title: ÐÐ·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ Ð¸Ð·Ð¾ÑÐ¾Ð¿Ð½Ð¾Ð³Ð¾ ÑÐ¾ÑÑÐ°Ð²Ð° Ð¾Ð±Ð»Ð°ÐºÐ¾Ð² Ð¼ÐµÐ¶Ð·Ð²ÐµÐ·Ð´Ð½Ð¾Ð¹ ÑÑÐµÐ´Ñ Ð²ÑÐ»ÐµÐ´ÑÑÐ²Ð¸Ðµ Ð°Ð½Ð½Ð¸Ð³Ð¸Ð»ÑÑÐ¸Ð¸ ÑÐ°ÑÑÐ¸Ñ ÑÐµÐ¼Ð½Ð¾Ð¹ Ð¼Ð°ÑÐµÑÐ¸Ð¸
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: Dark matter annihilation effect on the composition of the interstellar medium
Creators: name: ÐÑÐ¾ÐºÐ°ÑÐµÐ²Ð°, Ð®Ð»Ð¸Ñ
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: 2022
Subjects: ÐºÐ¾ÑÐ¼Ð¾Ð»Ð¾Ð³Ð¸Ñ
Ð¿ÐµÑÐ²Ð¸ÑÐ½ÑÐ¹ ÑÐ¾ÑÑÐ°Ð² Ð²ÐµÑÐµÑÑÐ²Ð°
ÑÐµÐ¼Ð½Ð°Ñ Ð¼Ð°ÑÐµÑÐ¸Ñ
Ð¿ÐµÑÐ²Ð¸ÑÐ½ÑÐ¹ Ð½ÑÐºÐ»ÐµÐ¾ÑÐ¸Ð½ÑÐµÐ·
cosmology
primordial abundances
dark matter
Big-Bang nucleosynthesis

description: Ð¢ÐµÐ¼Ð° Ð²ÑÐ¿ÑÑÐºÐ½Ð¾Ð¹ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÑ: Â«ÐÐ·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ Ð¸Ð·Ð¾ÑÐ¾Ð¿Ð½Ð¾Ð³Ð¾ ÑÐ¾ÑÑÐ°Ð²Ð° Ð¾Ð±Ð»Ð°ÐºÐ¾Ð² Ð¼ÐµÐ¶Ð·Ð²ÐµÐ·Ð´Ð½Ð¾Ð¹ ÑÑÐµÐ´Ñ Ð²ÑÐ»ÐµÐ´ÑÑÐ²Ð¸Ðµ Ð°Ð½Ð½Ð¸Ð³Ð¸Ð»ÑÑÐ¸Ð¸ ÑÐ°ÑÑÐ¸Ñ ÑÐµÐ¼Ð½Ð¾Ð¹ Ð¼Ð°ÑÐµÑÐ¸Ð¸Â». ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¾ Ð²Ð»Ð¸ÑÐ½Ð¸Ðµ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² Ð°Ð½Ð½Ð¸Ð³Ð¸Ð»ÑÑÐ¸Ð¸ Ï--ÑÐ°ÑÑÐ¸Ñ -- ÑÐ°ÑÑÐ¸Ñ ÑÐµÐ¼Ð½Ð¾Ð¹ Ð¼Ð°ÑÐµÑÐ¸Ð¸ -- Ð½Ð° Ð¸Ð·Ð¾ÑÐ¾Ð¿Ð½ÑÐ¹ ÑÐ¾ÑÑÐ°Ð² Ð²ÐµÑÐµÑÑÐ²Ð° Ð²Ð¾ ÐÑÐµÐ»ÐµÐ½Ð½Ð¾Ð¹. ÐÑÐ»Ð¸ ÑÐ°ÑÑÑÐ¸ÑÐ°Ð½Ñ ÑÐºÐ¾ÑÐ¾ÑÑÐ¸ ÑÐ°Ð·ÑÑÑÐµÐ½Ð¸Ñ Ð¸ Ð½Ð°ÑÐ°Ð±Ð¾ÑÐºÐ¸ ÑÐ´ÐµÑ D, 3He Ð¸ 4He Ð² ÑÑÐ»Ð¾Ð²Ð¸ÑÑ Ð¾Ð±Ð»ÑÑÐµÐ½Ð¸Ñ Ð¿Ð¾ÑÐ»Ðµ Ð¿ÐµÑÐ²Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð½ÑÐºÐ»ÐµÐ¾ÑÐ¸Ð½ÑÐµÐ·Ð° Ð´Ð»Ñ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð¼Ð°ÑÑÑ Ð¸ ÑÐµÑÐµÐ½Ð¸Ñ Ð°Ð½Ð½Ð¸Ð³Ð¸Ð»ÑÑÐ¸Ð¸ Ï--ÑÐ°ÑÑÐ¸Ñ. ÐÐ¾ÐºÐ°Ð·Ð°Ð½Ð¾, ÑÑÐ¾ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ ÑÐ¾Ð´ÐµÑÐ¶Ð°Ð½Ð¸Ñ D Ð¸ 3He Ð¿ÑÐ¸ ÑÑÑÐµÑÑÐ²ÑÑÑÐ¸Ñ Ð¾Ð³ÑÐ°Ð½Ð¸ÑÐµÐ½Ð¸Ñ Ð½Ð° ÑÐµÐ¿Ð»Ð¾Ð²Ð¾Ðµ ÑÐµÐ»Ð¸ÐºÑÐ¾Ð²Ð¾Ðµ ÑÐµÑÐµÐ½Ð¸Ðµ Ð°Ð½Ð½Ð¸Ð³Ð¸Ð»ÑÑÐ¸Ð¸ Ð¼Ð¾Ð¶ÐµÑ Ð´Ð¾ÑÑÐ¸Ð³Ð°ÑÑ 1e-7 - 1e-8. ÐÑÐµÐ´Ð¿Ð¾Ð»Ð°Ð³Ð°Ð»Ð¾ÑÑ, ÑÑÐ¾ Ð¿ÑÐ¾ÑÐµÑÑÑ Ð°Ð½Ð½Ð¸Ð³Ð¸Ð»ÑÑÐ¸Ð¸ Ð² Ð¾Ð±Ð»Ð°ÑÑÑÑ Ð¿Ð¾Ð²ÑÑÐµÐ½Ð½Ð¾Ð¹ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÐ¸ ÑÐ°ÑÑÐ¸Ñ ÑÐµÐ¼Ð½Ð¾Ð¹ Ð¼Ð°ÑÐµÑÐ¸Ð¸ ÑÐ°ÐºÐ¶Ðµ Ð¼Ð¾Ð³ÑÑ Ð¿ÑÐ¸Ð²Ð¾Ð´Ð¸ÑÑ Ðº Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ñ Ð¸Ð·Ð¾ÑÐ¾Ð¿Ð½Ð¾Ð³Ð¾ ÑÐ¾ÑÑÐ°Ð²Ð° ÑÑÐµÐ´Ñ. ÐÐ»Ñ Ð²ÐµÑÑÐ½ÐµÐ¹ Ð¾ÑÐµÐ½ÐºÐ¸ ÑÑÑÐµÐºÑÐ° Ð±ÑÐ»Ð¸ Ð²ÑÐ±ÑÐ°Ð½Ñ ÑÑÐµÐ·Ð²ÑÑÐ°Ð¹Ð½Ð¾ Ð¾Ð±Ð¾Ð³Ð°ÑÐµÐ½Ð½ÑÐµ ÑÐµÐ¼Ð½Ð¾Ð¹ Ð¼Ð°ÑÐµÑÐ¸ÐµÐ¹ ÐºÐ°ÑÐ»Ð¸ÐºÐ¾Ð²ÑÐµ Ð³Ð°Ð»Ð°ÐºÑÐ¸ÐºÐ¸. ÐÐ¾ÐºÐ°Ð·Ð°Ð½Ð¾, ÑÑÐ¾ Ð² ÑÐ°ÐºÐ¸Ñ Ð¾Ð±ÑÐµÐºÑÐ°Ñ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ ÑÐ¾Ð´ÐµÑÐ¶Ð°Ð½Ð¸Ñ D Ð¿Ð¾ Ð¾ÑÐ½Ð¾ÑÐµÐ½Ð¸Ñ Ðº Ð¿ÐµÑÐ²Ð¸ÑÐ½Ð¾Ð¼Ñ Ð¼Ð¾Ð¶ÐµÑ Ð´Ð¾ÑÑÐ¸Ð³Ð°ÑÑ Ð·Ð½Ð°ÑÐµÐ½Ð¸Ñ 0.1, 3He Ð·Ð½Ð°ÑÐµÐ½Ð¸Ñ 0.1-1. Ð­ÑÐ¾, Ð¾Ð´Ð½Ð°ÐºÐ¾, Ð¿ÑÐ¸Ð²Ð¾Ð´Ð¸Ð»Ð¾ Ð±Ñ Ðº Ð¿Ð¾ÑÐ²Ð»ÐµÐ½Ð¸Ñ Ð¸Ð·Ð±ÑÑÐ¾ÑÐ½Ð¾Ð³Ð¾ Ð³Ð°Ð¼Ð¼Ð°--ÑÐ¾Ð½Ð°. ÐÐ°Ð½Ð½ÑÐµ Ð¿Ð¾ Ð½Ð°Ð±Ð»ÑÐ´Ð°ÐµÐ¼Ð¾Ð¼Ñ Ð³Ð°Ð¼Ð¼Ð°--ÑÐ¾Ð½Ñ Ð¾Ð³ÑÐ°Ð½Ð¸ÑÐ¸Ð²Ð°ÑÑ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð¾Ðµ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ D Ð½Ð° ÑÑÐ¾Ð²Ð½Ðµ 1e-5 Ð¸ 3He Ð½Ð° ÑÑÐ¾Ð²Ð½Ðµ 1e-4 Ð² ÐºÐ°ÑÐ»Ð¸ÐºÐ¾Ð²ÑÑ Ð³Ð°Ð»Ð°ÐºÑÐ¸ÐºÐ°Ñ. Â 
description: The subject of this research is âDark matter annihilation effect on the composition of the interstellar mediumâ. Â We study effects of dark matter particles annihilation on the composition of the Universe. The aim of research is to calculate abundances of light nuclei and, using the result, to derive constraints on Ï-particle properties.We will see, that D and 3He production provide upper bounds on annihilation cross section and Ï-particle abundance. However, according to the independent constraints on annihilation cross section, D and 3He abundances variation are allowed at the level 1e-8 - 1e-7. We also study annihilation effects in old and extremely enriched in dark matter regions -- dwarf galaxies. We will see that D and 3He abundances may vary at the level 0.01 - 1, but it would cause an excess gamma-ray flux. Therefore, 3He and D abundances variation are allowed at the level 1e-4-1e-5 in the ordinary dwarf galaxy.