High-Resolution X-Ray Spectroscopy of SNR 1987a: Chandra Letg and Hetg Observations in 2007

Zhekov, Svetozar A.; McCray, Richard; Dewey, Daniel; Canizares, C. R.; Borkowski, Kazimierz J.; Burrows, D. N.; Park, Sangwook

doi:10.1088/0004-637x/692/2/1190

Cited by 54 publications

(129 citation statements)

References 28 publications

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“…both plasmas with a μ∼ 1.0, could be accommodated with some adjustments to the density profile. (2) Our values for the relative abundances of the heavier elements in the CSM are consistent with those for the CSM around SN 1987A derived from fitting the LETG and HETG spectra (Zhekov et al 2009). Those abundances were found to be consistent with those of the Large Magellanic Cloud (LMC), and with supernova remnants in the LMC.…”

Section: Discussionsupporting

confidence: 85%

“…The H, He, N and O values are shown with very small error bars to indicate that they are fixed (H, He) or undetermined (N, O). In the figure we also compare the abundances to those derived from low‐energy transmission grating (LETG) and HETG observations of SN 1987A (Zhekov et al 2009), as well as those given for WCE stars by Mellema & Lundqvist (2002). These comparisons lead to the following observations.…”

Section: Discussionmentioning

confidence: 95%

“…Therefore one possibility is that the winds are enhanced in Si and S. An alternate possibility is that the shocked CSM could actually be a mixture of CSM and ejecta material, due to mixing at the interface between the shocked CSM and shocked ejecta, which can lead to Rayleigh–Taylor ‘fingers’ of ejecta propagating into the CSM. In order to test this possibility, we have assumed a modified CSM composition, which is made up of equal parts (by number) of the SN 1987A CSM (Zhekov et al 2009) and SN 1996cr ejecta. Such a 50–50 mixture has a resulting abundance similar to that of our ‘CSM’, and, if used in place of our CSM abundance values, gives a similar light curve and spectra.…”

Section: Discussionmentioning

confidence: 99%

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Bursting SN 1996cr's bubble: hydrodynamic and X-ray modelling of its circumstellar medium

Dwarkadas

Dewey

Bauer

2010

Monthly Notices of the Royal Astronomical Society

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SN1996cr is one of the five closest supernovae (SNe) to explode in the past 30 yr. Due to its fortuitous location in the Circinus galaxy at ∼3.7 Mpc, there is a wealth of recently acquired and serendipitous archival data available to piece together its evolution over the past decade, including a recent 485‐ks Chandra high‐energy transmission grating spectrum. In order to interpret these data, we have explored hydrodynamic simulations, followed by computations of simulated spectra and light curves under non‐equilibrium ionization conditions, and directly compared them to the observations. Our simulated spectra manage to fit both the X‐ray continuum and lines at four epochs satisfactorily, while our computed light curves are in good agreement with additional flux‐monitoring data sets. These calculations allow us to infer the nature and structure of the circumstellar medium (CSM), the evolution of the SN shock wave, and the abundances of the ejecta and surrounding medium. The data imply that SN 1996cr exploded in a low‐density medium before interacting with a dense shell of material about 0.03 pc away from the progenitor star. We speculate that the shell could be due to the interaction of a blue supergiant or Wolf–Rayet wind with a previously existing red supergiant (RSG) wind. The shock wave has now exited the shell and is expanding in the medium exterior to it, possibly the undisturbed continuation of the dense RSG wind. The narrow lines that earned SN 1996cr its IIn designation possibly arise from dense, shocked clumps in the CSM. Although the possibility for a luminous blue variable progenitor for this Type IIn SN cannot be completely excluded, it is inconsistent with much of the data. These calculations allow us to probe the stellar mass‐loss in the very last phases (<104 yr) of a massive star's life (>106 yr), and provide another means to deducing the progenitor of the SN.

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Section: Discussionsupporting

confidence: 85%

Section: Discussionmentioning

confidence: 95%

Section: Discussionmentioning

confidence: 99%

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Bursting SN 1996cr's bubble: hydrodynamic and X-ray modelling of its circumstellar medium

Dwarkadas

Dewey

Bauer

2010

Monthly Notices of the Royal Astronomical Society

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“…This is evident in the brightening in X-rays , infrared (Bouchet et al 2006), andoptical (McCray 2005), the continuous softening of the X-ray spectrum (Park et al 2006b;Zhekov et al 2005), deceleration of the radial expansion of the SNR (Park et al 2004;Zhekov et al 2005), and slower shock velocities from line broadening Dewey et al 2008;Zhekov et al 2009). (Zhekov et al , 2006(Zhekov et al , 2009). In the standard LETG configuration, the long-wavelength oxygen lines are positioned on the sensitive ACIS-S3 chip, which consequently places the zeroth-order image 1.…”

Section: Predictionsmentioning

confidence: 99%

X-Ray Evolution of SNR 1987a: The Radial Expansion

Racusin¹,

Park²,

Zhekov³

et al. 2009

ApJ

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We present the evolution of the radial expansion of SNR 1987A as measured using Chandra X-ray observations taken over the last 10 years. To characterize the complex structure of the remnant and isolate the expansion measurement, we fit the images to several empirical models including: a simple circular torus, a torus with bilateral lobes, and a torus with four tangentially extended lobes. We discuss the results of this measure in the context of the overall evolution of the supernova remnant, for which we believe we have measured the end of the free expansion phase and its transition to the adiabatic phase (at least along the equatorial ring). The timing of this event is in agreement with early predictions of the remnant evolution.

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“…5). Zhekov et al (2009Zhekov et al ( , 2010 fit the in-plane components of this model 74 D. N. Burrows et al to ACIS light curves and spectra up to 2007. D12 fit this model, including the outof-plane Hii regions, to the measured X-ray fluxes and line profiles to determine the parameters of a set of hydro models that reproduce both the spectra and light curves.…”

Section: Physical Model Figure 5 Cross-section (±15mentioning

confidence: 96%

SN1987A: the X-ray remnant at age 25 years

et al. 2011

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Abstract. SN1987A is the best-studied core-collapse supernova in the sky. We know what the progenitor was, what the circumstellar environment was, and what the explosion looked like over a broad electromagnetic bandpass and in neutrinos. For over a decade, the Chandra X-ray Observatory has been monitoring SN1987A on a regular basis, obtaining resolved images of the developing interaction with the circumstellar material, as well as high resolution grating spectroscopy of the X-ray emission. We highlight the latest results from this campaign and discuss the overall picture of the remnant's structure that emerges from these observations.

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High-Resolution X-Ray Spectroscopy of SNR 1987a: Chandra Letg and Hetg Observations in 2007

Cited by 54 publications

References 28 publications

Bursting SN 1996cr's bubble: hydrodynamic and X-ray modelling of its circumstellar medium

Bursting SN 1996cr's bubble: hydrodynamic and X-ray modelling of its circumstellar medium

X-Ray Evolution of SNR 1987a: The Radial Expansion

SN1987A: the X-ray remnant at age 25 years

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