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Paredes, J. M.; Ribó, M.; Martı́, Josep; Massi, M.

doi:10.1023/a:1011652708923

Cited by 165 publications

(256 citation statements)

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“…3 and 4, during the transient microblazar phase the X-and soft γ-ray spectrum will be softer than in the normal hard state, when the coronal emission dominates. This is an unavoidable consequence of the steepening produced by Compton losses in the injected electron spectrum and can be used to test our proposal, not only through new observations of Cygnus X-1, but also of other potential microblazars as LS5039 (Paredes et al 2000).…”

Section: Non-thermal High-energy Emission For Cygnus X-1mentioning

confidence: 76%

Recurrent microblazar activity in Cygnus X-1?

Romero

Bernado

Mirabel

2002

A&A

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Abstract. Recurrent flaring events at X-and soft gamma-ray energies have been recently reported for the galactic black hole candidate Cygnus X-1. The observed fluxes during these transient outbursts are far higher than what is observed in "normal" episodes. Here we suggest that the origin of this radiation is non-thermal and produced by inverse Compton interactions between relativistic electrons in the jet and external photon fields, with a dominant contribution from the companion star field. The recurrent and relatively rapid variability could be explained by the precession of the jet, which results in a variable Doppler amplification.

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Section: Non-thermal High-energy Emission For Cygnus X-1mentioning

confidence: 76%

Recurrent microblazar activity in Cygnus X-1?

Romero

Bernado

Mirabel

2002

A&A

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“…1). Figure 1 already illustrates that in particular the highenergy emission from blazars can easily vary by more than an order of magnitude between different EGRET observing , BL Lacertae (Böttcher and Bloom, 2000;Böttcher and Reimer, 2004), and Mrk 501 (Petry et al, 2000). For each object, two simultaneous broadband spectra at two different epochs are shown.…”

Section: Phenomenology Of Blazarsmentioning

confidence: 98%

“…), the tentative EGRET detections of at least two Galactic microquasars at MeV-GeV γ -ray energies, namely LS 5039 (Paredes et al, 2000) and LSI+61 • 303 (Gregory and Taylor, 1978;Taylor et al, 1992;Kniffen et al, 1997), the detection of X-ray jet structures in several microquasars using Chandra and XMM-Newton (Corbel et al, 2002;Tomsick, 2002, e.g.,), and, most recently, the detection of veryhigh-energy (VHE) γ -ray emission from LS 5039 (Aharonian et al, 2005) have re-ignited interest in jet models for the high-energy emission from microquasars, analogous to the commonly favored models for blazars. A jet origin of the Xray emission of microquasars has been suggested by several authors, e.g., Markoff et al (2001Markoff et al ( , 2003a, who discussed the possibility of synchrotron emission from relativistic electrons in the jet extending from the radio all the way into the X-ray regime.…”

Section: The Jets Of Microquasarsmentioning

confidence: 99%

Astrophysical Jets of Blazars and Microquasars

Böttcher

2006

Astrophys Space Sci

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Some recent developments in the study of relativistic jets in active galactic nuclei and microquasars are reviewed. While it has been well established for some time that extragalactic jets found in radio galaxies, quasars, and BL Lac objects are the site of ultrarelativistic particle acceleration, the recent identification of the Galactic jet source and microquasar LS 5039 as a source of very-high-energy gamma-ray emission has underlined the striking similarity between the two types of astrophysical jet sources. In this paper, I will present an overview of the dominant radiation and particle acceleration processes and observational tests to distinguish between such processes. The wide-ranging analogies between Galactic and extragalactic jets, but also their distinct differences, in particular those caused by the presence of the companion star in Galactic microquasar systems, will be exposed.

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“…Several of these low-latitude, presumably galactic sources seem to display significant levels of variability over timescales of months (Tompkins 1999;Torres et al 2001a, b). A few particular cases of variable gamma-ray sources at low latitudes have been recently studied by Tavani et al (1997Tavani et al ( , 1998, Paredes et al (2000) and Punsly et al (2000), but there is not yet consensus on their nature. The variety of behaviours displayed by the sources seems to suggest that more than a single class of gammaray emitting objects exists in the Galaxy.…”

Section: Introductionmentioning

confidence: 99%

Variable gamma-ray emission from the Be/X-ray transient A0535+26?

Romero

Bernado

Combi

et al. 2001

A&A

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Abstract. We present a study of the unidentified gamma-ray source 3EG J0542+2610. This source is spatially superposed on the supernova remnant G180.0-1.7, but its time variability makes a physical link unlikely. We have searched in the EGRET location error box for compact radio sources that could be the low energy counterpart of the gamma-ray source. Although 29 point-like radio sources were detected and measured, none of them is strong enough to be considered the counterpart of a background gamma-ray emitting AGN. We suggest that the only object within the 95% error box capable of producing the required gamma-ray flux is the X-ray transient A0535+26. We show that this Be/accreting pulsar can produce variable hadronic gamma-ray emission through the mechanism originally proposed by Cheng & Ruderman (1989), where a proton beam accelerated in a magnetospheric electrostatic gap impacts the transient accretion disk.

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Untitled

Cited by 165 publications

References 0 publications

Recurrent microblazar activity in Cygnus X-1?

Recurrent microblazar activity in Cygnus X-1?

Astrophysical Jets of Blazars and Microquasars

Variable gamma-ray emission from the Be/X-ray transient A0535+26?

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