title: ÐÐ½Ð°Ð»Ð¸Ð· ÐºÑÐ¸Ð²ÑÑ Ð±Ð»ÐµÑÐºÐ° Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð² ÐºÐ¾Ð½ÑÐµÐºÑÑÐµ Ð¸Ñ ÐºÐ»Ð°ÑÑÐ¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¸
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: Analysis of gamma-ray burst light curves in the context of their classification
Creators: name: ÐÐ±ÑÐ·Ð°ÐºÑÐ¸, ÐÐ°Ð»Ð»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: 2024
Subjects: Ð³Ð°Ð¼Ð¼Ð°-Ð°ÑÑÑÐ¾Ð½Ð¾Ð¼Ð¸Ñ
Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¸
ÑÑÐ°Ð½Ð·Ð¸ÐµÐ½ÑÐ½ÑÐµ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ¸
ÐºÐ¾Ð½ÑÑ-Ð²Ð¸Ð½Ð´
ÐºÐ»Ð°ÑÑÐ¸ÑÐ¸ÐºÐ°ÑÐ¸Ñ
gamma-ray astronomy
gamma-ray bursts
transient sources
konus-wind
classification

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð°Ð½Ð°Ð»Ð¸Ð·Ñ ÐºÑÐ¸Ð²ÑÑ Ð±Ð»ÐµÑÐºÐ° Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ð² ÐºÐ¾Ð½ÑÐµÐºÑÑÐµ Ð¸Ñ ÐºÐ»Ð°ÑÑÐ¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¸. ÐÐ°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¸ â ÑÑÐ¾ ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¸Ðµ Ð²Ð½ÐµÐ³Ð°Ð»Ð°ÐºÑÐ¸ÑÐµÑÐºÐ¸Ðµ ÑÐ²Ð»ÐµÐ½Ð¸Ñ, Ð²Ð¾ Ð²ÑÐµÐ¼Ñ ÐºÐ¾ÑÐ¾ÑÑÑ Ð¿ÑÐ¾Ð¸ÑÑÐ¾Ð´ÑÑ Ð¸Ð½ÑÐµÐ½ÑÐ¸Ð²Ð½ÑÐµ Ð²ÑÐ±ÑÐ¾ÑÑ Ð³Ð°Ð¼Ð¼Ð°-Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ, Ð´Ð»Ð¸ÑÐµÐ»ÑÐ½Ð¾ÑÑÑÑ Ð¾Ñ Ð´ÐµÑÑÑÐºÐ¾Ð² Ð¼Ð¸Ð»Ð»Ð¸ÑÐµÐºÑÐ½Ð´ Ð´Ð¾ Ð½ÐµÑÐºÐ¾Ð»ÑÐºÐ¸Ñ ÑÐ°ÑÐ¾Ð² Ð¸ ÑÐ½ÐµÑÐ³Ð¸ÑÐ¼Ð¸ Ð¾Ñ Ð´ÐµÑÑÑÐºÐ¾Ð² ÐºÑÐ Ð´Ð¾ ÐÑÐ Ð¸ Ð²ÑÑÐµ. Ð ÐºÐ¾Ð½ÑÐµÐºÑÑÐµ Ð¼Ð¾Ð´ÐµÐ»Ð¸ ÐºÐ¾Ð»Ð»Ð°Ð¿ÑÐ°ÑÐ° Ð¿Ð¾ÑÐ²Ð»ÐµÐ½Ð¸Ðµ Ð¿Ð»Ð°ÑÐ¾ Ð² Ð´Ð¸ÑÑÐµÑÐµÐ½ÑÐ¸Ð°Ð»ÑÐ½Ð¾Ð¼ ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ð¸ Ð´Ð»Ð¸ÑÐµÐ»ÑÐ½Ð¾ÑÑÐ¸ Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² ÑÐ²Ð»ÑÐµÑÑÑ Ð·Ð½Ð°ÑÐ¸Ð¼ÑÐ¼ Ð½Ð°Ð±Ð»ÑÐ´ÐµÐ½Ð¸ÐµÐ¼ Ð¸ Ð¿ÑÐµÐ´ÑÑÐ°Ð²Ð»ÑÐµÑ ÑÐ¾Ð±Ð¾Ð¹ ÐºÐ¾ÑÐ²ÐµÐ½Ð½Ð¾Ðµ Ð¿Ð¾Ð´ÑÐ²ÐµÑÐ¶Ð´ÐµÐ½Ð¸Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸ ÐºÐ¾Ð»Ð»Ð°Ð¿ÑÐ°ÑÐ°[4], Ð¿Ð¾ÑÑÐ¾Ð¼Ñ Ð±ÑÐ»Ð¾ Ð¿Ð¾ÑÑÑÐ¾ÐµÐ½Ð¾ Ð´Ð¸ÑÑÐµÑÐµÐ½ÑÐ¸Ð°Ð»ÑÐ½Ð¾Ðµ ÑÐ°ÑÐ¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ð¸Ðµ Ð¿Ð¾ Ð´Ð»Ð¸ÑÐµÐ»ÑÐ½Ð¾ÑÑÐ¸ Ð³Ð°Ð¼Ð¼Ð°-Ð²ÑÐ¿Ð»ÐµÑÐºÐ¾Ð² Ñ Ð¸Ð·Ð²ÐµÑÑÐ½ÑÐ¼ ÐºÑÐ°ÑÐ½ÑÐ¼ ÑÐ¼ÐµÑÐµÐ½Ð¸ÐµÐ¼, Ð·Ð°ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½ÑÑ Ð¿ÑÐ¸Ð±Ð¾ÑÐ°Ð¼Ð¸ ÐÐ¾Ð½ÑÑ-ÐÐ¸Ð½Ð´ Ð¸ Fermi/GBM. Ð Ð°Ð½ÐµÐµ ÑÐ°ÐºÐ¾Ð³Ð¾ Ð°Ð½Ð°Ð»Ð¸Ð·Ð° Ð´Ð»Ñ Ð¿ÑÐ¸Ð±Ð¾ÑÐ° ÐÐ¾Ð½ÑÑ-ÐÐ¸Ð½Ð´ Ð½Ðµ Ð¿ÑÐ¾Ð²Ð¾Ð´Ð¸Ð»Ð¾ÑÑ, ÑÑÐ¾ Ð´ÐµÐ»Ð°ÐµÑ Ð½Ð°ÑÐµ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¾ÑÐ¸Ð³Ð¸Ð½Ð°Ð»ÑÐ½ÑÐ¼ Ð¸ Ð²Ð°Ð¶Ð½ÑÐ¼ Ð´Ð»Ñ Ð´Ð°Ð»ÑÐ½ÐµÐ¹ÑÐµÐ³Ð¾ Ð¿Ð¾Ð´ÑÐ²ÐµÑÐ¶Ð´ÐµÐ½Ð¸Ñ ÑÐµÐ¾ÑÐ¸Ð¸ ÐºÐ¾Ð»Ð»Ð°Ð¿ÑÐ°ÑÐ¾Ð².
description: This work is dedicated to the analysis of gamma-ray burst light curves in the context of their classification. Gamma-ray bursts are cosmic events during which intense bursts of gamma radiation occur, varying in duration from tens of milliseconds to several hours, and covering a wide range of energies from tens of keV to MeV and above. In the context of the collapsar model, the appearance of a plateau in the differential distribution of gamma-ray burst durations is a significant observation and serves as indirect confirmation of the collapsar model.[4] Therefore, a differential distribution of gamma-ray bursts by duration with known redshift was constructed, recorded by the Konus-Wind and Fermi/GBM instruments. Such an analysis for gamma-ray bursts with known redshift has not been conducted previously, making our study important for further confirmation of the collapsar theory. Gamma-ray bursts are cosmic extragalactic phenomena during which intense gammaâray emissions occur, lasting from tens of milliseconds to several hours and energies from tens of keV to MeV and higher. In the context of the collapsar model, the appearance of a plateau in the differential distribution of the duration of gamma-ray bursts is a significant observation and represents an indirect confirmation of the collapsar model [4]. Therefore, a differential distribution of durations of gamma-ray bursts with known redshifts, detected by Konus-Wind (KW) and Fermi/GBM, was computed. Previously, no such analysis was performed for KW, which makes our study original and important for further confirmation of the collapsar theory.