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.
Title resolution pending
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
years
2026 2verdicts
UNVERDICTED 2representative citing papers
In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.
citing papers explorer
-
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.
-
Cosmological perturbations with $f(R)$ gravity scalarons : Galaxy power spectra and the scalaron mass
In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.