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The linear polarization produced by scattering processes in the hydrogenLyman alpha line of the solar disk radiation is a key observable for probingthe chromosphere-corona transition region (TR) and the underlying chromosphericplasma. While the line-center signal encodes information on the magnetic fieldand three-dimensional structure of the TR, the sizable scattering polarizationsignals that the joint action of partial frequency redistribution (PRD) andJ-state interference produce in the Lyman alpha wings have generally beenthought to be sensitive only to the thermal structure of the solar atmosphere.Here we show that the wings of the Q/I and U/I scattering polarization profilesof this line are actually sensitive to the presence of chromospheric magneticfields, with strengths similar to those that produce the Hanle effect in theline core (i.e., between 5 and 100 gauss, approximately). In spite of the factthat the Zeeman splitting induced by such weak fields is very small compared tothe total width of the line, the magneto-optical effects that couple thetransfer equations for Stokes Q and U are actually able to produce sizablechanges in the Q/I and U/I wings. The theoretical results presented herefurther expand the diagnostic content of the unprecedented spectropolarimetricobservations provided by the Chromospheric Lyman-Alpha Spectropolarimeter(CLASP).

Magnetic sensitivity in the wing scattering polarization signals of the hydrogen Lyman-alpha line of the solar disk radiation