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We investigate how a phase transition from neutron-star matter tospin-polarized neutron matter affects the equation of state and mass-radiusrelation of neutron stars. While general extension schemes for the equation ofstate allow for high pressures inside neutron stars, we find that a phasetransition to spin-polarized neutron matter excludes extreme regimes. Hence,such a transition limits the maximum mass of neutron stars to lie below2.6$-$$2.9 \, M_{\odot}$, depending on the microscopic nuclear forces used,while significantly larger masses could be reached without these constraints.These limits are in good agreement with recent constraints extracted from theneutron-star merger GW170817 and its electromagnetic counterpart. Assuming thedescription in terms of spin-polarized neutron matter to be valid in the centerof neutron stars, we find that stars with a large spin-polarized domain intheir core are ruled out by GW170817.

Spin-polarized neutron matter, the maximum mass of neutron stars, and GW170817