title: ÐÐÐ-Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ Ð°Ð½Ð¸Ð·Ð¾ÑÑÐ¾Ð¿Ð¸Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿Ð¾Ð»ÐµÐ¹ Ð²Ð±Ð»Ð¸Ð·Ð¸ Ð°ÑÑÑÐ¾ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ñ ÑÐ´Ð°ÑÐ½ÑÑ Ð²Ð¾Ð»Ð½
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: MHD modeling of magnetic field anisotropy in the vicinity of astrophysical shocks
Creators: name: ÐÐ¾Ð¼Ð»ÐµÐ², ÐÐ¾Ð½ÑÑÐ°Ð½ÑÐ¸Ð½
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: 2024
Subjects: ÐÐÐ-Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ
Ð±ÐµÑÑÑÐ¾Ð»ÐºÐ½Ð¾Ð²Ð¸ÑÐµÐ»ÑÐ½ÑÐµ ÑÐ´Ð°ÑÐ½ÑÐµ Ð²Ð¾Ð»Ð½Ñ
Ð¾ÑÑÐ°ÑÐºÐ¸ ÑÐ²ÐµÑÑ Ð½Ð¾Ð²ÑÑ
Ð¿Ð¾Ð»ÑÑÐ¸Ð·Ð°ÑÐ¸Ñ
ÑÑÐ¸Ð»ÐµÐ½Ð¸Ðµ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿Ð¾Ð»ÐµÐ¹
MHD modeling
collisionless shocks
supernova remnants
polarization
magnetic fields amplification

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ Ð¿Ð¾Ð²ÐµÐ´ÐµÐ½Ð¸Ñ ÐºÐ¾Ð¼Ð¿Ð¾Ð½ÐµÐ½Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ Ð·Ð° ÑÑÐ¾Ð½ÑÐ¾Ð¼ ÑÐ´Ð°ÑÐ½Ð¾Ð¹ Ð²Ð¾Ð»Ð½Ñ Ð¿Ð¾ÑÐ»Ðµ Ð¿ÑÐ¾ÑÐ¾Ð¶Ð´ÐµÐ½Ð¸Ðµ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÐ¼Ð¸ ÑÐ»ÑÐºÑÑÐ°ÑÐ¸ÑÐ¼Ð¸ ÑÑÐ¾Ð½ÑÐ°. ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¿ÑÐ¾Ð²Ð¾Ð´Ð¸Ð»Ð¾ÑÑ Ñ Ð¿Ð¾Ð¼Ð¾ÑÑÑ Ð¼Ð°Ð³Ð½Ð¸ÑÐ¾Ð³Ð¸Ð´ÑÐ¾Ð´Ð¸Ð½Ð°Ð¼Ð¸ÑÐµÑÐºÐ¾Ð³Ð¾ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ Ñ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸ÐµÐ¼ ÐºÐ¾Ð´Ð° PLUTO. ÐÐ·ÑÑÐµÐ½Ð¸Ðµ Ð²ÑÑÐµÐ¾Ð¿Ð¸ÑÐ°Ð½Ð½Ð¾Ð³Ð¾ ÑÐ²Ð»ÐµÐ½Ð¸Ñ ÑÐ²ÑÐ·Ð°Ð½Ð¾ Ð½Ð°Ð¿ÑÑÐ¼ÑÑ Ñ Ð¸Ð½ÑÐµÑÐµÑÐ¾Ð¼ ÐºÐ°ÑÐ°ÑÐµÐ»ÑÐ½Ð¾ Ð¿Ð¾ÑÐ²Ð»ÐµÐ½Ð¸Ñ Ð°Ð½Ð¸Ð·Ð¾ÑÑÐ¾Ð¿Ð¸Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿Ð¾Ð»ÐµÐ¹ Ð·Ð° ÑÑÐ¾Ð½ÑÐ¾Ð¼ Ð°ÑÑÑÐ¾ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ñ ÑÐ´Ð°ÑÐ½ÑÑ Ð²Ð¾Ð»Ð½. ÐÐ¿Ð¸ÑÐ°Ð½Ð½Ð°Ñ Ð°Ð½Ð¸Ð·Ð¾ÑÑÐ¾Ð¿Ð¸Ñ Ð²Ð»Ð¸ÑÐµÑ Ð½Ð° Ð¿Ð¾ÑÐ²Ð»ÐµÐ½Ð¸Ðµ Ð¿Ð¾Ð»ÑÑÐ¸Ð·Ð°ÑÐ¸Ð¸ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ, Ð±Ð»Ð¸Ð·ÐºÐ¾Ð¹ Ðº ÑÐ°Ð´Ð¸Ð°Ð»ÑÐ½Ð¾Ð¹ Ð² ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð¾ÑÑÐ°ÑÐºÐ°Ñ ÑÐ²ÐµÑÑÐ½Ð¾Ð²ÑÑ, Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð½ÑÑ Ñ Ð¿Ð¾Ð¼Ð¾ÑÑÑ ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¾Ð¹ Ð¾Ð±ÑÐµÑÐ²Ð°ÑÐ¾ÑÐ¸Ð¸ IXPE â SN 1006, Ð¢Ð¸ÑÐ¾. Ð ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÐµ Ð±ÑÐ»Ð¾ Ð¿ÑÐ¾Ð²ÐµÐ´ÐµÐ½Ð¾ Ð¼Ð½Ð¾Ð¶ÐµÑÑÐ²Ð¾ ÑÐ°ÑÑÑÑÐ¾Ð² Ð´Ð»Ñ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð¼Ð¾Ð´ÐµÐ»ÐµÐ¹, Ð¿Ð¾Ð·Ð²Ð¾Ð»ÑÑÑÐ¸Ðµ Ð¿ÑÐ¾Ð´ÐµÐ¼Ð¾Ð½ÑÑÑÐ¸ÑÐ¾Ð²Ð°ÑÑ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ñ ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ñ ÐºÐ¾Ð¼Ð¿Ð¾Ð½ÐµÐ½Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿Ð¾Ð»ÐµÐ¹ Ð·Ð° ÑÑÐ¾Ð½ÑÐ¾Ð¼ ÑÐ´Ð°ÑÐ½Ð¾Ð¹ Ð²Ð¾Ð»Ð½Ñ Ð² Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÐ¸ Ð¾Ñ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð¿Ð»Ð°Ð·Ð¼Ñ Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ Ð¿ÐµÑÐµÐ´ ÑÑÐ¾Ð½ÑÐ¾Ð¼ ÑÐ´Ð°ÑÐ½Ð¾Ð¹ Ð²Ð¾Ð»Ð½Ñ. ÐÐ¾Ð´ÐµÐ»Ð¸ Ð±ÑÐ»Ð¸ ÑÐ°Ð·Ð´ÐµÐ»ÐµÐ½Ñ Ð½Ð° Ð´Ð²Ðµ Ð³ÑÑÐ¿Ð¿Ñ: Ð¿ÑÐ¾ÑÑÐµÐ¹ÑÐ¸Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸ Ñ Ð¿Ð¾ÑÑÐ¾ÑÐ½Ð½ÑÐ¼ Ð¿Ð¾Ð»ÐµÐ¼ Ð¸ Ð¿ÑÐ¾ÑÑÐ¾Ð¹ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾ÑÑÑÑ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ, Ð° ÑÐ°ÐºÐ¶Ðµ Ñ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾ÑÑÑÑ, Ð¾Ð±ÑÑÐ»Ð¾Ð²Ð»ÐµÐ½Ð½Ð¾Ð¹ Ð½ÐµÑÑÑÐ¾Ð¹ÑÐ¸Ð²Ð¾ÑÑÑÑ ÐÐµÐ»Ð»Ð°. ÐÑÑÐ²Ð»ÐµÐ½Ð¾, ÑÑÐ¾ Ð´Ð°Ð½Ð½Ð°Ñ Ð°Ð½Ð¸Ð·Ð¾ÑÑÐ¾Ð¿Ð¸Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ Ð·Ð° ÑÑÐ¾Ð½ÑÐ¾Ð¼ ÑÐ´Ð°ÑÐ½Ð¾Ð¹ Ð²Ð¾Ð»Ð½Ñ Ð²Ð¾Ð·Ð½Ð¸ÐºÐ°ÐµÑ Ð¿ÑÐ¸ Ð¿ÑÐ¾ÑÐ¾Ð¶Ð´ÐµÐ½Ð¸Ñ ÐºÐ¾Ð»ÐµÐ±Ð°Ð½Ð¸Ð¹ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÐ¸ ÑÐµÑÐµÐ· ÑÐ´Ð°ÑÐ½ÑÑ Ð²Ð¾Ð»Ð½Ñ (Ð² ÑÐ°ÑÑÐ½Ð¾ÑÑÐ¸, Ð¿ÑÐ¸ ÑÐ°Ð·Ð²Ð¸ÑÐ¸Ð¸ Ð±ÐµÐ»Ð»Ð¾Ð²ÑÐºÐ¾Ð¹ Ð½ÐµÑÑÑÐ¾Ð¹ÑÐ¸Ð²Ð¾ÑÑÐ¸ Ð² Ð¿ÑÐµÐ´ÑÑÐ¾Ð½ÑÐµ ÑÐ´Ð°ÑÐ½Ð¾Ð¹ Ð²Ð¾Ð»Ð½Ñ Ð²Ð¾Ð·Ð½Ð¸ÐºÐ°ÑÑ ÑÐ¸Ð»ÑÐ½ÑÐµ ÐºÐ¾Ð»ÐµÐ±Ð°Ð½Ð¸Ñ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÐ¸).
description: This given work is devoted to the study of the behavior of the magnetic field components behind the shock wave front after the passage of magnetic fluctuations of the front. The study was conducted using magnetohydrodynamic modeling using the PLUTO code. The research of the above phenomenon is related to the interest in the appearance of anisotropy of magnetic fields behind the front of astrophysical shocks. The described anisotropy affects the appearance of polarization of X-ray radiation close to radial in various supernova remnants studied using IXPE â SN 1006, Tycho. As a result, many calculations were performed for various models, which made it possible to demonstrate changes in the distribution of magnetic field components behind the shock wave front depending on various plasma parameters and the magnetic field in front of the shock wave front. The models were divided into two groups: the simplest models with a constant field and simple turbulence of the magnetic field, as well as turbulence caused by Bell instability. It is revealed that this anisotropy of the magnetic field behind the shock wave front occurs when density fluctuations pass through the shock wave (in particular, with the development of the Bell instability, strong density fluctuations occur in the front of the shock wave).