Observed interstellar magnetized supershells and stellar-wind theories

Early theories of stellar winds from an association of OB stars predicted the formation of a common superbubble enclosed by athin, dense supershell, through the combined effort of the winds from the stars at the center. These early theories were adequate for explaining the primary observational features (defined as: shell age, outer radius, shell speed, shell mass, shell energy), but they were not adequate to explain the secondary features (defined as: shell thickness, shell magnetic field, shell gas density). A recently published theory for a stellar-wind-bubble and supershell, predicting a range ofthick supershells, can now be compared with the secondary observational features.Using the observed parameters from all large (> 100 pc) interstellar magnetized supershells near the sun (< 1 kpc away), I assemble for comparison with stellar-wind theories: (a) the primary observational features of these shells — I find: large shell age, large outer radius, low shell speed, large shell mass, large shell energy; and (b) some of their secondary observational features — I find: thick shell, low shell magnetic field strengh, low shell gas density.