The Evolution of Supernovae in Circumstellar Wind‐Blown Bubbles. I. Introduction and One‐Dimensional Calculations

Dwarkadas, Vikram V.

doi:10.1086/432109

Cited by 159 publications

(191 citation statements)

References 58 publications

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“…The interaction of the SN shocks with the modified CSM results in a different evolution compared to that in a constant-density ISM. Dwarkadas (2005Dwarkadas ( , 2007, and references therein) explored the evolution of remnants in wind-blown cavities. It was shown that it critically depends on one parameter (coined Λ), the ratio of the mass of the dense shell to that of the ejected material.…”

Section: X-ray Luminosity Function Of Snrs In the Local Groupmentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

146

205

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Aims. We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily XMM-Newton observations, we conduct a systematic spectral analysis of LMC SNRs to gain new insight into their evolution and the interplay with their host galaxy. Methods. We combined all the archival XMM-Newton observations of the LMC with those of our Very Large Programme LMC survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59 objects compiled from the literature and augmented with newly found objects. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. The locations of SNRs are compared to the distributions of stars, cold gas, and warm gas in the LMC, and we investigated the connection between the SNRs and their local environment, characterised by various star formation histories. We tentatively typed all LMC SNRs, in order to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We also compared the column densities derived from X-ray spectra to H i maps, thus probing the three-dimensional structure of the LMC. Results. This work provides the first homogeneous catalogue of the X-ray spectral properties of SNRs in the LMC. It offers a complete census of LMC remnants whose X-ray emission exhibits Fe K lines (13% of the sample), or reveals the contribution from hot supernova ejecta (39%), which both give clues to the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the hot phase of the LMC interstellar medium are found to be between 0.2 and 0.5 times the solar values with a lower abundance ratio [α/Fe] than in the Milky Way. The current ratio of core-collapse to type Ia SN rates in the LMC is constrained to N CC /N Ia = 1.35( +0.11 −0.24 ), which is lower than in local SN surveys and galaxy clusters. Our comparison of the X-ray luminosity functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33) reveals an intriguing excess of bright objects in the LMC. Finally, we confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC to the far and near sides, respectively.

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Section: X-ray Luminosity Function Of Snrs In the Local Groupmentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

146

205

View full text Add to dashboard Cite

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“…They therefore exc 0000 RAS hibit a wide range of morphologies that can be used to constrain their progenitors and/or ambient medium properties. The distribution of circumstellar matter depends on the progenitor properties (Bedogni & D'Ercole 1988;Ciotti & D'Ercole 1989;Dwarkadas 2005Dwarkadas , 2007 and the presence of ISM structures, e.g. borders of neighbouring diffuse nebulae or filaments that affect the propagation of the supernova ejecta.…”

Section: Introductionmentioning

confidence: 99%

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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“…Several analytical and numerical studies have been devoted to the exploration of the interaction between supernova (SN) ejecta and wind-driven shells (e.g., Franco et al 1991, and references therein;Dwarkadas 2005). SN 1987A is probably the clearest observational example of the influence of the past history of the exploding star in shaping the observed remnant.…”

Section: Introductionmentioning

confidence: 99%

Radio and X-ray study of two multi-shell supernova remnants: Kes 79 and G352.7-0.1

Giacani¹,

Smith

Dubner³

et al. 2009

A&A

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Aims. We investigate two multi-shell galactic supernova remnants (SNRs), Kes 79, and G352.7−0.1, to understand the causes of this morphology. Methods. The research was carried out based on new and reprocessed archival VLA observations and XMM-Newton archival data. The surrounding gas was investigated based on data extracted from the HI Canadian Galactic Plane Survey, the 13 CO Galactic Ring Survey, and the HI Southern Galactic Plane Survey.Results. The present study infers that the overall morphology of both SNRs is the result of the mass-loss history of their respective progenitor stars. Kes 79 is likely to be the product of the gravitational collapse of a massive O9 star evolving near a molecular cloud and within the precursor's wind-driven bubble, while G352.7−0.1 should be the result of interactions of the SNR with an asymmetric wind from the progenitor together with projection effects. No radio point source or pulsar wind nebula was found to be associated with the X-ray pulsar CXOU J185238.6+004020 in Kes 79. The X-ray study of G352.7−0.1 found that most of the thermal X-ray radiation completely fills the interior of the remnant and originates in heated ejecta. Characteristic parameters, such as radio flux, radio spectral index, age, distance, shock velocity, initial energy, and luminosity, were estimated for both SNRs.

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The Evolution of Supernovae in Circumstellar Wind‐Blown Bubbles. I. Introduction and One‐Dimensional Calculations

Cited by 159 publications

References 58 publications

The population of X-ray supernova remnants in the Large Magellanic Cloud

The population of X-ray supernova remnants in the Large Magellanic Cloud

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Radio and X-ray study of two multi-shell supernova remnants: Kes 79 and G352.7-0.1

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