title: ÐÐ°ÑÑÑÐ°Ð±Ñ Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð¶ÐµÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ Ð¸Ð½ÑÑÑÑÐ¼ÐµÐ½ÑÐ° ÐÐ¾Ð½ÑÑ-ÐÐ¸Ð½Ð´
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: Scales of variability of hard X-ray emission of solar flares based on the KONUS-WIND experiment data
Creators: name: ÐÑÐµÐ¹Ð¼ÐµÑ, ÐÑÑÐµÐ½Ð¸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: 2024
Subjects: ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÐµ Ð²ÑÐ¿ÑÑÐºÐ¸
Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ðµ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ðµ
Ð¶ÑÑÑÐºÐ¾Ðµ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ
Ð¼Ð¸Ð½Ð¸Ð¼Ð°Ð»ÑÐ½ÑÐ¹ Ð¼Ð°ÑÑÑÐ°Ð± Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸
Ð±Ð°Ð¹ÐµÑÐ¾Ð²ÑÐºÐ¸Ðµ Ð±Ð»Ð¾ÐºÐ¸
konus-wind
solar flares
magnetic reconnection
hard x-ray emission
minimum variability scale
bayesian blocks

description: ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð¶ÑÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ (HXR) ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº ÑÐ²Ð»ÑÐµÑÑÑ Ð²Ð°Ð¶Ð½ÑÐ¼ Ð´Ð»Ñ Ð¿Ð¾Ð½Ð¸Ð¼Ð°Ð½Ð¸Ñ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ñ Ð² ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ ÐºÐ¾ÑÐ¾Ð½Ðµ. Ð Ð°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð°Ð½Ð°Ð»Ð¸Ð·Ñ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ Ð¿ÑÐ¾ÑÐ¸Ð»ÐµÐ¹ HXR ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ ÑÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ° KONUS-WIND Ñ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸ÐµÐ¼ Ð¼ÐµÑÐ¾Ð´Ð° ÐÐ°Ð¹ÐµÑÐ¾Ð²ÑÐºÐ¸Ñ Ð±Ð»Ð¾ÐºÐ¾Ð² Ð´Ð»Ñ Ð¾ÑÐµÐ½ÐºÐ¸ Ð¼Ð¸Ð½Ð¸Ð¼Ð°Ð»ÑÐ½ÑÑ Ð¼Ð°ÑÑÑÐ°Ð±Ð¾Ð² Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸ (ÐÐÐ). ÐÐ½Ð°Ð»Ð¸Ð· Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½ Ð½Ð° Ð¾ÑÐ½Ð¾Ð²Ðµ Ð´Ð°Ð½Ð½ÑÑ Ñ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐ¼ ÑÐ°Ð·ÑÐµÑÐµÐ½Ð¸ÐµÐ¼ 16 Ð¸ 64 Ð¼Ð¸Ð»Ð»Ð¸ÑÐµÐºÑÐ½Ð´Ñ, Ð·Ð°ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½ÑÑ Ð´ÐµÑÐµÐºÑÐ¾ÑÐ°Ð¼Ð¸ S2 Ð½Ð° Ð±Ð¾ÑÑÑ ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¾Ð³Ð¾ Ð°Ð¿Ð¿Ð°ÑÐ°ÑÐ° KONUS-WIND Ð² Ð¿ÐµÑÐ¸Ð¾Ð´ Ñ 2000 Ð¿Ð¾ 2023 Ð³Ð¾Ð´. ÐÑÐ»Ð¸ Ð²ÑÑÐ²Ð»ÐµÐ½Ñ Ð¼Ð¸Ð½Ð¸Ð¼Ð°Ð»ÑÐ½ÑÐµ Ð¼Ð°ÑÑÑÐ°Ð±Ñ Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð´Ð»Ñ 839 Ð²ÑÐ¿ÑÑÐµÐº Ð¼ÐµÑÐ¾Ð´Ð¾Ð¼ ÐÐ°Ð¹ÐµÑÐ¾Ð²ÑÐºÐ¸Ñ Ð±Ð»Ð¾ÐºÐ¾Ð². Ð ÐµÐ·ÑÐ»ÑÑÐ°ÑÑ Ð¿Ð¾ÐºÐ°Ð·Ð°Ð»Ð¸, ÑÑÐ¾ Ð¼Ð¸Ð½Ð¸Ð¼Ð°Ð»ÑÐ½ÑÐ¹ Ð¼Ð°ÑÑÑÐ°Ð± Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð´Ð»Ñ Ð±Ð¾Ð»ÑÑÐ¸Ð½ÑÑÐ²Ð° Ð²ÑÐ¿ÑÑÐµÐº ÑÐ¾ÑÑÐ°Ð²Ð»ÑÐµÑ Ð¾ÐºÐ¾Ð»Ð¾ 1 ÑÐµÐºÑÐ½Ð´Ñ. Ð­ÑÐ¾ ÑÐ¾Ð¾ÑÐ²ÐµÑÑÑÐ²ÑÐµÑ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐ¼ Ð¼Ð°ÑÑÑÐ°Ð±Ð°Ð¼ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð¸ ÑÐºÐ¾ÑÐ¾ÑÑÐ¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ñ. ÐÐ¾Ð»ÑÑÐµÐ½Ð½ÑÐµ Ð´Ð°Ð½Ð½ÑÐµ Ð¿Ð¾Ð·Ð²Ð¾Ð»ÑÑÑ Ð»ÑÑÑÐµ Ð¿Ð¾Ð½ÑÑÑ Ð´Ð¸Ð½Ð°Ð¼Ð¸ÐºÑ Ð¸ ÑÑÑÐµÐºÑÐ¸Ð²Ð½Ð¾ÑÑÑ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ ÑÐ°ÑÑÐ¸Ñ Ð² ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ ÐºÐ¾ÑÐ¾Ð½Ðµ. Ð Ð°Ð±Ð¾ÑÐ° Ð²Ð½Ð¾ÑÐ¸Ñ Ð²ÐºÐ»Ð°Ð´ Ð² ÑÐ°Ð·Ð²Ð¸ÑÐ¸Ðµ ÑÐµÐ¾ÑÐ¸Ð¸ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð¸ Ð¼Ð¾Ð¶ÐµÑ Ð±ÑÑÑ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð° Ð´Ð»Ñ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¸Ñ Ð¾Ð³ÑÐ°Ð½Ð¸ÑÐµÐ½Ð¸Ð¹ Ð½Ð° Ð¼ÐµÑÐ°Ð½Ð¸Ð·Ð¼Ñ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð² ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐºÐ°Ñ.
description: The study of the variability of hard X-ray (HXR) emission of solar flares is crucial for understanding the processes of electron acceleration and magnetic reconnection in the solar corona. This work is devoted to the analysis of the HXR temporal profiles of solar flares using the KONUS-WIND experiment data, employing the Bayesian blocks method to estimate the minimum variability scales (MVS). The analysis was based on data with a time resolution of 16 and 64 milliseconds, recorded by the S2 detectors on board the KONUS-WIND spacecraft from 2000 to 2023. Minimum variability scales were identified for 839 flares using the Bayesian blocks method. The results showed that the minimum variability scale for most flares is approximately 1 second, corresponding to the temporal scales of electron acceleration and the rate of magnetic reconnection processes. The obtained data provide a better understanding of the dynamics and efficiency of particle acceleration processes in the solar corona. This work contributes to the development of solar flare theory and can be used for obtaining limitations on the acceleration mechanisms in solar flares .