Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter

LI Wen-Fei; ZHANG Feng-Shou; CHEN Lie-Wen

Chinese Physics C> 2001, Vol. 25> Issue(9) : 877-883

Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter

Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China2 Institute of Modern Physics, The Chinese Academy of Sciences, Lanzhou 730000, China3 CCAST World Laboratory, Beijing 100080, China

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Abstract：
By resolving Tolman Oppenheimer Volkoff equation based on a temperature, density, and isospin dependent nuclear equation of state of nuclear matter, we obtained the mass of neutron star as a function of central density, and the radius of neutron star was also investigated. It is found that both the maximum mass and the radius of neutron star strongly depend on the incompressibility, symmetry energy strength coefficient, and effective mass of nucleon. With the increment of the incompressibility and symmetry energy strength coefficient and the decrement of the nucleon effective mass, the maximum mass of nentron star increases. Meanwhile, the nuclear equation of state with large incompressibility, symmetry energy strength coefficient and nucleon effective mass results in relatively large neutron radius. These results imply that one can get some information about the nuclear equation of state by investigating the macroscopical variables of neutron stars such as mass and radius etc. The relationship of the mass and radius of neutron star is also investigated.

References

[1]

. Hofmann F ,Keil C M ,Lenske H .Nucl-th/0008038,2000 2. ZHANG Feng-Shou,GE Ling-Xiao.Nuclear Multifragmentation,Beijing:Science Press,1998(in Chinese)(张丰收,葛凌霄.原子核多重碎裂,北京:科学出版社,1998) 3. ZHANG Feng-Shou,CHEN Lie-Wen.High Energy Phys.and Nucl.Phys.,1999,23(12):1190(in Chinese)(张丰收,陈列文.高能物理与核物理,1999,23(12):1190)4. ZHAN GFeng-Shou,GE Ling-Xiao.High Energy Phys.and Nucl.Phys.,1992,16:666(in Chinese)(张丰收,葛凌霄.高能物理与核物理,1992,16:666) 5. ZHANG F S.Z .Phys.,1996,A356:163 6. ZHANG F S,CHEN L W .Chin.Phys.Lett.,2000(in press) 7. Tolman R C .Proc.Nat.Acad.Sci.USA ,1934,20:38. Oppenheimer J R ,Volkoff G M .Phys.Rev.,1939,55:374 9. Hewish A ,Bell S J,Pikington J D H et al.Nature,1968,217:709 10. Van Kerkwijk M .H .Astro.Astrophys.,1995,303:49711. Rhoades C ,Ruffini R .Phys.Rev.Lett.,1974,32:324 12. Chandrasekhar.An Introduction to the Study of Stellar Structure,Chicago:University of Chicago Press,1939 13. Wasserman I,Shapiro S L .Ap.J.,1983,265:103614. gelman H .The Lives of Neutron Stars.In:Kluwer,Dordrecht.NATO ASI Series,C450.10115. Link B ,Epstein R I,Lattimer J M .Phys.Rev.Lett.,2000,astr-ph/9909146(in press)

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[18]	Zhang Fengshou , Chen Liewen . An Isospin-Dependent Nuclear Equation of State. Chinese Physics C, 1999, 23(12): 1190-1196.
[19]	ZHANG Dong , ZHANG Xiao-Ze , JIN Xing-Nan , SA Ben-Hao . EQUATION OF STATE OF HOT NUCLEI BEFORE BREAK-UP. Chinese Physics C, 1989, 13(8): 706-713.
[20]	SHEN QING-BIAO , TIAN YE , MA ZHONG-YU , ZHANG JING-SHANG , ZHUO YI-ZHONG . SEMI-MICROSCOPIC OPTICAL POTENTIAL CALCULATION USING NUCLEAR MATTER APPROACH II. ASYMMETRIC NUCLEAR MATTER. Chinese Physics C, 1982, 6(2): 185-197.

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LI Wen-Fei, ZHANG Feng-Shou and CHEN Lie-Wen. Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter[J]. Chinese Physics C, 2001, 25(9): 877-883.

LI Wen-Fei, ZHANG Feng-Shou and CHEN Lie-Wen. Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter[J]. Chinese Physics C, 2001, 25(9): 877-883. shu

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Received: 2000-07-18
Revised: 1900-01-01

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沈阳化工大学材料科学与工程学院沈阳 110142

Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter

Corresponding author: LI Wen-Fei,

Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China2 Institute of Modern Physics, The Chinese Academy of Sciences, Lanzhou 730000, China3 CCAST World Laboratory, Beijing 100080, China

Received Date: 2000-07-18

Accepted Date: 1900-01-01

Available Online: 2001-09-05

Abstract: By resolving Tolman Oppenheimer Volkoff equation based on a temperature, density, and isospin dependent nuclear equation of state of nuclear matter, we obtained the mass of neutron star as a function of central density, and the radius of neutron star was also investigated. It is found that both the maximum mass and the radius of neutron star strongly depend on the incompressibility, symmetry energy strength coefficient, and effective mass of nucleon. With the increment of the incompressibility and symmetry energy strength coefficient and the decrement of the nucleon effective mass, the maximum mass of nentron star increases. Meanwhile, the nuclear equation of state with large incompressibility, symmetry energy strength coefficient and nucleon effective mass results in relatively large neutron radius. These results imply that one can get some information about the nuclear equation of state by investigating the macroscopical variables of neutron stars such as mass and radius etc. The relationship of the mass and radius of neutron star is also investigated.

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Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter

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