Context :

Aims : We present the first high-resolution non-equilibrium ionization simulation of the joint evolution of the Local Bubble ( LB ) and Loop I superbubbles in the turbulent supernova-driven interstellar medium ( ISM ) .
The time variation and spatial distribution of the Li-like ions C iv , N v , and O vi inside the LB are studied in detail .

Methods : This work uses the parallel adaptive mesh refinement code EAF-PAMR coupled to the newly developed atomic and molecular plasma emission module E ( A+M ) PEC , featuring the time-dependent calculation of the ionization structure of H through Fe , using the latest revision of solar abundances .
The finest AMR resolution is 1 pc within a grid that covers a representative patch of the Galactic disk ( with an area of 1 kpc ^ { 2 } in the midplane ) and halo ( extending up to 10 kpc above and below the midplane ) .

Results : The evolution age of the LB is derived by the match between the simulated and observed absorption features of the Li-like ions C iv , N v , and O vi .
The modeled LB current evolution time is bracketed between 0.5 and 0.8 Myr since the last supernova reheated the cavity in order to have { N ( O { \textsc { vi } } ) } < 8 \times 10 ^ { 12 } cm ^ { -2 } , \log [ { N ( C { \textsc { iv } } ) } / { N ( O { \textsc { vi } } ) } ] < -0.9 and \log [ { N ( N { \textsc { v } } ) } / { N ( O { \textsc { vi } } ) } ] < -1 inside the simulated LB cavity , as found in Copernicus , IUE , GHRS-IST and FUSE observations .

Conclusions :