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The top documents tagged [core h]
Stellar Evolution II. The Upper End of the Main Sequence: How massive can a star get? Larger clouds of gas (GMCs) tend to fragment into smaller ones before
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1208.5816 Solar Radiation
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1 QCD Thermodynamics at High Temperature Peter Petreczky Large Scale Computing and Storage Requirements for Nuclear Physics (NP), Bethesda MD, April 29-30,
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The s-process Fe Co Ni Rb Ga Ge Zn Cu Se Br As Zr Y Sr Kr (n, ) ()() ()() r-process p-process 63 Ni, t 1/2 =100 a 64 Cu, t 1/2 =12 h, 40 % (
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Improving our understanding of Stellar Evolution with PLATO 2.0 Santi Cassisi INAF - Astronomical Observatory of Teramo, Italy
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Activity #32, pages 111-112 (pages 109-110 were done last Friday)
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Memory restriction, limits and heterogeneous grids. A case study. Txema Heredia Or an example of how to adapt your policies to your needs
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Astronomy 1020 Stellar Astronomy Spring_2015 Day-33
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Astronomy 1 – Fall 2014 Lecture 12; November 18, 2014
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Stellar Evolution – the Life and Death of a Star…
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Our sun does not have a solid surface. Most of the energy comes from the core
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The Sun
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