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Optical and infrared continuum polarization from the interstellar medium isknown to generally be due to irregular dust grains aligned with the magneticfield. This provides an important tool to probe the geometry and strength ofthose fields, particularly if the variations in the grain alignmentefficiencies can be understood. Here, we examine polarization variationsobserved throughout the wall of the Local Bubble, using a large polarizationsurvey of the North Galactic cap (\textit{b}$>30^\circ$) from\citet{berdyugin2014}. These data are analyzed together with archivalphotometric and spectroscopic data along with the mapping of the Local Bubbleby \citet{lallement2003}. We can model the observational data by assuming thatthe alignment driving mechanism is due to the radiation from the surroundingstar field. In particular we find that the fractional polarization is dominatedby the light from the OB associations within 150 pc of the sun, but is largelyinsensitive to the radiation field from red field stars. This behavior isconsistent with the expected wavelength dependence of radiative grain alignmenttheory. We also probe the relative strength of the magnetic field in the wallof the Local Bubble using the Davis-Chandrasekhar-Fermi method. We findevidence for a systematically varying field strength distribution, where thevariations in the field are correlated with the variations in grain alignmentefficiency, indicating that the relatively higher field strength regions mightrepresent a compression of the wall by the interaction of the outflow in theLocal Bubble and the opposing flows by the surrounding OB associations.

Magnetic Field Strengths and Grain Alignment Variations in the Local Bubble Wall