title: ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð½Ð°ÑÐ°Ð»ÑÐ½Ð¾Ð¹ ÑÐ°Ð·Ñ Ð´Ð»Ð¸Ð½Ð½ÑÑ Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ ÑÐºÑÐ¿ÐµÑÐ¸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: A study of the initial phase of long gamma-ray bursts according to the Konus-Wind experiment data
Creators: name: Ð¢ÐµÐ¼Ð¸ÑÐ°ÐµÐ², Ð®ÑÐ¸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: 2020
Subjects: Ð´Ð»Ð¸Ð½Ð½ÑÐµ Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¸
ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½Ð°Ñ ÑÐ²Ð¾Ð»ÑÑÐ¸Ñ
Ð¼Ð¾Ð´ÐµÐ»Ñ ÐÐ°Ð½Ð´Ð°
Ð¿ÑÐµÐºÑÑÑÐ¾Ñ
ÑÐ¾Ð¾ÑÐ½Ð¾ÑÐµÐ½Ð¸Ðµ Ð¶ÑÑÑÐºÐ¾ÑÑÑâÐ¸Ð½ÑÐµÐ½ÑÐ¸Ð²Ð½Ð¾ÑÑÑ
Ð½ÐµÑÐµÐ¿Ð»Ð¾Ð²Ð¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ
ÐÐ¾Ð½ÑÑ-ÐÐ¸Ð½Ð´
long gamma-ray bursts
spectral evolution
Band model
precursor
hardnessâintensity correlation
nonthermal emission
Konus-Wind

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½Ð¾Ð¹ ÑÐ²Ð¾Ð»ÑÑÐ¸Ð¸ Ð½Ð°ÑÐ°Ð»ÑÐ½Ð¾Ð¹ ÑÐ°Ð·Ñ ÑÑÐºÐ¸Ñ Ð´Ð»Ð¸Ð½Ð½ÑÑ Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð², Ð·Ð°ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½ÑÑ Ð² ÑÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐµ ÐÐ¾Ð½ÑÑ-ÐÐ¸Ð½Ð´. ÐÐ°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¸ â ÑÐ°Ð¼ÑÐµ ÑÑÐºÐ¸Ðµ Ð¿Ð¾ Ð²ÑÐ´ÐµÐ»ÐµÐ½Ð¸Ñ ÑÐ»ÐµÐºÑÑÐ¾Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð¹ ÑÐ½ÐµÑÐ³Ð¸Ð¸ ÑÐ¾Ð±ÑÑÐ¸Ñ Ð²Ð¾ ÐÑÐµÐ»ÐµÐ½Ð½Ð¾Ð¹. ÐÐµÑÐ¼Ð¾ÑÑÑ Ð½Ð° ÑÐ¾, ÑÑÐ¾ ÑÑÐ¸ ÑÐ¾Ð±ÑÑÐ¸Ñ Ð±ÑÐ»Ð¸ Ð¾ÑÐºÑÑÑÑ Ð±Ð¾Ð»ÐµÐµ 50 Ð»ÐµÑ Ð½Ð°Ð·Ð°Ð´, Ð¼ÐµÑÐ°Ð½Ð¸Ð·Ð¼Ñ Ð³ÐµÐ½ÐµÑÐ°ÑÐ¸Ð¸ ÑÐ°ÐºÐ¾Ð³Ð¾ Ð¼Ð¾ÑÐ½Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð´Ð¾ ÑÐ¸Ñ Ð¿Ð¾Ñ Ð½ÐµÑÑÐ½Ñ. Ð Ð´Ð°Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÐµ Ð¿ÑÐµÐ´ÑÑÐ°Ð²Ð»ÑÐµÑÑÑ ÑÐ°Ð·ÑÐµÑÑÐ½Ð½ÑÐ¹ Ð¿Ð¾ Ð²ÑÐµÐ¼ÐµÐ½Ð¸ ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½ÑÐ¹ Ð°Ð½Ð°Ð»Ð¸Ð· 34 ÑÑÐºÐ¸Ñ Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð², 14 Ð¸Ð· ÐºÐ¾ÑÐ¾ÑÑÑ Ð¿Ð¾ÐºÐ°Ð·ÑÐ²Ð°ÑÑ ÑÐ¸Ð»ÑÐ½ÑÑ ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½ÑÑ ÑÐ²Ð¾Ð»ÑÑÐ¸Ñ Ð½Ð° Ð½Ð°ÑÐ°Ð»ÑÐ½Ð¾Ð¹ ÑÐ°Ð·Ðµ. ÐÐ¾ÐºÐ°Ð·ÑÐ²Ð°ÐµÑÑÑ, ÑÑÐ¾ Ð´Ð»Ñ ÑÑÐ¸Ñ Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð½Ð°ÑÐ°Ð»ÑÐ½ÑÐ¹ Ð¸Ð¼Ð¿ÑÐ»ÑÑ Ð¾Ð¿Ð¸ÑÑÐ²Ð°ÐµÑÑÑ Ð¿ÑÐ¾ÑÑÑÐ¼ ÑÐºÑÐ¿Ð¾Ð½ÐµÐ½ÑÐ¸Ð°Ð»ÑÐ½ÑÐ¼ Ð·Ð°ÐºÐ¾Ð½Ð¾Ð¼. ÐÐ»Ñ ~70% Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð²ÑÐ±Ð¾ÑÐºÐ¸ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑ "Ð°Ð»ÑÑÐ°" Ð¼Ð¾Ð´ÐµÐ»Ð¸ ÐÐ°Ð½Ð´Ð° Ð½Ðµ ÑÐ¾Ð³Ð»Ð°ÑÑÐµÑÑÑ Ñ "Ð»Ð¸Ð½Ð¸ÑÐ¼Ð¸ ÑÐ¼ÐµÑÑÐ¸" ÑÐ¸Ð½ÑÑÐ¾ÑÑÐ¾Ð½Ð½Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ. ÐÑÐ¾Ð¸Ð·Ð²Ð¾Ð´Ð¸ÑÑÑ Ð°Ð½Ð°Ð»Ð¸Ð· ÑÐ¾Ð¾ÑÐ½Ð¾ÑÐµÐ½Ð¸Ñ Ð¶ÑÑÑÐºÐ¾ÑÑÑ-Ð¸Ð½ÑÐµÐ½ÑÐ¸Ð²Ð½Ð¾ÑÑÑ Ð¾ÑÐ¾Ð±ÑÐ°Ð½Ð½ÑÑ Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð², ÐºÐ¾ÑÐ¾ÑÐ°Ñ Ð´Ð»Ñ ÑÐ°Ð·Ð½ÑÑ ÑÐ¿Ð¸Ð·Ð¾Ð´Ð¾Ð² Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð°Ð¿Ð¿ÑÐ¾ÐºÑÐ¸Ð¼Ð¸ÑÑÐµÑÑÑ ÑÑÐµÐ¿ÐµÐ½Ð½ÑÐ¼ Ð·Ð°ÐºÐ¾Ð½Ð¾Ð¼: Ep ~ F^q. ÐÐ¾ÐºÐ°Ð·ÑÐ²Ð°ÐµÑÑÑ, ÑÑÐ¾ Ð´Ð»Ñ Ð±Ð¾Ð»ÑÑÐ¸Ð½ÑÑÐ²Ð° Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð²ÑÐ±Ð¾ÑÐºÐ¸ ÑÐ¾Ð¾ÑÐ½Ð¾ÑÐµÐ½Ð¸Ðµ Ð¿Ð¸ÐºÐ¾Ð²Ð¾Ð¹ ÑÐ½ÐµÑÐ³Ð¸Ð¸ Ep ÑÐ¿ÐµÐºÑÑÐ° Ð¾Ñ Ð¿Ð¾ÑÐ¾ÐºÐ° ÑÐ½ÐµÑÐ³Ð¸Ð¸ Ð¸Ð¼ÐµÐµÑ Ð²Ð¸Ð´ Ep ~ F^0.5, ÑÑÐ¾ ÑÐ¾Ð³Ð»Ð°ÑÑÐµÑÑÑ Ñ Ð¼Ð¾Ð´ÐµÐ»ÑÑ ÑÐ¸Ð½ÑÑÐ¾ÑÑÐ¾Ð½Ð½Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ. ÐÐ»Ñ 5 ÑÐ°ÐºÐ¸Ñ Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð½Ð°ÐºÐ»Ð¾Ð½ Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÐ¸ Ep(F) ÐºÑÑÑÐµ Ð¸ Ð´Ð¾ÑÑÐ¸Ð³Ð°ÐµÑ Ð·Ð½Ð°ÑÐµÐ½Ð¸Ð¹ Ð´Ð¾ q ~ 3. ÐÐ¾Ð»ÑÑÐµÐ½Ð½ÑÐµ ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÑ ÐºÑÐ°ÑÐºÐ¾ Ð¾Ð±ÑÑÐ¶Ð´Ð°ÑÑÑÑ Ð² ÑÐ°Ð¼ÐºÐ°Ñ ÑÐ¸Ð½ÑÑÐ¾ÑÑÐ¾Ð½Ð½Ð¾Ð¹ Ð¸ ÑÐµÐ¿Ð»Ð¾Ð²Ð¾Ð¹ Ð¼Ð¾Ð´ÐµÐ»ÐµÐ¹ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ.
description: The given work is devoted to spectral evolution analysis of the initial phase of bright long gamma-ray bursts detected by the Konus-Wind experiment. Gamma-ray bursts are the most electromagnetically energetic events in the Universe. Although 50 years have passed since their discovery, the radiative mechanisms that produce such powerful emission are still unknown. In this work, we present the temporal and spectral analysis of 34 bright bursts, 14 of which show strong spectral evolution during the initial phase. We show that for these bursts, the initial pulse is well fitted with a simple exponential law. For ~70% of the bursts in our sample, the Band function parameter âalphaâ violates the synchrotron âline of deathâ limits. We analyze the hardnessâintensity correlation and fit it with a power law Ep ~ F^q. We show that for most of the bursts in the sample the peak energy â energy flux relation has the form of Ep ~ F^0.5 consistent with the synchrotron model. For 5 of these bursts, the slope is steeper and reaches values up to q ~ 3. The obtained results are briefly discussed in the context of synchrotron and thermal radiation models.