2018
DOI: 10.1038/s41550-018-0384-5
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Order parameters for the high-energy spectra of pulsars

Abstract: From the hundreds of gamma-ray pulsars known (Atwood et al. 2009), only a handful show non-thermal X-ray pulsations (Kuiper & Hermsen 2015). Instead, nine objects pulse in non-thermal X-rays but lack counterparts at higher energies. Here, we present a physical model for the non-thermal emission of pulsars above 1 keV. With just four physical parameters, we fit the spectrum of the gamma/X-ray pulsars along seven orders of magnitude. We find that all detections can be encompassed in a continuous variation of the… Show more

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Cited by 48 publications
(77 citation statements)
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“…For instance, they are of particular interest to probe the models developed by Takata et al (2008); Takata & Cheng (2017); Hirotani (2015); Harding et al (2018); Viganò et al (2015); Torres (2018), to name a few. In particular, we have recently developed a model that was successfully applied to the broad-band SEDs of some gamma-ray pulsars with detected non-thermal X-ray emission (Torres 2018). Testing this model against an extended sample of X-ray and gamma-ray pulsars is needed to gain insight into the physics of pulsar emission, e.g., to corroborate the correlations between model parameters, unveil new trends between these parameters, and test model limitations.…”
Section: Introductionmentioning
confidence: 99%
“…For instance, they are of particular interest to probe the models developed by Takata et al (2008); Takata & Cheng (2017); Hirotani (2015); Harding et al (2018); Viganò et al (2015); Torres (2018), to name a few. In particular, we have recently developed a model that was successfully applied to the broad-band SEDs of some gamma-ray pulsars with detected non-thermal X-ray emission (Torres 2018). Testing this model against an extended sample of X-ray and gamma-ray pulsars is needed to gain insight into the physics of pulsar emission, e.g., to corroborate the correlations between model parameters, unveil new trends between these parameters, and test model limitations.…”
Section: Introductionmentioning
confidence: 99%
“…Close to the light cylinder, and for some lines at least, the overall twist may become important, as numerical simulations show, see e.g., Spitkovsky (2006). On the other hand, though, from what we know after our spectral-only model (see Torres (2018); Torres et al (2019)), the relevant region of emission is always small in comparison with the scale of the light cylinder. In these small regions, the torsion of the lines can indeed be negligible, even if it is not negligible for the whole line.…”
Section: Differential Geometry Of the Linesmentioning
confidence: 70%
“…If one assumes that IE is given by the synchro-curvature emission as derived in Viganò et al (2015a), then it will depend on the photon energy E, and on the values of α, rc and B. They are ultimately reduced to a λ-dependency if the particle trajectory is solved as well for a specific pulsar of period P and accelerating region properties (E , b), where the latter is the magnetic gradient as defined in Torres (2018) and references therein. In that case, the expression (24) depends on (E, λ, Ψµ, ξµ, ΨΩ).…”
Section: Emission Mapmentioning
confidence: 99%
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