High Energy Emission from Microquasars

Fender, Rob; Maccarone, Tom

doi:10.1007/978-1-4020-2256-2_9

Cited by 7 publications

(3 citation statements)

References 68 publications

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“…First, it is emphasized that this paper focuses on massive non-degenerate stars in binary or higher multiplicity systems, leading to a wind-wind interaction region characerized by two shocks likely responsible for the acceleration of particles through the diffusive shock acceleration (DSA) mechanism Reimer et al 2006;. As a result, this study does not concern massive X-ray and/or γ-ray binaries or microquasars that include a compact object (Fender & Maccarone 2004;Khangulyan & Aharonian 2005;Bosch-Ramon 2007;Bosch-Ramon & Rieger 2011) and is neither related to supernova remnants, known to be efficient particle accelerators (Romero 2004;Reynolds 2011;Vink 2013). Moreover, the class of objects debated does not include rapidlymoving runaway massive stars whose stellar wind interacts with the interstellar medium, producing strong shocks likely to accelerate particles (Benaglia et al 2010b;Romero et al 2011;Peri et al 2011;del Valle & Romero 2012).…”

Section: The Cataloguementioning

confidence: 99%

Catalogue of particle-accelerating colliding-wind binaries

Becker

Raucq

2013

A&A

118

138

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Massive systems made of two or more stars are known to be the site for interesting physical processes -including at least in some cases -particle acceleration. Over the past decade, this topic motivated a particular effort to unveil the properties of these systems and characterize the circumstances responsible for the acceleration of particles and the potential role of pre-supernova massive stars in the production of high energy particles in our Galaxy. Although previous studies on this topic were mostly devoted to processes in general, or to a few individual objects in particular, a unified target-oriented census of particle-accelerating colliding-wind binaries (hereafter PACWBs) does not exist yet. This paper aims at making a general and unified census of these systems, emphasizing their main properties. A general discussion includes energetic considerations along with wind properties in relation with non-thermal emission processes that are likely at work in colliding-wind binaries. Finally, some guidelines for future observational and theoretical studies are drawn.

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Section: The Cataloguementioning

confidence: 99%

Catalogue of particle-accelerating colliding-wind binaries

Becker

Raucq

2013

A&A

118

138

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“…A hot corona sandwiches the disk at small radii, which can affect the reflection spectrum through Compton scattering. From Fender and Maccarone [130].…”

Section: Black Hole X-ray Binariesmentioning

confidence: 99%

“…These sources are called microquasars [128] [129], exploiting an analogy discussed in more detail below. Figure 2, from [130], is a sketch of an X-ray binary, presenting the major physical components and sites of emission in such systems. The basic underlying idea behind the analogy between quasars and microquasars is that the physics in all black hole systems is essentially governed by scaling laws, whose order parameter is the black hole mass.…”

Section: Microquasars and Jetsmentioning

confidence: 99%

Atomic X-ray spectroscopy of accreting black holes

Liedahl¹,

Torres²

2005

Can. J. Phys.

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Current astrophysical research suggests that the most persistently luminous objects in the Universe are powered by the flow of matter through accretion disks onto black holes. Accretion disk systems are observed to emit copious radiation across the electromagnetic spectrum, each energy band providing access to rather distinct regimes of physical conditions and geometric scale. X-ray emission probes the innermost regions of the accretion disk, where relativistic effects prevail. While this has been known for decades, it also has been acknowledged that inferring physical conditions in the relativistic regime from the behavior of the X-ray continuum is problematic and not satisfactorily constraining. With the discovery in the 1990s of iron X-ray lines bearing signatures of relativistic distortion came the hope that such emission would more firmly constrain models of disk accretion near black holes, as well as provide observational criteria by which to test general relativity in the strong field limit. Here we provide an introduction to this phenomenon. While the presentation is intended to be primarily tutorial in nature, we aim also to acquaint the reader with trends in current research. To achieve these ends, we present the basic applications of general relativity that pertain to X-ray spectroscopic observations of black hole accretion disk systems, focusing on the Schwarzschild and Kerr solutions to the Einstein field equations. To this we add treatments of the fundamental concepts associated with the theoretical and modeling aspects of accretion disks, as well as relevant topics from observational and theoretical X-ray spectroscopy. PACS Nos.: 32.30. Rj, 32.80.Hd, 95.30.Dr, 95.30.Sf, 95.85.Nv, 97.10.Gz. 97.80.Jp, 98.35.Mp, 98.62.Mw

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Towards a Population of Hmxb/Ns Microquasars as Counterparts of Low-Latitude Unidentified Egret Sources

Ribó

Combi

Mirabel

2005

Astrophys Space Sci

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The discovery of the microquasar LS 5039 well within the 95% confidence contour of the Unidentified EGRET Source (UES) 3EG J1824−1514 was a major step towards the possible association between microquasars (MQs) and UESs. The recent discovery of precessing relativistic radio jets in LS I +61 303, a source associated for long time with 2CG 135+01 and with the UES 3EG J0241+6103, has given further support to this idea. Finally, the very recently proposed association between the microquasar candidate AX J1639.0−4642 and the UES 3EG J1639−4702 points towards a population of High Mass X-ray Binary (HMXB)/Neutron Star (NS) microquasars as counterparts of low-latitude unidentified EGRET sources.

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High Energy Emission from Microquasars

Cited by 7 publications

References 68 publications

Catalogue of particle-accelerating colliding-wind binaries

Catalogue of particle-accelerating colliding-wind binaries

Atomic X-ray spectroscopy of accreting black holes

Towards a Population of Hmxb/Ns Microquasars as Counterparts of Low-Latitude Unidentified Egret Sources

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