Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



  history
ID: 421702.0, MPI für Astronomie / Publikationen_mpia
Primordial mass segregation in starburst stellar clusters
Authors:Dib, S.; Shadmehri, M.; Gopinathan, M.; Kim, J.; Henning, Th
Language:English
Publisher:ASP
Date of Publication (YYYY-MM-DD):2008
Title of Proceedings:Massive Star Formation: Observations Confront Theory
Start Page:282
End Page:289
Title of Series:ASP Conf. Ser.
Volume (in Series):387
Name of Conference/Meeting:Astronomical Society of the Pacific Conference Series
Review Status:not specified
Audience:Experts Only
Abstract / Description:We present a model to explain the mass segregation and shallow mass functions observed in the central parts of dense and young starburst stellar clusters. The model assumes that the initial pre-stellar cores mass function resulting from the turbulent fragmentation of the proto-cluster cloud is significantly altered by the cores coalescence before they collapse to form stars. With appropriate, yet realistic parameters, this model based on the competition between cores coalescence and collapse reproduces the mass spectra of the well studied Arches cluster. Namely, the slopes at the intermediate and high mass ends are reproduced, as well as the peculiar bump observed at 6 M_{o}. This coalescence-collapse process occurs on short timescale of the order of one fourth the free fall time of the proto-cluster cloud (i.e., a few 10^{4} years), suggesting that mass segregation in Arches and similar clusters is primordial. The best fitting model implies the total mass of the Arches cluster is 1.45 × 10^{5} M_{o}, which is slightly higher than the often quoted, but completeness affected, observational value of a few 10^{4} M_{o}. The derived star formation efficiency is Ëœ 30 percent which implies that the Arches cluster is likely to be gravitationally bound.
Comment of the Author/Creator:Date: 2008, May 1, 2008
External Publication Status:published
Document Type:Conference-Paper
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2008ASPC..387..282D [ID No:1]
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.