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Could the interaction of jet and SN ejecta be the cause of X-ray knots observed in a radio galaxy?

Jia-Chun He, Xiao-Na Sun, Hao-Qiang Zhang, Yun-Feng Liang, Hai-Ming Zhang, Da-Bin Lin, En-Wei Liang

Abstract

We investigate the interaction between relativistic jets and supernova (SN) ejecta as a potential origin of X-ray knots in radio galaxies, employing knot A in M 87 as a test case. By modeling the dynamical evolution of the interaction, we evaluate this scenario based on particle acceleration efficiency and spatial morphology. Our modeling indicates that the ejecta shock expands to only ~ 30 pc, which is inconsistent with the observed spatial scale of knot A (~ 60 pc). In contrast, the jet shock can successfully reproduce the observed scale after approximately 3000 yr, with the ejecta being accelerated to a bulk velocity of β~ 0.43. We fit the multi-wavelength spectral energy distribution (SED) using a one-zone leptonic framework, attributing the X-rays to synchrotron radiation from electrons accelerated up to~1 PeV at the jet shock. The derived magnetic field is approximately 70 uG in the SN ejecta rest frame, which is significantly below the equipartition value. Protons may be accelerated up to ~ EeV, supporting the hypothesis that the jets of radio galaxies (RGs) may be the potential site for ultra-high-energy cosmic-ray (UHECR) acceleration within the framework of the jet-ejecta interaction.

Could the interaction of jet and SN ejecta be the cause of X-ray knots observed in a radio galaxy?

Abstract

We investigate the interaction between relativistic jets and supernova (SN) ejecta as a potential origin of X-ray knots in radio galaxies, employing knot A in M 87 as a test case. By modeling the dynamical evolution of the interaction, we evaluate this scenario based on particle acceleration efficiency and spatial morphology. Our modeling indicates that the ejecta shock expands to only ~ 30 pc, which is inconsistent with the observed spatial scale of knot A (~ 60 pc). In contrast, the jet shock can successfully reproduce the observed scale after approximately 3000 yr, with the ejecta being accelerated to a bulk velocity of β~ 0.43. We fit the multi-wavelength spectral energy distribution (SED) using a one-zone leptonic framework, attributing the X-rays to synchrotron radiation from electrons accelerated up to~1 PeV at the jet shock. The derived magnetic field is approximately 70 uG in the SN ejecta rest frame, which is significantly below the equipartition value. Protons may be accelerated up to ~ EeV, supporting the hypothesis that the jets of radio galaxies (RGs) may be the potential site for ultra-high-energy cosmic-ray (UHECR) acceleration within the framework of the jet-ejecta interaction.
Paper Structure (10 sections, 19 equations, 4 figures, 4 tables)

This paper contains 10 sections, 19 equations, 4 figures, 4 tables.

Table of Contents

  1. Introduction
  2. Model
  3. The dynamical evolution of shock system
  4. Particle acceleration and radiation
  5. Application to knot A in M87 jet
  6. Physical properties of knot A
  7. SED fitting
  8. Summary and discussion
  9. data availability
  10. Data analysis of Chandra

Figures (4)

  • Figure 1: The schematic illustration of the jet-ejecta scenarios. The solid and dashed arcs denote the jet shock and the ejecta shock, respectively. The red circle is the profile of SN ejecta.
  • Figure 2: The multiwavelength SED of knot A in M 87 reproduced by synchrotron and IC/CMB radiation of two electron populations in the jet-ejecta interaction framework. The solid lines show the total non-thermal emission from two electron populations. The blue, green, and yellow dashed lines represent the synchrotron, IC/CMB, and SSC radiation of the LE population, respectively. The blue, green, and yellow dotted lines are the synchrotron, IC/CMB, and SSC radiation of the HE population, respectively. The red points are the data in the X-ray energy band that we analyzed in this paper. See the text for details on the data from other instruments.
  • Figure 3: Deconvolved ACIS image of the Chandra observation on July 30, 2000 (ObsID 1808), binned in 0.1 per pixel. The cyan circle indicates the knot A region. The units of RA-- TAN and DEC--TAN are degrees.
  • Figure 4: The corner image of the fitting parameters of knot A.