The Magnetic Field Strength in the Wall of the Local Bubble toward l, b 300°, 0

We present polarization measurements in the region around /, b = 300, 0, toward stars with well-determined distances, primarily in the range 40-200 pc. We argue that these observations trace polarization caused by dust in the wall of the Local Bubble (LB). Using a Chandrasekhar-Fermi analysis, we derive a plane-of-the-sky magnetic field strength, in the wall of the LB in this direction, of ( super(B))= 8 super(+) sub(-) super(5) sub(3) kG, equivalent to a magnetic pressure of P sub(B)/k - 1.8 x 10 K cm super(-3). This pressure equals, to within the uncertainties, that in the bubble interior, as derived from EUVE observations, assuming collisional ionization equilibrium. Such a magnetic field could help us explain the observed low O VI column density associated with the LB wall.