An evolutionary model for pulsar-driven supernova remnants

Swaluw, E. van der; Downes, T. P.; Keegan, Ronan

doi:10.1051/0004-6361:20035700

Cited by 95 publications

(89 citation statements)

References 22 publications

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“…The Sedov phase is expected to occur on a timescale of t Sedov ≈ 3 kyr for an explosion of 10 51 erg, an ejecta mass of 10 M , and an ambient medium density of 0.1 cm −3 (Truelove & McKee 1999). Eventually, the inward moving SNR reverse shock collides with the expanding PWN, which can happen as late as 5 times the transition to the Sedov phase (van der Swaluw et al 2004). The interaction of the PWN and the SNR reverse shock compresses the PWN, resulting in an increased magnetic field.…”

Section: Discussionmentioning

confidence: 99%

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Rousseau

Grondin

Etten

et al. 2012

A&A

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Context. Since its launch, the Fermi satellite has firmly identified 5 pulsar wind nebulae plus a large number of candidates, all powered by young and energetic pulsars. HESS J1857+026 is a spatially extended γ-ray source detected by H.E.S.S. and classified as a possible pulsar wind nebula candidate powered by PSR J1856+0245. Aims. We search for γ-ray pulsations from PSR J1856+0245 and explore the characteristics of its associated pulsar wind nebula. Methods. Using a rotational ephemeris obtained from the Lovell telescope at Jodrell Bank Observatory at 1.5 GHz, we phase-fold 36 months of γ-ray data acquired by the Large Area Telescope (LAT) aboard Fermi. We also perform a complete γ-ray spectral and morphological analysis. Results. No γ-ray pulsations were detected from PSR J1856+0245. However, significant emission is detected at a position coincident with the TeV source HESS J1857+026. The γ-ray spectrum is well described by a simple power-law with a spectral index of Γ = 1.53 ± 0.11 stat ± 0.55 syst and an energy flux of G(0.1-100 GeV) = (2.71 ± 0.52 stat ± 1.51 syst ) × 10 −11 erg cm −2 s −1 . The γ-ray luminosity is L γ PWN (0.1-100 GeV) = (2.5 ± 0.5 stat ± 1.5 syst ) × 10 35 d 9 kpc 2 erg s −1 , assuming a distance of 9 kpc. This implies a γ-ray efficiency of ∼5% forĖ = 4.6 × 10 36 erg s −1 , in the range expected for pulsar wind nebulae. Detailed multi-wavelength modeling provides new constraints on its pulsar wind nebula nature.

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Section: Discussionmentioning

confidence: 99%

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Rousseau

Grondin

Etten

et al. 2012

A&A

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“…The offset of the VHE centroid from the pulsar position is not atypical as is exemplified by Vela pulsar PSR B0833−45 associated with HESS J0835−455 (Aharonian et al 2006a) and PSR B1823−13 with HESS J1825−137 (Aharonian et al 2006b). This PWNe offset can be explained by either a high spatial velocity of the pulsar (van der Swaluw et al 2004) or the evolution of the SNR blastwave into an inhomogeneous interstellar medium (ISM). Thus, an asymmetric reverse SNR shock reaches one side of the PWN sooner than the other side, crushing the PWN (Blondin et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Unveiling the origin of HESS J1809−193

