Evolving supernova remnants in multiphase interstellar media

Villagran, Marco A.; Velázquez, P. F.; Gomez, Daniel Osvaldo; Giacani, E.

doi:10.1093/mnras/stz2811

Cited by 8 publications

(4 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Therefore, the large Faraday depth variation observed in these SNRs may be caused by internal effects from the SNR itself. Considering an SNR as a spherical shell, as the shell expands, variation in ISM densities will cause nonuniform expansion, and variations in density in the SNR shell through different lines of sight (Villagran et al 2020). When considering the internal environment of an SNR, a complex structure of free electrons and magnetic field is expected inside the SNR shell (Orlando et al 2019).…”

Section: Discussionmentioning

confidence: 99%

Polarized Emission from Four Supernova Remnants in the THOR Survey

Shanahan

Stil

Beuther

et al. 2022

ApJ

View full text Add to dashboard Cite

We present polarization and Faraday rotation for the supernova remnants (SNRs) G46.8 − 0.3, G43.3 − 0.2, G41.1 − 0.3, and G39.2 − 0.3 in the L-band (1–2 GHz) radio continuum in the H i/OH/Recombination line survey. We detect polarization from G46.8 − 0.3, G43.3 − 0.2, and G39.2 − 0.3 but find upper limits at the 1% level of Stokes I for G41.1 − 0.3. For G46.8 − 0.3 and G39.2 − 0.3, the fractional polarization varies on small scales from 1% to ∼6%. G43.3 − 0.2 is less polarized with fractional polarization ≲3%. We find upper limits at the 1% level for the brighter regions in each SNR with no evidence for associated enhanced Faraday depolarization. We observe significant variation in Faraday depth and fractional polarization on angular scales down to the resolution limit of 16″. Approximately 6% of our polarization detections from G46.8 − 0.3 and G39.2 − 0.3 exhibit two-component Faraday rotation and 14% of polarization detections in G43.3 − 0.2 are multicomponent. For G39.2 − 0.3, we find a bimodal Faraday depth distribution with a narrow peak and a broad peak for all polarization detections as well as for the subset with two-component Faraday rotation. We identify the narrow peak with the front side of the SNR and the broad peak with the back side. Similarly, we interpret the observed Faraday depth distribution of G46.8 − 0.3 as a superposition of the distributions from the front side and the back side. We interpret our results as evidence for a partially filled shell with small-scale magnetic field structure and internal Faraday rotation.

show abstract

Section: Discussionmentioning

confidence: 99%

Polarized Emission from Four Supernova Remnants in the THOR Survey

Shanahan

Stil

Beuther

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…Older SNRs will most certainly have their shape affected by the ambient medium, which is not uniform on >pc scales. For recent simulation work on the impact of a turbulent or cloudy ISM on the development of the SNR, relevant to Type Ia SNe, see Wang et al (2018); Peng et al (2020) and Villagran et al (2020).…”

Section: Other Physical Effectsmentioning

confidence: 99%

From Supernova to Supernova Remnant: The Three-dimensional Imprint of a Thermonuclear Explosion

Ferrand

Warren

Ono

et al. 2019

ApJ

View full text Add to dashboard Cite

Recent progress in the three-dimensional modeling of supernovae (SN) has shown the importance of asymmetries for the explosion. This calls for a reconsideration of the modeling of the subsequent phase, the supernova remnant (SNR), which has commonly relied on simplified ejecta models. In this paper we bridge SN and SNR studies by using the output of a SN simulation as the input of a SNR simulation carried on until 500 yr. We consider the case of a thermonuclear explosion of a carbonoxygen white dwarf star as a model for a Type Ia SN; specifically we use the N100 delayed detonation model of Seitenzahl et al 2013. In order to analyze the morphology of the SNR, we locate the three discontinuities that delineate the shell of shocked matter: the forward shock, the contact discontinuity, and the reverse shock, and we decompose their radial variations as a function of angular scale and time. Assuming a uniform ambient medium, we find that the impact of the SN on the SNR may still be visible after hundreds of years. Previous 3D simulations aiming at reproducing Tycho's SNR, that started out from spherically symmetric initial conditions, failed to reproduce structures at the largest angular scales observed in X-rays. Our new simulations strongly suggest that the missing ingredient was the initial asymmetries from the SN itself. With this work we establish a way of assessing the viability of SN models based on the resulting morphology of the SNR.

show abstract

“…Therefore, the large Faraday depth variation observed in these SNRs may be caused by internal effects from the SNR itself. Considering a SNR as a spherical shell, as the shell expands, variation in ISM densities will cause non-uniform expansion and variations in density in the SNR shell through different lines-of-sight (Villagran et al 2020). When considering the internal environment of a SNR, a complex structure of free electrons and magnetic field is expected inside the SNR shell (Orlando et al 2019).…”

Section: Snr G411−03mentioning

confidence: 99%

Polarized Emission From Four Supernova Remnants In The THOR Survey

Shanahan¹,

Stil²,

Beuther³

et al. 2022

Preprint

View full text Add to dashboard Cite

We present polarization and Faraday rotation for the supernova remnants (SNRs) G46.8−0.3, G43.3−0.2, G41.1−0.3, and G39.2−0.3 in L-band (1-2 GHz) radio continuum in The HI/OH/Recombination line (THOR) survey. We detect polarization from G46.8−0.3, G43.3−0.2 and G39.2−0.3 but find upper limits at the 1% level of Stokes I for G41.1−0.3. For G46.8−0.3 and G39.2−0.3 the fractional polarization varies on small scales from 1% to ∼6%. G43.3−0.2 is less polarized with fractional polarization 3%. We find upper limits at the 1% level for the brighter regions in each SNR with no evidence for associated enhanced Faraday depolarization. We observe significant variation in Faraday depth and fractional polarization on angular scales down to the resolution limit of 16 . Approximately 6% of our polarization detections from G46.8−0.3 and G39.2−0.3 exhibit twocomponent Faraday rotation and 14% of polarization detections in G43.3−0.2 are multi-component. For G39.2−0.3 we find a bimodal Faraday depth distribution with a narrow peak and a broad peak for all polarization detections as well as for the subset with two-component Faraday rotation. We identify the narrow peak with the front side of the SNR and the broad peak with the back side. Similarly, we interpret the observed Faraday depth distribution of G46.8−0.3 as a superposition of the distributions from the front side and the back side. We interpret our results as evidence for a partially filled shell with small-scale magnetic field structure and internal Faraday rotation.

show abstract

Evolving supernova remnants in multiphase interstellar media

Cited by 8 publications

References 40 publications

Polarized Emission from Four Supernova Remnants in the THOR Survey

Polarized Emission from Four Supernova Remnants in the THOR Survey

From Supernova to Supernova Remnant: The Three-dimensional Imprint of a Thermonuclear Explosion

Polarized Emission From Four Supernova Remnants In The THOR Survey

Contact Info

Product

Resources

About