title: ÐÐµÑÑÐµÑÐ¸ÑÐµÑÐºÐ¸Ðµ Ð°ÑÐ¾Ð¼Ð½ÑÐµ ÑÐ´ÑÐ° Ð²Ð¾ Ð²Ð½ÑÑÑÐµÐ½Ð½ÐµÐ¹ ÐºÐ¾ÑÐµ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½Ð¾Ð¹ Ð·Ð²ÐµÐ·Ð´Ñ: ÐºÐ°Ð¿ÐµÐ»ÑÐ½Ð°Ñ Ð¼Ð¾Ð´ÐµÐ»Ñ, Ð¾ÑÐ½Ð¾Ð²Ð°Ð½Ð½Ð°Ñ Ð½Ð° Ð¿Ð¾ÑÐµÐ½ÑÐ¸Ð°Ð»Ð°Ñ ÑÐ¸Ð¿Ð° Ð¡ÐºÐ¸ÑÐ¼Ð°
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÐ°
titleType: Subtitle
title: Non-spherical atomic nuclei in the inner crust of a neutron star: a drop model based on Skyrme-type potentials
Creators: name: ÐÐµÐ¼Ð»ÑÐºÐ¾Ð², ÐÐ¸ÐºÐ¸ÑÐ°
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2021
Subjects: Ð¿Ð»Ð¾ÑÐ½Ð¾Ðµ Ð²ÐµÑÐµÑÑÐ²Ð¾
Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½Ð°Ñ Ð·Ð²ÐµÐ·Ð´Ð°
ÑÑÑÐµÐºÑÐ¸Ð²Ð½ÑÐ¹ ÑÐ´ÐµÑÐ½ÑÐ¹ Ð¿Ð¾ÑÐµÐ½ÑÐ¸Ð°Ð»
ÑÐ¶Ð¸Ð¼Ð°ÐµÐ¼Ð°Ñ ÐºÐ°Ð¿ÐµÐ»ÑÐ½Ð°Ñ Ð¼Ð¾Ð´ÐµÐ»Ñ
Ð²ÑÑÐ¾Ð¶Ð´ÐµÐ½Ð½Ð¾Ðµ Ð²ÐµÑÐµÑÑÐ²Ð¾
Ð½ÐµÑÑÐµÑÐ¸ÑÐµÑÐºÐ¸Ðµ Ð°ÑÐ¾Ð¼Ð½ÑÐµ ÑÐ´ÑÐ°
ÑÐ°Ð²Ð½Ð¾Ð²ÐµÑÐ½Ð¾Ðµ ÑÐ¾ÑÑÐ¾ÑÐ½Ð¸Ðµ Ð²ÐµÑÐµÑÑÐ²Ð°
dense matter
neutron star
effective nuclear potential
compressible liquid drop model
degenerate matter
non-spherical atomic nuclei
equilibrium state of matter

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ Ð½ÐµÑÑÐµÑÐ¸ÑÐµÑÐºÐ¸Ñ ÑÐ´ÐµÑ Ð²Ð¾ Ð²Ð½ÑÑÑÐµÐ½Ð½ÐµÐ¹ ÐºÐ¾ÑÐµ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½Ð¾Ð¹ Ð·Ð²ÐµÐ·Ð´Ñ Ð½Ð° Ð¾ÑÐ½Ð¾Ð²Ðµ ÑÐ¶Ð¸Ð¼Ð°ÐµÐ¼Ð¾Ð¹ ÐºÐ°Ð¿ÐµÐ»ÑÐ½Ð¾Ð¹ Ð¼Ð¾Ð´ÐµÐ»Ð¸. Ð Ð°ÑÑÐµÑÑ Ð¿ÑÐ¾Ð²ÐµÐ´ÐµÐ½Ñ Ð´Ð»Ñ Ð½ÐµÑÐºÐ¾Ð»ÑÐºÐ¸Ñ Ð²Ð¸Ð´Ð¾Ð² ÑÑÑÐµÐºÑÐ¸Ð²Ð½Ð¾Ð³Ð¾ ÑÐ´ÐµÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾ÑÐµÐ½ÑÐ¸Ð°Ð»Ð° ÑÐ¸Ð¿Ð° Ð¡ÐºÐ¸ÑÐ¼Ð° SLy4, BSk24, BSk25, BSk26. ÐÐ»Ñ ÐºÐ°Ð¶Ð´Ð¾Ð³Ð¾ Ð¸Ð· Ð½Ð¸Ñ Ð²ÑÑÐ¸ÑÐ»ÐµÐ½Ñ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÐ¸ ÑÐ½ÐµÑÐ³Ð¸Ð¸ Ð´Ð»Ñ ÑÐµÑÑÐ¸ ÐºÐ¾Ð½ÑÐ¸Ð³ÑÑÐ°ÑÐ¸Ð¹ ÑÐ´ÐµÑÐ½Ð¾Ð³Ð¾ Ð²ÐµÑÐµÑÑÐ²Ð° (ÑÑÐµÑÐ¸ÑÐµÑÐºÐ¾Ðµ ÑÐ´ÑÐ¾, ÑÐ´ÑÐ¾ ÑÐ¸Ð»Ð¸Ð½Ð´ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÑÐ¾ÑÐ¼Ñ, Ð¿Ð»Ð¾ÑÐºÐ¾Ð¿Ð°ÑÐ°Ð»Ð»ÐµÐ»ÑÐ½ÑÐ¹ ÑÐ»Ð¾Ð¹, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¸Ð½Ð²ÐµÑÑÐ½ÑÐµ Ð¸Ð¼ ÐºÐ¾Ð½ÑÐ¸Ð³ÑÑÐ°ÑÐ¸Ð¸ Ð¸ Ð¾Ð´Ð½Ð¾ÑÐ¾Ð´Ð½Ð¾Ðµ ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ðµ Ð½ÑÐºÐ»Ð¾Ð½Ð¾Ð²). ÐÑÑÐ²Ð»ÐµÐ½Ð° Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÑ Ð½Ð°Ð¸Ð±Ð¾Ð»ÐµÐµ ÑÐ½ÐµÑÐ³ÐµÑÐ¸ÑÐµÑÐºÐ¸ Ð²ÑÐ³Ð¾Ð´Ð½Ð¾Ð³Ð¾ ÑÐ¾ÑÑÐ¾ÑÐ½Ð¸Ñ Ð¾Ñ ÐºÐ¾Ð½ÑÐµÐ½ÑÑÐ°ÑÐ¸Ð¸ Ð½ÑÐºÐ»Ð¾Ð½Ð¾Ð². ÐÐ»Ñ SLy4 Ð¼Ð¾Ð´ÐµÐ»Ñ Ð¿Ð¾ÐºÐ°Ð·Ð°Ð»Ð°, ÑÑÐ¾ ÑÐ½ÐµÑÐ³ÐµÑÐ¸ÑÐµÑÐºÐ¸ Ð²ÑÐ³Ð¾Ð´Ð½ÑÐ¼Ð¸ Ð´Ð¾ Ð¿ÐµÑÐµÑÐ¾Ð´Ð° Ðº Ð¾Ð´Ð½Ð¾ÑÐ¾Ð´Ð½Ð¾Ð¹ Ð¼Ð°ÑÐµÑÐ¸Ð¸ Ð¾ÑÑÐ°ÑÑÑÑ ÑÑÐµÑÐ¸ÑÐµÑÐºÐ¸Ðµ ÑÐ´ÑÐ°. ÐÐ»Ñ Ð±Ð¾Ð»ÐµÐµ ÑÐ¾Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ Ð¼Ð¾Ð´ÐµÐ»ÐµÐ¹ BSk Ð±ÑÐ»Ð° Ð¿Ð¾ÐºÐ°Ð·Ð°Ð½Ð° Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð¾ÑÑÑ ÑÑÑÐµÑÑÐ²Ð¾Ð²Ð°Ð½Ð¸Ñ Ð½ÐµÑÑÐµÑÐ¸ÑÐµÑÐºÐ¸Ñ ÑÐ´ÐµÑ. Ð ÐµÐ·ÑÐ»ÑÑÐ°ÑÑ Ð¼Ð¾Ð³ÑÑ Ð±ÑÑÑ Ð²Ð°Ð¶Ð½Ñ Ð´Ð»Ñ Ð¾Ð¿Ð¸ÑÐ°Ð½Ð¸Ñ ÐºÐ¸Ð½ÐµÑÐ¸ÑÐµÑÐºÐ¸Ñ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² (ÑÐ»ÐµÐºÑÑÐ¾Ð¿ÑÐ¾Ð²Ð¾Ð´Ð½Ð¾ÑÑÑ, ÑÐµÐ¿Ð»Ð¾Ð¿ÑÐ¾Ð²Ð¾Ð´Ð½Ð¾ÑÑÑ), Ð¸Ð³ÑÐ°ÑÑÐ¸Ñ ÐºÐ»ÑÑÐµÐ²ÑÑ ÑÐ¾Ð»Ñ Ð² Ð¾ÑÑÑÐ²Ð°Ð½Ð¸Ð¸ Ð¸ ÑÐ²Ð¾Ð»ÑÑÐ¸Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½ÑÑ Ð·Ð²ÑÐ·Ð´. ÐÐ½Ð¸ ÑÐ°ÐºÐ¶Ðµ Ð¼Ð¾Ð³ÑÑ Ð¾ÐºÐ°Ð·Ð°ÑÑÑÑ Ð²Ð°Ð¶Ð½ÑÐ¼Ð¸ Ð´Ð»Ñ Ð¾Ð¿Ð¸ÑÐ°Ð½Ð¸Ñ ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ñ ÑÐ¾ÑÑÐ¾ÑÐ½Ð¸Ñ Ð°ÐºÐºÑÐµÑÐ¸ÑÑÑÑÐ¸Ñ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½ÑÑ Ð·Ð²ÑÐ·Ð´.
description: The work is devoted to study of non-spherical nuclei in the inner crust of a neutron star within compressible liquid drop model. We apply several models of effective Skyrme type nuclear potentials SLy4, BSk24, BSk25, BSk26. For each of them we calculate the energy density for six configurations of nuclear matter (spherical nuclei, cylindrical nuclei, plate-like nuclei, inverse configurations, uniform distribution of protons and neutrons). It allows to identify the sequence of equilibrium nuclei shapes in the inner crust. For SLy4 spherical nuclei remain energetically favorable up to the transition to homogeneous matter. For more recent BSk models, the non-spherical nuclei predicted to exist in the inner layers of inner crust. The results are important for describing the kinetic processes (electrical and thermal conductivities) that play a key role in the cooling and evolution of the magnetic field of neutron stars. They may also be important for describing the equation of state of accreting neutron stars.