The high energy spectrum of Proxima Centauri simultaneously observed at X-ray and FUV wavelengths

The M dwarf Proxima~Centauri is known to be magnetically active and it hosts a likely Earth-like planet in its habitable zone. Understanding the characteristics of stellar radiation by understanding properties emitting plasma paramount importance for proper assessment conditions on Proxima~Centauri~b exoplanets around dwarfs general. We determine temperature structure coronal transition region Proxima Centauri from simultaneous X-ray far-ultraviolet (FUV) observations. differential emission measure distribution (DEM) was constructed flaring quiescent periods analysing optically thin FUV lines. Four observations were conducted LETGS instrument board Chandra Observatory four carried out using Hubble STIS spectrograph. From light curves, we determined variation count rate factor two within 20\% rotation period. To obtain DEM, 18 lines analysed (12 six FUV). flare fluxes differ quiescence factors 4-20 1-30 (X-ray). corona both state fitting DEM(T) with Chebyshev polynomials range $\log$T = 4.25 - 8. Compared quiescence, increases during flares temperatures below 0.3\,MK (FUV dominated region) beyond 3.6\,MK (X-ray region). reconstructed DEM shape provides acceptable line flux predictions compared measured values. provide synthetic spectra at 1-1700 \AA, which may considered as representative high-energy irradiation Proxima~Cen~b periods.