Dust in the Tycho, Kepler and Crab supernova remnants

Douvion, T.; Lagage, Pierre-Olivier; Césarsky, C. J.; Dwek, Eli

doi:10.1051/0004-6361:20010447

Cited by 92 publications

(122 citation statements)

References 59 publications

(65 reference statements)

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“…There is only little observational evidence that SNe can be very efficient (e.g., Wilson & Batrla 2005;Douvion et al 2001;Dunne et al 2009), and theoretical models predict significant dust destruction in reverse shocks of SNe (e.g., Bianchi & Schneider 2007;Nozawa et al 2007Nozawa et al , 2010. On the other hand, these models also show that the effectiveness of dust destruction depends on various properties such as the geometry of the shocks, the density of the ejecta and the ISM, the size and shape of the grains, clumping in the SNe ejecta, and different SN types.…”

Section: Sn Efficiency and Mass Of The Galaxymentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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Aims. We intend to assess the most plausible scenarios for generating large amounts of dust in high-z quasars (QSOs) on the basis of observationally derived physical properties of QSOs at z 6. Methods. We use a chemical evolution model to compute the temporal progression of quantities such as the amount of dust and gas, stellar masses, star formation rates (SFRs) and the metallicity for various combinations of the initial mass function (IMF), the mass of the galaxy, dust production efficiencies, and the degree of dust destruction in the ISM. We investigate the influence of the SFR on the evolution of these quantities, and determine the earliest epochs at which agreement with observations can be achieved. We apply the obtained results to individual QSOs at z 6. Results. We find that large quantities of dust can be generated rapidly as early as 30 Myr after the onset of the starburst when the SFR of the starburst is 10 3 M yr −1 . The amount of dust and several other physical quantities of individual QSOs at z 6 are satisfactorily reproduced by models at epochs 30, 70, 100, and 170 Myr for galaxies with initial gas masses of 1-3 × 10 11 M . The best agreement with observations is obtained with top-heavy IMFs. A sizable dust contribution from supernovae (SNe) is however required, while at these epochs dust production by asymptotic giant branch (AGB) stars is negligible. Moderate dust destruction in the ISM can be accommodated.

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Section: Sn Efficiency and Mass Of The Galaxymentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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“…Using optical spectroscopy, Chevalier & Kirshner (1979) demonstrated abundance inhomogeneities in the oxygen burning products S, Ar, and Ca among the outlying fast moving knots, and suggested differing completeness levels of oxygen burning could explain these variations. Macroscopic mixing of similar nucleosynthetic products was suggested by Douvion et al (1999) using ISO MIR line maps of Ar, Ne, and S covering a portion of the bright rim. Hughes et al (2000) used Chandra X-ray spectroscopy to identify spatial inversion of iron and oxygen burning products.…”

Section: Apparent Inhomogenous Mixing and The Neon Crescentsmentioning

confidence: 99%

SPITZERSPECTRAL MAPPING OF SUPERNOVA REMNANT CASSIOPEIA A

Smith¹,

Rudnick²,

DeLaney³

et al. 2009

ApJ

114

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We present the global distribution of fine-structure infrared line emission in the Cassiopeia A supernova remnant using data from the Spitzer Space Telescope's infrared spectrograph. We identify emission from ejecta materials in the interior, prior to their encounter with the reverse shock, as well as from the postshock bright ring. The global electron density increases by 100 at the shock to ∼ 10 4 cm −3 , providing evidence for strong radiative cooling. There is also a dramatic change in ionization state at the shock, with the fading of emission from low-ionization interior species like [Si ii] giving way to [S iv] and, at even further distances, highenergy X-rays from hydrogenic silicon. Two compact, crescent-shaped clumps with highly enhanced neon abundance are arranged symmetrically around the central neutron star. These neon crescents are very closely aligned with the "kick" direction of the compact object from the remnant's expansion center, tracing a new axis of explosion asymmetry. They indicate that much of the apparent macroscopic elemental mixing may arise from different compositional layers of ejecta now passing through the reverse shock along different directions.

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“…The optical emission comes entirely from the forward shock, and the infrared emission is also associated with the forward shock (Douvion et al 2001), while the radio emission is due to electrons accelerated at the shock rather than to ions. The general distribution of the ejecta is evident in the broadband X-ray image (Fig.…”

Section: Ejecta Distributionmentioning

confidence: 99%

Thermal and Nonthermal X‐Ray Emission from the Forward Shock in Tycho’s Supernova Remnant

Hwang

Decourchelle

Holt

et al. 2002

ApJ

158

172

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We present Chandra X-ray images of Tycho's supernova remnant that delineate its outer shock as a thin, smooth rim along the straight northeastern edge and most of the circular western half. The images also show that the Si and S ejecta are highly clumpy and have reached near the forward shock at numerous locations. Most of the X-ray spectra that we examine along the rim show evidence of line emission from Si and S ejecta, while the continuum is well represented by either a thermal or a nonthermal model. If the continuum is assumed to be thermal, the electron temperatures at the rim are all similar at about 2 keV, while the ionization ages are very low because of the overall weakness of the line emission. These electron temperatures are substantially below those expected for equilibration of the electron and ion temperatures, assuming shock velocities inferred from radio and X-ray expansion measurements; the electron-to-mean temperature ratios are d0.1-0.2, indicating that collisionless heating of the electrons at the shock is modest. The nonthermal contribution to these spectra might be important, but cannot be strongly constrained by these data. It could account for as much as half of the flux in the 4-6 keV energy range, based on an extrapolation of the hard X-ray spectrum above 10 keV.

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Dust in the Tycho, Kepler and Crab supernova remnants

Cited by 92 publications

References 59 publications

Genesis and evolution of dust in galaxies in the early Universe

Genesis and evolution of dust in galaxies in the early Universe

SPITZERSPECTRAL MAPPING OF SUPERNOVA REMNANT CASSIOPEIA A

Thermal and Nonthermal X‐Ray Emission from the Forward Shock in Tycho’s Supernova Remnant

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