Plumbing neutron stars to new depths with the binding energy of the exotic nuclide Zn82. Wolf, R., N., Beck, D., Blaum, K., Böhm, C., Borgmann, C., Breitenfeldt, M., Chamel, N., Goriely, S., Herfurth, F., Kowalska, M., Kreim, S., Lunney, D., Manea, V., Minaya Ramirez, E., Naimi, S., Neidherr, D., Rosenbusch, M., Schweikhard, L., Stanja, J., Wienholtz, F., & Zuber, K. Physical Review Letters, 110(4):041101, American Physical Society, 1, 2013. ![Plumbing neutron stars to new depths with the binding energy of the exotic nuclide Zn82 [link]](https://bibbase.org/img/filetypes/link.svg "link")
Website doi abstract bibtex 2 downloads Modeling the composition of neutron-star crusts depends strongly on binding energies of neutron-rich nuclides near the N=50 and N=82 shell closures. Using a recent development of time-of-flight mass spectrometry for on-line purification of radioactive ion beams to access more exotic species, we have determined for the first time the mass of Zn82 with the ISOLTRAP setup at the ISOLDE-CERN facility. With a robust neutron-star model based on nuclear energy-density-functional theory, we solve the general relativistic Tolman-Oppenheimer-Volkoff equations and calculate the neutron-star crust composition based on the new experimental mass. The composition profile is not only altered but now constrained by experimental data deeper into the crust than before. © 2013 American Physical Society.
@article{
title = {Plumbing neutron stars to new depths with the binding energy of the exotic nuclide Zn82},
type = {article},
year = {2013},
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abstract = {Modeling the composition of neutron-star crusts depends strongly on binding energies of neutron-rich nuclides near the N=50 and N=82 shell closures. Using a recent development of time-of-flight mass spectrometry for on-line purification of radioactive ion beams to access more exotic species, we have determined for the first time the mass of Zn82 with the ISOLTRAP setup at the ISOLDE-CERN facility. With a robust neutron-star model based on nuclear energy-density-functional theory, we solve the general relativistic Tolman-Oppenheimer-Volkoff equations and calculate the neutron-star crust composition based on the new experimental mass. The composition profile is not only altered but now constrained by experimental data deeper into the crust than before. © 2013 American Physical Society.},
bibtype = {article},
author = {Wolf, R. N. and Beck, D. and Blaum, K. and Böhm, Ch and Borgmann, Ch and Breitenfeldt, M. and Chamel, N. and Goriely, S. and Herfurth, F. and Kowalska, M. and Kreim, S. and Lunney, D. and Manea, V. and Minaya Ramirez, E. and Naimi, S. and Neidherr, D. and Rosenbusch, M. and Schweikhard, L. and Stanja, J. and Wienholtz, F. and Zuber, K.},
doi = {10.1103/PHYSREVLETT.110.041101/FIGURES/3/MEDIUM},
journal = {Physical Review Letters},
number = {4}
}
Downloads: 2
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