Whence the Interstellar Magnetic Field Shaping the Heliosphere?

Abstract Measurements of starlight polarized by aligned interstellar dust grains are used to probe the relation between orientation ambient magnetic field (ISMF) and ISMF traced ribbons energetic neutral atoms discovered Interstellar Boundary Explorer spacecraft. We utilize polarization data, many acquired specifically for this study, trace configuration within 40 pc. A statistical analysis yields a best-fit orientation, B magpol , with Galactic coordinates ℓ = 42°, b 49°. Further shows is more orderly “downfield” stars located over 90° from . The data subset downfield an nearby at ecliptic λ β ≈ 219° ± 15°, 43° 9° (Galactic l 40°, 56°, ±17°). This close direction obtained ribbon models. agreement suggests that shaping heliosphere belongs extended ordered field. Extended filamentary structures found throughout sky. previously filament traversing nose region, “Filament A,” extends 300° sky, crosses upwind flowing into heliosphere. Filament overlaps locations Voyager kilohertz emissions, three quasar intraday variables, cosmic microwave background (CMB) components, inflow sampled Ulysses Galileo. These features likely in upstream outer heliosheath where drapes heliosphere, suggesting coincides dusty magnetized plasma. 55° long possible shock interface local clouds. dark spot CMB seen 5° 10° direction. Two large arcs centered on directions heliotail. overlap components forming indicates entrained interacting provides measurable foreground CMB.