Results 31 to 40 of about 1,197,942 (368)
An excess of massive stars in the local 30 Doradus starburst [PDF]
Science, 2018 Observing more massive stars The number of stars that form at each mass is known as the initial mass function (IMF). For most masses, the IMF follows a power-law distribution, first determined by Edwin Salpeter in 1955. Schneider et al. used observations
F. Schneider +38 more
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Massive Stars and Their Supernovae [PDF]
, 2010 Massive stars and their supernovae are prominent sources of radioactive isotopes, the observations of which thus can help to improve our astrophysical models of those. Our understanding of stellar evolution and the final explosive endpoints such as supernovae or hypernovae or gamma-ray bursts relies on the combination of magneto-hydrodynamics, energy ...
Friedrich-Karl Thielemann +3 more
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Nucleonic Direct Urca Processes and Cooling of the Massive Neutron Star by Antikaon Condensations
Advances in Astronomy, 2020 Nucleonic direct Urca processes and cooling of the massive neutron stars are studied by considering antikaon condensations. Calculations are performed in the relativistic mean field and isothermal interior approximations.
Yan Xu +3 more
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Stellar populations dominated by massive stars in dusty starburst galaxies across cosmic time [PDF]
Nature, 2018 All measurements of cosmic star formation must assume an initial distribution of stellar masses—the stellar initial mass function—in order to extrapolate from the star-formation rate measured for typically rare, massive stars (of more than eight solar ...
Zhi-Yu Zhang +4 more
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The stability of massive stars [PDF]
Symposium - International Astronomical Union, 1994 An investigation of the stability properties of stellar models describing massive stars is motivated observationally by the necessity to explain the observed Humphreys - Davidson (HD) limit and the variability of the most massive stars known, i.e. the existence of luminous blue variables (LBVs).
M. Kiriakidis, K. J. Fricke, W. Glatzel
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The Origin of Massive Stars: The Inertial-inflow Model [PDF]
Astrophysical Journal, 2019 We address the problem of the origin of massive stars, namely the origin, path, and timescale of the mass flows that create them. Based on extensive numerical simulations, we propose a scenario where massive stars are assembled by large-scale, converging,
P. Padoan +4 more
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Symposium - International Astronomical Union, 1999 The evolution of massive stars is far from being fully understood, as we outline by pointing to a number of open problems related to massive stars in the Magellanic Clouds. We argue that rotation may be a key ingredient in the physics of massive stars.
Langer, Norbert, Heger, Alexander
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The Astrophysical Journal, 2023 Extinction toward the Galactic Center (GC) is extreme and limits observations of its stars to the infrared. In addition, the extinction varies on scales of arcseconds.
Shogo Nishiyama +2 more
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Constraining mixing in massive stars in the Small Magellanic Cloud [PDF]
Astronomy & Astrophysics, 2019 Context. The evolution of massive stars is strongly influenced by internal mixing processes such as semiconvection, convective core overshooting, and rotationally induced mixing. None of these processes are currently well constrained. Aims.
A. Schootemeijer +3 more
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, 2014 The enormous radiative and mechanical luminosities of massive stars impact a vast range of scales and processes, from the reionization of the universe, to the evolution of galaxies, to the regulation of the interstellar medium, to the formation of star clusters, and even to the formation of planets around stars in such clusters.
J. C. Tan +7 more
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