Cosmic rays from microquasars: A narrow component to the CR spectrum?

Heinz, Sebastian; Sunyaev, R.

doi:10.1051/0004-6361:20020615

Cited by 149 publications

(155 citation statements)

References 61 publications

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“…Velázquez & Raga 2000;Heinz 2002;Heinz & Sunyaev 2002;Bosch-Ramon et al 2005;Zavala et al 2008;Bordas et al 2009;Bosch-Ramon et al 2011). On the other hand, PSR B1259−63 is a system formed by an O9.5 V star and a nonaccreting millisecond pulsar (Johnston et al 1992;Negueruela et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Large-scale flow dynamics and radiation in pulsarγ-ray binaries

Bosch‐Ramon

Barkov

2011

A&A

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Context. Several gamma-ray binaries show extended X-ray emission that may be associated to interactions of an outflow with the medium. Some of these systems are, or may be, high-mass binaries harboring young nonaccreting pulsars, in which the stellar and the pulsar winds collide, generating a powerful outflow that should terminate at some point in the ambient medium. Aims. This work studies the evolution and termination, as well as the related radiation, of the shocked-wind flow generated in highmass binaries hosting powerful pulsars. Methods. A characterization, based on previous numerical work, is given for the stellar/pulsar wind interaction. Then, an analytical study of the further evolution of the shocked flow and its dynamical impact on the surrounding medium is carried out. Finally, the expected nonthermal emission from the flow termination shock, likely the dominant emitting region, is calculated. Results. The shocked wind structure, initially strongly asymmetric, becomes a quasi-spherical, supersonically expanding bubble, with its energy coming from the pulsar and mass from the stellar wind. This bubble eventually interacts with the environment on ∼pc scales, producing a reverse and, sometimes, a forward shock. Nonthermal leptonic radiation can be efficient in the reverse shock. Radio emission is expected to be faint, whereas X-rays can easily reach detectable fluxes. Under very low magnetic fields and large nonthermal luminosities, gamma rays may also be significant. Conclusions. The complexity of the stellar/pulsar wind interaction is likely to be smoothed out outside the binary system, where the wind-mixed flow accelerates and eventually terminates in a strong reverse shock. This shock may be behind the extended Xrays observed in some binary systems. For very powerful pulsars, part of the unshocked pulsar wind may directly interact with the large-scale environment.

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Section: Introductionmentioning

confidence: 99%

Large-scale flow dynamics and radiation in pulsarγ-ray binaries

Bosch‐Ramon

Barkov

2011

A&A

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“…Nevertheless, hints or evidence of these interactions have been observed, at different wavelengths, in SS 433 (Zealey et al 1980), 1E 1740.7−2942 (Mirabel et al 1992), XTE J1550−564 (Corbel et al 2002), Cygnus X-3 (Heindl et al 2003), Cygnus X-1 (Martí et al 1996;Gallo et al 2005), GRS 1915+105 (Kaiser et al 2004), H1743−322 (Corbel et al 2005), LS I +61 303 (Paredes et al 2007a), and Circinus X-1 (Tudose et al 2006), although little theoretical work has been completed regarding the hydrodynamics of the interaction, or the resulting non-thermal emission (e.g. Aharonian & Atoyan 1998;Velázquez & Raga 2000;Heinz & Sunyaev 2002;Bosch-Ramon et al 2005;Perucho & Bosch-Ramon 2008). MQ ejections can transport significant amounts of kinetic energy and momentum far from the binary system.…”

Section: Introductionmentioning

confidence: 99%

Non-thermal emission from microquasar/ISM interaction

Bordas¹,

Bosch‐Ramon

Paredes³

et al. 2009

A&A

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Context. The interaction of microquasar jets with their environment can produce non-thermal radiation as in the case of extragalactic outflows impacting on their surroundings. Significant observational evidence of jet/medium interaction in galactic microquasars has been collected in the past few years, although little theoretical work has been done regarding the resulting non-thermal emission. Aims. In this work, we investigate the non-thermal emission produced in the interaction between microquasar jets and their environment, and the physical conditions for its production. Methods. We developed an analytical model based on those successfully applied to extragalactic sources. The jet is taken to be a supersonic and mildly relativistic hydrodynamical outflow. We focus on the jet/shocked medium structure in its adiabatic phase, and assume that it grows in a self-similar way. We calculate the fluxes and spectra of the radiation produced via synchrotron, inverse Compton, and relativistic bremsstrahlung processes by electrons accelerated in strong shocks. A hydrodynamical simulation is also performed to investigate further the jet interaction with the environment and check the physical parameters used in the analytical model. Results. For reasonable values of the magnetic field, and using typical values of the external matter density, the non-thermal particles could produce significant amounts of radiation at different wavelengths, although they do not cool primarily radiatively, but by adiabatic losses. The physical conditions of the analytical jet/medium interaction model are consistent with those found in the hydrodynamical simulation. Conclusions. Microquasar jet termination regions could be detectable at radio wavelengths for current instruments sensitive to ∼arcminute scales. At X-ray energies, the expected luminosities are moderate, although the emitter is more compact than the radio one. The source may be detectable by XMM-Newton or Chandra, with 1-10 arcsec of angular resolution. The radiation at gamma-ray energies may be within the detection limits of the next generation of satellite and ground-based instruments.

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“…The interaction regions between the SS 433 jets and the surrounding W50 nebula could also produce VHE gamma-ray emission, for example through IC scattering of cosmic microwave background (CMB) photons by electrons accelerated at the eastern (e1, e2, e3) and western (w1, w2) termination regions (Safi-Harb & Ögelman 1997;Aharonian & Atoyan 1998;Bordas et al 2009), or through pp interactions if protons are efficiently accelerated at the interaction shocks (Heinz & Sunyaev 2002;Bosch-Ramon et al 2005). Non-thermal emission from these regions has indeed been observed from radio to Xray energies (Brinkmann et al 1996, Dubner et al 1998Safi-Harb & Ögelman 1997;Safi-Harb & Petre 1999;Fuchs 2002;Brinkmann et al 2007.…”

Section: Gamma-ray Emission and Absorption Processes In Ss 433/w50mentioning

confidence: 99%

Constraints on particle acceleration in SS433/W50 from MAGIC and H.E.S.S. observations

Ahnen¹,

Ansoldi²,

Antonelli³

et al. 2018

A&A

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Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system.Aim. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses (Porb~ 13.1 days) and precession of the circumstellar disk (Ppre ~ 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations.Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to ~40–80 h, depending on the region, was employed.Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be ≲ 10−12–10−13 TeV−1 cm−2 s−1 in an energy interval ranging from ~few × 100 GeV to ~few TeV. Integral flux limits down to ~ 10−12–10−13 ph cm−2 s−1 and ~ 10−13–10−14 ph cm−2 s−1 are obtainedat 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jetregions and on the physics of the jet/medium interactions.Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, qp ≤ 2.5 × 10−5, to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields ≳10 μG is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with Ee− up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions.

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Cosmic rays from microquasars: A narrow component to the CR spectrum?

Cited by 149 publications

References 61 publications

Large-scale flow dynamics and radiation in pulsarγ-ray binaries

Large-scale flow dynamics and radiation in pulsarγ-ray binaries

Non-thermal emission from microquasar/ISM interaction

Constraints on particle acceleration in SS433/W50 from MAGIC and H.E.S.S. observations

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