title: ÐÑÐ¾ÑÑÑÐ°Ð½ÑÑÐ²ÐµÐ½Ð½Ð¾-Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐ¹ Ð°Ð½Ð°Ð»Ð¸Ð· ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð½Ð° ÑÑÐ±ÑÐµÐºÑÐ½Ð´Ð½Ð¾Ð¼ Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð¼ Ð¼Ð°ÑÑÑÐ°Ð±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: Spatio-temporal analysis of solar flares on a subsecond time scale
Creators: name: Ð§ÐµÑÐ½ÑÑÐ¾Ð²Ð°, ÐÐ²Ð³ÐµÐ½Ð¸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: 2023
Subjects: ÑÐ¾Ð»Ð½ÐµÑÐ½Ð°Ñ Ð²ÑÐ¿ÑÑÐºÐ°
Ð·Ð°Ð»Ð¸Ð¼Ð±Ð¾Ð²Ð¾Ðµ ÑÐ¾Ð±ÑÑÐ¸Ðµ
ÑÐ¿Ð°Ð¹ÐºÐ¾Ð²ÑÐµ ÑÑÑÑÐºÑÑÑÑ
Ð¶ÐµÑÑÐºÐ¾Ðµ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ
BATSE
Konus-Wind
solar flare
limb event
spike structures
hard X-ray emission

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð²ÑÑÐ²Ð»ÐµÐ½Ð¸Ñ ÑÑÐ±ÑÐµÐºÑÐ½Ð´Ð½ÑÑ (ÑÐ¿Ð°Ð¹ÐºÐ¾Ð²ÑÑ) ÑÑÑÑÐºÑÑÑ Ð² ÐºÐ¾ÑÐ¾Ð½Ð°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ°Ñ ÐÐ  Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº, Ñ Ð¿Ð¾Ð¼Ð¾ÑÑÑ ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¾Ð² Konus-Wind, BATSE, RHESSI. ÐÑÐ¸Ð²Ð»ÐµÐºÐ°ÑÐµÐ»ÑÐ½Ð¾ÑÑÑ Ð¸Ð·ÑÑÐµÐ½Ð¸Ñ Ð·Ð°Ð»Ð¸Ð¼Ð±Ð¾Ð²ÑÑ ÑÐ¾Ð±ÑÑÐ¸Ð¹ ÑÐ¾ÑÑÐ¾Ð¸Ñ Ð² ÑÐ¾Ð¼, ÑÑÐ¾ ÑÑÐºÐ¸Ðµ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ¸ ÐÐ  Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¸Ð· Ð¾ÑÐ½Ð¾Ð²Ð°Ð½Ð¸Ð¹ Ð²ÑÐ¿ÑÑÐµÑÐ½ÑÑ Ð¿ÐµÑÐµÐ»Ñ Ð½Ðµ Ð²Ð¸Ð´Ð½Ñ Ð´Ð»Ñ Ð½Ð°Ð±Ð»ÑÐ´ÐµÐ½Ð¸Ð¹. ÐÐ¾ÑÑÐ¾Ð¼Ñ ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÑÐµÐ¼Ð¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ Ð³ÐµÐ½ÐµÑÐ¸ÑÑÐµÑÑÑ Ð² Ð²ÐµÑÑÐ½ÐµÐ¹ ÑÐ°ÑÑÐ¸ Ð¿ÐµÑÐµÐ»Ñ. ÐÑ ÑÐµÐ³Ð¸ÑÑÑÐ°ÑÐ¸Ñ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð° Ð´ÐµÑÐµÐºÑÐ¾ÑÐ°Ð¼Ð¸ Ð¿Ð¾Ð»Ð½Ð¾Ð³Ð¾ Ð¡Ð¾Ð»Ð½ÑÐ°. ÐÐ»Ñ Ð°Ð½Ð°Ð»Ð¸Ð·Ð° Ð²ÑÐ¿ÑÑÐµÑÐ½Ð¾Ð³Ð¾ ÐÐ  Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¼Ð¸Ð»Ð»Ð¸ÑÐµÐºÑÐ½Ð´Ð½ÑÑ ÑÐ¿Ð°Ð¹ÐºÐ¾Ð²ÑÑ ÑÑÑÑÐºÑÑÑ Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼Ð¾ ÑÑÑÐ°Ð½Ð¾Ð²Ð¸ÑÑ ÐºÑÐ¸ÑÐµÑÐ¸Ð¸ Ð¸Ñ Ð¾Ð¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ñ, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¼ÐµÑÐ¾Ð´Ñ Ð¸Ñ Ð²ÑÑÐ²Ð»ÐµÐ½Ð¸Ñ, Ð¾ÑÐ½Ð¾Ð²Ð°Ð½Ð½ÑÐµ Ð½Ð° Ð²ÑÑÐ¸ÑÐ»ÐµÐ½Ð¸Ð¸ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ ÑÑÐ¾Ð²Ð½ÐµÐ¹ 3Ï. ÐÑÐ¾Ð¼Ðµ ÑÐ¾Ð³Ð¾, Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼Ð¾ Ð¿ÑÐ¾Ð°Ð½Ð°Ð»Ð¸Ð·Ð¸ÑÐ¾Ð²Ð°ÑÑ ÑÑÐ»Ð¾Ð²Ð¸Ñ Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼ÑÐµ Ð´Ð»Ñ Ð¾Ð±Ð½Ð°ÑÑÐ¶ÐµÐ½Ð¸Ñ ÐÐ  ÑÐ¿Ð°Ð¹ÐºÐ¾Ð² Ð² ÐºÐ¾ÑÐ¾Ð½Ð°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ°Ñ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº, ÑÐ°ÑÐ°ÐºÑÐµÑÐ¸ÑÑÐ¸ÐºÐ¸ Ð¿ÑÑÐºÐ° ÑÑÐºÐ¾ÑÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð¸ Ð¿Ð»Ð°Ð·Ð¼Ñ Ð² Ð¿ÐµÑÐµÐ»ÑÐ½ÑÑ ÑÑÑÑÐºÑÑÑÐ°Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ. Ð ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÐµ Ð°Ð½Ð°Ð»Ð¸Ð·Ð° Ð´Ð°Ð½Ð½ÑÑ Ð±ÑÐ»Ð¸ Ð¾ÑÐ¾Ð±ÑÐ°Ð½Ñ 5 Ð·Ð°Ð»Ð¸Ð¼Ð±Ð¾Ð²ÑÑ ÑÐ¾Ð±ÑÑÐ¸Ð¹. ÐÐµÑÐ°Ð»ÑÐ½ÑÐ¹ Ð°Ð½Ð°Ð»Ð¸Ð· ÐÐ  Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð½Ðµ Ð²ÑÑÐ²Ð¸Ð» ÑÐ¿Ð°Ð¹ÐºÐ¾Ð²ÑÐµ ÑÑÑÑÐºÑÑÑÑ Ð² ÐºÐ¾ÑÐ¾Ð½Ð°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ°Ñ Ð¶ÐµÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð² ÑÑÐ¸Ñ ÑÐ¾Ð±ÑÑÐ¸ÑÑ. ÐÐ¾Ð·Ð¼Ð¾Ð¶Ð½ÑÐ¼ Ð¾Ð±ÑÑÑÐ½ÐµÐ½Ð¸ÐµÐ¼ Ð¾ÑÑÑÑÑÑÐ²Ð¸Ñ ÑÐ¿Ð°Ð¹ÐºÐ¾Ð²Ð¾Ð¹ ÑÑÑÑÐºÑÑÑÑ Ð² Ð²ÐµÑÑÐ¸Ð½Ð°Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿ÐµÑÐµÐ»Ñ ÑÐ²Ð»ÑÐµÑÑÑ Ð½ÐµÐ´Ð¾ÑÑÐ°ÑÐ¾ÑÐ½Ð¾ Ð²ÑÑÐ¾ÐºÐ°Ñ ÐºÐ¾Ð½ÑÐµÐ½ÑÑÐ°ÑÐ¸Ñ Ð²ÑÐ¿ÑÑÐµÑÐ½Ð¾Ð¹ Ð¿Ð»Ð°Ð·Ð¼Ñ (Ð½Ð¸Ð¶Ðµ 5â10^(10) ÑÐ¼^(-3)) Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿Ð¸ÑÑ - ÑÐ³Ð»Ð¾Ð²Ð¾Ðµ ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ðµ ÑÑÐºÐ¾ÑÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð², Ð² ÐºÐ¾ÑÐ¾ÑÐ¾Ð¼ Ð¼Ð°Ð»Ð¾ (Ð¸Ð»Ð¸ Ð¾ÑÑÑÑÑÑÐ²ÑÑÑ Ð²Ð¾Ð²ÑÐµ) ÐºÐ²Ð°Ð·Ð¸Ð¿Ð¾Ð¿ÐµÑÐµÑÐ½Ð¾ ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð½ÑÑ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð².Â 
description: This work is devoted to the detection of subsecond (spike) structures in a coronal sources of solar flare hard X-rays using Konus-Wind, BATSE, RHESSI spectrometers. The attractiveness of the study of events behind the limb is that bright sources from the footpoints of flare loops are not visible for observations. Therefore, the observed radiation is generated in the upper part of the loops. Their registration is possible with the full Sun detectors. To analyze the flare hard X-ray radiation of millisecond spike structures, it is necessary to establish criteria for their determination, as well as methods for their detection based on the calculation of different levels 3Ï. In addition, it is necessary to analyze the conditions necessary for the detection of hard X-ray spikes in coronal sources of solar flares, the characteristics of the accelerated electron beam and plasma in the loop structures of the magnetic field. As a result of data analysis, 5 beyond-limb events were selected. A detailed analysis of the HR radiation did not reveal spike structures in the coronal hard X-ray sources in these events. A possible explanation for the absence of a spike structure at the tops of magnetic loops is an insufficiently high concentration of flare plasma (below 5â10^(10) cm^(-3)) as well as a pitch - angular distribution of accelerated electrons, in which there are few (or no at all) quasi-transversely distributed electrons.