银河系中最强大的 maser 是源 G25.65+1.05,宇宙中最强大的发射器是 AGN S 0528+134

IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS
A. E. Volvach, L. N. Volvach, M. G. Larionov
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引用次数: 0

摘要

从2000年到2024年,RT-22射电望远镜(Simeiz)对银河源G25.65\(+\)1.05进行了长期监测,因此记录到了几次强大的耀斑事件。最强大耀斑的振幅迅速增大,达到了该源的创纪录水平,为 130 kJy。根据监测数据推测出了双星系统中负责发生耀斑的大质量O5级恒星的轨道周期(7.5年)和前周期(60年)。持续时间不超过一个月的单个短耀斑可能属于未饱和状态的maser。接近最大相位的 maser 线中心部分的形状表明,通量密度增加的大部分是由一个单组分源造成的。因此,银河系中出现了频率为22.2千兆赫的水蒸气线中最强大的千兆赫G25.65\(+\)1.05。活动星系核S 0528\(+\)134 是在1969年克里米亚天体物理天文台(Crimean Astrophysical Observatory)使用射电望远镜RT-22(Simeiz)在8550 MHz频率的搜索巡天中发现的--这项研究的目的是寻找新的活动星系核(AGN)。本文的目标是确定近双星系统 S 0528\(+\)134 的物理特性,以便随后评估来自它的引力辐射水平。在以 8 千兆赫的频率对该天体进行长期监测期间,出现了一些强大的通量密度耀斑,从而有可能将该源视为宇宙中最强大的发射器。在S 0528\(+\)134 的通量密度变化中存在着选定的谐波成分,这使得我们能够获得超大质量黑洞(SMBHs)双星系统的主要物理特征,从而使S 0528\(+\)134 成为质量最大的SMBHs之一。这个AGN也可以被认为是利用国际脉冲星定时阵列引力波探测器探测GW的最强大来源。
本文章由计算机程序翻译,如有差异,请以英文原文为准。

Most powerful maser in the Galaxy is source G25.65+1.05 and the most powerful emitter in the Universe AGN S 0528+134

Most powerful maser in the Galaxy is source G25.65+1.05 and the most powerful emitter in the Universe AGN S 0528+134

Several powerful flare events have been recorded because of long-term monitoring on the RT-22 radio telescope (Simeiz) of the galactic source G25.65\(+\)1.05 from 2000 to 2024. The amplitude of the most powerful flare increased rapidly and reached a record level for this source of 130 kJy. The orbital (7.5 years) and precessional (60 years) periods in the binary system of massive O5 class stars responsible for the occurrence of flares based on monitoring data have been presumably determined. Individual short flares, lasting no more than a month, presumably belonged to a maser in an unsaturated state. The shape of the central part of the maser line, near the maximum phase, suggests a single-component source responsible for the bulk of the increase in flux density. Thus, the most powerful kilomaser G25.65\(+\)1.05 in the water vapor line at frequency 22.2 GHz has been registered in the Galaxy. The possibility of detecting gravitational waves (GWs) coming from the massive stellar binary system is considered.

The active galactic nucleus S 0528\(+\)134 was discovered in a search survey at a frequency of 8550 MHz in 1969 using the radio telescope RT-22 (Simeiz) at the Crimean Astrophysical Observatory—the study aimed to search for new active galactic nuclei (AGN). In this article, the goal was to determine the physical characteristics of the close binary system S 0528\(+\)134 for the subsequent assessment of the level of gravitational radiation coming from it. During long-term monitoring of the object at a frequency of 8 GHz, some powerful flares of flux density occurred, which made it possible to consider the source the most powerful emitter in the Universe. The presence of selected harmonic components in the flux density variations of S 0528\(+\)134 allowed obtaining the main physical characteristics of a binary system of supermassive black holes (SMBHs), which placed S 0528\(+\)134 in the rank of one of the most massive SMBHs. This AGN can also be considered the most powerful source for detecting GWs by using International Pulsar Timing Array gravitational wave detectors.

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来源期刊
Journal of Astrophysics and Astronomy
Journal of Astrophysics and Astronomy 地学天文-天文与天体物理
CiteScore
1.80
自引率
9.10%
发文量
84
审稿时长
>12 weeks
期刊介绍: The journal publishes original research papers on all aspects of astrophysics and astronomy, including instrumentation, laboratory astrophysics, and cosmology. Critical reviews of topical fields are also published. Articles submitted as letters will be considered.
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