The initial mass function for massive stars in the Magellanic Clouds. 2: Interstellar reddening toward 14 OB associations

1994 ◽  
Vol 429 ◽  
pp. 192 ◽  
Author(s):  
Robert J. Hill ◽  
Barry F. Madore ◽  
Wendy L. Freedman
Keyword(s):  
Massive Stars ◽  
Mass Function ◽  
Magellanic Clouds ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Ob Associations

scholarly journals The Stellar Initial Mass Function in Starburst Galaxies

1999 ◽  
Vol 186 ◽  
pp. 243-250
Author(s):  
Claus Leitherer
Keyword(s):  
Massive Stars ◽  
Mass Function ◽  
Starburst Galaxies ◽  
Initial Mass Function ◽  
Initial Mass ◽  
H Ii Regions ◽  
Environmental Properties ◽  
Stellar Initial Mass Function ◽  
Low Mass ◽  
Star Formation Histories

Starburst galaxies are currently forming massive stars at prodigious rates. I discuss the star-formation histories and the shape of the initial mass function, with particular emphasis on the high- and on the low-mass end. The classical Salpeter IMF is consistent with constraints from observations of the most massive stars, irrespective of environmental properties. The situation at the low-mass end is less clear: direct star counts in nearby giant H II regions show stars down to ~1 M⊙, whereas dynamical arguments in some starburst galaxies suggest a deficit of such stars.

scholarly journals Supernova Nucleosynthesis in Massive Stars

1996 ◽  
Vol 145 ◽  
pp. 157-164
Author(s):  
M. Hashimoto ◽  
K. Nomoto ◽  
T. Tsujimoto ◽  
F.-K. Thielemann
Keyword(s):  
Main Sequence ◽  
Massive Stars ◽  
Mass Function ◽  
Stellar Mass ◽  
Initial Mass Function ◽  
Explosion Energy ◽  
Initial Mass ◽  
Explosive Nucleosynthesis ◽  
Solar Abundances

Presupernova evolution and explosive nucleosynthesis in massive stars for main-sequence masses from 13 Mʘ to 70 Mʘ are calculated. We examine the dependence of the supernova yields on the stellar mass, 12C(α, γ)16O rate, and explosion energy. The supernova yields integrated over the initial mass function are compared with the solar abundances.

The initial mass function for massive stars

1982 ◽  
Vol 263 ◽  
pp. 777 ◽  
Author(s):  
C. D. Garmany ◽  
P. S. Conti ◽  
C. Chiosi
Keyword(s):  
Massive Stars ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass

scholarly journals Transition of the initial mass function in the metal-poor environments

2021 ◽  
Author(s):  
Sunmyon Chon ◽  
Kazuyuki Omukai ◽  
Raffaella Schneider
Keyword(s):  
Star Formation ◽  
Mass Distribution ◽  
Massive Stars ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Low Mass Stars ◽  
Filamentary Structure ◽  
Low Mass ◽  
Cloud Core

Abstract We study star cluster formation in a low-metallicity environment using three dimensional hydrodynamic simulations. Starting from a turbulent cloud core, we follow the formation and growth of protostellar systems with different metallicities ranging from 10−6 to 0.1 Z⊙. The cooling induced by dust grains promotes fragmentation at small scales and the formation of low-mass stars with M* ∼ 0.01–0.1 M⊙ While the number of low-mass stars increases with metallicity, when Z/Z⊙ ≳ 10−5. the stellar mass distribution is still top-heavy for Z/Z⊙ ≲ 10−2 compared to the Chabrier initial mass function (IMF). In these cases, star formation begins after the turbulent motion decays and a single massive cloud core monolithically collapses to form a central massive stellar system. The circumstellar disk preferentially feeds the mass to the central massive stars, making the mass distribution top-heavy. When Z/Z⊙ = 0.1, collisions of the turbulent flows promote the onset of the star formation and a highly filamentary structure develops owing to efficient fine-structure line cooling. In this case, the mass supply to the massive stars is limited by the local gas reservoir and the mass is shared among the stars, leading to a Chabrier-like IMF. We conclude that cooling at the scales of the turbulent motion promotes the development of the filamentary structure and works as an important factor leading to the present-day IMF.

scholarly journals On the Bulk Yields of Nucleosynthesis from Massive Stars

1977 ◽  
Vol 45 ◽  
pp. 161-164
Author(s):  
W. David Arnett
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Massive Stars ◽  
Mass Function ◽  
Initial Mass Function ◽  
Initial Mass ◽  
Iron Group ◽  
Helium Stars ◽  
The Absolute ◽  
The Imf

Preliminary estimates are made of the absolute yields of abundant nuclei synthesized in observed stars. The compositions of helium stars of mass 3 ≤ Mα / Mʘ≤ 64 are presented, taken at the instant of instability. These stars of mass Mα are identified with stars of main sequence mass M. The amount of synthesized matter for each mass M ≥ MʘHe is estimated (Table 1). Using a variety of choices for the initial mass function (IMF) the yield per stellar generation is calculated. For standard choices of the IMF the absolute and relative yields of12C,16O,20Ne,24Mg, the Si to Ca group and the iron group agree with solar system values, to the accuracy of the calculations.

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