The interstellar medium (ISM) is heated and ionized by radiation, by stellar winds, and finally, by supernova explosions of massive stars. Since these processes are often correlated in space and time, they can form large interstellar structures called superbubbles, which are filled with hot thin plasma. Supernova remnants and superbubbles can be studied best in soft X-ray line and continuum emission, since the plasma in their interiors is very hot (10^6 − 10^7 K), while non-thermal particles accelerated in the shock waves can also cause X-ray emission. We will present recent results of studies of the hot ISM in the Milky Way and nearby galaxies, in particular in the Magellanic Clouds, and discuss the physics of the hot plasma, the evolution of supernova remnants and superbubbles, and the implications for the star formation history of the galaxies. We will also present first maps of the hot interstellar plasma in the LMC observed with eROSITA.
|Presenter status||eROSITA consortium member|