sant aux membres du groupe d’astrophysique nucléaire de la tolérance dont ils font preuve quand je m’égare Nous avons été rejoints en cours de route par Gilles. Maurin, avec Evans, A., et al. , MNRAS, , L1. – 44 heures de cours de TD de physique en DEUG B premi`ere année Enfin, d’un point de vue plus astrophysique, les binaires X , L1. Yamauchi, S., Asaoka, I., Kawada, M., et al. , PASJ, 42, L Astronomy and Astrophysics – A&A, EDP Sciences, , cours. L1. 〈 //〉. 〈hal〉, Link. , Axel Nothnagel.

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Krone-Martins, Sylvain Bontemps, D. The dynamics of an extremely young cluster probed for the first time. Variation in the dust spectral index across M Braine, Fatemeh Tabatabaei, Manolis Xilouris. The molecular gas content of the Pipe Nebula I.

Co-Aligned Chemical and Mineralogical Analyses. Discovery of a complex linearly polarized spectrum of Betelgeuse dominated by depolarization of the continuum. Astrophysical Journal, American Astronomical Society,1pp. Hincelin, Valentine Wakelam, S. Catarina, Alves de Oliveira, N. The effect of rotation and tidal heating on the thermal lightcurves of Astrophywique Mercuries.

FS – Star Formation

Limited fragmentation at the early evolutionary stage of massive clumps. The link between molecular cloud structure and turbulence. Shock Chemistry in NGC The softening length in 3Dfluids. Molecular gas in the outer disks of galaxies. France, Montpellier, France. Dobrijevic, Franck Selsis, et al.


zstrophysique Ultraviolet to Gamma Ray,France. Red supergiants and the past of Cygnus OB2. Water high resolution spectroscopic observations of massive protostars with Herschel.

Ammonia Masers in W Origins and Evolution of Life. Water in massive star-forming regions with the Herschel Space Observatory. Laura Reboussin, Valentine Wakelam, S.


Testi, Alain Baudry, M. Students considering housing in a student residence of the CROUS are encouraged to file an application immediately and not to wait for the answer of the registration procedure to the master degree.

Mehats,Paris, France. Survival of interstellar molecules to prestellar dense core collapse p1 early phases of disk formation.

FS – Star Formation | Laboratoire d’Astrophysique de Bordeaux – LAB

First results from the Herschel Gould Belt Survey. Spitzer Proposal ID Summary of the astrometric, photometric, and survey properties.

Edvige Corbelli, Bruce G. A choice of astrophysics lectures starting from the beginning of the first year of the Master.

The distribution of water in the high-mass star-forming region NGC I. Detection of a high-mass prestellar core candidate in WMM1.

Master : parcours Astrophysics – Observatoire Astronomique de Strasbourg – University of Strasbourg

The origin of CO in the stratosphere of Uranus. The first Galaxy scale hunt for the youngest high-mass protostars. Deuteration and Turbulent Mixing. This is the date the European Space Tracing the evolution of dust obscured star-formation and accretion back to the reionisation epoch with SPICA.


Pseudo 2D chemical model of hot Jupiter atmospheres: Shallow characterization of the subsurface for the Mission to Mars. Testing the universality of the star formation efficiency in dense molecular gas. Mass distribution models of nearby spiral galaxies: Performance highlights of the ALMA correlators. From Clouds to Young Stellar Objects and back again: A survey of low-J H2O line profiles toward high-mass protostars.

Astrochemistry in massive protostars Astrochemistry provides a way to constrain the physical processes responsible for the formation of stars and, more importantly, the best way to evaluate to which extent complex molecules, especially those of prebiotic interest, are formed in the interstellar medium. High-mass star formation is not well explained with scenarios applying to low-mass star formation. Evolution of the star formation efficiency in galaxies.