Origin of r-process elements

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Heavy elements are formed

at the later stage of wind.

Nuclear Fireworks in Stars via the Breakout from the CNO Cycle

Nuclear Physics (and Astrophysics) of Core Collapse Supernovae

ARIS 2014 - Joint Institute for Nuclear Astrophysics

Topics in Nuclear Astrophysics II Stellar Reaction Rates

Nuclear Physics in Stars - The Joint Institute for Nuclear Astrophysics

7th Russbach Workshop on Nuclear Astrophysics

PYCNONUCLEAR REACTIONS in dense stellar matter

Description of the proposed Facility for Rare-Isotope Beams (FRIB)

Nucleosynthesis in massive stars, the role of

Theoretical calculation II (Wilson et al. 2006) Wilson’s new simulation(2006) M=20M progenitor mass Improved EOS Improved numerical method Entropy~500k timescale ~0.1sec

Heavy elements are formed at the later stage of wind.

Page 1 and 2: Origin of r-process elements Kaori
Page 3 and 4: Network code Full dynamical netwo
Page 5 and 6: Theoretical calculation II (Wilson
Page 7 and 8: Theoretical calculation II (Wilson
Page 9: Theoretical calculation II (Wilson

Origin of r-process elements

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