title: ÐÐ½ÑÑÑÐµÐ½Ð½ÑÑ ÐºÐ¾ÑÐ° Ð°ÐºÐºÑÐµÑÐ¸ÑÑÑÑÐ¸Ñ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½ÑÑ Ð·Ð²ÐµÐ·Ð´: Ð½ÐµÐ¸Ð·Ð±ÐµÐ¶Ð½Ð¾ÑÑÑ Ð´Ð¸ÑÑÑÐ·Ð¸Ð¸ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð¾Ð² Ð¸ ÐµÐµ Ð¿Ð¾ÑÐ»ÐµÐ´ÑÑÐ²Ð¸Ñ
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¼Ð°Ð³Ð¸ÑÑÑÐ°
titleType: Subtitle
title: Inner crust of the accreting neutron stars: the inevitability of neutron diffusion and its consequences
Creators: name: Ð©ÐµÑÐ¸Ð»Ð¸Ð½, ÐÐ¸ÐºÐ¾Ð»Ð°Ð¹
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: 2020
Subjects: Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½Ð°Ñ Ð·Ð²ÐµÐ·Ð´Ð°
ÑÐ²ÐµÑÑ Ð¿Ð»Ð¾ÑÐ½Ð¾Ðµ Ð²ÐµÑÐµÑÑÐ²Ð¾
Ð²ÑÑÐ¾Ð¶Ð´ÐµÐ½Ð½Ð°Ñ Ð¼Ð°ÑÐµÑÐ¸Ñ
ÑÐ´ÐµÑÐ½ÑÐµ ÑÐµÐ°ÐºÑÐ¸Ð¸
ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ðµ ÑÐ¾ÑÑÐ¾ÑÐ½Ð¸Ñ
Ð´Ð¸ÑÑÑÐ·Ð¸Ð¾Ð½Ð½Ð¾Ðµ ÑÐ°Ð²Ð½Ð¾Ð²ÐµÑÐ¸Ðµ
Ð¼Ð°Ð»Ð¾Ð¼Ð°ÑÑÐ¸Ð²Ð½ÑÐµ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ðµ Ð´Ð²Ð¾Ð¹Ð½ÑÐµ Ð·Ð²ÐµÐ·Ð´Ñ
neutron star
superdense matter
degenerate matter
nuclear reactions
equation of state
diffusion equilibrium
low-mass x-ray binaries

description: Ð Ð°Ð·ÑÐ°Ð±Ð¾ÑÐ°Ð½ ÑÐ¿ÑÐ¾ÑÐµÐ½Ð½ÑÐ¹ Ð¼ÐµÑÐ¾Ð´ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ Ð¼Ð½Ð¾Ð³Ð¾ÐºÐ¾Ð¼Ð¿Ð¾Ð½ÐµÐ½ÑÐ½Ð¾Ð³Ð¾ ÑÐ¾ÑÑÐ°Ð²Ð°, ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ñ ÑÐ¾ÑÑÐ¾ÑÐ½Ð¸Ñ Ð¸ ÑÐ½ÐµÑÐ³Ð¾Ð²ÑÐ´ÐµÐ»ÐµÐ½Ð¸Ñ Ð² ÐºÐ¾ÑÐµ Ð°ÐºÐºÑÐµÑÐ¸ÑÑÑÑÐµÐ¹ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½Ð¾Ð¹ Ð·Ð²ÐµÐ·Ð´Ñ. Ð ÑÐ°Ð¼ÐºÐ°Ñ Ð¿ÑÐµÐ½ÐµÐ±ÑÐµÐ³Ð°ÑÑÐµÐ³Ð¾ Ð´Ð¸ÑÑÑÐ·Ð¸ÐµÐ¹ ÑÑÐ°Ð´Ð¸ÑÐ¸Ð¾Ð½Ð½Ð¾Ð³Ð¾ Ð¿Ð¾Ð´ÑÐ¾Ð´Ð° Ð¿ÑÐ¾Ð²ÐµÐ´ÐµÐ½ ÑÐ°ÑÑÐµÑ ÑÐ°ÑÐ°ÐºÑÐµÑÐ¸ÑÑÐ¸Ðº ÐºÐ¾ÑÑ Ð²Ð¿Ð»Ð¾ÑÑ Ð´Ð¾ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÐ¸ Ð¿Ð¾ÑÑÐ´ÐºÐ° Ï â 3.0 Ã 10^(12) Ð³/ÑÐ¼^3 . ÐÑÑÐ²Ð»ÐµÐ½Ð° Ð½ÐµÑÐ¾Ð³Ð»Ð°ÑÐ¾Ð²Ð°Ð½Ð½Ð¾ÑÑÑ Ð´Ð°Ð½Ð½Ð¾Ð³Ð¾ Ð¿Ð¾Ð´ÑÐ¾Ð´Ð°, Ð·Ð°ÐºÐ»ÑÑÐ°ÑÑÐ°ÑÑÑ Ð² Ð½Ð°ÑÑÑÐµÐ½Ð¸Ð¸ Ð´Ð¸ÑÑÑÐ·Ð¸Ð¾Ð½Ð½Ð¾Ð³Ð¾ ÑÐ°Ð²Ð½Ð¾Ð²ÐµÑÐ¸Ñ Ð´Ð»Ñ ÐºÐ¾Ð¼Ð¿Ð¾Ð½ÐµÐ½Ñ Ð²ÐµÑÐµÑÑÐ²Ð°. ÐÑÐµÐ´Ð»Ð¾Ð¶ÐµÐ½ Ð¼ÐµÑÐ¾Ð´ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ ÐºÐ¾ÑÑ Ð°ÐºÐºÑÐµÑÐ¸ÑÑÑÑÐ¸Ñ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½ÑÑ Ð·Ð²ÑÐ·Ð´ Ð² Ð¿ÑÐµÐ´ÐµÐ»Ðµ Ð±ÑÑÑÑÐ¾Ð¹ Ð´Ð¸ÑÑÑÐ·Ð¸Ð¸ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð¾Ð², Ð¸ Ð¿ÑÐ¾Ð¸Ð·Ð²ÐµÐ´ÐµÐ½ ÑÐ°ÑÑÐµÑ Ñ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÐ¼Ð¸ ÑÐ°Ð±Ð»Ð¸ÑÐ°Ð¼Ð¸ Ð°ÑÐ¾Ð¼Ð½ÑÑ Ð¼Ð°ÑÑ. ÐÐ¾ÐºÐ°Ð·Ð°Ð½Ð¾, ÑÑÐ¾ ÑÐ²Ð¾Ð¹ÑÑÐ²Ð° ÐºÐ¾ÑÑ ÑÑÑÐµÑÑÐ²ÐµÐ½Ð½Ð¾ Ð¾ÑÐ»Ð¸ÑÐ°ÑÑÑÑ Ð¾Ñ ÑÐ°ÑÑÑÐ¸ÑÐ°Ð½Ð½ÑÑ Ð² ÑÑÐ°Ð´Ð¸ÑÐ¸Ð¾Ð½Ð½Ð¾Ð¼ Ð¿Ð¾Ð´ÑÐ¾Ð´Ðµ. Ð ÑÐ°ÑÑÐ½Ð¾ÑÑÐ¸, Ð¿Ð¾Ð»Ð½Ð¾Ðµ ÑÐ½ÐµÑÐ³Ð¾Ð²ÑÐ´ÐµÐ»ÐµÐ½Ð¸Ðµ Ð² Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð½Ð¾Ð¹ Ð¾Ð±Ð»Ð°ÑÑÐ¸ (Ï . 3.0 Ã 10^(12) Ð³/ÑÐ¼^3 ) Ð½Ðµ Ð¿ÑÐµÐ²ÑÑÐ°ÐµÑ 0.4 ÐÑÐ Ð½Ð° Ð±Ð°ÑÐ¸Ð¾Ð½ Ð°ÐºÐºÑÐµÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ð³Ð¾ Ð²ÐµÑÐµÑÑÐ²Ð°, Ð° Ð½ÐµÐ¾Ð´Ð½Ð¾ÑÐ¾Ð´Ð½Ð¾ÑÑÑ ÑÐ¾ÑÑÐ°Ð²Ð°
Ð¼Ð¾Ð¶ÐµÑ Ð¿Ð¾Ð»Ð½Ð¾ÑÑÑÑ Ð¾Ð¿ÑÐµÐ´ÐµÐ»ÑÑÑÑ ÑÐµÐ°ÐºÑÐ¸ÑÐ¼Ð¸ Ð²Ð±Ð»Ð¸Ð·Ð¸ Ð³ÑÐ°Ð½Ð¸ÑÑ Ð²Ð½ÐµÑÐ½ÐµÐ¹ Ð¸ Ð²Ð½ÑÑÑÐµÐ½Ð½ÐµÐ¹ ÐºÐ¾ÑÑ. Ð ÐµÐ·ÑÐ»ÑÑÐ°ÑÑ ÑÐ°ÑÑÐµÑÐ¾Ð² Ð´ÐµÐ¼Ð¾Ð½ÑÑÑÐ¸ÑÑÑÑ Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼Ð¾ÑÑÑ Ð¿ÐµÑÐµÑÐ¼Ð¾ÑÑÐ° Ð¿ÑÐµÐ´ÑÐµÑÑÐ²ÑÑÑÐ¸Ñ Ð¸Ð½ÑÐµÑÐ¿ÑÐµÑÐ°ÑÐ¸Ð¹ Ð½Ð°Ð±Ð»ÑÐ´Ð°ÑÐµÐ»ÑÐ½ÑÑ Ð´Ð°Ð½Ð½ÑÑ Ð¿Ð¾ Ð¼Ð°Ð»Ð¾Ð¼Ð°ÑÑÐ¸Ð²Ð½ÑÐ¼ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ð¼ Ð´Ð²Ð¾Ð¹Ð½ÑÐ¼ ÑÐ¸ÑÑÐµÐ¼Ð°Ð¼ Ð¸ ÑÐ¾Ð¾ÑÐ²ÐµÑÑÑÐ²ÑÑÑÐ¸Ñ Ð¾Ð³ÑÐ°Ð½Ð¸ÑÐµÐ½Ð¸Ð¹ Ð½Ð° Ð²Ð·Ð°Ð¸Ð¼Ð¾Ð´ÐµÐ¹ÑÑÐ²Ð¸Ñ Ð²ÐµÑÐµÑÑÐ²Ð° Ð² ÑÐºÑÑÑÐµÐ¼Ð°Ð»ÑÐ½ÑÑ ÑÑÐ»Ð¾Ð²Ð¸ÑÑ Ð½ÐµÐ´Ñ Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½ÑÑ Ð·Ð²ÐµÐ·Ð´.
description: We construct a simplified multicomponent reaction network for calculating composition, equation of state, and heat release in the crust of accreting neutron stars. We calculate the crust properties up to Ï â 3.0 Ã 10^(12) g/cm^3 within the traditional approach, which neglects diffusion. It allows us to reveal the inconsistency of the traditional approach, caused by the violation of diffusion equilibrium for matter components. We propose a method for modeling the crust of accreting neutron stars in the limit of fast diffusion of neutrons and implement it, using a set of atomic masses models. The accreted crust properties are shown to be in strong contrast with previously discussed predictions of the traditional approach. In particular, the total heat release is less than 0.4 MeV per accreted baryon at the end of the simulation (Ï â 3.0 Ã 10^(12) g/cm^3 ), and the inner crust composition becomes simpler. These results call for a reinterpretation of observations of low-mass X-ray binaries and corresponding constraints on matter interactions in the extreme conditions of the neutron stars interior.