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This paper investigates the neutral gas phase of galactic winds via the Na ID$\lambda\lambda 5890,5895${\AA} feature within $z \sim 0.04$ MaNGA galaxies,and directly compares their incidence and strength to the ionized windsdetected within the same parent sample. We find evidence for neutral outflowsin 127 galaxies ($\sim 5$ per cent of the analysed line-emitting sample). Na ID winds are preferentially seen in galaxies with dustier central regions andboth wind phases are more often found in systems with elevated SFR surfacedensities, especially when there has been a recent upturn in the star formationactivity according to the SFR$_{5Myr}$/SFR$_{800Myr}$ parameter. We find theionized outflow kinematics to be in line with what we measure in the neutralphase. This demonstrates that, despite their small contributions to the totaloutflow mass budget, there is value to collecting empirical measurements of theionized wind phase to provide information on the bulk motion in the outflow.Depending on dust corrections applied to the ionized gas diagnostics, theneutral phase has $\sim 1.2 - 1.8$ dex higher mass outflow rates($\dot{M}_{out}$), on average, compared to the ionized phase. We quantifyscaling relations between $\dot{M}_{out}$ and the strengths of the physicalwind drivers (SFR, $L_{AGN}$). Using a radial-azimuthal stacking method, and byconsidering inclination dependencies, we find results consistent with biconicaloutflows orthogonal to the disk plane. Our work complements other multi-phaseoutflow studies in the literature which consider smaller samples, more extremeobjects, or proceed via stacking of larger samples.

Cool outflows in MaNGA: a systematic study and comparison to the warm phase