2025MNRAS.539.2806K

This paper presents the results of a detailed timing and spectral analysis of the TeV-detected blazar 1ES 1218$+$304, focused on the observations performed with the different instruments onboard the Neil Gehrels Swift Observatory in the period 2005-2024. The source showed various strengths of X-ray flaring activity and 0.3-10 keV states differing by a factor up to 20 in brightness, exceeding a level of 2.7 $\times$ 10$^{-10}$ erg cm$^{-2}$ s$^{-1}$ and representing the third brightest blazar during the strongest flare. We detected tens of intraday variability instances, the majority of which occurred on sub-hour time-scales and were consistent with the shock-in-jet scenario. The spectral properties were strongly and fastly variable, characterized by a frequent occurrence of very hard photon indices in the 0.3-10 keV and Fermi 0.3-300 GeV bands. The source exhibited very fast transitions of log-parabolic-to-power-law spectra or conversely, possibly caused by changes of magnetic field properties over small spatial scales or by turbulence-driven relativistic magnetic reconnection. We detected various spectral features, which demonstrate the importance of the first-order Fermi mechanism operating by the magnetic field of changing confinement efficiencies and by the electron populations with different initial energy distributions, stochastic acceleration, and cooling processes. In some periods, the source showed a softening at higher GeV-band energies, possibly due to the inverse-Compton upscatter of X-ray photons in the Klein-Nishina regime reflected in the positive correlation between X-ray and high-energy emissions.