<i>Chandra</i>
                    Observations of the Gamma-Ray Binary [OBJECTNAME STATUS="NOLINK"]LS I +61 303[/OBJECTNAME]: Extended X-Ray Structure?

Paredes, J. M.; Ribó, M.; Bosch‐Ramon, V.; West, Jennifer Rittenhouse; Butt, Y.; Torres, D. F.; Martı́, Josep

doi:10.1086/520674

Cited by 59 publications

(68 citation statements)

References 24 publications

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“…In Sect. 3, the general properties of the interaction between the flow and the external medium, the 1 Rea et al (2010) did not find evidence of extended X-rays in LS I +61 303 in longer observations than those studied in Paredes et al 2007. However, in their observations the X-ray counts were integrated along one spatial dimension in the CCDs, which only allows finding an extension signal in specific directions.…”

Section: Introductionmentioning

confidence: 87%

“…Several gamma-ray binaries present hints or clear evidence of interactions between an outflow and their medium on large scales: Cygnus X-3, LS I +61 303, LS 5039, PSR B1259−63, and the gamma-ray emitter candidate Cygnus X-1 (Heindl et al 2003;Sánchez-Sutil et al 2008;Paredes et al 2007;Pavlov et al 2011a;Durant et al 2011;Martí et al 1996;Gallo et al 2005;Russell et al 2007). …”

Section: Introductionmentioning

confidence: 99%

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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: 87%

Section: Introductionmentioning

confidence: 99%

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

Bosch‐Ramon

Barkov

2011

A&A

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“…In the case of MQs, evidence of jet interaction with the interstellar medium (ISM) are not numerous, partially due to the relatively small number of known sources. 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).…”

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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“…Given this coincidence, this burst was associated with magnetar-like activity linked to a young highly magnetized pulsar in the binary system (Dubus & Giebels 2008). Unusual X-ray activity (hard high flux and QPOs) had also been reported by Ray et al (2008) just a few weeks before based on PCA data from the RXTE satellite. If the QPOs originate in LS I +61 303, an accretion disk would be necessary to explain the nature of this source.…”

Section: Introductionmentioning

confidence: 65%

Candidate counterparts to the soft gamma-ray flare in the direction of LS I +61 303

Muñoz‐Arjonilla

Martı́

Combi

et al. 2009

A&A

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Context. A short duration burst reminiscent of a soft gamma-ray repeater/anomalous X-ray pulsar behaviour was detected in the direction of LS I +61 303 by the Swift satellite. While the association with this well known gamma-ray binary is likely, a different origin cannot be excluded. Aims. We explore the error box of this unexpected flaring event and establish the radio, near-infrared and X-ray sources in our search for any peculiar alternative counterpart. Methods. We carried out a combined analysis of archive Very Large Array radio data of LS I +61 303 sensitive to both compact and extended emission. We also reanalysed previous near infrared observations with the 3.5 m telescope of the Centro Astronómico Hispano Alemán and X-ray observations with the Chandra satellite. Results. Our deep radio maps of the LS I +61 303 environment represent a significant advancement on previous work and 16 compact radio sources in the LS I +61 303 vicinity are detected. For some detections, we also identify near infrared and X-ray counterparts. Extended emission features in the field are also detected and confirmed. The possible connection of some of these sources with the observed flaring event is considered. Based on these data, we are unable to claim a clear association between the Swift-BAT flare and any of the sources reported here. However, this study represents the most sophisticated attempt to determine possible alternative counterparts other than LS I +61 303.

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Chandra Observations of the Gamma-Ray Binary [OBJECTNAME STATUS="NOLINK"]LS I +61 303[/OBJECTNAME]: Extended X-Ray Structure?

Cited by 59 publications

References 24 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

Candidate counterparts to the soft gamma-ray flare in the direction of LS I +61 303

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