Collisionless shock heating of heavy ions in SN 1987A

Miceli, M.; Orlando, S.; Burrows, D. N.; Frank, Kari A.; Argiroffi, C.; Reale, F.; Peres, G.; Petruk, O.; Bocchino, F.

doi:10.1038/s41550-018-0677-8

Cited by 53 publications

(52 citation statements)

References 36 publications

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“…The dependence 𝜒 ∝ 𝑚/𝑞, and mass dependence of the energization (11,13) could explain observations that heavy ions in the C,N,O group have fluxes larger than protons at high energies (Stasiewicz et al 2013;Turner et al 2018). This is also consistent with observation of heavy ion temperatures 𝑇 𝑖 ∝ 𝑚 𝑖 /𝑚 𝑝 in post-shocks of supernova remnants (Raymond et al 2017;Miceli et al 2019;Gedalin 2020). However, there are also other explanations for the preferential heating of heavy ions (Zank et al 1996(Zank et al , 2001Shapiro et al 2001).…”

Section: Comparison With Observationssupporting

confidence: 63%

Ion acceleration to 100 keV by the ExB wave mechanism in collision-less shocks

Stasiewicz

Eliasson

2021

Monthly Notices of the Royal Astronomical Society

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It is shown that ions can be accelerated to about 100 keV in the direction perpendicular to the magnetic field by the ExB mechanism of electrostatic waves. The acceleration occurs in discrete steps of duration being a small fraction the gyroperiod and can explain observations of ion energisation to 10 keV at quasi-perpendicular shocks and to hundreds keV at quasi-parallel shocks. A general expression is provided for the maximum energy of ions accelerated in shocks of arbitrary configuration. The waves involved in the acceleration are related to three cross-field current-driven instabilities: the lower hybrid drift (LHD) instability induced by the density gradients in shocks and shocklets, followed by the modified two-stream (MTS) and electron cyclotron drift (ECD) instabilities, induced by the ExB drift of electrons in the strong LHD wave electric field. The ExB wave mechanism accelerates heavy ions to energies proportional to the atomic mass number, which is consistent with satellite observations upstream of the bow shock and also with observations of post-shocks in supernovae remnants. The results are compared with other acceleration mechanisms traditionally discussed in the literature.

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Section: Comparison With Observationssupporting

confidence: 63%

Ion acceleration to 100 keV by the ExB wave mechanism in collision-less shocks

Stasiewicz

Eliasson

2021

Monthly Notices of the Royal Astronomical Society

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“…From the model results, we synthesized the thermal X-ray emission originating from the impact of the blast wave with the nebula, by following the approach outlined in previous studies (Orlando et al 2015;Miceli et al 2019). The system was rotated about the three axes to fit the orientation of the ring in the plane of the sky inferred from the analysis of optical data (Sugerman et al 2005): i x = 41 o , i y = −8 o , and i z = −9 o .…”

