Light Curve and SED Modeling of the Gamma-Ray Binary 1FGL J1018.6–5856: Constraints on the Orbital Geometry and Relativistic Flow

An, Hongjun; Romani, Roger W.

doi:10.3847/1538-4357/aa6623

Cited by 25 publications

(38 citation statements)

References 30 publications

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“…There are relativistic electrons and positrons stochastically accelerated in the shock, hence synchrotron radiation is expected. Then the particles will inverse-Compton upscatter the synchrotron photons (synchrotron-self Compton, SSC) and the stellar optical/UV photons external to the shock (external Compton, EC); these emissions will be in the ∼TeV band [6,10]. Due to these emissions, the energy distribution of the particles evolves in time and space, so does the emitted photon spectrum.…”

Section: The Ibs Emission Modelmentioning

confidence: 99%

“…The model we develop [10] is basically a combination of the above. Using the masses of the two stars and the orbital EPJ Web of Conferences 168, 04013 (2018) https://doi.org/10.1051/epjconf/201816804013 Joint International Conference of ICGAC-XIII and IK-15 on Gravitation, Astrophysics and Cosmology period measurement, we can determine the orbital separation (D) using the Kepler's law.…”

Section: The Ibs Modelmentioning

confidence: 99%

“…Therefore, studying IBS requires detailed numerical simulations and comparison of simulations and observations. However, these simulations are yet to be improved for the relativistic pulsar wind, so instead, we use a relatively simple phenomenological model for IBS emission in order to infer the flow properties and the orbital geometry using high-energy observations [10].…”

Section: The Ibs Emission Modelmentioning

confidence: 99%

“…Around the CD, shocks are � e-mail: hjan@chungbuk.ac.kr formed of which the relativistic pulsar wind shock is of interest in regard to the high-energy emission in these systems [6]. In the pulsar wind shock, particles are stochastically accelerated and are believed to be bulk accelerated as they flow [7,8]; Lorentz beaming is expected which may be observed as spikes in the orbital light curve [9,10].…”

Section: Introductionmentioning

confidence: 99%

“…Using the IBS scenario, we develop a phenomenological model for the high-energy emission [10] in pulsar binaries. Below we show details of the model components and present the results of application to the gamma-ray binary 1FGL J1018.6−5856.…”

Section: Introductionmentioning

confidence: 99%

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A model for high-energy emission of the Intrabinary shock in pulsar binaries

2018

EPJ Web Conf.

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Abstract. We present our studies of intrabinary shock emission for astrophysical binary systems with a neutron star. We construct a model for the shock emission and compare the model calculation with the light curve and the spectral energy distribution of the gamma-ray binary 1FGL J1018.6−5856. The model assumes a slow and a fast population of particles accelerated in the shock, and computes the high-energy emission spectra and orbital light curves produced by synchrotron, self-Compton and external Compton processes of the high-energy particles in the shock. The model allows one to study plasma properties and to constrain the binary geometry, most importantly the inclination angle (i). We discuss potential use of this model for other pulsar binaries to determine the inclination angle of the binary hence the mass of the neutron star.

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Section: The Ibs Emission Modelmentioning

confidence: 99%

Section: The Ibs Modelmentioning

confidence: 99%

Section: The Ibs Emission Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A model for high-energy emission of the Intrabinary shock in pulsar binaries

2018

EPJ Web Conf.

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Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Kim

2020

Astron Nachr

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We investigate the broadband emission properties of the pulsar wind nebula (PWN) 3C 58 using a spectral energy distribution (SED) model. We attempt to match simultaneously the broadband SED and spatial variations of X‐ray emission in the PWN. We further use the model to explain a possible far‐IR feature of which a hint was recently suggested in 3C 58: a small bump at ∼1011 GHz in the PLANCK and Herschel bands. While external dust emission may easily explain the observed bump, it may be the internal emission of the source, implying an additional population of particles. Although significance for the bump is not high, here we explore possible origins of the IR bump using the emission model, and find that a population of electrons with GeV energies can explain it. If it is produced in the PWN, it may provide new insights into particle acceleration and flows in PWNe.

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Sizing up the population of gamma-ray binaries

Dubus

Guillard

Petrucci

et al. 2017

A&A

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Context. Gamma-ray binaries are thought to be composed of a young pulsar in orbit around a massive O or Be star, with their gamma-ray emission powered by pulsar spindown. The number of such systems in our Galaxy is not known. Aims. We aim to estimate the total number of gamma-ray binaries in our Galaxy and to evaluate the prospects for new detections in the GeV and TeV energy range, taking into account that their gamma-ray emission is modulated on the orbital period. Methods. We model the population of gamma-ray binaries and evaluate the fraction of detected systems in surveys with the Fermi-LAT (GeV), HESS, HAWC and CTA (TeV) using observation-based and synthetic template lightcurves. Results. The detected fraction depends more on the orbit-average flux than on the lightcurve shape. Our best estimate for the number of gamma-ray binaries is 101 +89 −52 systems. A handful of discoveries are expected by pursuing the Fermi-LAT survey. Discoveries in TeV surveys are less likely. However, this depends on the relative amounts of power emitted in GeV and TeV domains. There could be as many as ≈ 200 HESS J0632+057-like systems with a high ratio of TeV to GeV emission compared to other gamma-ray binaries. Statistics allow for as many as three discoveries in five years of HAWC observations and five discoveries in the first two years of the CTA Galactic Plane survey. Conclusions. Continued Fermi-LAT observations are favoured over ground-based TeV surveys to find new gamma-ray binaries. Gamma-ray observations are most sensitive to short orbital period systems with a high spindown pulsar power. Radio pulsar surveys (SKA) are likely to be more efficient in detecting long orbital period systems, providing a complementary probe into the gamma-ray binary population.

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Light Curve and SED Modeling of the Gamma-Ray Binary 1FGL J1018.6–5856: Constraints on the Orbital Geometry and Relativistic Flow

Cited by 25 publications

References 30 publications

A model for high-energy emission of the Intrabinary shock in pulsar binaries

A model for high-energy emission of the Intrabinary shock in pulsar binaries

Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Sizing up the population of gamma-ray binaries

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