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Revista mexicana de física
versión impresa ISSN 0035-001X
Rev. mex. fis. vol.52 supl.4 México nov. 2006
Constraining properties of neutron stars with heavyion reactions
BaoAn Li*, LieWen Chen,** Che Ming Ko*** and A.W. Steiner****
* Department of Chemistry and Physics, P.O. Box 419, Arkansas State University, State University, AR 724670419, U.S.A.
** Institute of Theoretical Physics, Shanghai Jiao Tong University, Shanghai 200240, and Center of Theoretical Nuclear Physics, National Laboratory of HeavyIon Accelerator, Lanzhou, 730000, China.
*** Cyclotron Institute and Physics Department, Texas A & M University, College Station, Texas 77843, U.S.A.
**** Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, U.S.A.
Recibido el 19 de enero de 2006
Aceptado el 24 de julio de 2006
Abstract
Nuclear reactions induced by stable and/or radioactive neutronrich nuclei provide the opportunity to pin down the equation of state of neutronrich matter, especially the density (ρ) dependence of its isospindependent part, i.e., the nuclear symmetry energy Esym. A conservative constraint, 32(ρ/ρ0)0.7 < Esym(ρ) < 32 (ρ /ρ0)1.1, around the nuclear matter saturation density ρ0 has recently been obtained from the isospin diffusion data in intermediate energy heavyion collisions. We review this exciting result and discuss its consequences and implications on nuclear effective interactions, radii and cooling mechanisms of neutron stars.
Keywords: Neutron stars; nuclear reaction models; equation of state.
Resumen
Se puede determinar la ecuacion de estado de materia con exceso de neutrones usando reacciones nucleares inducidas por haces estables y radioactivos de núcleos con exceso de neutrones, en particular cómo depende la contribución del isoespín, es decir la energía de simetría nuclear Esym, de la densidad (ρ). Recientemente, se obtuvo una restricción conservadora, 32 (ρ/ρ0)0.7 < Esym(ρ) < 32 (ρ /ρ0)1.1 cerca de la densidad de saturación de la materia nuclear ρ0 de los datos experimentales para la difusión de isoespín en colisiones de iones pesados a energías intermediarias. Se presenta una revisión de este resultado alentador y se discuten sus consecuencias e implicaciones para interacciones efectivas nucleares, radios y mecanismos de enfriamiento de estrellas de neutrones.
Descriptores: Estrellas de neutrones; modelos de reacciones nucleares; ecuación de estado.
PACS: 26.60.+c; 24.10.i
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Acknowledgments
This Work work was supported in part by the US National Science Foundation under Grant No. PHYS0354572 and PHYS0456890, and the NASAArkansas Space Grants Consortium award ASU15154 (BAL); National Natural Science Foundation of China under Grant No. 10105008 and 10575071 (LWC); the US National Science Foundation under Grant No. PHY0457265 and the Welch Foundation under Grant No. A1358 (CMK); and the US Department of Energy under grant No. DOE/W7405ENG36 (AWS).
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