Kavli Affiliate: Lijing Shao
| First 5 Authors: Peixiang Ji, Peixiang Ji, , ,
| Summary:
Compact stars in scalar-tensor gravity have been extensively investigated,
but relatively few studies have focused on highly relativistic neutron stars
(NSs) with an extremely dense core region where the trace of the
energy-momentum tensor reverses its sign. In this regime, we identify the
origin of the phenomenon where it multiple scalarized solutions exist for a
it fixed central density, arising from the oscillatory profile of the scalar
field inside the star. This origin further indicates that the multi-branch
structure emerges for both negative and positive $beta$, the quadratic-term
coefficient in the effective coupling function between the scalar field and
conventional matter in the Einstein frame. By comparing the
Damour–Esposito-Far`ese and Mendes-Ortiz models of the scalar-tensor gravity,
we demonstrate that their distinct scalarization behaviors stem from whether
the effective coupling function is bounded. We also compute for scalarized NSs
with a highly relativistic dense core in scalar-tensor theories the moment of
inertia and tidal deformability that are relevant to pulsar-timing and
gravitational-wave experiments.
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