Modelling interaction of relativistic and non-relativistic winds in binary system PSR B1259−63/SS2883 – I. Hydrodynamical limit

Bogovalov, S. V.; Khangulyan, D.; Koldoba, A. V.; Ustyugova, G. V.; Aharonian, F.

doi:10.1111/j.1365-2966.2008.13226.x

Cited by 147 publications

(226 citation statements)

References 54 publications

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“…The shocked wind flows away from the companion star forming a comet-like tail of emission. Relativistic hydrodynamical calculations show the flow is conical with an opening angle set by η and can reach highly relativistic speeds (Bogovalov et al 2008). High energy electrons emit VHE gamma-rays and synchrotron X-rays close to the pulsar and lose energy as they flow out, emitting in the radio band far from the system (Dubus 2006).…”

Section: Relativistic Doppler Boostingmentioning

confidence: 99%

“…An offset of 0.275 should be added to the above phases to compare with the radio-based ephemeris of LS I +61 • 303. Bogovalov et al (2008) carried out relativistic hydrodynamical simulations of a pulsar wind interacting with a stellar wind with the specific case of PSR B1259-63 in mind. They found that the shocked pulsar wind can accelerate from bulk Lorentz factors ≈1 close to the termination shock up to 100 far away.…”

Section: Psr B1259-63mentioning

confidence: 99%

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Relativistic Doppler-boosted emission in gamma-ray binaries

Dubus¹,

Cerutti²,

Henri³

2010

A&A

104

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Context. Gamma-ray binaries could be compact pulsar wind nebulae formed when a young pulsar orbits a massive star. The pulsar wind is contained by the stellar wind of the O or Be companion, creating a relativistic comet-like structure accompanying the pulsar along its orbit. Aims. The X-ray and the very high energy (>100 GeV, VHE) gamma-ray emission from the binary LS 5039 are modulated on the orbital period of the system. Maximum and minimum flux occur at the conjunctions of the orbit, suggesting that the explanation is linked to the orbital geometry. The VHE modulation has been proposed to be due to the combined effect of Compton scattering and pair production on stellar photons, both of which depend on orbital phase. The X-ray modulation could be due to relativistic Doppler boosting in the comet tail where both the X-ray and VHE photons would be emitted. Methods. Relativistic aberrations change the seed stellar photon flux in the comoving frame so Doppler boosting affects synchrotron and inverse Compton emission differently. The dependence with orbital phase of relativistic Doppler-boosted (isotropic) synchrotron and (anisotropic) inverse Compton emission is calculated, assuming that the flow is oriented radially away from the star (LS 5039) or tangentially to the orbit (LS I +61 • 303, PSR B1259-63).Results. Doppler boosting of the synchrotron emission in LS 5039 produces a lightcurve whose shape corresponds to the X-ray modulation. The observations imply an outflow velocity of 0.15-0.33c consistent with the expected flow speed at the pulsar wind termination shock. In LS I +61 • 303, the calculated Doppler boosted emission peaks in phase with the observed VHE and X-ray maximum. Conclusions. Doppler boosting is not negligible in gamma-ray binaries, even for mildly relativistic speeds. The boosted modulation reproduces the X-ray modulation in LS 5039 and could also provide an explanation for the puzzling phasing of the VHE peak in LS I +61 • 303.

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Section: Relativistic Doppler Boostingmentioning

confidence: 99%

Section: Psr B1259-63mentioning

confidence: 99%

Relativistic Doppler-boosted emission in gamma-ray binaries

Dubus¹,

Cerutti²,

Henri³

2010

A&A

104

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“…An important parameter that characterizes the wind interaction region is the pulsar to stellar wind momentum flux ratio (e.g. Bogovalov et al 2008):…”

Section: Physical Scenariomentioning

confidence: 99%

“…The distance between the CD and the star is then ≈2.3 × 10 12 cm. The CD, which separates the shocked stellar and pulsar winds, has an asymptotic half-opening angle (see Bogovalov et al 2008 and references therein):…”

Section: Physical Scenariomentioning

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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“…Electrons accelerated in the shock between the PW and stellar wind can produce synchrotron radiation and/or upscatter stellar or disk photons from LS2883to produce inverse-Compton (IC) radiation (Tavani & Arons 1997;Kirk et al 1999;Dubus 2006;Bogovalov et al 2008;Khangulyan et al 2011;Kong et al 2011;Takata et al 2012;Mochol & Kirk 2013). The unshocked PW particles may also generate γ-rays (Khangulyan et al 2012).…”

Section: Introductionmentioning

confidence: 99%

The Hour-timescale GeV Flares of PSR B1259–63 in 2017

Tam

Pal

et al. 2018

ApJ

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GeV flares from PSRB1259−63/LS2883 were seen starting around 30 days after the two periastron passages in 2010 and 2014. The flares are clearly delayed compared to the occurrence of the X-ray and TeV flux peaks during the post-periastron disk crossing. Although several attempts have been put forward to explain this phenomenon, the origin of these GeV flares remains a puzzle. Here we present a detailed analysis of the observational data taken by the Fermi and Swift observatories over the 2017 September periastron passage. For the first time, we find shortlived but powerful GeV flares on timescales of down to three hours. The onset of the GeV flaring period in 2017 is also delayed compared to that seen in 2011 and 2014. Supplemented by a reanalysis of previous data, we compare the Fermi/LAT, Swift/XRT, and Swift/UVOT light curves in 2017 with those taken over the 2010 and 2014 periastrons, and differences in UVOT light curves are noted.

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Modelling interaction of relativistic and non-relativistic winds in binary system PSR B1259−63/SS2883 – I. Hydrodynamical limit

Cited by 147 publications

References 54 publications

Relativistic Doppler-boosted emission in gamma-ray binaries

Relativistic Doppler-boosted emission in gamma-ray binaries

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

The Hour-timescale GeV Flares of PSR B1259–63 in 2017

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