Takayuki Muto and Sijme-Jan Paardekooper for insightful comments on the corotation torque calculation in adiabatic discs. Aur´elien Crida for clarifying remarks on the migration of massive planets. Alessandro Morbidelli for a thorough reading of the two articles written during my thesis. Andres Carmona for an illuminating question about self-gravity during the IAU meeting in Suzhou. It was my honor to have them as committee members. Gennaro D’Angelo for a detailed reading of the manuscript, and for insightful comments and questions I appreciated much. Jean-Marc Hure´ qui a r´ev´el´een moi un goˆut certain pour les simulations hydrodynamiques. Wilhelm Kley for fruitful discussions during the conferences I attended to. Douglas Lin for his reading of the manuscript, and for having quickly enrolled me as a postdoc at UCSC ! Bruno Sicardy pour m’avoir passionn´epour les r´esonances de Lindblad lors de son cours de Master, et pour m’avoir inspir´eun travail sur la capture en r´esonance de Pluton. Et enfin Caroline Terquem pour ses commentaires avis´es sur les disques radiatifs. J’en viens `arendre hommage `ames amis. Aux complices Guilhem Lavaux, Elisabetta Micelotta, Gwena¨el Boue´, que je remercie d’avoir relu les deux premiers chapitres de ce manuscrit, Isabelle et S´ebastien Esnault, Herv´e Boisson et sa famille. Une pens´ee toujours ´emue `anotre promotion du Master de l’Observatoire : Kevin Baillie, Virginie Batista, Gwena¨el Boue´, encore lui, Josselin Desmars, Jordi Fontdecaba i Baig, Julie Gayon, vi Magali Maroccia, Arielle Moullet, Christophe Ouzeau et Arianne Sauvenier. Viennent encore Aur´elien Benoit-Levy, Kumiko Kotera, Elisabete Da Cunha, Sara Caucci, pour son cours d’italien, la famille Rimada pour son accueil chaleureux au Mexique et la famille Hurpin. A tous je souhaite mes plus vifs voeux de bonheur. Une pens´ee chaleureuse `a ma famille d’hier, d’aujourd’hui et de demain : Catherine, Georges, Maurice, Nicole, Claire, Camille, Fran¸cois, Gabriel, H´el`ene, Gerald, Agn`es, Stefan, Alice, Matthieu, et Sarah, mi vida. Peut-ˆetre les th`eses se suivent et se ressemblent. Comme toi, j’ai gard´ele meilleur pour la fin. A toi, Fr´ed´eric Masset, mon directeur de th`ese, pour m’avoir aiguill´esur le chemin de la recherche. Travailler avec toi a ´et´eune exp´erience enthousiasmante et ˆocombien enrichissante. Je mesure la chance que j’ai eue de pouvoir b´en´eficier de tes intuitions, de tes commentaires et discussions ´eclair´es, de ta disponibilit´e`atoute ´epreuve, mˆeme `al’autre bout de la Terre. Merci aussi pour ta relecture de ce manuscrit. Comme le jour de la soutenance, je vais te vieillir un peu : j’esp`ere ˆetre comme toi dans quinze ans ! Vers des sc´enarios pr´edictifs de la migration plan´etaire La d´etection r´ecente des exoplan`etes a fourni un formidable laboratoire d’exp´erimentation des th´eories de formation et d’´evolution plan´etaire. Un r´esultat troublant est la proportion de plan`etes g´eantes situ´ees plus pr`es de leur ´etoile que ne l’est Mercure de notre Soleil ! Si, comme il est admis, ces plan`etes se sont form´ees `aplus grande distance de l’´etoile dans le disque protoplan´etaire, il reste `aexpliquer comment elles ont pu s’en rapprocher. Remarquablement, une telle th´eorie est apparue bien avant la d´ecouverte de la premi`ere exoplan`ete. Elle explique que sous l’interaction avec le disque protoplan´etaire, les plan`etes se rapprochent de leur ´etoile en spiralant. On parle de migration plan´etaire. De nombreuses ´etudes ont montr´eque le temps de migration des plan`etes de faible masse est bien plus court que le temps de dissipation du disque. Toutes les plan`etes devraient avoir migr´ejusqu’`aleur ´etoile ! Ce qui est d´ej`aremis en cause par notre Syst`eme Solaire. Afin d’inscrire la migration plan´etaire dans un sc´enario pr´edictif de formation et d’´evolution plan´etaire, il est primordial d’affiner notre compr´ehension de l’interaction disque-plan`ete. La prise en compte de l’auto-gravit´edu disque est un exemple de progr`es en ce sens. Je montre que n´egliger l’auto-gravit´econduita ` surestimer significativement le couple diff´erentiel de Lindblad. Une autre branche explor´ee dans cette th`ese est l’impact des processus thermiques sur la migration. Je montre que l’´evolution thermodynamique du disque g´en`ere une contribution suppl´ementaire au couple de corotation, capable de ralentir consid´erablement, voire de renverser, la migration des plan`etes de faible masse. Mots cl´e: migration plan´etaire, disques protoplan´etaires, hydrodynamique, analyse lin´eaire, simulations num´eriques Toward predictive scenarios of planetary migration The recent detection of extrasolar planets has provided an exciting opportunity to test our theories of planet formation and evolution. An impressive result is the significant proportion of giant planets located much closer to their star than Mercury is from our own Sun! These planets should have formed further out in the protoplanetary disc, thus one needs to explain how they could move closer to their host star. Remarkably enough, such an explanation was proposed well before the discovery of the first exoplanet. It considered the interaction between a planet and the protoplanetary disc, which leads to a decrease of the planet’s semi-major axis.
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