Implications of Interstellar Dust and Interstellar Magnetic Field at the Heliosphere

Tiny interstellar dust grains causing the polarization of light from the nearest stars are deflected sideways in the outer heliosheath regions, along with the interstellar magnetic field. Observations of optical polarization of stars beyond the heliosphere nose, and at distances 5– 200 pc, suggest the direction of the upwind interstellar magnetic field is relatively constant. The polarization vectors indicate an orientation of the local interstellar magnetic field consistent with the position angle in galactic coordinates of PAG∼ 40. This position angle is consistent with the offset between interstellar He and H flowing into the heliosphere, indicating that the interstellar magnetic field, BIS, is inclined by ∼ 55 and ∼ 65, respectively, with respect to the galactic and ecliptic planes. The heliosphere nose is towards Loop I, and if the expansion of Loop I distorted the interarm BIS close to the Sun then the local BIS is directed from southern to northern ecliptic latitudes. The hot and cold poles of the measured Cosmic Microwave Background (CMB) dipole moment are nearly symmetric around the heliosphere nose direction, to within ∼ 5. The v quadrupole vector is directed towards the heliosphere nose. The area vectors of the CMB quadrupole and octopole moments are directed towards the band perpendicular to the ecliptic plane formed by the alternate locations for the 3 kHz emissions detected by Voyagers 1 and 2. In the upwind direction, the position angle of the null plane separating the CMB dipole hot and cold poles is almost aligned with the interstellar magnetic field direction at the Sun. The mechanisms and symmetries of possible heliospheric contamination of the low-l CMB modes now require detailed studies based on the interactions of the interstellar magnetic field and charged particles with an asymmetric heliosphere. The inferred dust composition in the surrounding interstellar medium is consistent with amorphous olivines.