Castelletti

Giacani

Petriella

2016

A&A

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Aims. The main goal of this paper is to provide new insights on the origin of the observable flux of γ rays from HESS J1809−193 using new high-quality observations in the radio domain. Methods. We used the Expanded Very Large Array (now known as the Karl G. Jansky Very large Array, JVLA) to produce a deep full-synthesis imaging at 1.4 GHz of the vicinity of PSR J1809−1917. These data were used in conjunction with 12 CO observations from the James Clerk Maxwell Telescope in the transition line J = 3−2 and atomic hydrogen data from the Southern Galactic Plane Survey to investigate the properties of the interstellar medium in the direction of the source HESS J1809−193. Results. The new radio continuum image, obtained with a synthesized beam of 8 × 4 and a sensitivity of 0.17 mJy beam −1 , reveals with unprecedented detail all the intensity structures in the field. No radio counterpart to the observed X-ray emission supposed to be a pulsar wind nebula powered by PSR J1809−1917 is seen in the new JVLA image. We discovered a system of molecular clouds on the edge of the supernova remnant (SNR) G11.0−0.0 shock front, which is positionally coincident with the brightest part of the TeV source HESS J1809−193. We determine, on the basis of kinematic and morphological evidences, a physical link of the SNR with the clouds for which we estimated a total (molecular plus atomic) mass of ∼3 × 10 3 M and a total proton density in the range 2-3 × 10 3 cm −3 . Conclusions. We propose as the most likely origin of the very high-energy γ-ray radiation from HESS J1809−193 a hadronic mechanism through collisions of ions accelerated at the SNR G11.0−0.0 shock with the molecular matter in the vicinity of the remnant.

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“…The interactions between the SNR and the evolving pulsar wind nebula (PWN) can reveal a wealth of information about the SNR properties, the SN ejecta, the central pulsar, and the spectrum of particles injected into the PWN. At the late stages of a composite SNR's evolution, the SN reverse shock crushes the PWN, resulting in complex filamentary structures and mixing of the PWN material with ejecta gas (e.g., Blondin et al 2001;van der Swaluw et al 2004). In cases where the reverse shock interacts with the PWN asymmetrically, either due to the pulsar's motion or a density gradient in the ambient ISM, the PWN can be swept away from the pulsar, resulting in a relic PWN (e.g., van der Swaluw et al 2004).…”

Section: Introductionmentioning

confidence: 99%

“…At the late stages of a composite SNR's evolution, the SN reverse shock crushes the PWN, resulting in complex filamentary structures and mixing of the PWN material with ejecta gas (e.g., Blondin et al 2001;van der Swaluw et al 2004). In cases where the reverse shock interacts with the PWN asymmetrically, either due to the pulsar's motion or a density gradient in the ambient ISM, the PWN can be swept away from the pulsar, resulting in a relic PWN (e.g., van der Swaluw et al 2004). Due to the burn-off of highenergy particles and the fact that new particles are no longer being injected into the relic PWN, their emission is usually observed at radio wavelengths.…”

Section: Introductionmentioning

confidence: 99%

HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

Temim

Slane

Castro

et al. 2013

ApJ

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MSH 15-56 (G326.3−1.8) is a composite supernova remnant (SNR) that consists of an SNR shell and a displaced pulsar wind nebula (PWN) in the radio. We present XMM-Newton and Chandra X-ray observations of the remnant that reveal a compact source at the tip of the radio PWN and complex structures that provide evidence for mixing of the supernova (SN) ejecta with PWN material following a reverse shock interaction. The X-ray spectra are well fitted by a non-thermal power-law model whose photon index steepens with distance from the presumed pulsar, and a thermal component with an average temperature of 0.55 keV. The enhanced abundances of silicon and sulfur in some regions, and the similar temperature and ionization timescale, suggest that much of the X-ray emission can be attributed to SN ejecta that have either been heated by the reverse shock or swept up by the PWN. We find one region with a lower temperature of 0.3 keV that appears to be in ionization equilibrium. Assuming the Sedov model, we derive a number of SNR properties, including an age of 16,500 yr. Modeling of the γ -ray emission detected by Fermi shows that the emission may originate from the reverse shock-crushed PWN.

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An evolutionary model for pulsar-driven supernova remnants

Cited by 95 publications

References 22 publications

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Fermi-LAT constraints on the pulsar wind nebula nature of HESS J1857+026

Unveiling the origin of HESS J1809−193

HIGH-ENERGY EMISSION FROM THE COMPOSITE SUPERNOVA REMNANT MSH 15-56

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