An X-ray map of SN 1006 from the Einstein Observatory

Pye, J. P.; Pounds, K. A.; Rolf, Daniel; Seward, F. D.; Smith, A.; Willingale, R.

doi:10.1093/mnras/194.3.569

Cited by 50 publications

(15 citation statements)

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“…SN 1006 has been observed at radio (Pye et al 1981), optical (Ghavamian et al 2002, hereafter GWRL02;Kirshner et al 1987;Smith et al 1991), ultraviolet (Raymond et al 1995), and X-ray (Winkler et al 2003;Long et al 2003;Bamba et al 2003) wavelengths. Gamma-ray observations (Tanimori 1998) were reported but not confirmed.…”

Section: Introductionmentioning

confidence: 99%

Far Ultraviolet Spectroscopic ExplorerObservation of the Nonradiative Collisionless Shock in the Remnant of SN 1006

Korreck

Raymond

Zurbuchen

et al. 2004

ApJ

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The appearance of the young supernova remnant SN 1006 is dominated by emission from nonradiative shocks in the northeast and northwest regions. At X-ray energies the northeast shock exhibits predominantly nonthermal synchrotron emission, while the northwest shock exhibits a thermal spectrum. We present far-ultraviolet spectra of the northeast (NE) and northwest (NW) portions of SN 1006 acquired with the Far Ultraviolet Spectroscopic Explorer (FUSE ). We have detected emission lines of O vi kk1032, 1038 and broad Ly k1025 in the NW filament but detect no emission lines in the NE region down to a level of 4:7 ; 10 À17 ergs cm À2 s À1 arcsec À2 . We observed in the NW an O vi intensity of 2:0 AE 0:2 ; 10 À16 ergs cm À2 s À1 arcsec À2 and measured an O vi line width of 2100 AE 200 km s À1 at a position where the H width was measured to be 2290 AE 80 km s À1 . This implies less than mass-proportional heating of the ions. Using the ratio of intensities I(NW)=I(NE) $ n(NW)=n(NE), the density ratio of the two regions is found to be !4, a value that is consistent with the uncertainties of the ratio of 2.5 measured in 2003 by Long and coworkers. The derived O vi kinetic temperature is compared to previous estimates of electron, proton, and ion temperatures in the remnant to study the relative heating efficiency of various species at the shock front. The degree of postshock temperature equilibration may be crucial to particle acceleration, since the temperature of each species determines the number of high-speed particles available for injection into an acceleration process that could produce Galactic cosmic rays. Subject headingg s: ISM: individual (SN 1006) -shock waves -supernova remnants -ultraviolet: ISM

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Section: Introductionmentioning

confidence: 99%

Far Ultraviolet Spectroscopic ExplorerObservation of the Nonradiative Collisionless Shock in the Remnant of SN 1006

Korreck

Raymond

Zurbuchen

et al. 2004

ApJ

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“…The crosses indicate the observed upper limits to the surface temperatures of various young supernova remnants assuming the presence of neutron stars in these objects (Pye et al 1981;Murray 1981;Fabbiano 1981;Helfand 1981). …”

Section: Comparison With Observation and Discussionmentioning

confidence: 99%

Cooling of neutron stars and X-ray observations

Nomoto

Tsuruta

1981

Space Sci Rev

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Cooling of neutron stars is calculated using an exact stellar evolution code.The full general relativistic version of the stellar structure equations are solved, with the best physical input currently available.For neutron stars with a stiff equation of state, we find that the deviation from the isothermality in the interior is significant and that it takes at least a few thousand years to reach the isothermal state.By comparing the most recent theoretical and observational results, we conclude that for Cas A, SNI006, and probably Tycho, "standard" cooling is inconsistent with the results from the Einstein Observatory, if neutron stars are assumed to be present in these objects. On the other hand, the "detection" points for RCWI03 and the Crab are consistent with these theoretical results.1.

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“…All of these super novae created remnants which are fairly strong X-ray emitters (Pye et al 1981;Reid, Becker, and Long 1982;White and Long 1982), which implies that they are interacting with moderately dense gas. Although there are uncertainties due to non-equilibrium ionization and heavy element over abundances.…”

Section: Type I Supernovaementioning

confidence: 99%

The Interaction of Supernova Ejecta with an Ambient Medium

Chevalier¹

1983

Symp. - Int. Astron. Union

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Plausible environments for supernovae are the interstellar medium with constant density or a circumstellar medium built up by mass loss with ρ ∝ r−n Self-similar solutions for the interaction region between the expanding supernova gas and the ambient gas exist provided that the expanding gas has ρ ∝ r−n with n > 5. The circumstellar medium case is likely to be important for the early evolution of Type II supernovae because their progenitor stars are probably red supergiants. The radio and X-ray emission observed from extragalactic supernovae may be from this interaction region. The early self-similar solutions can also be applied to the young galactic remnants.

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An X-ray map of SN 1006 from the Einstein Observatory

Cited by 50 publications

References 0 publications

Far Ultraviolet Spectroscopic ExplorerObservation of the Nonradiative Collisionless Shock in the Remnant of SN 1006

Far Ultraviolet Spectroscopic ExplorerObservation of the Nonradiative Collisionless Shock in the Remnant of SN 1006

Cooling of neutron stars and X-ray observations

The Interaction of Supernova Ejecta with an Ambient Medium

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