The Crab Nebula: An Astrophysical Chimera

By J. Hester. 2008

335 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c8d54d8f624fe2d347bfa9cf6b8dab143a3919ce

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In Astronomy and Astrophysics

1. N. Langer
2. T. Tauris
3. Bernhard Müller
4. Stan Woosley
5. J. Vink
6. Alexander Heger
7. J. Arons
8. Hans-Thomas Janka

In Nuclear and High Energy Physics

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2. E. Orlando
3. Anna Franckowiak
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8. T. Tauris

Citations in the corpus

• Pulsar Wind Nebulae as Cosmic Pevatrons: A Current Sheet’s Tale (2012, background): “…identified with the prominent ring of emission seen in the Chandra image of the inner nebula modeled as a MHD shock wave, located at about the same location as the other signs of activity seen as indicating the termination of the free wind from the pulsar (“wisps”, etc., reviewed by Hester 2008).”
• GAMMA-RAY ACTIVITY IN THE CRAB NEBULA: THE EXCEPTIONAL FLARE OF 2011 APRIL (2011, background): “The spectral energy distribution (SED) of the nebula is, accordingly, dominated by a synchrotron component extending from radio wavelengths into the gammaray band (Hester 2008).”
• The Crab Nebula as a standard candle in very high-energy astrophysics (2010, background): “The Crab Nebula has been and remains an intensely studied object in astrophysics (for a recent review see e.g. Hester 2008).”
• Three-dimensional magnetohydrodynamic simulations of the Crab nebula (2013, background): “Extrapolating from the simulations, we expect todays Crab Nebula to contain a total energy of ' 1049erg in good agreement with the previous estimates (e.g. Hester 2008a).”
• Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae (2011, methodology): “Recently published optical polarimetry of the Crab Nebula using the Hubble Space Telescope has revealed spectacular details of this PWN’s large-scale magnetic field (Hester 2008).”
• Teraelectronvolt Astronomy (2010, background): “Ground-based γ-ray astronomy effectively began in 1989, with the first robust detection of a TeV γ-ray source, the Crab Nebula, using the 10m diameter airCherenkov telescope of the Whipple Observatory (Weekes et al. 1989).”
• The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “1050 erg (Fesen et al. 1997; Hester 2008) as expected for an ECSN-like event.”
• Supernova remnants: the X-ray perspective (2011, background): “In fact, it is still puzzling why a young object like the Crab Nebula does not show a SNR shell (see Hester, 2008, for a discussion).”
• The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000 (2014, neutral): “The Crab Nebula, or Tau A, is an extended polarized supernova remnant whose emission below ≈ 1 THz is dominated by synchrotron radiation (see, e.g., Hester 2008).”
• A COOL DUST FACTORY IN THE CRAB NEBULA: A HERSCHEL STUDY OF THE FILAMENTS (2012, background): “Grains will be destroyed via thermal sputtering in the reverse shock due to collisions with electrons and/or ions, yet unlike the Cas A and SN1987A remnants, the Crab does not have a visible reverse shock today (Hester 2008).”
• Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “Observationally, there are examples of short spin periods of young neutron stars with low kicks; the Crab pulsar is the most prominent example with a kick of ∼160 km s−1 (Kaplan et al. 2008; Hester 2008) and a birth spin period of .20 ms (Lyne et al. 2015).”
• The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope (2018, background): “The Crab Nebula is a PWN associated with the young pulsar PSRJ0534+2200, which is the compact remnant of a supernova explosion that occurred in the year 1054 AD, at a distance of ∼2 kpc(see, e.g., Hester 2008, for a review).”
• A comment on the emission from the Galactic Center as seen by the Fermi telescope (2010, background): “The pulsar wind nebula, associated with the Crab has an angular size∼ 0.05◦ (Hester 2008).”