Elastic scattering cross-sections of 16,18O + 120Sn reactions based on the potential of the modified Thomas - Fermi method with consideration of the core by O. I. Davydovska, V. О. Nesterov, V. Yu. Denisov

Subjects: “…modified thomas - fermi method…”
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The potential of the modified Thomas - Fermi method and its analytical representation on the example of the interaction of 16O with tin isotopes 112,114,116,118,120,122,124Sn by V. O. Nesterov

“…Nucleon distribution densities and nucleus-nucleus interaction potentials for the 16O nucleus and 112,114,116,118,120,122,124Sn isotopes were calculated within the framework of the modified Thomas - Fermi method, taking into account all terms to the second-order of ħ in the quasiclassical expansion of kinetic energy. …”
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Comparison between the Thomas–Fermi and Hartree–Fock–Bogoliubov Methods in the Inner Crust of a Neutron Star: The Role of Pairing Correlations by Matthew Shelley, Alessandro Pastore

“…We investigated the role of a pairing correlation in the chemical composition of the inner crust of a neutron star with the extended Thomas–Fermi method, using the Strutinsky integral correction. …”
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Approximate Solution of the Thomas–Fermi Equation for Free Positive Ions by Aleksey A. Mavrin, Alexander V. Demura

“…The approximate solution of the nonlinear Thomas–Fermi (TF) equation for ions is found by the Fermi method. The solution is based on the new asymptotic representation of the TF ion size valid for any ionization degree. …”
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Is there pasta in neutron stars? by Chamel Nicolas, Pearson John Michael, Shchechilin Nikolai

“…Adding shell and pairing effects perturbatively and consistently to the fourth-order extended Thomas-Fermi method using the Brussels-Montreal functional BSk24, we find that nuclear pastas are much less abundant than previously thought from liquid-drop models, thus questioning their very existence in neutron stars.…”
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Nuclear Pasta in Cold Non-Accreting Neutron Stars: Symmetry Energy Effects by Nikolai N. Shchechilin, John M. Pearson, Nicolas Chamel

“…Within the fourth-order extended Thomas–Fermi method, we find that pasta occupies a wider region of the crust for models with a lower slope of the symmetry energy (and higher symmetry energy at relevant densities) in agreement with previous studies based on pure Thomas–Fermi approximation and compressible liquid-drop models. …”
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Magnetic Fields in the Southern Coalsack and Beyond by M. J. F. Versteeg, Y. Angarita, A. M. Magalhães, M. Haverkorn, C. V. Rodrigues, R. Santos-Lima, Koji S. Kawabata

“…For the Southern Coalsack, we find an average magnetic field orientation of θ ∼ 75° with respect to the Galactic north pole and an average plane-of-sky magnetic field strength of approximately B _POS = 10 μ G, using the Davis–Chandrasekhar–Fermi method. These values are in agreement with some earlier estimates of the Coalsack’s magnetic field. …”
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Magnetic Fields and Fragmentation of Filaments in the Hub of California-X by Eun Jung Chung, Chang Won Lee, Woojin Kwon, Mario Tafalla, Shinyoung Kim, Archana Soam, Jungyeon Cho

“…Using the modified Davis–Chandrasekhar–Fermi method, we estimated the magnetic field strengths ( B _pos ) of the filaments, which are 110 ± 80 and 90 ± 60 μ G, respectively. …”
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Magnetic Fields of the Starless Core L 1512 by Sheng-Jun Lin, Shih-Ping Lai, Kate Pattle, David Berry, Dan P. Clemens, Laurent Pagani, Derek Ward-Thompson, Travis J. Thieme, Tao-Chung Ching

“…In this study, we use the Davis–Chandrasekhar–Fermi method to derive a plane-of-sky magnetic field strength ( B _pos ) of 18 ± 7 μ G and an observed mass-to-flux ratio ( λ _obs ) of 3.5 ± 2.4, suggesting that L 1512 is magnetically supercritical. …”
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Increasing Mass-to-flux Ratio from the Dense Core to the Protostellar Envelope around the Class 0 Protostar HH 211 by Hsi-Wei Yen, Patrick M. Koch, Chin-Fei Lee, Naomi Hirano, Nagayoshi Ohashi, Jinshi Sai (Insa Choi), Shigehisa Takakuwa, Ya-Wen Tang, Ken’ichi Tatematsu, Bo Zhao

“…The magnetic field strength in the dense core on a 0.1 pc scale was estimated with the single-dish line and polarization data using the Davis–Chandrasekhar–Fermi method, and that in the protostellar envelope on a 600 au scale was estimated from the force balance between the gravity and magnetic field tension by analyzing the gas kinematics and magnetic field structures with the ALMA data. …”
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SOFIA Observations of 30 Doradus. II. Magnetic Fields and Large-scale Gas Kinematics by Le Ngoc Tram, Lars Bonne, Yue Hu, Enrique Lopez-Rodriguez, Jordan A. Guerra, Pierre Lesaffre, Antoine Gusdorf, Thiem Hoang, Min-Young Lee, Alex Lazarian, B-G Andersson, Simon Coudé, Archana Soam, William D. Vacca, Hyeseung Lee, Michael Gordon

“…Our B -field strength maps, estimated using the Davis–Chandrasekhar–Fermi method and structure-function, show variations across the cloud within a maximum of 600, 450, and 350 μ G at 89, 154, and 214 μ m, respectively. …”
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