CSENGERI, T.; BONTEMPS, Sylvain; SCHNEIDER, N.; MOTTE, F.

doi:10.1017/S1743921311000172

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CSENGERI, T.
Astrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]

BONTEMPS, Sylvain
Observatoire aquitain des sciences de l'univers [OASU]
Université Sciences et Technologies - Bordeaux 1 [UB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]

SCHNEIDER, N.
Astrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]

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Computational Star Formation, Proceedings of the International Astronomical Union, IAU Symposium, Volume 270, p. 53-56, 2011, Computational Star Formation, Proceedings of the International Astronomical Union, IAU Symposium, Volume 270, p. 53-56, 2011, Computational Star Formation, International Astronomical Union, 2011. 2011-04, vol. 270, p. 53-56

Resumen en inglés

A systematic, high angular-resolution study of IR-quiet Massive Dense Cores (MDCs) of Cygnus-X in continuum and high-density molecular tracers is presented. The results are compared with the quasi-static and the dynamical evolutionary scenario. We find that the fragmentation properties are not compatible with the quasi-static, monolithic collapse scenario, nor are they entirely compatible with the formation of a cluster of mostly low-mass stars. The kinematics of MDCs shows individual velocity components appearing as coherent flows, which indicate important dynamical processes at the scale of the mass reservoir around high-mass protostars.< Leer menos

Palabras clave en inglés

stars: formation

ISM: kinematics and dynamics

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Fragmentation and dynamics in Massive Dense Cores in Cygnus-X

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