Inverse Compton origin of pulsar <i>γ</i> ‐ray emission and the reconnection model of Crab Nebula flares

Lyutikov, Maxim

doi:10.1002/asna.201312023

Cited by 3 publications

(3 citation statements)

References 34 publications

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“…These flares are not yet well understood -see discussions in e.g. Arons (2012); Bykov et al (2012); Lyutikov, Balsara & Matthews (2012); Lyutikov (2014); Sturrock & Aschwanden (2012), and Komissarov & Lyutikov (2011), although they likely involve regions moving relativistically towards us and/or perhaps magnetic reconnection. While there are occasionally small sudden changes in the spindown rate of the pulsar known as glitches, Espinoza et al (2010) and Mickaliger et al (2012) have shown glitches do not seem to occur in conjunction with the gamma ray flares.…”

Section: Introductionmentioning

confidence: 99%

The variability of the Crab nebula in radio: no radio counterpart to gamma-ray flares

Bietenholz

Yuan

Buehler

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present new Jansky Very Large Array (VLA) radio images of the Crab Nebula at 5.5 GHz, taken at two epochs separated by 6 days about two months after a gamma-ray flare in 2012 July. We find no significant change in the Crab's radio emission localized to a region of < 2 light-months in radius, either over the 6-day interval between our present observations or between the present observations and ones from 2001. Any radio counterpart to the flare has a radio luminosity of < ∼ 2 × 10 −4 times that of the nebula. Comparing our images to one from 2001, we do however find changes in radio brightness, up to 10% in amplitude, which occur on decade timescales throughout the nebula. The morphology of the changes is complex suggesting both filamentary and knotty structures. The variability is stronger, and the timescales likely somewhat shorter, nearer the centre of the nebula. We further find that even with the excellent u-v coverage and signal-to-noise of the VLA, deconvolution errors are much larger than the noise, being up to 1.2% of peak brightness of the nebula in this particular case.

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Section: Introductionmentioning

confidence: 99%

The variability of the Crab nebula in radio: no radio counterpart to gamma-ray flares

Bietenholz

Yuan

Buehler

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Not really! In a recent paper, [101] has reported the detection of up to 200 GeV photons from an old, socalled millisecond pulsar (MSP; they spin rapidly, at periods of several milliseconds).…”

Section: B W49a: a Galactic Mini-starburstmentioning

confidence: 99%

Chapter 2 Galactic Gamma-ray Sources *

Chen¹,

Zhang²

2022

Chinese Phys. C

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In the gamma-ray sky, the highest fluxes come from Galactic sources: supernova remnants (SNRs), pulsars and pulsar wind nebulae, star forming regions, binaries and micro-quasars, giant molecular clouds, Galactic center, and the large extended area around the Galactic plane. The radiation mechanisms of -ray emission and the physics of the emitting particles, such as the origin, acceleration, and propagation, are of very high astrophysical significance. A variety of theoretical models have been suggested for the relevant physics and emission with energies E_1014 eV are expected to be crucial in testing them. In particular, this energy band is a direct window to test at which maximum energy a particle can be accelerated in the Galactic sources and whether the most probable source candidates such as Galactic center and SNRs are “PeVatrons”. Designed aiming at the very high energy (VHE, >100 GeV) observation, LHAASO will be a very powerful instrument in these astrophysical studies. Over the past decade, great advances have been made in the VHE -ray astronomy. More than 170 VHE -ray sources have been observed, and among them, 42 Galactic sources fall in the LHAASO field-of-view. With a sensitivity of 10 milli-Crab, LHAASO can not only provide accurate spectrum for the known -ray sources, but also search new TeV -ray sources. In the following sub-sections, the observation of all the Galactic sources with LHAASO will be discussed in details.

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“…Bednarek & Idec (2011) propose that the variable gamma-ray emission observed during the 2010 events in the Crab Nebula is caused by an emission region behind the shock in the pulsar wind, which is moving mildly relativistically to the observer. In this region, electrons can be accelerated at different maximum energies as a result of the reconnection of the magnetic field compressed by the decelerating pulsar wind (Cerutti et al 2012;Lyutikov 2014;Bühler & Blandford 2014, and references therein). These electrons produce synchrotron emission in the MeV-GeV range, and IC gamma rays above 1 TeV by scattering of the CMB photons and the low-energy synchrotron radiation.…”

Section: Pos(frapws2014)017mentioning

confidence: 99%

VHE Astrophysics: Theory vs Observations

Paredes¹,

Munar-Adrover²

2016

Proceedings of Frontier Research in Astrophysics — PoS(FRAPWS2014)

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In the last two decades we have seen the dawn of the high energy gamma-ray astrophysics era. With the advent of the new Cherenkov telescopes and the space-based telescopes a new window to the extreme universe has been opened, bringing up an unprecedented sensitivity and resolution to study all kinds of very-high energy emitters, from AGNs to gamma-ray binaries. Here we describe some of the most important highlights in the very-high energy domain of the last fifteen years. Specifically, we overview the confirmation of galactic cosmic ray acceleration inside the supernova remnants IC 433 and W44, observations of the gamma-ray binaries PSR B1259−63 and LS 5039, the detection of rapid variability in blazars, and the detection of unprecedented flaring episodes of the Crab Nebula, among others. We also describe the theoretical challenges that such observational achievements have implied and how the new models may help to explain the data.

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Inverse Compton origin of pulsar γ ‐ray emission and the reconnection model of Crab Nebula flares

Cited by 3 publications

References 34 publications

The variability of the Crab nebula in radio: no radio counterpart to gamma-ray flares

The variability of the Crab nebula in radio: no radio counterpart to gamma-ray flares

Chapter 2 Galactic Gamma-ray Sources *

VHE Astrophysics: Theory vs Observations

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