scholarly journals The Mass Spectra of Cores in Turbulent Molecular Clouds and Implications for the Initial Mass Function

2006 ◽  
Vol 637 (1) ◽  
pp. 384-391 ◽  
Author(s):  
Javier Ballesteros‐Paredes ◽  
Adriana Gazol ◽  
Jongsoo Kim ◽  
Ralf S. Klessen ◽  
Anne‐Katharina Jappsen ◽  
...  
Keyword(s):  
Molecular Clouds ◽  
Mass Spectra ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass

The Most Luminous Protostars in Molecular Clouds: A Hint to Understand the Stellar Initial Mass Function

2002 ◽  
Vol 4 ◽  
pp. 139-139 ◽  
Author(s):  
K. Dobashi ◽  
Y. Yonekura ◽  
T. Matsumoto ◽  
M. Momose ◽  
F. Sato ◽  
...  
Keyword(s):  
Molecular Clouds ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Stellar Initial Mass Function

scholarly journals The Most Luminous Protostars in Molecular Clouds: A Hint to Understand the Stellar Initial Mass Function

2001 ◽  
Vol 53 (1) ◽  
pp. 85-92 ◽  
Author(s):  
Kazuhito Dobashi ◽  
Yoshinori Yonekura ◽  
Tomoaki Matsumoto ◽  
Munetake Momose ◽  
Fumio Sato ◽  
...  
Keyword(s):  
Molecular Clouds ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Stellar Initial Mass Function

scholarly journals Observations of the IMF in clusters

2010 ◽  
Vol 6 (S270) ◽  
pp. 89-97 ◽  
Author(s):  
Joana Ascenso
Keyword(s):  
Mass Distribution ◽  
Molecular Clouds ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Wide Range ◽  
The Imf

AbstractStars form from molecular clouds, mostly in clusters with tens to tens of thousands of members, and the mass distribution within these clusters, or the Initial Mass Function, seems to be invariable against many parameters and over a wide range of masses. However, masses are a very difficult quantity to assess, and the precision of our determinations of the IMF is systematically lower than usually quoted. I will discuss the process of determining masses from observations and the type of uncertainties associated with this process.

scholarly journals The role of molecular filaments in the origin of the prestellar core mass function and stellar initial mass function

2019 ◽  
Vol 629 ◽  
pp. L4 ◽  
Author(s):  
Ph. André ◽  
D. Arzoumanian ◽  
V. Könyves ◽  
Y. Shimajiri ◽  
P. Palmeirim
Keyword(s):  
Power Law ◽  
Molecular Clouds ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Core Mass ◽  
Filamentary Structure ◽  
Star Forming ◽  
Prestellar Cores ◽  
Stellar Initial Mass Function

Context. The origin of the stellar initial mass function (IMF) is one of the most debated issues in astrophysics. Aims. Here we explore the possible link between the quasi-universal filamentary structure of star-forming molecular clouds and the origin of the IMF. Methods. Based on our recent comprehensive study of filament properties from Herschel Gould Belt survey observations, we derive, for the first time, a good estimate of the filament mass function (FMF) and filament line mass function (FLMF) in nearby molecular clouds. We use the observed FLMF to propose a simple toy model for the origin of the prestellar core mass function (CMF), relying on gravitational fragmentation of thermally supercritical but virialized filaments. Results. We find that the FMF and the FLMF have very similar shapes and are both consistent with a Salpeter-like power-law function (dN/dlog Mline ∝ Mline−1.5±0.1) in the regime of thermally supercritical filaments (Mline >  16 M⊙ pc−1). This is a remarkable result since, in contrast, the mass distribution of molecular clouds and clumps is known to be significantly shallower than the Salpeter power-law IMF, with dN/dlog Mcl ∝ Mcl−0.7. Conclusions. Since the vast majority of prestellar cores appear to form in thermally transcritical or supercritical filaments, we suggest that the prestellar CMF and by extension the stellar IMF are at least partly inherited from the FLMF through gravitational fragmentation of individual filaments.

Low‐Mass Star Formation and the Initial Mass Function in IC 348

1998 ◽  
Vol 508 (1) ◽  
pp. 347-369 ◽  
Author(s):  
K. L. Luhman ◽  
G. H. Rieke ◽  
C. J. Lada ◽  
E. A. Lada
Keyword(s):  
Star Formation ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Mass Star ◽  
Low Mass
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