Thermal plasma emission in the soft X-ray band (0.1 – 2.0 keV) is believed to be responsible for the bulk of the X-ray intensity seen from the Local Bubble, a low-density cavity extending over ∼ 70 – 200 pc around the Sun. The state of the hot plasma is still a matter of discussion as previous instrumentation like aboard ROSAT was not able to unambiguously distinguish between equilibrium and non-equilibrium emission models and thus to pin-point the origin of the Local Bubble. Recent missions like DXS, XQC, and XMM-Newton have shed more light on this subject and observations indicate that collisional ionization equilibrium with solar abundances cannot explain the data: lines appear at positions and with intensities in contradiction to standard models. Analysis of EPIC-pn data of X-ray shadowing observations (MBM 12, Ophiuchus molecular cloud) suggest a component with higher temperature (kT ∼ 0.14 keV) besides the standard kT ∼ 0.09 keV plasma.