The S 1 Shell and Interstellar Magnetic Field and Gas near the

The S1 subshell of the Loop I supernova remnant is consistent with observations of interstellar material close to the Sun. The magnetic field direction of the S1 shell at the Sun agrees with the field direction found from starlight polarization for stars that sample the ecliptic plane at the heliosphere nose, but is barely consistent with the field direction implied by the the offset angle between interstellar H and He flowing into the heliosphere. The configuration of the S1 bubble also explains the spatial pattern of high average interstellar Ca column densities seen for stars within 50 pc and in the third and fourth galactic quadrants. The structure of the S1 shell indicates that the parts of the S1 shell with longitudes l> 180◦ and within 50 pc are more exposed to the bright EUV source Adhara, than S1 shell regions with l< 180◦. The S1 shell configuration thus predicts higher ionization levels based on Adhara emissions for nearby l> 180◦ regions, explaining the higher averaged Ca column densities. Subject headings: ISM: magnetic fields, dust, heliosphere— cosmology: miscellaneous— solar system: general