Skip to content
DraconiticResearch
Search Sources API
186,123 studies31 sourcesUpdated 54 min ago
Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

Investigating the nature of magnetic turbulence in Tycho’s SNR using X-ray observation

  • Ashwin Aravindaraj1
  • Hui Zhu2
  • Adrien Picquenot3
  • Hsiang-Kuang Chang1,4,5,6
6 affiliations
  1. 1Institute of Astronomy, National Tsing Hua University , Hsinchu 300044 ,
  2. 2State Key Laboratory of Radio Astronomy and Technology, National Astronomical Observatories , CAS, Beijing 100012 ,
  3. 3Department of Physics & Astronomy, Louisiana State University , 202 Nicholson Hall, Baton Rouge, LA 70803 ,
  4. 4Department of Physics, National Tsing Hua University , Hsinchu 300044 ,
  5. 5Institute of Space Engineering, National Tsing Hua University , Hsinchu 300044 ,
  6. 6Center for Theory-Computation-Data Science Research (CTCD), National Tsing Hua University , Hsinchu 300044 ,
Open at sourcePDFDOICite

Abstract

Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic cosmic ray acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the magnetic energy spectrum from the non-thermal X-ray flux image of Tycho’s SNR. This image was obtained using Poissonian-based generalized morphological component analysis. The turbulence length-scale observed in the resulting spectrum is shorter than the turbulence scale derived from previous studies of radio observations of Tycho’s SNR. Additionally, we use the X-ray rim thickness measured across Tycho, which is an indicator of magnetic field strength to estimate the magnetic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.

Versions

Related

  1. Investigating the Nature of Discontinuous Shear Thickening: Beyond a Mean-Field Description
    Jetin E. Thomas, Abhay Goyal, Deshpreet Singh Bedi +3
    arXivPreprintCC BY 4.0Full textCondensed matterFluid dynamicsarXiv
  2. First Observation of a Polar Coronal Hole-like Fast Solar Wind Stream in the Sub-Alfvénic Solar Corona: an Analysis of Turbulence Properties
    Riddhi Bandyopadhyay, Sujan Prasad Gautam, William H. Matthaeus +2
    arXivPreprintCC BY 4.0Full textSolar & stellar physicsPlasma physicsarXiv
  3. Helical Magnetic Nature of β-Mn Structured CoZn Thin-Films Determined by a Bayesian Approach to Modeling Polarized Neutron Reflectivity Data
    M. Dearg, A. J. Caruana, C. J. Kinane +4
    arXivPreprintCC BY 4.0Full textCondensed matterarXiv
  4. Magnetic Turbulence Boosts Supernova Signals of Axion-Photon Conversion
    Damiano F. G. Fiorillo, Ángel Gil Muyor, Georg G. Raffelt +1
    arXivPreprintarXiv licenceFull textCosmologyHigh-energy astrophysicsarXiv
  5. Recovering 3D Magnetic Turbulence from Single-frequency Faraday Screens
    A. Melnichenka, A. Lazarian, D. Pogosyan
    The Astrophysical JournalPeer-reviewedCC BY 4.0Full textHigh-energy & particle physicsCrossref

Cite

BibTeXRIS
BibTeX
@article{aravindaraj2026investigating,
  title = {{Investigating the nature of magnetic turbulence in Tycho’s SNR using X-ray observation}},
  author = {Ashwin Aravindaraj and Hui Zhu and Adrien Picquenot and Hsiang-Kuang Chang},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag1944},
  url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1944/8914588},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Investigating the nature of magnetic turbulence in Tycho’s SNR using X-ray observation
AU  - Ashwin Aravindaraj
AU  - Hui Zhu
AU  - Adrien Picquenot
AU  - Hsiang-Kuang Chang
PY  - 2026
DA  - 2026/10/13
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1944
UR  - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1944/8914588
AB  - Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic cosmic ray acceleration and the particles are energized at the shock front of SNRs through the diffusive shock acceleration mechanism, gaining energy by repeatedly crossing the shock. Magnetic turbulence plays a crucial role in scattering these particles back and forth, making the investigation of turbulence essential to understanding the acceleration process. In this study, we apply the two-point correlation method to derive the magnetic energy spectrum from the non-thermal X-ray flux image of Tycho’s SNR. This image was obtained using Poissonian-based generalized morphological component analysis. The turbulence length-scale observed in the resulting spectrum is shorter than the turbulence scale derived from previous studies of radio observations of Tycho’s SNR. Additionally, we use the X-ray rim thickness measured across Tycho, which is an indicator of magnetic field strength to estimate the magnetic energy spectrum. The turbulence scale inferred from this method is consistent with that obtained from the non-thermal X-ray flux analysis.
SN  - 0035-8711
SN  - 1365-2966
ER  -