Pulsar Wind Nebulae with Bow Shocks: Non-thermal Radiation and Cosmic Ray Leptons

Bykov, A. M.; Amato, Elena; Petrov, A. E.; Krassilchtchikov, A. M.; Levenfish, K. P.

doi:10.1007/978-94-024-1292-5_8

Cited by 4 publications

(6 citation statements)

References 174 publications

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“…The measurements in broad F125LP and F140LP filters (wavelength bands are 1250-2000 Å and 1350-2000 Å, respectively) do not allow us to establish the spectral model. The existing data are consistent with both a simple power-law spectrum, which could be continuum synchrotron emission from relativistic electrons trapped in the forward shock region (Bykov et al 2017), and the collisionless plasma emission (spectral lines plus continuum) from the ISM matter compressed and heated in the forward shock region (Bykov et al 2013).…”

Section: Forward Shock Emissionsupporting

confidence: 70%

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Pulsar wind nebulae created by fast-moving pulsars

et al. 2017

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We review multiwavelength properties of pulsar wind nebulae created by supersonically moving pulsars and the effects of pulsar motion on the pulsar wind nebulae morphologies and the ambient medium. Supersonic pulsar wind nebulae are characterized by bow-shaped shocks around the pulsar and/or cometary tails filled with the shocked pulsar wind. In the past several years significant advances in supersonic pulsar wind nebula studies have been made in deep observations with the Chandra and XMM-Newton X-ray observatories and the Hubble Space Telescope. In particular, these observations have revealed very diverse supersonic pulsar wind nebula morphologies in the pulsar vicinity, different spectral behaviours of long pulsar tails, the presence of puzzling outflows misaligned with the pulsar velocity and far-UV bow shocks. Here we review the current observational status focusing on recent developments and their implications.

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Section: Forward Shock Emissionsupporting

confidence: 70%

“…In this review we will focus on observational properties of supersonic pulsar wind nebulae (SPWNe). For a recent theoretical review, see Bykov et al (2017).…”

Section: Introductionmentioning

confidence: 99%

Pulsar wind nebulae created by fast-moving pulsars

et al. 2017

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“…The current data regarding the non-thermal radiation (in Radio and X-ray frequencies) emitted from several well-observed PWNe [58] require a lepton spectrum which has the shape of a broken power law, with a hard spectrum (with slope 1 Γ inj 2) below a break at ∼ 200 -400 GeV, and a steeper one (Γ inj > 2) at larger energies (see [20,[59][60][61]). The hard, low-energy spectrum has been object of debate over the years, and several acceleration mechanisms were proposed, including magnetic reconnection at the TS and resonant absorption of ion-cyclotron waves.…”

Section: Setting the Stage: Basic Aspects Of Pulsar Acceleration In P...mentioning

confidence: 99%

Features in cosmic-ray lepton data unveil the properties of nearby cosmic accelerators

Fornieri

Gaggero

Grasso

2020

J. Cosmol. Astropart. Phys.

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We present a comprehensive discussion about the origin of the features in the leptonic component of the cosmic-ray spectrum. Working in the framework of a up-to-date CR transport scenario tuned on the most recent AMS-02 and Voyager data, we show that the prominent features recently found in the positron and in the all-electron spectra by several experiments are explained in a scenario in which pulsar wind nebulae (PWNe) are the dominant sources of the positron flux, and nearby supernova remnants shape the highenergy peak of the electron spectrum. In particular we argue that the drop-off in positron spectrum found by AMS-02 at ∼ 300 GeV can be explained -under different assumptionsin terms of a prominent PWN that provides the bulk of the observed positrons in the ∼ 100 GeV domain, on top of the contribution from a large number of older objects. Finally, we turn our attention to the spectral softening at ∼ 1 TeV in the all-lepton spectrum, recently reported by several experiments, showing that it requires the presence of a nearby supernova remnant at its final stage.

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“…[23], to which we refer for further details. Pulsars are rotating neutron stars with a strong surface magnetic field, and magnetic dipole radiation is believed to provide a good description for its observed loss of rotational energy [15,16]. We consider a model in which e ± are continuously injected at a rate that follows the pulsar spin-down energy.…”

Section: Injection Of E ± From Pulsarsmentioning

confidence: 99%

“…Among the investigated explanations [6][7][8][9][10][11][12][13][14], pulsars have been consolidating as significant factories of high-energy CR e ± in the Galaxy, and thus as main candidates to explain the e + excess. First, the pulsar spin-down mechanism effectively produces e ± pairs, which are possibly accelerated to multi-TeV energies at the termination shock between the relativistic wind and the surrounding medium (see [15,16] for recent reviews on the acceleration mechanism). Secondly, observations of pulsars and their surrounding environment, including their pulsar wind nebula (PWN), across the entire electromagnetic spectrum reveal e ± accelerated at very-highenergies and generating photons through synchrotron and inverse Compton scattering (ICS) processes [17,18].…”

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confidence: 99%

Constraining positron emission from pulsar populations with AMS-02 data

Orusa,

Manconi,

Donato

et al. 2021

Preprint

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The cosmic-ray flux of positrons is measured with high precision by the spaceborne particle spectrometer AMS-02. The hypothesis that pulsar wind nebulae (PWNe) can significantly contribute to the excess of the positron (e + ) cosmic-ray flux has been consolidated after the observation of a γ-ray emission at TeV energies of a few degree size around Geminga and Monogem PWNe. In this work we undertake massive simulations of galactic pulsars populations, adopting different distributions for their position in the Galaxy, intrinsic physical properties, pair emission models, in order to overcome the incompleteness of the ATNF catalogue. We fit the e + AMS-02 data together with a secondary component due to collisions of primary cosmic rays with the interstellar medium. We find that several mock galaxies have a pulsar population able to explain the observed e + flux, typically by few, bright sources. We determine the physical parameters of the pulsars dominating the e + flux, and assess the impact of different assumptions on radial distributions, spin-down properties, Galactic propagation scenarios and e + emission time.

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Pulsar Wind Nebulae with Bow Shocks: Non-thermal Radiation and Cosmic Ray Leptons

Cited by 4 publications

References 174 publications

Pulsar wind nebulae created by fast-moving pulsars

Pulsar wind nebulae created by fast-moving pulsars

Features in cosmic-ray lepton data unveil the properties of nearby cosmic accelerators

Constraining positron emission from pulsar populations with AMS-02 data

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