Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-collapse Supernova Remnant G292.0+1.8

Bhalerao, Jayant; Park, Sangwook; Schenck, Andrew; Post, Seth; Hughes, John P.

doi:10.3847/1538-4357/aafafd

Cited by 21 publications

(62 citation statements)

References 95 publications

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“…Observations of 44 Ti ejection velocities in SN 1987A (Boggs et al 2015) suggest an even higher level of asymmetry in that supernova. X-ray observations of G292.0+1.8 (Bhalerao et al 2019) reveal gross elemental asymmetries in the ejecta of this young, oxygenrich, Galactic supernova remnant, echoing earlier work on Cassiopeia A (Hughes et al 2000). In this work, we present state-of-the-art core-collapse supernova (CCSN) simulations that explore the development and evolution of these asymmetries as the supernova shock progresses through the entire star.…”

Section: Introductionmentioning

confidence: 57%

Three Dimensional Core-Collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

Sandoval,

Hix,

Messer

et al. 2021

Preprint

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We present three-dimensional simulations of core-collapse supernovae using the FLASH code that follow the progression of the explosion to the stellar surface, starting from neutrino-radiation hydrodynamic simulations of the first seconds performed with the CHIMERA code. We consider a 9.6-M zero-metallicity progenitor starting from both 2D and 3D CHIMERA models, and a 10-M solar-metallicity progenitor starting from a 2D CHIMERA model, all simulated until shock breakout in 3D while tracking 160 nuclear species. The relative velocity difference between the supernova shock and the metal-rich Rayleigh-Taylor (R-T) "bullets" determines how the ejecta evolves as it propagates through the density profile of the progenitor and dictates the final morphology of the explosion. We find maximum 56 Ni velocities of ∼1950 km s −1 and ∼1750 km s −1 at shock breakout from 2D and 3D 9.6-M CHIMERA models, respectively, due to the bullets' ability to penetrate the He/H shell. When mapping from 2D, we find that the development of higher velocity structures is suppressed when the 2D CHIMERA model and 3D FLASH model meshes are aligned. The development of faster growing sphericalbubble structures, as opposed to the slower growing toroidal structure imposed by axisymmetry, allows for interaction of the bullets with the shock and seeds further R-T instabilities at the He/H interface. We see similar effects in the 10-M model, which achieves maximum 56 Ni velocities of ∼2500 km s −1 at shock breakout.

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Section: Introductionmentioning

confidence: 57%

Three Dimensional Core-Collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

Sandoval,

Hix,

Messer

et al. 2021

Preprint

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“…In particular, O, Ne, and Mg are observed to be distributed within the whole remnant, whereas Si-rich ejecta are concentrated mainly in the north-west area (e.g. Park et al 2002;Yang et al 2014;Bhalerao et al 2019). Recently, Fe-rich ejecta have been found concentrated in Si-rich regions to the north-west (Bhalerao et al 2019).…”

Section: Distribution Of Ejecta At Later Timesmentioning

confidence: 99%

“…Ghavamian et al 2005;Winkler et al 2009;Gonzalez & Safi-Harb 2003) and average forward and reverse shock radii of ≈ 7.7 pc and ≈ 3.8 pc, respectively (at a distance of ≈ 6 kpc; Park et al 2007;Gaensler & Wallace 2003;Bhalerao et al 2015), similar to those derived at the end of our simulations (≈ 8.2 pc and ≈ 4.2 pc, respectively, at the age of ≈ 2000 years). The progenitor was most likely a star with a zero-age-main-sequence mass in the range between 13 and 30 M ⊙ (Bhalerao et al 2019). The total ejecta mass inferred from radio and X-ray observations is in the range of 6 − 8 M ⊙ (Gaensler & Wallace 2003;Bhalerao et al 2015), whereas the estimated explosion energy is E exp ≤ 1 B (Gonzalez & Safi-Harb 2003), although the latter value has large uncertainties.…”

Section: Distribution Of Ejecta At Later Timesmentioning

confidence: 99%

“…21). The analysis of Chandra observations of G292 has revealed electron temperatures ranging, in general, between 0.5 and 2 keV, although there are isolated knots in the north-west hemisphere with significantly higher electron temperatures (up to kT e ≈ 4 keV; Bhalerao et al 2019). The ionization time ranges, in general, between 3.4 × 10 10 cm −3 s and 3 × 10 12 cm −3 s, with few small regions in the north-west with values up to n e t ≈ 10 13 cm −3 s. In Fig.…”

