On the relativistic and electrodynamical stability of massive nuclear density cores

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dc.creatorPopov, Vladimir
dc.creatorRotondo, Michael
dc.creatorRuffini, Remo
dc.creatorXue, She-Sheng
dc.date2009-03-22
dc.date.accessioned2026-07-07T12:55:35Z
dc.date.available2026-07-07T12:55:35Z
dc.descriptionWe present a unified treatment of nuclear density cores recovering the classic results for neutral atoms with heavy nuclei having a mass number $A\approx 10^2--10^6$ and extrapolating these results to massive nuclear density cores with $A\approx(m_{\rm Planck}/m_n)^3 \sim 10^{57}$. The treatment consists of solving the relativistic Thomas-Fermi equation describing a system of $N_n$ neutrons, $N_p$ protons and $N_e$ electrons in beta decay equilibrium. The $N_p$ protons are distributed at a constant density within a spherical core of radius $R_c$. A new island of stability is found for $A > A_R = 0.039(N_p/A)^{1/2}(m_{Planck}/m_n)^3$. The Coulomb repulsion, screened by relativistic electrons, is balanced by the gravitational self-interaction of the core. In analogy to heavy nuclei they present, near their surface, an overcritical electric field. The relation between $A$ and $N_p$ is generalized to an arbitrary value of the mass number, and the phenomenological relations for $A < 1.5\cdot 10^2$ are obtained as a limiting case.
dc.description5 pages, 3 figures
dc.identifierhttps://arxiv.org/abs/0903.3727
dc.identifierhttp://arxiv.org/abs/0903.3727
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/224297
dc.subjectSolar and Stellar Astrophysics
dc.titleOn the relativistic and electrodynamical stability of massive nuclear density cores
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