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Journal Article

Nuclear masses and neutron stars

MPS-Authors
http://pubman.mpdl.mpg.de/cone/persons/resource/persons30722

Kreim,  Susanne
CERN;
Division Prof. Dr. Klaus Blaum, MPI for Nuclear Physics, Max Planck Society;

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Fulltext (public)

1303.1343v1
(Preprint), 325KB

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There is no public supplementary material available
Citation

Kreim, S., Hempel, M., Lunney, D., & Schaffner-Bielich, J. (2013). Nuclear masses and neutron stars. International Journal of Mass Spectrometry, 349-350, 63-68. doi:10.1016/j.ijms.2013.02.015.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0014-503F-6
Abstract
Precision mass spectrometry of neutron-rich nuclei is of great relevance for astrophysics. Masses of exotic nuclides impose constraints on models for the nuclear interaction and thus affect the description of the equation of state of nuclear matter, which can be extended to describe neutron-star matter. With knowledge of the masses of nuclides near shell closures, one can also derive the neutron-star crustal composition. The Penning-trap mass spectrometer ISOLTRAP at CERN-ISOLDE has recently achieved a breakthrough measuring the mass of 82Zn, which allowed constraining neutron-star crust composition to deeper layers [1]. We perform a more detailed study on the sequence of nuclei in the outer crust of neutron stars with input from different nuclear models to illustrate the sensitivity to masses and the robustness of neutron-star models. The dominant role of the N = 50 and N = 82 closed neutron shells for the crustal composition is confirmed