title: ÐÑÐµÐ¼ÐµÐ½Ð½ÑÐµ Ð·Ð°Ð´ÐµÑÐ¶ÐºÐ¸ Ð¸ ÑÐ¿ÐµÐºÑÑÑ Ð»Ð¾ÐºÐ°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ¾Ð² 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
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: Time delays and spectra of local sources of hard x-ray radiation from solar flares
Creators: name: ÐÐ»ÐµÐ¼ÐµÐ½ÐºÐ¾Ð², ÐÐ¸ÑÐ¸Ð»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: ÑÐ¾Ð»Ð½ÐµÑÐ½Ð°Ñ Ð²ÑÐ¿ÑÑÐºÐ°
Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐµ Ð·Ð°Ð´ÐµÑÐ¶ÐºÐ¸
ÑÐ¿ÐµÐºÑÑÑ Ð»Ð¾ÐºÐ°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ¾Ð²
RHESSI
OSPEX
Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÑ ÑÑÐºÐ¾ÑÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð²
Ð¶ÐµÑÑÐºÐ¾Ðµ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ
Ð¼Ð¾Ð´ÐµÐ»Ñ ÑÐ¾Ð½ÐºÐ¾Ð¹ Ð¼Ð¸ÑÐµÐ½Ð¸
Ð¼Ð¾Ð´ÐµÐ»Ñ ÑÐ¾Ð»ÑÑÐ¾Ð¹ Ð¼Ð¸ÑÐµÐ½Ð¸
solar flare
time delays
spectra of local sources
parameters of accelerated electrons
hard x-ray emission
thin target model
thick target model

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð°Ð½Ð°Ð»Ð¸Ð·Ñ ÑÐ¿ÐµÐºÑÑÐ¾Ð² Ð¸ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ Ð·Ð°Ð´ÐµÑÐ¶ÐµÐº Ð¸Ð· Ð»Ð¾ÐºÐ°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ¾Ð² Ð¶ÐµÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ. ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¿ÑÐ¾Ð¸Ð·Ð²Ð¾Ð´Ð¸ÑÑÑ Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ Ð¿ÑÐ¸Ð±Ð¾ÑÐ° RHESSI Ð´Ð»Ñ Ð´Ð²ÑÑ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº: SOL2013-05-13T02:12 (X1.7) Ð¸ SOL2004-08-18T17:40 (X1.8). Ð Ð¿ÑÐ¾Ð³ÑÐ°Ð¼Ð¼Ð½ÑÑ Ð¿Ð°ÐºÐµÑÐ°Ñ SolarSoft Ð¸ OSPEX [11, 8], Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½Ð° Ð°Ð¿Ð¿ÑÐ¾ÐºÑÐ¸Ð¼Ð°ÑÐ¸Ñ 4 ÑÐµÐºÑÐ½Ð´Ð½ÑÑ ÑÐ¿ÐµÐºÑÑÐ¾Ð² ÐÐ  Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ ÑÐºÐ°Ð·Ð°Ð½Ð½ÑÑ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº. ÐÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð»Ð¸ÑÑ Ð´Ð²Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸: ÑÐµÐ¿Ð»Ð¾Ð²Ð°Ñ Ð¼Ð¾Ð´ÐµÐ»Ñ Ð¾Ð´Ð½Ð¾ÑÐµÐ¼Ð¿ÐµÑÐ°ÑÑÑÐ½Ð¾Ð¹ Ð¿Ð»Ð°Ð·Ð¼Ñ Ð² ÑÐ²ÑÐ·ÐºÐµ Ñ Ð¼Ð¾Ð´ÐµÐ»ÑÑ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ ÑÑÐºÐ¾ÑÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð² ÑÐ¾Ð½ÐºÐ¾Ð¹ Ð¸Ð»Ð¸ ÑÐ¾Ð»ÑÑÐ¾Ð¹ Ð¼Ð¸ÑÐµÐ½Ð¸. ÐÑÐµÐ´Ð¿Ð¾ÑÑÐ¸ÑÐµÐ»ÑÐ½Ð°Ñ Ð¼Ð¾Ð´ÐµÐ»Ñ Ð²ÑÐ±Ð¸ÑÐ°Ð»Ð°ÑÑ Ð¸ÑÑÐ¾Ð´Ñ Ð¸Ð· ÑÑÐ°Ð²Ð½Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð³Ð¾ Ð°Ð½Ð°Ð»Ð¸Ð·Ð° Ð´Ð»Ð¸Ð½Ñ ÑÐ²Ð¾Ð±Ð¾Ð´Ð½Ð¾Ð³Ð¾ Ð¿ÑÐ¾Ð±ÐµÐ³Ð° Ð¸Ð·Ð»ÑÑÐ°ÑÑÐ¸Ñ ÑÑÐºÐ¾ÑÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð¸ Ð³ÐµÐ¾Ð¼ÐµÑÑÐ¸ÑÐµÑÐºÐ¸Ñ ÑÐ°Ð·Ð¼ÐµÑÐ¾Ð² ÐÐ  Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ°. Ð¢Ð°ÐºÐ¶Ðµ Ð±ÑÐ»Ð¸ Ð¿Ð¾Ð»ÑÑÐµÐ½Ñ ÑÐ¿ÐµÐºÑÑÑ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ Ð·Ð°Ð´ÐµÑÐ¶ÐµÐº Ð¶ÐµÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¸ Ð¿ÑÐµÐ´Ð»Ð¾Ð¶ÐµÐ½Ð° Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð°Ñ Ð¸Ð½ÑÐµÑÐ¿ÑÐµÑÐ°ÑÐ¸Ñ ÑÑÐ¸Ñ ÑÐ¿ÐµÐºÑÑÐ¾Ð². ÐÑÐ¾Ð²ÐµÐ´ÐµÐ½Ð½ÑÐ¹ Ð°Ð½Ð°Ð»Ð¸Ð· Ð¿Ð¾Ð·Ð²Ð¾Ð»Ð¸Ð» Ð¾Ð±Ð¾ÑÐ½Ð¾Ð²Ð°ÑÑ Ð²ÑÐ±Ð¾Ñ Ð¼Ð¾Ð´ÐµÐ»Ð¸ ÑÐ¾Ð½ÐºÐ¾Ð¹ Ð¼Ð¸ÑÐµÐ½Ð¸ Ð¿ÑÐ¸ Ð°Ð¿Ð¿ÑÐ¾ÐºÑÐ¸Ð¼Ð°ÑÐ¸Ð¸ ÑÑÐµÐ¿ÐµÐ½Ð½Ð¾Ð¹ Ð¾Ð±Ð»Ð°ÑÑÐ¸ Ð² ÑÐ¿ÐµÐºÑÑÐ°Ñ Ð»Ð¾ÐºÐ°Ð»ÑÐ½ÑÑ ÐÐ  Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ¾Ð² Ð² Ð¾ÑÐ¾Ð±ÑÐ°Ð½Ð½ÑÑ Ð²ÑÐ¿ÑÑÐµÑÐ½ÑÑ ÑÐ¾Ð±ÑÑÐ¸ÑÑ. Ð Ð°ÑÑÑÐ¸ÑÐ°Ð½Ð½ÑÐµ ÑÐ¿ÐµÐºÑÑÑ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ Ð·Ð°Ð´ÐµÑÐ¶ÐµÐº ÐÐ  Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¼Ð¾Ð¶Ð½Ð¾ Ð¸Ð½ÑÐµÑÐ¿ÑÐµÑÐ¸ÑÐ¾Ð²Ð°ÑÑ, ÐµÑÐ»Ð¸ Ð´Ð¾Ð¿ÑÑÑÐ¸ÑÑ, ÑÑÐ¾ Ð² Ð¾Ð±Ð»Ð°ÑÑÐ¸ Ð¶ÐµÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¿ÑÐ¸ÑÑÑÑÑÐ²ÑÑÑ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÐµ Ð¿ÐµÑÐ»Ð¸ Ñ Ð²ÑÑÐ¾ÐºÐ¾Ð¹ Ð°ÑÐ¸Ð¼Ð¼ÐµÑÑÐ¸ÐµÐ¹ Ð² ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ, Ð²ÑÐ»ÐµÐ´ÑÑÐ²Ð¸Ðµ ÑÐµÐ³Ð¾ Ð·Ð°ÑÐ²Ð°Ñ Ð¸Ð¼Ð¸ ÑÑÐºÐ¾ÑÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð¾ÐºÐ°Ð·ÑÐ²Ð°ÐµÑÑÑ Ð½Ðµ ÑÑÑÐµÐºÑÐ¸Ð²Ð½ÑÐ¼.
description: The given work is devoted to the analysis of spectra and time delays from local hard X-ray sources. The study is based on RHESSI data for two solar flares: SOL2013-05-13T02:12 (X1.7) and SOL2004-08-18T17:40 (X1.8). Using SolarSoft, IDL and the OSPEX interface, the solar flare spectra were approximated by two models: a thermal model in conjunction with a thin or thick target model. The preferred model was chosen based on an analysis of the mean free path of the accelerated electrons and radiating volume dimensions. The time delay spectra of the hard X-rays were also obtained, and a possible interpretation of these spectra was provided. The results showed that, for the selected solar flares, the model of a thin target is the most suitable. The obtained spectra of time delays can be explained if we assume that in the region of hard X-rays, there are magnetic loops with high asymmetry in the magnetic field distribution, so that accelerated electrons are not efficiently captured.