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Abstrak :
[ABSTRAK
Di permukaan bintang neutron, perubahan kerapatan partikel yang signikan dapat menghasilkan separasi muatan dalam bentuk lapisan dipol listrik. Pada penelitian ini dipelajari efek medan listrik akibat lapisan tersebut terhadap properti dari bintang neutron. Untuk memodelkan kerapatan lapisan dipol listrik, kami menggunakan dua fungsi Gaussian. Pada perhitungan ini kami gunakan dua model dengan asumsi berbeda, yakni: model dengan asumsi bahwa bintang neutron hanya tersusun atas p, n, e dan  serta model dengan asumsi bintang neutron tersusun dari p, n, e,  dan hyperon. Hasil yang diperoleh menunjukkan bahwa massa maksimum tidak sensitif terhadap medan listrik di permukaan, tetapi radius bintang dengan massa kanonik 1:4Mb cukup sensitif terhadap medan listrik. Bintang neutron dengan hyperon bersifat lebih soft dibandingkan bintang neutron tanpa hyperon

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ABSTRACT
On the surface of a neutron star, a signicant particle density changes can produce charge separation in the form electric dipole layer. This research studied electric eld eect from the dipole layer on the properties of neutron star. For modeling electric dipole layer density, we use two Gaussian functions. We use two models with dierent assumptions: namely a model which assumes the neutron star is only composed of p, n, e and  and a model which assumes the neutron star is composed of p, n, e,  and hyperon. The result showes that the maximum mass is not sensitive to the electric elds on the surface, but the radius of star with canonical mass 1:4Mb is quite sensitive to electric elds. The neutron star with hyperon is softer than without hyperon;On the surface of a neutron star, a signicant particle density changes can produce charge separation in the form electric dipole layer. This research studied electric eld eect from the dipole layer on the properties of neutron star. For modeling electric dipole layer density, we use two Gaussian functions. We use two models with dierent assumptions: namely a model which assumes the neutron star is only composed of p, n, e and  and a model which assumes the neutron star is composed of p, n, e,  and hyperon. The result showes that the maximum mass is not sensitive to the electric elds on the surface, but the radius of star with canonical mass 1:4Mb is quite sensitive to electric elds. The neutron star with hyperon is softer than without hyperon, On the surface of a neutron star, a signicant particle density changes can produce charge separation in the form electric dipole layer. This research studied electric eld eect from the dipole layer on the properties of neutron star. For modeling electric dipole layer density, we use two Gaussian functions. We use two models with dierent assumptions: namely a model which assumes the neutron star is only composed of p, n, e and  and a model which assumes the neutron star is composed of p, n, e,  and hyperon. The result showes that the maximum mass is not sensitive to the electric elds on the surface, but the radius of star with canonical mass 1:4Mb is quite sensitive to electric elds. The neutron star with hyperon is softer than without hyperon]

Abstrak :
[ABSTRAK
Fenomena halo neutron dalam nuklir digambarkan adanya kemunculan 'ekor' dan adanya 'ruang kosong' antara core dan ekor pada distribusi neutron akibat energi ikat yang lemah. Metode analisa halo yang dikembangkan oleh V. Rotival dkk [Phys. Rev. C79, 054308 (2009)] untuk menghitung besaran-besaran halo berdasarkan mo- del Hartree-Fock-Bogoulibov (HFB) pada isotop Cr dan isotop Sn menjadi salah sa- tu alternatif untuk mempelajari fenomena halo. Berbeda dengan Rotival dkk, kami menggunakan model Relativistic Mean Field (RMF) pada penelitian ini. Berbeda dengan hasil perhitungan berdasarkan model HFB, kami fokus mengamati perilaku spektrum single particle energy level 1g9~2 terhadap kemunculan halo pada isotop Cr. Selain itu, pada penelitian ini kami juga memperlajari dampak dari suku cross coupling meson ! − , suku-suku tensor dan suku pertukaran elektromagnetik pada model RMF terhadap kemunculan halo pada isotop Cr dan isotop Sn. Hasil perhi- tungan prediksi kemunculan halo berdasarkan model RMF lebih besar dibandingkan dengan hasil perhitungan berdasarkan model HFB (`NhaloeRMF > `NhaloeHFB):

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ABSTRACT
In neutron halo phenomenon, the neutron density displays an unusually extended 'tail' and 'empty space' between the core and the tail due to weak binding energy. New analysis method of the halo was developed by V. Rotival, et al.[Phys. Rev. C79, 054308 (2009)] in Cr-isotopes and Sn-isotopes, its usually applied with Hartree-Fock- Bogoliubov (HFB) model. Unlike them, we use the model of the Relativistic Mean Field (RMF) in this research. We observed dierent behavior at the level 1g9~2 in line with appearance of halo in Cr-isotopes. Moreover, in this research we also studied the eects of cross coupling meson ! − , tensor, and electromagnetic exchange in RMF model appearance of halo in Cr-isotopes and Sn-isotopes. The prediction of the existence of halo based on RMF model is greater than the prediction based on HFB model (`NhaloeRMF > `NhaloeHFB):, In neutron halo phenomenon, the neutron density displays an unusually extended 'tail' and 'empty space' between the core and the tail due to weak binding energy. New analysis method of the halo was developed by V. Rotival, et al.[Phys. Rev. C79, 054308 (2009)] in Cr-isotopes and Sn-isotopes, its usually applied with Hartree-Fock- Bogoliubov (HFB) model. Unlike them, we use the model of the Relativistic Mean Field (RMF) in this research. We observed dierent behavior at the level 1g9~2 in line with appearance of halo in Cr-isotopes. Moreover, in this research we also studied the eects of cross coupling meson ! − , tensor, and electromagnetic exchange in RMF model appearance of halo in Cr-isotopes and Sn-isotopes. The prediction of the existence of halo based on RMF model is greater than the prediction based on HFB model (`NhaloeRMF > `NhaloeHFB):]