title: ÐÐ·Ð¾ÑÐ¾Ð¿Ð½ÑÐµ Ð°Ð½Ð¾Ð¼Ð°Ð»Ð¸Ð¸ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¸Ñ Ð»ÑÑÐµÐ¹
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: Isotopic anomalies of solar cosmic rays
Creators: name: Ð¨Ð°ÑÐ°Ð³, Ð¡ÐµÑÐ³ÐµÐ¹
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: 2023
Subjects: Ð¸Ð·Ð¾ÑÐ¾Ð¿Ð½ÑÐµ Ð°Ð½Ð¾Ð¼Ð°Ð»Ð¸Ð¸
ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÐµ ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¸Ðµ ÑÐ°ÑÑÐ¸ÑÑ
ÑÐ¾Ð»Ð½ÑÐµ
ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÐ¹ Ð²ÐµÑÐµÑ
ÑÑÐ¾Ñ Ð°ÑÑÐ¸ÑÐµÑÐºÐ¾Ðµ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ðµ
isotopic anomalies
solar cosmic particles
sun
solar wind
stochastic acceleration

description: Ð ÑÐ°Ð±Ð¾ÑÐµ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¾ Ð°Ð½Ð°Ð»Ð¸ÑÐ¸ÑÐµÑÐºÐ¾Ðµ ÑÐµÑÐµÐ½Ð¸Ðµ ÑÑÐ°ÑÐ¸Ð¾Ð½Ð°ÑÐ½Ð¾Ð³Ð¾ ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ñ Ð¤Ð¾ÐºÐºÐµÑÐ°-ÐÐ»Ð°Ð½ÐºÐ°, Ð¾Ð¿Ð¸ÑÑÐ²Ð°ÑÑÐµÐ³Ð¾ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ðµ Ð¸ ÑÑÐµÑÐºÑ Ð¸Ð¾Ð½Ð¾Ð² Ð¸Ð· Ð½ÐµÐºÐ¾ÑÐ¾ÑÐ¾Ð¹ Ð²ÑÐ¿ÑÑÐµÑÐ½Ð¾Ð¹ Ð¾Ð±Ð»Ð°ÑÑÐ¸ Ð½Ð° Ð¡Ð¾Ð»Ð½ÑÐµ. ÐÐ¾Ð»Ð°Ð³Ð°Ð»Ð¾ÑÑ, ÑÑÐ¾ Ð¼ÐµÑÐ°Ð½Ð¸Ð·Ð¼ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ â ÑÑÐ¾ÑÐ°ÑÑÐ¸ÑÐµÑÐºÐ¾Ðµ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ðµ Ð¿ÑÐ¸ Ð²Ð·Ð°Ð¸Ð¼Ð¾Ð´ÐµÐ¹ÑÑÐ²Ð¸Ð¸ Ñ Ð¾Ð´Ð½Ð¾Ð¼ÐµÑÐ½ÑÐ¼Ð¸ ÐÐ»ÑÐ²ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ð¼Ð¸ Ð²Ð¾Ð»Ð½Ð°Ð¼Ð¸ Ð² Ð¾Ð´Ð½Ð¾ÑÐ¾Ð´Ð½Ð¾Ð¼ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð¼ Ð¿Ð¾Ð»Ðµ, Ð° ÑÑÐµÑÐºÐ° Ð¿ÑÐ¾Ð¸ÑÑÐ¾Ð´Ð¸Ñ Ð¿ÑÐ¸ Ð¿ÑÐ¾ÑÑÑÐ°Ð½ÑÑÐ²ÐµÐ½Ð½Ð¾Ð¹ Ð´Ð¸ÑÑÑÐ·Ð¸Ð¸ ÑÐ°ÑÑÐ¸Ñ Ð¸Ð· Ð¾Ð±Ð»Ð°ÑÑÐ¸ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ (Ð² Ð¿ÑÐ¸Ð±Ð»Ð¸Ð¶ÐµÐ½Ð¸Ð¸ Ð²ÑÐµÐ¼ÐµÐ½Ð¸ Ð²ÑÑÐ¾Ð´Ð°). ÐÐ¾ÑÑÑÐ¸ÑÐ¸ÐµÐ½ÑÑ Ð¿ÑÐ¾ÑÑÑÐ°Ð½ÑÑÐ²ÐµÐ½Ð½Ð¾Ð¹ Ð¸ Ð¸Ð¼Ð¿ÑÐ»ÑÑÐ½Ð¾Ð¹ Ð´Ð¸ÑÑÑÐ·Ð¸Ð¸ Ð¿ÑÐ¸ ÑÑÐ¾Ð¼ Ð·Ð°Ð²Ð¸ÑÑÑ Ð¾Ñ Ð¾ÑÐ½Ð¾ÑÐµÐ½Ð¸Ñ Ð·Ð°ÑÑÐ´Ð¾Ð²Ð¾Ð³Ð¾ Ð¸ Ð¼Ð°ÑÑÐ¾Ð²Ð¾Ð³Ð¾ ÑÐ¸ÑÐ»Ð° Ð¸Ð¾Ð½Ð¾Ð², Q/A, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¾Ñ Ð¿Ð¾ÐºÐ°Ð·Ð°ÑÐµÐ»Ñ ÑÐ¿ÐµÐºÑÑÐ° ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾ÑÑÐ¸, s. ÐÐ¾ÐºÐ°Ð·Ð°Ð½Ð¾, ÑÑÐ¾ Ð´Ð°Ð¶Ðµ Ð² ÑÑÐ¾Ð¹ Ð¿ÑÐ¾ÑÑÐ¾Ð¹ Ð¼Ð¾Ð´ÐµÐ»Ð¸ ÑÐ´Ð°ÐµÑÑÑ Ð¾Ð±ÑÑÑÐ½Ð¸ÑÑ Ð½Ð°Ð±Ð»ÑÐ´Ð°ÐµÐ¼Ð¾Ðµ Ð¾Ð±Ð¾Ð³Ð°ÑÐµÐ½Ð¸Ðµ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¸Ñ Ð»ÑÑÐµÐ¹ ÑÐµÐ´ÐºÐ¸Ð¼Ð¸ Ð¸Ð·Ð¾ÑÐ¾Ð¿Ð°Ð¼Ð¸ Ð¿Ð¾ ÑÑÐ°Ð²Ð½ÐµÐ½Ð¸Ñ Ñ Ð¸Ñ ÑÐ°ÑÐ¿ÑÐ¾ÑÑÑÐ°Ð½ÑÐ½Ð½Ð¾ÑÑÑÑ Ð² ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¼ Ð²ÐµÑÑÐµ (Ð² 1.3 â 4.4 ÑÐ°Ð·Ð°) Ð¿ÑÐ¸ s = 2.5 â 3. ÐÑÑÐ¾ÐºÐ¸Ð¹ Ð¿Ð¾ÐºÐ°Ð·Ð°ÑÐµÐ»Ñ ÑÐ¿ÐµÐºÑÑÐ° ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾ÑÑÐ¸, ÑÐºÐ¾ÑÐµÐµ Ð²ÑÐµÐ³Ð¾, ÑÐ¾Ð¾ÑÐ²ÐµÑÑÑÐ²ÑÐµÑ Ð½ÐµÑÑÑÐ°Ð½Ð¾Ð²Ð¸Ð²ÑÐµÐ¼ÑÑÑ Ð¿ÑÐ¾ÑÐµÑÑÑ Ð³ÐµÐ½ÐµÑÐ°ÑÐ¸Ð¸ ÑÑÐ¾Ð¹ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾ÑÑÐ¸ Ð² Ð¾Ð±Ð»Ð°ÑÑÐ¸ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ Ð²Ð¾ Ð²ÑÐµÐ¼Ñ ÑÐ°Ð¼Ð¾Ð¹ ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ Ð²ÑÐ¿ÑÑÐºÐ¸.
description: We obtained an analytical solution of the stationary Fokker-Planck equation describing the acceleration and leakage of ions from some flare region on the Sun. It was assumed that the acceleration mechanism is stochastic acceleration during in-teraction with one-dimensional Alvenov waves in a homogeneous magnetic field, while the leakage occurs during spatial diffusion of particles from the acceleration region (in the exit-time approximation). The spatial and momentum diffusion coef-ficients in this case depend on the charge and mass ion number ratio, Q/A, as well as on the power law index of turbulence, s. It is shown that even in this simple model the observed enrichment of solar cosmic rays with rare isotopes in compari-son with their distribution in the solar wind (1.3 - 4.4 times) at s = 2.5 - 3 can be explained. The high index of the turbulence spectrum most likely corresponds to the unsteady process of generation of this turbulence in the acceleration region dur-ing the solar flare itself.