Section: Synthesis Of X-ray Emissionmentioning

confidence: 99%

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

Orlando

Ono

Nagataki

et al. 2020

A&A

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Context. Massive stars end their lives with catastrophic supernova (SN) explosions. Key information on the explosion processes and on the progenitor stars can be extracted from observations of supernova remnants (SNRs), the outcome of SNe. Deciphering these observations however is challenging because of the complex morphology of SNRs. Aims. We aim at linking the dynamical and radiative properties of the remnant of SN 1987A to the geometrical and physical characteristics of the parent aspherical SN explosion and to the internal structure of its progenitor star. Methods. We performed comprehensive three-dimensional hydrodynamic simulations which describe the long-term evolution of SN 1987A from the onset of the SN to the full-fledged remnant at the age of 50 years, accounting for the pre-SN structure of the progenitor star. The simulations include all physical processes relevant for the complex phases of SN evolution and for the interaction of the SNR with the highly inhomogeneous ambient environment around SN 1987A. Furthermore the simulations follow the life cycle of elements from the synthesis in the progenitor star, through the nuclear reaction network of the SN, to the enrichment of the circumstellar medium through mixing of chemically homogeneous layers of ejecta. From the simulations, we synthesize observables to be compared with observations. Results. By comparing the model results with observations, we constrained the initial SN anisotropy causing Doppler shifts observed in emission lines of heavy elements from ejecta, and leading to the remnant evolution observed in the X-ray band in the last thirty years. In particular, we found that the high mixing of ejecta unveiled by high redshifts and broadenings of [Fe II] and 44 Ti lines require a highly asymmetric SN explosion channeling a significant fraction of energy along an axis almost lying in the plane of the central equatorial ring around SN 1987A, roughly along the line-of-sight but with an offset of 40 o , with the lobe propagating away from the observer slightly more energetic than the other. Furthermore, we found unambiguously that the observed distribution of ejecta and the dynamical and radiative properties of the SNR can be best reproduced if the structure of the progenitor star was that of a blue supergiant resulted from the merging of two massive stars.

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“…By adopting the approach described in Greco et al 2020 (see also Miceli et al 2019), we self-consistently synthesized X-ray spectra from our simulations in a format virtually identical to that of Chandra ACIS-S observations. The synthesis includes the deviations from equilibrium of ionization and from temperature-equilibration between electrons and protons, and takes into account the chemical composition of ejecta and ISM resulting from the simulations in each computational cell (see e.g., Miceli et al 2019;Orlando et al 2019 for more details). For the spectral synthesis, we assume a distance of 1 kpc and a column density N H = 2 × 10 21 cm −2 with an exposure time of 100 ks.…”

Section: Synthesis Of X-ray Emissionmentioning

confidence: 99%

Three-dimensional modeling from the onset of the SN to the full-fledged SNR

Tutone

Orlando

Miceli

et al. 2020

A&A

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Context. The manifold phases in the evolution of a core-collapse (CC) supernova (SN) play an important role in determining the physical properties and morphology of the resulting supernova remnant (SNR). Thus, the complex morphology of SNRs is expected to reflect possible asymmetries and structures developed during and soon after the SN explosion. Aims. The aim of this work is to bridge the gap between CC SNe and their remnants by investigating how post-explosion anisotropies in the ejecta influence the structure and chemical properties of the remnant at later times. Methods. We performed three-dimensional magneto-hydrodynamical simulations starting soon after the SN event and following the evolution of the system in the circumstellar medium, which includes the wind of the stellar progenitor, for 5000 yr, obtaining the physical scenario of a SNR. Here we focused the analysis on the case of a progenitor red supergiant of 19.8 M⊙. We also investigated how a post-explosion large-scale anisotropy in the SN affects the ejecta distribution and the matter mixing of heavy elements in the remnant during the first 5000 yr of evolution. Results. In the case of a spherically symmetric SN explosion without large-scale anisotropies, the remnant roughly keeps memory of the original onion-like layering of ejecta soon after the SN event. Nevertheless, as the reverse shock hits the ejecta, the element distribution departs from a homologous expansion because of the slowing down of the outermost ejecta layers due to interaction with the reverse shock. In the case of a large-scale anisotropy developed after the SN, we found that the chemical stratification in the ejecta can be strongly modified and the original onion-like layering is not preserved. The anisotropy may cause spatial inversion of ejecta layers, for instance leading to Fe/Si-rich ejecta outside the O shell, and may determine the formation of Fe/Si-rich jet-like features that may protrude the remnant outline. The level of matter mixing and the properties of the jet-like feature are sensitive to the initial physical (density and velocity) and geometrical (size and position) initial characteristics of the anisotropy.

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Collisionless shock heating of heavy ions in SN 1987A

Cited by 53 publications

References 36 publications

Ion acceleration to 100 keV by the ExB wave mechanism in collision-less shocks

Ion acceleration to 100 keV by the ExB wave mechanism in collision-less shocks

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

Three-dimensional modeling from the onset of the SN to the full-fledged SNR

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