Section: Distribution Of Ejecta At Later Timesmentioning

confidence: 99%

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The fully developed remnant of a neutrino-driven supernova: Evolution of ejecta structure and asymmetries in SNR Cassiopeia A

Orlando,

Wongwathanarat,

Janka

et al. 2020

Preprint

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Context. The remnants of core-collapse supernovae (SNe) are probes of the physical processes associated with their parent SNe. Aims. Here we aim at exploring to which extent the remnant keeps memory of the asymmetries that develop stochastically in the neutrino-heating layer due to hydrodynamic instabilities (e.g., convective overturn and the standing accretion shock instability; SASI) during the first second after core bounce. Methods. We coupled a 3D hydrodynamic model of a neutrino-driven SN explosion which has the potential to reproduce the observed morphology of the Cassiopeia A (Cas A) remnant, with 3D (magneto)-hydrodynamic simulations of the remnant formation. The simulations cover ≈ 2000 years of expansion and include all physical processes relevant to describe the complexities in the SN evolution and the subsequent interaction of the stellar debris with the wind of the progenitor star.Results. The interaction of large-scale asymmetries left from the earliest phases of the explosion with the reverse shock produces, at the age of ≈ 350 years, an ejecta structure and a remnant morphology which are remarkably similar to those observed in Cas A. Small-scale structures in the large-scale Fe-rich plumes created during the initial stages of the SN, combined with hydrodynamic instabilities that develop after the passage of the reverse shock, naturally produce a pattern of ring-and crown-like structures of shocked ejecta. The consequence is a spatial inversion of the ejecta layers with Si-rich ejecta being physically interior to Fe-rich ejecta. The full-fledged remnant shows voids and cavities in the innermost unshocked ejecta (in most cases physically connected with ring-like features of shocked ejecta in the main shell) resulting from the expansion of Fe-rich plumes and their inflation due to the decay of radioactive species. The asymmetric distributions of 44 Ti and 56 Fe (mostly concentrated in the northern hemisphere, pointing opposite to the kick velocity of the neutron star) and their abundance ratio are both compatible with those inferred from high-energy observations of Chandra and NuSTAR. Finally, the simulations show that the fingerprints of the SN can still be evident ≈ 2000 years after the explosion. Conclusions. The main asymmetries and features observed in the ejecta distribution of Cas A can be explained by the interaction of the reverse shock with the initial large-scale asymmetries that developed from stochastic processes (convective overturn and SASI activity) that originate during the first seconds of the SN blast.

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“…While the centroid energy-luminosity correlation can be seen in both theoretical modeling and Y14, many recent studies (Sezer et al 2018;Bhalerao et al 2019;Sawada et al 2019;Quirola-Vásquez et al 2019;Martínez-Rodríguez et al 2020) have continued to treat the Fe Kα line centroid as the sole discriminant. The Y14 calibration appears to hold for many SNRs.…”

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confidence: 99%

Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?

Siegel,

Dwarkadas,

Frank

et al. 2021

Preprint

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The centroid energy of the Fe Kα line has been used to identify the progenitors of supernova remnants (SNRs). These investigations generally considered the energy of the centroid derived from the spectrum of the entire remnant. Here we use XMM-Newton data to investigate the Fe Kα centroid in 6 SNRs: 3C 397, N132D, W49B, DEM L71, 1E 0102.2-7219, and Kes 73. In Kes 73 and 1E 0102.2-7219, we fail to detect any Fe Kα emission. We report a tentative first detection of Fe Kα emission in SNR DEM L71, with a centroid energy consistent with its Type Ia designation. In the remaining remnants, the spatial and spectral sensitivity is sufficient to investigate spatial variations of the Fe Kα centroid. We find in N132D and W49B that the centroids in different regions are consistent with that derived from the overall spectrum, although not necessarily with the remnant type identified via other means. However, in SNR 3C 397, we find statistically significant variation in the centroid of up to 100 eV, aligning with the variation in the density structure around the remnant. These variations span the intermediate space between centroid energies signifying core-collapse and Type Ia remnants. Shifting the dividing line downwards by 50 eV can place all the centroids in the CC region, but contradicts the remnant type obtained via other means. Our results show that caution must be used when employing the Fe Kα centroid of the entire remnant as the sole diagnostic for typing a remnant.

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Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-collapse Supernova Remnant G292.0+1.8

Cited by 21 publications

References 95 publications

Three Dimensional Core-Collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

Three Dimensional Core-Collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

The fully developed remnant of a neutrino-driven supernova: Evolution of ejecta structure and asymmetries in SNR Cassiopeia A

Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?

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