X-ray morphology of the Crab nebula

Brinkmann, W.; Aschenbach, B.; Langmeier, A.

doi:10.1038/313662a0

Cited by 79 publications

(90 citation statements)

References 11 publications

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“…1). The Chandra image clearly shows the X-ray torus (Aschenbach & Brinkmann 1975) and jet and counterjet previously observed (Brinkmann et al 1985;Hester et al 1995;Greiveldinger & Aschenbach 1999), which define the southeast-to-northwest axis of the inner Crab Nebula. On somewhat larger scales, the image shows a sharply bounded notch (west-southwest of the pulsar) into the X-ray nebular emission, earlier associated with the "west bay" of the Crab Nebula (Hester et al 1995).…”

Section: Observation and Analysismentioning

confidence: 99%

“…In a remarkable synthesis from lunar-occultation, modulation-collimator, and lowresolution-imaging X-ray observations, Aschenbach & Brinkmann (1975) had interpreted the extant data in terms of an X-ray torus. Subsequent, higher resolution X-ray data-from Einstein (Brinkmann, Aschenbach, & Langmeier 1985), ROSAT (Hester et al 1995;Greiveldinger & Aschenbach 1999) and detect a jet and counterjet nearly along the axis of the torus.…”

Section: Introductionmentioning

confidence: 99%

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Discovery of Spatial and Spectral Structure in the X-Ray Emission from the Crab Nebula

Weisskopf

Hester

Tennant

et al. 2000

The Astrophysical Journal

400

419

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The Chandra X-Ray Observatory observed the Crab Nebula and pulsar during orbital calibration. Zeroth-order images with the High-Energy Transmission Grating (HETG) readout by the Advanced CCD Imaging Spectrometer spectroscopy array (ACIS-S) show a striking richness of X-ray structure at a resolution comparable to that of the best ground-based visible-light observations. The HETG-ACIS-S images reveal, for the first time, an X-ray inner ring within the X-ray torus, the suggestion of a hollow-tube structure for the torus, and X-ray knots along the inner ring and (perhaps) along the inward extension of the X-ray jet. Although complicated by instrumental effects and the brightness of the Crab Nebula, the spectrometric analysis shows systematic variations of the Xray spectrum throughout the nebula.

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Section: Observation and Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Discovery of Spatial and Spectral Structure in the X-Ray Emission from the Crab Nebula

Weisskopf

Hester

Tennant

et al. 2000

The Astrophysical Journal

400

419

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“…The spectacular X-ray binary system SS 433 is located at the center of the SNR (e.g. Brinkmann et al 1996). Two relativistic jets from SS 433 are precessing around the major axis of W50.…”

Section: G397−20 (W50)mentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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Context.Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. Aims. The total intensity and polarization properties of 16 large SNRs in the Galactic plane are investigated based on observations of the Urumqi λ6 cm polarization survey of the Galactic plane with an angular resolution of 9. 5. Methods. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi λ6 cm survey, obtained their integrated flux densities, and derived the radio spectra by using these flux densities together with previously published flux densities at various frequencies. In particular, Effelsberg λ11 cm and λ21 cm survey data were used to calculate integrated flux densities. The λ6 cm polarization data also delineate the magnetic field structures of the SNRs. Results. We present the first total intensity maps at λ6 cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at λ6 cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi λ6 cm, Effelsberg λ11 cm and λ21 cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7−0.2, and G114.3+0.3. We find that G192.8−1.1 (PKS 0607+17) consists of background sources, H ii regions, and extended diffuse emission of thermal nature, and conclude that G192.8−1.1 is not a SNR.

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“…In the last decade, thanks to the unprecedented imaging power of Chandra, high resolution observations of the inner region of the CN have become available also in the X-ray band, revealing a striking jet-torus structure, knots and rings (Weisskopf et al 2000), previously just barely inferred (Brinkmann et al 1985;Hester 1995). These observations prompted a theoretical effort at modelling PWNe, and the CN in particular, within the framework of time-dependent multi-D MHD.…”

Section: Introductionmentioning

confidence: 99%

Constraints on particle acceleration sites in the Crab nebula from relativistic magnetohydrodynamic simulations

Olmi

Zanna

Amato

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The Crab Nebula is one of the most efficient accelerators in the Galaxy and the only galactic source showing direct evidence of PeV particles. In spite of this, the physical process behind such effective acceleration is still a deep mystery. While particle acceleration, at least at the highest energies, is commonly thought to occur at the pulsar wind termination shock, the properties of the upstream flow are thought to be non-uniform along the shock surface, and important constraints on the mechanism at work come from exact knowledge of where along this surface particles are being accelerated. Here we use axisymmetric relativistic MHD simulations to obtain constraints on the acceleration site(s) of particles of different energies in the Crab Nebula. Various scenarios are considered for the injection of particles responsible for synchrotron radiation in the different frequency bands, radio, optical and X-rays. The resulting emission properties are compared with available data on the multi wavelength time variability of the inner nebula. Our main result is that the X-ray emitting particles are accelerated in the equatorial region of the pulsar wind. Possible implications on the nature of the acceleration mechanism are discussed.

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X-ray morphology of the Crab nebula

Cited by 79 publications

References 11 publications

Discovery of Spatial and Spectral Structure in the X-Ray Emission from the Crab Nebula

Discovery of Spatial and Spectral Structure in the X-Ray Emission from the Crab Nebula

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Constraints on particle acceleration sites in the Crab nebula from relativistic magnetohydrodynamic simulations

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