Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.
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In EMSG, neutron star trace anomaly profiles increase monotonically from core to surface and curvature invariants organize into bands versus the trace anomaly, extending the GR correspondence with coupling-dependent splitting.
citing papers explorer
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General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly
Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.
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Trace anomaly and interior curvature of neutron stars in energy-momentum squared gravity
In EMSG, neutron star trace anomaly profiles increase monotonically from core to surface and curvature invariants organize into bands versus the trace anomaly, extending the GR correspondence with coupling-dependent splitting.