Academic literature on the topic 'Collection Étoiles'
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Journal articles on the topic "Collection Étoiles"
Sauvajol Buferne, Christine. "De la collection «?Plein Vent?» à Nos étoiles contraires, quarante?ans de littérature pour les adolescents." Enfances & Psy N° 82, no. 2 (2019): 69. http://dx.doi.org/10.3917/ep.082.0069.
Full textGlowczewski, Barbara, and Anne Querrien. "Les esprits de la terre en soulèvements." EcoRev' N° 55, no. 2 (December 28, 2023): 105–18. http://dx.doi.org/10.3917/ecorev.055.0105.
Full textDel Rossi, Sara. "L’humanisme panaméricain de Jacques Stephen Alexis." Il Tolomeo, no. 1 (December 19, 2019). http://dx.doi.org/10.30687/tol/2499-5975/2019/01/016.
Full text"Commission 35: Stellar Constitution (Constitution Des Étoiles)." Transactions of the International Astronomical Union 23, no. 1 (1997): 293–302. http://dx.doi.org/10.1017/s0251107x00027875.
Full textLarsen, Bjarne, Willem van Dooijeweert, Charles-Eric Durel, Caroline Denancé, Marcel Rutten, and Nicholas P. Howard. "SNP genotyping Dutch heritage apple cultivars allows for germplasm characterization, curation, and pedigree reconstruction using genotypic data from multiple collection sites across the world." Tree Genetics & Genomes 20, no. 4 (June 11, 2024). http://dx.doi.org/10.1007/s11295-024-01655-9.
Full textDissertations / Theses on the topic "Collection Étoiles"
Martin, Noël. "Modes collectifs et hydrodynamique dans la croûte interne des étoiles à neutrons." Thesis, Université Paris-Saclay (ComUE), 2016. http://www.theses.fr/2016SACLS251/document.
Full textNeutron stars have been extensively studied since Baade and Zwicky have proposed their existence in 1934. Their description is at the interface of numerous domains of physics, e.g., X-ray astrophysics, pulsar signal observation, general relativity and nowadays gravitational waves, solid state physics, and also nuclear physics. In this thesis we will concentrate on the nuclear physics description, especially of the inner crust. These stars are charaterized by their large mass from one to two solar masses, in a radius of 10 km. Their inner structure can be divded in three major layers: the outer crust, the inner crust and the core. The outer crust consists of nuclei coexisting with an electron gas to ensure charge neutrality. If one goes deeper into the crust, the ratio of neutrons with respect to the total nucleon number increases. Eventually, the excess of neutrons in the nuclei gets so high that they drip out from the nuclei and create a dilute neutron gas. From now on, we will speak of nuclear clusters instead of nuclei. This phenomenon defines the limit between the outer crust and the inner crust. This complicated structure and composition is at the origin of many characteristic properties of neutron stars. Hence, we will construct our work in three major parts. First, we start to account for the neutron gas surrounding the clusters, which we treat as uniform. Here, the neutron gas is assumed to be superfluid, and one can expect a Goldstone mode. This description will be done in the framework of QRPA. Second, we will focus on the study of properties of the clusters contained in the inner crust. Under these conditions we expect to see cystal of spheres, rods and plates of bound nucleons, that we will describe with the help of the ETF approximation. Third, we will finish by treating the interaction between the clusters and the gas with hydrodynamics. The results will be applied to astrophysics and in particular to glitches
M, Urban. "Appariement et mouvement collectif dans des systèmes à N corps fermioniques : gaz d'atomes froids et étoiles à neutrons." Habilitation à diriger des recherches, Université Paris Sud - Paris XI, 2012. http://tel.archives-ouvertes.fr/tel-00674944.
Full textMonrozeau, Charlotte. "Nouvelle méthode expérimentale dédiée à l'étude des modes collectifs dans les noyaux exotiquesInfluence de la superfluidité sur le temps de refroidissement d'une étoile à neutrons." Paris 11, 2007. http://www.theses.fr/2007PA112324.
Full textGiant monopole (GMR) and quadrupole (GQR) resonances have been measured in the 56Ni using inelastic scattering of 50 A. MeV deuteron at the Grand Accélérateur National d’Ions Lourds facility. This is the first experimental observation of isoscalar collective modes in a short-lived nucleus. The secondary beam was impinged on the active target Maya filled with a pure deuterium gas. Recoiling deuterons were detected in Maya and in a wall of nine silicon detectors. The GMR and GQR are centered at 19. 3(0. 5) MeV and 16. 2(0. 5) MeV, respectively. Corresponding angular distributions were extracted from 3 to 7 degrees in the centre of masse frame. DWBA analysis based on RPA transition densities yields the percentage of the energy weighted sum rule exhausted : 136(27) % for the GMR et 76(13) % for the GQR. A finite temperature Hartree-Fock-Bogoliubov model was implemented to describe the ten Wigner-Seitz cells which compose the inner crust of neutron stars and to microscopically c! alculate their specific heat. Calculations are performed with two contact pairing forces chosen to simulate the pairing properties of uniform neutron matter corresponding to the BCS approximation and to polarisation effects. Under the assumption of a rapid cooling of the core and an initial temperature of 100 keV in the inner crust, the cooling time of the star was estimated at 9 and 34 years, respectively
Monrozeau, Charlotte. "Nouvelle méthode expérimentale dédiée à l'étude des modes collectifs dans les noyaux exotiques.Influence de la superfluidité sur le temps de refroidissement d'une étoile à neutrons." Phd thesis, Université Paris Sud - Paris XI, 2007. http://tel.archives-ouvertes.fr/tel-00221226.
Full textUn modèle Hartree-Fock-Bogoliubov à température finie a été mis au point pour décrire les dix cellules de Wigner-Seitz composant l'écorce interne des étoiles à neutrons et calculer microscopiquement leur chaleur spécifique. Les calculs ont été réalisés en utilisant deux forces d'appariement de contact : une force reproduisant les propriétés d'appariement obtenues dans l'approximation BCS et une force simulant les effets d'écrantage du milieu. En faisant l'hypothèse d'un scénario de refroidissement rapide du cœur et une température initiale de 100 keV dans l'écorce, le temps de refroidissement de l'étoile a été estimé à 9 et 34 ans respectivement.
Books on the topic "Collection Étoiles"
n/a. Sous le paysage des étoiles (Collection Harlequin). Harlequin, 1987.
Find full textCassidy, Cathy. La belle étoile (Hors collection sériel) (French Edition). POCKET JEUNESSE, 2021.
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