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The Orion-Eridanus superbubble has been blown by supernovae and supersonicwinds of the massive stars in the Orion OB associations. The formation historyand current structure of the superbubble are still poorly understood. Itpossibly consists of a combination of nested shells along the line of sight. Wehave investigated the composite structure of the Eridanus side of thesuperbubble in the light of a new decomposition of the atomic and moleculargas. We used HI and CO emission lines to separate coherent gas shells in spaceand velocity, and we studied their relation to the warm ionised gas probed inH$\alpha$ emission, to the hot plasma emitting X-rays, and to the magneticfields traced by dust polarised emission. We also constrained the relativedistances to the clouds using dust reddening maps and X-ray absorption. We usedthe dust polarisation data to estimate the plane-of-sky components of themagnetic field in several clouds and along the outer rim of the superbubble.Our gas decomposition has revealed several shells inside the superbubble thatspan distances from about 150 pc to 250 pc. One of these shells forms a nearlycomplete ring filled with hot plasma. Other shells likely correspond to thelayers of swept-up gas that is compressed behind the expanding outer shockwave. We used the gas and magnetic-field data downstream of the shock to derivea shock expansion velocity close to 20 km/s. Taking the X-ray absorption by thegas into account, we find that the pressure of the hot plasma inside thesuperbubble exceeds that in the Local Bubble. It comprises a mix of hotter (3-9MK) and cooler (0.3-1.2 MK) gas along the lines of sight. The magnetic fieldalong the western and southern rims and in the approaching wall of thesuperbubble appears to be shaped and compressed by the ongoing expansion. Wefind plane-of-sky magnetic strengths ranging from 3 to 15 $\mu$G along the rim.

Gas shells and magnetic fields in the Orion-Eridanus superbubble