Scalarization occurs across most of the parameter space for negative coupling parameter β_d in self-interacting dark matter stars, over a broader range than in conventional neutron stars.
Chameleon dark matter stars
1 Pith paper cite this work. Polarity classification is still indexing.
1
Pith paper citing it
abstract
We consider static, spherically symmetric equilibrium configurations consisting of fermionic dark matter nonminimally coupled to dark energy in the form of a quintessence scalar field. With the scalar field coupling function, the form of which is taken to meet cosmological observations, we estimate the effect of such a nonminimal coupling on the properties of dark matter compact configurations. We show that the masses and sizes of the resulting chameleon dark matter stars are smaller than those of systems with no field present.
fields
gr-qc 1years
2026 1verdicts
UNVERDICTED 1representative citing papers
citing papers explorer
-
Scalarization of dark matter stars
Scalarization occurs across most of the parameter space for negative coupling parameter β_d in self-interacting dark matter stars, over a broader range than in conventional neutron stars.