Leptonic/hadronic models for electromagnetic emission in microquasars: the case of GX 339-4

Vila, Gabriela S.; Romero, Gustavo E.

doi:10.1111/j.1365-2966.2010.16208.x

Cited by 44 publications

(38 citation statements)

References 62 publications

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“…In this section, we seek the relation between the jet power and the observed radio flux density. First, we consider the jet power in the observer frame defined as P j = γ jṀj c 2 , (C.1) which follows, e.g., from [see also Vila & Romero (2010)], and for which we need to evaluateṀ j using Eq. A.7.…”

Section: Discussionmentioning

confidence: 99%

Ultra-high-energy cosmic rays from low-luminosity active galactic nuclei

Duţan

Caramete

2015

Astroparticle Physics

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We investigate the production of ultra-high-energy cosmic ray (UHECR) in relativistic jets from low-luminosity active galactic nuclei (LLAGN). We start by proposing a model for the UHECR contribution from the black holes (BHs) in LLAGN, which present a jet power P j 10 46 erg s −1 . This is in contrast to the opinion that only high-luminosity AGN can accelerate particles to energies 50 EeV. We rewrite the equations which describe the synchrotron selfabsorbed emission of a non-thermal particle distribution to obtain the observed radio flux density from sources with a flat-spectrum core and its relationship to the jet power. We find that the UHECR flux is dependent on the observed radio flux density, the distance to the AGN, and the BH mass, where the particle acceleration regions can be sustained by the magnetic energy extraction from the BH at the center of the AGN. We use a complete sample of 29 radio sources with a total flux density at 5 GHz greater than 0.5 Jy to make predictions for the maximum particle energy, luminosity, and flux of the UHECRs from nearby AGN. These predictions are then used in a semi-analytical code developed in Mathematica (SAM code) as inputs for the Monte-Carlo simulations to obtain the distribution of the arrival direction at the Earth and the energy spectrum of the UHECRs, taking into account their deflection in the intergalactic magnetic fields. For comparison, we also use the CRPropa code with the same initial conditions as for the SAM code. Importantly, to calculate the energy spectrum we also include the weighting of the UHECR flux per each UHECR source. Next, we compare the energy spectrum of the UHECRs with that obtained by the Pierre Auger Observatory.

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Section: Discussionmentioning

confidence: 99%

Ultra-high-energy cosmic rays from low-luminosity active galactic nuclei

Duţan

Caramete

2015

Astroparticle Physics

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“…The power injected in the form of relativistic particles (L rel ) is considered to be a small fraction q rel of the total jet kinetic power and the relation between proton and electron powers is given by the parameter a such that L p = a L e (see e.g. Romero & Vila 2008;Vila & Romero 2010).…”

Section: Basic Scenariomentioning

confidence: 99%

A lepto-hadronic model for high-energy emission from FR I radiogalaxies

Reynoso

Medina

Romero

2011

A&A

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Context. The well known radiogalaxy Cen A has been recently detected as a source of very high energy (VHE) γ-rays by the HESS experiment just before Fermi/LAT detected it at high energies (HE). The detection, together with that of M 87, established radiogalaxies as VHE γ-ray emitters. Aims. The aim of this work is to present a lepto-hadronic model for the VHE emission from the relativistic jets in FR I radiogalaxies. Methods. We consider that protons and electrons are accelerated in a compact region near the base of the jet, and they cool emitting multi wavelength radiation as propagating along the jet. The proton and electron distributions are obtained through steady-state transport equation taking into account acceleration, radiative and non-radiative cooling processes, as well as particle transport by convection. Results. Considering the effects of photon absorption at different wavelengths, we calculate the radiation emitted by the primary protons and electrons, as well as the contribution of secondaries particles (e ± , πs and μs). The expected high-energy neutrino signal is also obtained and the possibility of detections with KM3NeT and IceCube is discussed. Conclusions. The spectral energy distribution obtained in our model with an appropriate set of parameters for an extended emission zone can account for much of the observed spectra for both AGNs.

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“…Such jets are known to emit across a broad range of the electromagnetic spectrum, from radio to X-rays, and perhaps even γ-rays. Sometimes jets can be imaged directly, but often their presence is inferred, such as from flat to slightly inverted spectral energy distribution (SED) in radio through IR (see, e.g., Markoff et al 2001;Maitra et al 2009a;Vila & Romero 2010), correlation between fluxes (see, e.g., Gallo et al 2003;Russell et al 2010), and scaling relations connecting radio and X-ray luminosities with the black hole mass (Merloni et al 2003;Falcke et al 2004;Gültekin et al 2009). …”

Section: Introductionmentioning

confidence: 99%

Jets at lowest mass accretion rates

et al. 2010

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Abstract. We present results of recent observations and theoretical modeling of data from black holes accreting at very low luminosities (L/L E dd 10 −8 ). We discuss our newly developed time-dependent model for episodic ejection of relativistic plasma within a jet framework, and a successful application of this model to describe the origin of radio flares seen in Sgr A*, the Galactic center black hole. Both the observed time lags and size-frequency relationships are reproduced well by the model. We also discuss results from new Spitzer data of the stellar black hole X-ray binary system A0620-00. Complemented by long term SMARTS monitoring, these observations indicate that once the contribution from the accretion disk and the donor star are properly included, the residual mid-IR spectral energy distribution of A0620-00 is quite flat and consistent with a non-thermal origin. The results above suggest that a significant fraction of the observed spectral energy distribution originating near black holes accreting at low luminosities could result from a mildly relativistic outflow. The fact that these outflows are seen in both stellar-mass black holes as well as in supermassive black holes at the heart of AGNs strengthens our expectation that accretion and jet physics scales with mass.

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Leptonic/hadronic models for electromagnetic emission in microquasars: the case of GX 339-4

Cited by 44 publications

References 62 publications

Ultra-high-energy cosmic rays from low-luminosity active galactic nuclei

Ultra-high-energy cosmic rays from low-luminosity active galactic nuclei

A lepto-hadronic model for high-energy emission from FR I radiogalaxies

Jets at lowest mass accretion rates

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