High-energy pulses and phase-resolved spectra by inverse Compton emission in the pulsar striped wind

Pétri, Jérôme

doi:10.1051/0004-6361/200811010

Cited by 25 publications

(35 citation statements)

References 26 publications

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“…The pulsation observability condition is constrained by relativistic beaming, retardation and geometrical effects. If emission occurs at a radius r and within a range r then according to Kirk, Skjaeraasen & Gallant (2002) and Pétri (2009aPétri ( , 2011 pulses are restricted to regions where…”

Section: Wind Observabilitymentioning

confidence: 99%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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Neutron stars are fascinating astrophysical objects immersed in strong gravitational and electromagnetic fields, at the edge of our current theories. These stars manifest themselves mostly as pulsars, emitting a timely very stable and regular electromagnetic signal. Even though discovered almost fifty years ago, they still remain mysterious compact stellar objects. In this review, we summarize the most fundamental theoretical aspects of neutron star magnetospheres and winds. The main competing models explaining their radiative properties like multi-wavelength pulse shapes and spectra and the underlying physical processes such as pair creation and radiation mechanisms are scrutinized. A global but still rather qualitative picture slowly emerges thanks to recent advances in numerical simulations on the largest scales. However considerations about pulsar magnetospheres remain speculative. For instance, the exact composition of the magnetospheric plasma is not yet known. Is it solely filled with a mixture of e ± leptons or does it contain a non-negligible fraction of protons and/or ions? Is it almost entirely filled or mostly empty except for some small anecdotal plasma filled regions? Answers to these questions will strongly direct the description of the magnetosphere to seemingly contradictory results leading sometimes to inconsistencies. Nevertheless, accounts are given as to the latest developments in the theory of pulsar magnetospheres and winds, the existence of a possible electrosphere and physical insight obtained from related observational signatures of multi-wavelength pulsed emission.

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Section: Wind Observabilitymentioning

confidence: 99%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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“…While we do not simulate MSP light curves using the annular gap model, we do discuss comparisons with results of light curve fitting using this model by other authors (see Section 7). Pétri (2009) proposed the striped wind model to explain HE pulsar emission. In this model, the observed gamma rays are produced via inverse Compton scattering of the cosmic microwave background off an electron-positron pair wind outside the light cylinder.…”

Section: Emission Modelsmentioning

confidence: 99%

Constraints on the Emission Geometries and Spin Evolution of Gamma-Ray Millisecond Pulsars

Johnson

Venter

Harding

et al. 2014

ApJS

102

157

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Millisecond pulsars (MSPs) are a growing class of gamma-ray emitters. Pulsed gamma-ray signals have been detected from more than 40 MSPs with the Fermi Large Area Telescope (LAT). The wider radio beams and more compact magnetospheres of MSPs enable studies of emission geometries over a broader range of phase space than non-recycled radio-loud gamma-ray pulsars. We have modeled the gamma-ray light curves of 40 LAT-detected MSPs using geometric emission models assuming a vacuum retarded-dipole magnetic field. We modeled the radio profiles using a single-altitude hollow-cone beam, with a core component when indicated by polarimetry; however, for MSPs with gamma-ray and radio light curve peaks occurring at nearly the same rotational phase, we assume that the radio emission is co-located with the gamma rays and caustic in nature. The best-fit parameters and confidence intervals are determined using a maximum likelihood technique. We divide the light curves into three model classes, with gamma-ray peaks trailing (Class I), aligned (Class II), or leading (Class III) the radio peaks. Outer gap and slot gap (two-pole caustic) models best fit roughly equal numbers of Class I and II, while Class III are exclusively fit with pair-starved polar cap models. Distinguishing between the model classes based on typical derived parameters is difficult. We explore the evolution of the magnetic inclination angle with period and spin-down power, finding possible correlations. While the presence of significant off-peak emission can often be used as a discriminator between outer gap and slot gap models, a hybrid model may be needed.

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“…However, this model results in worse fits to the data, according to J14. 18 There exist other models for γ-ray emission (Qiao et al 2004;Pétri 2009;Du et al 2010), as well as more detailed (patched cone) models of the radio profiles of MSPs (Craig 2014), but we will not focus on them in this work.…”

Section: Magnetic Field At the Light Cylindermentioning

confidence: 99%

A Broadband Radio Study of the Average Profile and Giant Pulses From PSR B1821-24a

Bilous

Pennucci

Demorest

et al. 2015

ApJ

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We present the results of a wideband (720-2400 MHz) study of PSR B1821-24A (J1824-2452A, M28A), an energetic millisecond pulsar (MSP) visible in radio, X-rays and γ-rays. In radio, the pulsar has a complex average profile that spans 85% of the spin period and exhibits strong evolution with observing frequency. For the first time we measure phase-resolved polarization properties and spectral indices of radio emission throughout almost all of the on-pulse window. We synthesize our findings with high-energy information to compare M28A to other known γ-ray MSPs and to speculate that M28A's radio emission originates in multiple regions within its magnetosphere (i.e., both in the slot or outer gaps near the light cylinder and at lower altitudes above the polar cap). M28A is one of a handful of pulsars that are known to emit giant radio pulses (GRPs)-short, bright radio pulses of unknown nature. We report a drop in the linear polarization of the average profile in both windows of GRP generation and also a "W"-shaped absorption feature (resembling a double notch), partly overlapping with one of the GRP windows. The GRPs themselves have broadband spectra consisting of multiple patches with Δν/ν ∼ 0.07. Although our time resolution was not sufficient to resolve the GRP structure on the μs scale, we argue that GRPs from this pulsar most closely resemble the GRPs from the main pulse of the Crab pulsar, which consist of a series of narrowband nanoshots.

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High-energy pulses and phase-resolved spectra by inverse Compton emission in the pulsar striped wind

Cited by 25 publications

References 26 publications

Theory of pulsar magnetosphere and wind

Theory of pulsar magnetosphere and wind

Constraints on the Emission Geometries and Spin Evolution of Gamma-Ray Millisecond Pulsars

A Broadband Radio Study of the Average Profile and Giant Pulses From PSR B1821-24a

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