X-rays from supernova remnants

Aschenbach, B.

doi:10.1016/s0920-5632(98)00188-1

Cited by 42 publications

(60 citation statements)

References 41 publications

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“…13a). In our picture, the south blowout region of the remnant is the low-density wake behind the progenitor in which the gas is the hottest (> 10 6 K), as noted in Aschenbach & Leahy (1999). Nevertheless, our models predict that the soft and hard X-rays emission should be limb-brightened, whereas the observations have a filled morphology.…”

Section: An Alternative Explanation For the Cygnus Loop Nebula ?mentioning

confidence: 55%

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Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Section: An Alternative Explanation For the Cygnus Loop Nebula ?mentioning

confidence: 55%

“…with ROSAT (Aschenbach & Leahy 1999) reveal a characteristic overall drop-like morphology. An early interpretation of this shape is a champagne blowout from the edge of a molecular cloud (Tenorio-Tagle et al 1985).…”

Section: An Alternative Explanation For the Cygnus Loop Nebula ?mentioning

confidence: 97%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Meanwhile, there is an apparent break of the cavity wall that is seen as the south blowout region (see, e.g., figures in Aschenbach & Leahy 1999). The wall of the cavity there is considered to be so thin (or negligible) that the blast wave already overran the wall, although Uyaniker et al (2002) proposed another possibility, i.e., a different SNR interacting with the Cygnus Loop, for the south blowout region.…”

Section: Speculation On the Origin Of The Abundance Inhomogeneity In mentioning

confidence: 99%

ChandraObservations of the Northeastern Rim of the Cygnus Loop

Katsuda

Tsunemi

Kimura

et al. 2008

ApJ

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We present results from spatially resolved spectral analyses of the northeastern (NE) rim of the Cygnus Loop supernova remnant (SNR) based on two Chandra observations. One pointing includes northern outermost abundance-enhanced regions discovered by recent Suzaku observations, while the other pointing is located on regions with ''normal'' abundances in the NE rim of the Cygnus Loop. The superior spatial resolving power of Chandra allows us to reveal that the abundance-enhanced region is concentrated in a $200 00 thickness region behind the shock front. We confirm absolute metal abundances (i.e., relative to H ), as well as abundance ratios between metals, are consistent with those of the solar values within a factor of $2. Also, we find that the emission measure in the region gradually decreases toward the shock front. These features are in contrast with those of the ejecta fragments around the Vela SNR, which leads us to believe that the abundance enhancements are not likely due to metal-rich ejecta. We suggest that the origin of the plasma in this region is the interstellar medium (ISM ). In the ''normal'' abundance regions, we confirm that abundances are depleted to the solar values by a factor of $5 that is not expected in the ISM around the Cygnus Loop. Introduction of nonthermal emission in our model fitting cannot naturally resolve the abundance-depletion problem. The origin of the depletion still remains as an open question.

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“…Aschenbach & Leahy (1999) have interpreted the southern part of the remnant as a breakout into a lower density medium. Their main reason was the smooth change of the X-ray emission from the northern to the southern area.…”

Section: Optical X-ray and Infrared Datamentioning

confidence: 99%

Is the Cygnus Loop two supernova remnants?

Uyanıker

Reich

Yar

et al. 2002

A&A

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Abstract. The Cygnus Loop is classified as a middle-aged supernova remnant (SNR) located below the Galactic equator ( = 74• , b = −8.• 6) and 770 pc away from us. Its large size and little confusion with Galactic emission makes it an ideal test ground for evolutionary and structural theories of SNRs. New radio continuum mapping of the Cygnus Loop at 2695 MHz with the Effelsberg 100-m telescope provides indications that the Cygnus Loop consists of two separate SNRs. Combining this result with data from the literature we argue that a secondary SNR exists in the south with a recently detected neutron star close to its center. Two interacting SNRs seem to be the best explanation to account for the Cygnus Loop observations at all wavelengths.

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X-rays from supernova remnants

Cited by 42 publications

References 41 publications

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Asymmetric supernova remnants generated by Galactic, massive runaway stars

ChandraObservations of the Northeastern Rim of the Cygnus Loop

Is the Cygnus Loop two supernova remnants?

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