We present the properties of the magnetic field (B-field) in the starburst ring of the galaxy NGC 1097. Thermal polarized emission at 89 $mu$m using HAWC+/SOFIA shows that the polarized flux is spatially located at the contact regions of the outer-bar with the starburst ring. The linear polarization decomposition analysis shows that the $89$ $mu$m and radio ($3.5$ and $6.2$ cm) polarization traces two different modes, $m$, of the B-field: a constant B-field orientation and dominated by $m=0$ at $89$ $mu$m, and a spiral B-field dominated by $m=2$ at radio. The $^{12}CO(2-1)$ integrated emission line peaks in the inner $sim0.69$ kpc, the FIR polarized flux peaks in the central $sim 1.02$ kpc, and the radio polarized flux peaks in the outer $sim1.39$ kpc of the starburst ring. Dust temperature is higher, $T_{89mu m} = 30.7pm0.4$ K, at the region of the FIR polarized flux than at the radios region, $T_{3.5cm} = 26.2pm1.7$ K. We argue that the B-field at 89 $mu$m is concentrated in the warmest region of a shock front caused by the galactic density wave in the contact regions between the outer-bar with the starburst ring. Radio polarization traces a superposition of the spiral B-field outside and within the starburst ring. According to Faraday rotation measures between $3.5$ and $6.2$ cm, the radial component of the B-field along the contact regions points toward the galaxys center on both sides. Gas streams follow the B-field, which feeds the black hole with matter from the host galaxy.
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