Extending the ‘energetic scaling of relativistic jets from black hole systems’ to include γ-ray-loud X-ray binaries

Lamb, Gavin P.; Kobayashi, S.; Pian, E.

doi:10.1093/mnras/stx1933

Cited by 6 publications

(4 citation statements)

References 72 publications

(89 reference statements)

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“…However, the empirical relation between the luminosity and kinetic power is valid not only for AGNs, but also for GRBs. Moreover, [21] traced the same relation down to the luminosities of X-ray binaries in the Milky Way so that the whole relation spans over ∼ 17 orders of magnitude in luminosity. This 'unified' relation has the form log P jet = α log L + β where L is the collimation corrected luminosity L = f b L iso γ , α = 0.98 ± 0.02 and β = 1.6 ± 0.9.…”

Section: Methodsmentioning

confidence: 79%

Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations

Nizamov,

Pshirkov

2018

Preprint

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It is well known that if the most energetic cosmic rays (E > 10 20 eV) were protons then their acceleration sites should possess some extreme properties, including gigantic luminosity. As no stationary sources with such properties are known in the local (D < 200 Mpc) neighborhood of the Milky Way, it is highly likely that the UHECR acceleration takes place in some transient events. In this paper we investigate scenario where the UHECRs are produced in strong AGN flares. Using more than 7 years of the Fermi-LAT observations we select candidate flares and, using correlation between jet kinetic luminosity and its bolometric luminosity, estimate local kinetic emissivity of giant AGN flares: L ∼ 3.7 × 10 44 erg Mpc −3 yr −1 . This value is about an order of magnitude larger than the emissivity in the CRs with E > 10 20 eV, thus making this scenario feasible, if the UHECR escape spectrum is rather hard and/or narrow. This shape of spectrum is predicted in a number of present models of strong relativistic collisionless shocks. Also the scenario of acceleration in AGN flares can accommodate constraints coming from the observed arrival distribution of UHECRs. Finally, we demonstrate that in case of heavier UHECR composition all the constraints are greatly relaxed.

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Section: Methodsmentioning

confidence: 79%

Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations

Nizamov,

Pshirkov

2018

Preprint

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show abstract

“…However, the empirical relation between the luminosity and kinetic power is valid not only for AGNs, but also for GRBs, although in the latter case it should be used with some degree of caution, as it is still a matter of debate. Moreover, [24] traced the same relation down to the luminosities of X-ray binaries in the Milky Way during flares so that the whole relation spans over ∼ 17 orders of magnitude in luminosity. This 'unified' relation has the form log P jet = α log L + β where L is the collimation corrected luminosity L = f b L iso γ , α = 0.98 ± 0.02 and β = 1.6 ± 0.9.…”

Section: Jcap03(2020)060mentioning

confidence: 77%

Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations

Nizamov

Пширков

2020

J. Cosmol. Astropart. Phys.

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It is well known that if the most energetic cosmic rays (E>1020 eV) were protons then their acceleration sites should possess some extreme properties, including gigantic luminosity. As no stationary sources with such properties are known in the local (D<200 Mpc) neighborhood of the Milky Way, it is highly likely that the UHECR acceleration takes place in some transient events. In this paper we investigate scenario where the UHECRs are produced in strong AGN flares. Using more than 7 years of the Fermi-LAT observations we select candidate flares and, using correlation between jet kinetic luminosity and its bolometric luminosity, estimate local kinetic emissivity of giant AGN flares: ℒ∼3.7×1044erg Mpc−3 yr−1. This value is about an order of magnitude larger than the emissivity in the CRs with E>1020 eV, thus making this scenario feasible, if the UHECR escape spectrum in these sources is rather hard and/or narrow. This shape of spectrum is predicted in a number of present models of strong relativistic collisionless shocks. Also the scenario of acceleration in AGN flares can accommodate constraints coming from the observed arrival distribution of UHECRs. Finally, we demonstrate that in case of heavier UHECR composition all the constraints are greatly relaxed.

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“…Based on the likelihood analysis results for the MJD 57623-57625 detection, the observed 0.3-500 GeV (isotropic) luminosity is ∼ 1.9 × 10 35 erg s −1 . The jet luminosity (collimation corrected; see Lamb et al 2017) from V404 Cygni could be a factor of ∼20 larger, that is ∼ 4 × 10 36 erg s −1 . From fitting the optical and infrared broad-band spectrum of the source, the mass accretion rate was estimated to be ∼ 7 × 10 16 g s −1 (Muno & Mauerhan 2006), indicating an accretion power of ∼ 6 × 10 37 η erg s −1 (where η is the efficiency) in the binary system.…”

Section: Discussionmentioning

confidence: 99%

Detection of the microquasar V404 Cygni at gamma-rays revisited: short flaring events in quiescence

Xing,

Wang

2020

Preprint

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The microquasar V404 Cygni (also known as GS 2023+338) was previously reported to have possible GeV γ-ray emission in two days during its 2015 outburst. In order to provide more detailed information at the high energy range for this black hole binary system, we conduct detailed analysis to the data obtained with the Large Area Telescope (LAT) onboard the Fermi Gamma Ray Space Telescope (Fermi). Both LAT database and source catalog used are the latest. From the analysis, we can not confirm the previous detection. Instead, we find one possible detection (∼ 4σ) of the source at the end of the outburst in the time period of 2015 Aug. 17-19, and one convincing detection (≃ 7σ) in 2016 Aug. 23-25. The latter shows that the γ-ray emission of the source is soft with photon index Γ ∼ 2.9, mostly detected below ∼ 1.3 GeV with Fermi LAT. As γ-ray emission from microquasars is likely associated with their jet activity, we discuss the results by comparing with those well studied cases, namely Cyg X-3 and Cyg X-1. The detection establishes V404 Cygni as one of four microquasars with detectable γ-ray emission, and adds interesting features to the small group, or in a more general context to X-ray binaries with jets.

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Extending the ‘energetic scaling of relativistic jets from black hole systems’ to include γ-ray-loud X-ray binaries

Cited by 6 publications

References 72 publications

Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations

Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations

Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations

Detection of the microquasar V404 Cygni at gamma-rays revisited: short flaring events in quiescence

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