title: ÐÑÐµÐ´Ð²ÐµÑÑÐ½Ð¸ÐºÐ¸ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº. ÐÐ½Ð°Ð»Ð¸Ð· ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸ ÑÐ»ÑÑÑÐ°ÑÐ¸Ð¾Ð»ÐµÑÐ¾Ð²Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð½Ð° ÑÑÐ°Ð´Ð¸Ð¸ Ð¿ÑÐµÐ´Ð²ÐµÑÑÐ½Ð¸ÐºÐ°
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: Precursors of solar flares. Analysis of X-ray and ultraviolet radiation at the precursor stage
Creators: name: Ð¨Ð¾ÑÐ¸Ð½, Ð¢Ð¸Ð¼Ð¾ÑÐµÐ¹
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Ð½ÑÐµ Ð²ÑÐ¿ÑÑÐºÐ¸
Ð¿ÑÐµÐ´Ð²ÐµÑÑÐ½Ð¸ÐºÐ¸
ÑÐ¾Ð»Ð½ÐµÑÐ½Ð°Ñ ÑÐ²ÐµÑÐ¸Ð¼Ð¾ÑÑÑ
Ð°ÐºÑÐ¸Ð²Ð½Ð°Ñ Ð¾Ð±Ð»Ð°ÑÑÑ
ÐºÐ¾Ð½ÑÐ¸Ð³ÑÑÐ°ÑÐ¸Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ
Ð°ÑÐ¼Ð¾ÑÑÐµÑÐ° Ð¡Ð¾Ð»Ð½ÑÐ°
ÑÐ»ÑÑÑÐ°ÑÐ¸Ð¾Ð»ÐµÑÐ¾Ð²Ð¾Ðµ Ð¸ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ
solar flares
precursors
solar irradiance
active region
magnetic field configuration
solar atmosphere
ultraviolet and x-ray radiation

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ ÑÐµÐ½Ð¾Ð¼ÐµÐ½Ð° âÐ¿ÑÐµÐ´Ð²ÐµÑÑÐ½Ð¸Ðºâ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº. ÐÐ¾Ð´ Â«Ð¿ÑÐµÐ´Ð²ÐµÑÑÐ½Ð¸ÐºÐ°Ð¼Ð¸Â» ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð¼Ñ Ð¿Ð¾Ð½Ð¸Ð¼Ð°ÐµÐ¼ ÐºÐ¾Ð¼Ð¿Ð»ÐµÐºÑ ÑÐ²Ð»ÐµÐ½Ð¸Ð¹ Ð² Ð°ÐºÑÐ¸Ð²Ð½Ð¾Ð¹ Ð¾Ð±Ð»Ð°ÑÑÐ¸, Ð½Ð°Ð±Ð»ÑÐ´Ð°ÐµÐ¼ÑÑ Ð´Ð¾ Ð½Ð°ÑÐ°Ð»Ð° Ð²ÑÐ¿ÑÑÐºÐ¸, ÑÐ²Ð¸Ð´ÐµÑÐµÐ»ÑÑÑÐ²ÑÑÑÐ¸Ñ Ð¾ ÑÐ¾ÑÐ¼Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ð¸ Ð¿ÑÐµÐ´Ð²ÑÐ¿ÑÑÐµÑÐ½Ð¾Ð¹ Ð½ÐµÑÑÐ°Ð±Ð¸Ð»ÑÐ½Ð¾Ð¹ ÐºÐ¾Ð½ÑÐ¸Ð³ÑÑÐ°ÑÐ¸Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ ÑÑÑÑÐºÑÑÑ Ð² Ð°ÑÐ¼Ð¾ÑÑÐµÑÐµ Ð¡Ð¾Ð»Ð½ÑÐ°, ÐºÐ¾ÑÐ¾ÑÑÐµ Ð² Ð±ÑÐ´ÑÑÐµÐ¼ Ð² ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÐµ Ð½ÐµÐºÐ¾ÑÐ¾ÑÐ¾Ð¹ Ð½ÐµÑÑÑÐ¾Ð¹ÑÐ¸Ð²Ð¾ÑÑÐ¸ Ð¸Ð½Ð¸ÑÐ¸Ð¸ÑÑÑÑ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐºÑ Ð¸ ÑÐ¾Ð¿ÑÑÑÑÐ²ÑÑÑÐ¸Ðµ ÑÐ²Ð»ÐµÐ½Ð¸Ñ (Ð½Ð°Ð¿ÑÐ¸Ð¼ÐµÑ, ÐÐÐ). ÐÐ·ÑÑÐµÐ½Ð¸Ðµ Ð¿ÑÐµÐ´Ð²ÐµÑÑÐ½Ð¸ÐºÐ¾Ð² Ð²Ð°Ð¶Ð½Ð¾ Ð´Ð»Ñ Ð¿Ð¾Ð½Ð¸Ð¼Ð°Ð½Ð¸Ñ ÑÑÐ¸Ð³Ð³ÐµÑÐ½ÑÑ Ð¼ÐµÑÐ°Ð½Ð¸Ð·Ð¼Ð¾Ð² Ð²ÑÐ¿ÑÑÐµÐº, Ð° ÑÐ°ÐºÐ¶Ðµ Ð´Ð»Ñ Ð¸Ñ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð¾Ð³Ð¾ Ð¿ÑÐ¾Ð³Ð½Ð¾Ð·Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ. ÐÐ¾Ð¼Ð¿Ð»ÐµÐºÑ ÑÐ²Ð»ÐµÐ½Ð¸Ð¹ Ð²ÐºÐ»ÑÑÐ°ÐµÑ Ð² ÑÐµÐ±Ñ ÑÑÑÑÐµÐ½Ð¸Ñ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð² ÑÐ»ÑÑÑÐ°ÑÐ¸Ð¾Ð»ÐµÑÐ¾Ð²Ð¼ Ð¸ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ð°Ñ, ÑÐ¾ÑÐ¼Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ Ð½Ð¾Ð²ÑÑ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ ÑÑÑÑÐºÑÑÑ, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¸Ð·Ð¼ÐµÐ½ÐµÐ½Ð¸Ðµ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð¿Ð»Ð°Ð·Ð¼Ñ Ð² Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿ÐµÑÐ»ÑÑ, ÑÐ°ÐºÐ¸Ñ ÐºÐ°Ðº ÑÐµÐ¼Ð¿ÐµÑÐ°ÑÑÑÐ° Ð¸ ÐºÐ¾Ð½ÑÐµÐ½ÑÑÐ°ÑÐ¸Ñ Ð·Ð°ÑÑÐ¶ÐµÐ½Ð½ÑÑ ÑÐ°ÑÑÐ¸Ñ. Ð ÑÐ°Ð±Ð¾ÑÐµ Ð±ÑÐ»Ð¸ ÑÑÐ¾ÑÐ¼ÑÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ñ ÐºÑÐ¸ÑÐµÑÐ¸Ð¸ Ð´Ð»Ñ Ð¿ÑÐµÐ´Ð²ÑÐ¿ÑÑÐµÑÐ½ÑÑ ÑÐ²Ð»ÐµÐ½Ð¸Ð¹, Ð¿Ð¾ ÐºÐ¾ÑÐ¾ÑÑÐ¼ Ð±ÑÐ»Ð¸ Ð²ÑÐ´ÐµÐ»ÐµÐ½Ñ Ð´Ð²Ð° ÑÐ¾Ð±ÑÑÐ¸Ñ Ð´Ð»Ñ Ð´Ð°Ð»ÑÐ½ÐµÐ¹ÑÐµÐ³Ð¾ Ð°Ð½Ð°Ð»Ð¸Ð·Ð° - Ð²ÑÐ¿ÑÑÐºÐ¸ X7 Sol2014.02.25.T00:47 Ð¸ X3 Sol2015.05.05.T22:11. ÐÐ»Ñ Ð´Ð°Ð½Ð½ÑÑ ÑÐ¾Ð±ÑÑÐ¸Ð¹ Ð±ÑÐ»Ð¸ Ð¿Ð¾ÑÑÑÐ¾ÐµÐ½Ñ Ð¸Ð·Ð¾Ð±ÑÐ°Ð¶ÐµÐ½Ð¸Ñ Ð² Ð£Ð¤ (Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ SDO/AIA) Ð¸ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¼ (Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ RHESSI) Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ð°Ñ Ð½Ð° ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ ÑÑÐ°Ð´Ð¸ÑÑ Ð¸Ð½Ð¸ÑÐ¸Ð°ÑÐ¸Ð¸ Ð²ÑÐ¿ÑÑÐºÐ¸. ÐÐ¾ Ð¸Ð·Ð¾Ð±ÑÐ°Ð¶ÐµÐ½Ð¸ÑÐ¼ Ð±ÑÐ»Ð¾ Ð¿ÑÐ¾Ð²ÐµÐ´ÐµÐ½Ð¾ Ð½Ð°Ð±Ð»ÑÐ´ÐµÐ½Ð¸Ðµ Ð·Ð° ÑÐ²Ð¾Ð»ÑÑÐ¸ÐµÐ¹ ÐÐ, Ð° ÑÐ°ÐºÐ¶Ðµ Ð½Ð° Ð²ÑÐµÑ ÑÑÐ°Ð´Ð¸ÑÑ Ð±ÑÐ»Ð¸ ÑÐ´ÐµÐ»Ð°Ð½Ñ Ð¾ÑÐµÐ½ÐºÐ¸ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð²Â  Ð¿Ð»Ð°Ð·Ð¼Ñ. ÐÑÐ»Ð° Ð¿ÑÐµÐ´Ð»Ð¾Ð¶ÐµÐ½Ð° ÑÐµÐ½Ð¾Ð¼ÐµÐ½Ð¾Ð»Ð¾Ð³Ð¸ÑÐµÑÐºÐ°Ñ Ð¼Ð¾Ð´ÐµÐ»Ñ ÑÐ²Ð¾Ð»ÑÑÐ¸Ð¸Â  Ð²ÑÐ¿ÑÑÐºÐ¸, Ð¾ÑÐ½Ð¾Ð²Ð°Ð½Ð½Ð°Ñ Ð½Ð° Ð¼Ð¾Ð´ÐµÐ»Ð¸ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÑ Ð¿Ð¾Ð»ÐµÐ¹ Ð´Ð²ÑÑ Ð±Ð¸Ð¿Ð¾Ð»ÐµÐ¹.
description: This paper is devoted to a study of the solar flare "precursor" phenomenon. By "precursors" of solar flares, we mean a set of phenomena in the active region observed before a flare, indicating the formation of a pre-flare unstable configuration of magnetic structures in the solar atmosphere that, as a result of some future instability, will initiate a solar flare and associated phenomena (e.g., CMEs). The study of precursors is important for understanding the triggering mechanisms of flares, as well as for their possible prediction. The set of phenomena includes brightening radiation in the ultraviolet and X-ray bands, the formation of new magnetic structures, and changes in plasma parameters in magnetic loops, such as temperature and concentrations of charged particles. The criteria for pre-flare events were formulated, which were used to select two events for further analysis: flares X7 Sol2014.02.25.T00:47 and X3 Sol2015.05.05.T22:11. For these events, images were constructed in the UV (according to SDO/AIA data) and X-ray (according to RHESSI data) bands at various stages of flare initiation. From the images, the AR evolution was observed, and estimates of plasma parameters were made at all stages. A phenomenological model of flare evolution, based on the model of reconnection of the magnetic fields of two bipoles, was proposed.