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NSR database version of May 9, 2024.

Search: Author = A.L.Pavlov

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2016FA02      Phys.Rev. C 93, 015801 (2016)

A.F.Fantina, N.Chamel, Y.D.Mutafchieva, Zh.K.Stoyanov, L.M.Mihailov, and R.L.Pavlov

Role of the symmetry energy on the neutron-drip transition in accreting and nonaccreting neutron stars

ATOMIC MASSES ^{100,101,102,103,104,105,106,107,108,109,110,111,112,113,114,115,116,117,118,119,120,121,122,123,124,125,126}Kr, ^{100,101,102,103,104,105,106,107,108,109,110,111,112,113,114,115,116,117,118,119,120,121,122,123,124,125,126,127,128,129,130}Sr; analyzed difference in mass predictions for two pairs of Brussels-Montreal nuclear mass models. ¹²²Kr, ^{122,124,126,128}Sr; calculated baryon density, and corresponding pressure for neutron-drip transition in the crust of nonaccreting magnetized neutron stars. ^60,64Ca, ^66,68Ti, ⁷⁶Cr, ¹⁰³Ga, ^98,104Ge, ¹⁰⁵As, ¹⁰⁶Se; calculated number of emitted neutrons, baryon density and corresponding pressure, S(n), neutron dip threshold. Role of symmetry energy on neutron-drip transition in accreting and nonaccreting neutron-star crusts. Microscopic nuclear mass models, from HFB-22 to HFB-25, developed by the Brussels-Montreal collaboration.

doi: 10.1103/PhysRevC.93.015801
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