title: ÐÐ¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ Ð·ÐµÑÐºÐ°Ð»ÑÐ½Ð¾Ð¹ Ð½ÐµÑÑÑÐ¾Ð¹ÑÐ¸Ð²Ð¾ÑÑÐ¸ Ð² ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¼ Ð²ÐµÑÑÐµ
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: Modeling of mirror instability in the solar wind
Creators: name: Ð¡ÐµÐ²ÑÑÐºÐ¾Ð²Ð°, ÐÐ»ÐµÐºÑÐ°Ð½Ð´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: 2023
Subjects: Ð·ÐµÑÐºÐ°Ð»ÑÐ½Ð°Ñ Ð½ÐµÑÑÑÐ¾Ð¹ÑÐ¸Ð²Ð¾ÑÑÑ
ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÐ¹ Ð²ÐµÑÐµÑ
Ð±ÐµÑÑÑÐ¾Ð»ÐºÐ½Ð¾Ð²Ð¸ÑÐµÐ»ÑÐ½Ð°Ñ Ð¿Ð»Ð°Ð·Ð¼Ð°
Ð°Ð»ÑÐ²ÐµÐ½Ð¾Ð²ÑÐºÐ°Ñ Ð¸Ð¾Ð½Ð½Ð¾-ÑÐ¸ÐºÐ»Ð¾ÑÑÐ¾Ð½Ð½Ð°Ñ Ð½ÐµÑÑÑÐ¾Ð¹ÑÐ¸Ð²Ð¾ÑÑÑ
ÐºÐ¸Ð½ÐµÑÐ¸ÑÐµÑÐºÐ¾Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ
ÐºÐ¾Ð´ Â«LEOPARDÂ»
ÐºÐ¾Ð´ Â«MaximusÂ»
mirror instability
solar wind
collisionless plasma
alfven ion-cyclotron instability
kinetic modeling
LEOPARD code
Maximus code

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description: Direct observations in the solar wind make it possible to investigate various types of plasma instabilities that can act on particles, scattering and/or accelerating them. Quite often, mirror structures are observed, which are characterized by relative-ly large wavelengths and significant variations in the amplitude of the magnetic field. Mirror instability can arise due to the temperature anisotropy transverse to the mag-netic field Ð¢â¥&gt;Tâ. However, the increment calculation shows that the Alfven ion-cyclotron instability develops much faster in this case. It leads to a decrease in the temperature anisotropy necessary for mirror instability. Thus, the question arises about the nature of the observed mirror structures. In this paper, we consider the dis-tribution of hydrogen ions, which consists of the Maxwellian main population and the ring distribution of fast particles. Such distributions can arise near shock waves due to the reflection of part of the plasma at the front and further rotation in the magnetic field. From the analysis of the dispersion equation and with the help of kinetic model-ing, we come to the conclusion that in this situation the mirror instability will oscillate and dominate. This means that the mirror structures observed in the solar wind can be the result of annular distributions that arise when ions are reflected from the shock wave front.