A 12.6-ms pulsar in Cygnus X-3

Chadwick, P. M.; Dipper, N. A.; Dowthwaite, J. C.; Gibson, A. I.; Harrison, A. B.; Kirkman, I. W.; Lotts, A. P.; Macrae, J. H.; McComb, T. J. L.; Orford, K. J.; Turver, K. E.; Walmsley, M.

doi:10.1038/318642a0

Cited by 79 publications

(26 citation statements)

References 14 publications

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“…There were some claims of detection of Cygnus X-3 at gamma-rays by instruments working at VHE and UHE instruments (e.g. [77]), although these detections are considered doubtful nowadays by the VHE community. In any case, a significant production of gamma-rays above 1 MeV in MQ was not thought as plausible.…”

Section: Discussionmentioning

confidence: 99%

Theoretical overview on high-energy emission in microquasars

Bosch‐Ramon

2007

The Multi-Messenger Approach to High-Energy Gamma-Ray Sources

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Microquasar (MQ) jets are sites of particle acceleration and synchrotron emission. Such synchrotron radiation has been detected coming from jet regions of different spatial scales, which for the instruments at work nowadays appear as compact radio cores, slightly resolved radio jets, or (very) extended structures (e.g.Because of the presence of relativistic particles and dense photon, magnetic and matter fields, these outflows are also the best candidates to generate the very high-energy (VHE) gamma-rays detected coming from two of these objects, LS 5039 and LS I +61 303 ([4,5], and [6], respectively), and may be contributing significantly to the X-rays emitted from the MQ core (e.g. [7], [8]). In addition, beside electromagnetic radiation, jets at different scales are producing some amount of leptonic and hadronic cosmic rays (CR), and evidences of neutrino production in these objects may be eventually found. In this work, we review on the different physical processes that may be at work in or related to MQ jets. The jet regions capable to produce significant amounts of emission at different wavelengths have been reduced to the jet base, the jet at scales of the order of the size of the system orbital semi-major axis, the jet middle scales (the resolved radio jets), and the jet termination point. The surroundings of the jet could be sites of multiwavelegnth emission as well, deserving also an insight. We focus on those scenarios, either hadronic or leptonic, in which it seems more plausible to generate both photons from radio to VHE and high-energy neutrinos. We briefly comment as well on the relevance of MQ as possible contributors to the galactic CR in the GeV-PeV range.

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Section: Discussionmentioning

confidence: 99%

Theoretical overview on high-energy emission in microquasars

Bosch‐Ramon

2007

The Multi-Messenger Approach to High-Energy Gamma-Ray Sources

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“…Помимо упомянутых выше в 1980-х г. было осу-ществлено еще несколько проектов черенковских гамма-телескопов, таких как CAT (Франция [27]), CANGAROO (Япония, Австралия [28]), его значительно более эф-фективная модификация CANGAROO II (см., напри-мер, [29]), TACTIC (Индия [30]), серия телескопов Mark 1−6 (Великобритания, с размещением в США, Ав-стралии и на Канарских островах, см., например, [31,32] и ссылки там же), ШАЛОН (Россия [33]) и др. Все эти инструменты, которые принято также относить ко второ-му поколению черенковских гамма-телескопов, работали в тераэлектроновольтном диапазоне энергий первичных частиц.…”

Section: краткая история развития черенковских гамма-телескоповunclassified

Черенковские Гамма-Телескопы: Прошлое, Настоящее, Будущее. Проект ALEGRO

Быков¹,

Агаронян

Красильщиков³

et al. 2017

Журнал Технической Физики

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Дан краткий обзор истории развития атмосферных черенковских гамма-телескопов, а также представлен перечень актуальных задач современной астрофизики и фундаментальной физики, которые могут быть решены с помощью этих инструментов. Представлен проект низкопороговой гамма-обсерватории ALEGRO, ключевой задачей которой является исследование космических гамма-источников с высокой статистикой детектируемых фотонов в диапазоне энергий 5−50 GeV, в особенности быстропеременных гамма-источников (гамма-транзиентов).

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“…The detection is bolstered by the fact that the TeV γ−rays are strongest during the X-ray maxima in the 4.8 hour orbital period (Chadwick et al 1985). Other groups have failed to detect Cygnus X-3 during the X-ray maximum (e.g.…”

Section: Observationsmentioning

confidence: 99%

“…Additionally, a 12.6 msec periodicity has been reported by multiple groups, although the period measurements are quite precise and seem not to be exactly consistent with one another (Chadwick et al 1985;Brazier et al 1990;Gregory et al 1990). On the other hand, these pulse periods are based on rather small numbers of photons.…”

Section: Observationsmentioning

confidence: 99%