Solar energy paper index
The emergence of X-ray emission lines during relativistic radio-jet formation in the changing-look active galactic nucleus 1ES 1927+654
One-line summary
A solar energy research paper on The emergence of X-ray emission lines during relativistic radio-jet formation in the changing-look active galactic nucleus 1ES 1927+654.
Engineering notes
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Chinese explanation / 中文解读
中文解读待补充：本站会优先为光伏效率、钙钛矿太阳能电池、储能技术、太阳能热利用、BIPV、并网技术等高价值论文补充中文说明。
Original abstract
We present results from a comprehensive multi-wavelength monitoring campaign of the changing-look active galactic nucleus 1ES 1927+654 during the onset and evolution of a radio jet (May 2022-August 2025). Using observations from XMM-Newton, Swift, TNG, ZTF, VLA, and VLBA, we characterize the spectral evolution of the source. Soft X-ray emission lines at ~0.56 keV and ~1 keV have appeared with variable strength and width during the formation of a nascent jet, with the ~1 keV feature persisting since the post-2017 flare phase. We also report the detection of a broad (~800 eV) Fe K emission feature at ~(6-7) keV in ~70 ks of stacked EPIC-pn spectra, marking the first such detection in this historically featureless source. Joint spectral fitting of XMM-Newton EPIC-pn and RGS data reveals the presence of ionized absorbers in 2022, followed by weaker absorption from 2023 to 2025. The emergence of emission features concurrent with the decline of ionized absorption suggests a transition in the inner accretion and outflow processes, indicating the reflection and reprocessing of X-rays from the inner accretion disk during jet formation. The apparent weakening of ionized outflows as the jet develops supports a scenario in which accreting material is preferentially channeled into the jet rather than expelled as winds. Furthermore, both the 0.3-2 keV soft X-ray and 5 GHz radio fluxes, which have increased by factors of ~10 and ~60, respectively, since 2022, have recently plateaued at elevated levels. Combined with steady optical emission, this indicates a stabilized accretion disk, corona, and jet configuration. Finally, the absence of broad optical emission lines suggests that the broad-line region is either not along our line of sight or insufficiently illuminated by the central source.
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