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As is well known, there are various mass limits for compact stars. Forexample, the maximum mass for non-rotating white dwarfs is given by the famousChandrasekhar limit about $1.4 M_\odot$ (solar masses). Although the mass limitfor neutron stars is not so clear to date, one of the widely accepted values isabout $2.1 M_\odot\,$. Recently, challenges to these mass limits appeared.Motivated by the super-Chandrasekhar mass white dwarfs with masses up to $2.4\sim 2.8 M_\odot\,$, and compact objects (probably neutron stars) in the massgap (from $2.5 M_\odot$ or $3 M_\odot$ to $5 M_\odot$) inferred fromgravitational waves detected by LIGO/Virgo in the third observing run (O3), wereconsider the mass limits for compact stars in the present work. Withoutinvoking strong magnetic field and/or exotic equation of state (EOS), we try toincrease the mass limits for compact stars in modified gravity theory. In thiswork, we propose an inverse chameleon mechanism, and show that the fifth-forcemediated by the scalar field can evade the severe tests on earth, in solarsystem and universe, but manifest itself in compact stars such as white dwarfsand neutron stars. The mass limits for compact stars in the inverse chameleonmechanism can be easily increased to $3 M_\odot\,$, $5 M_\odot$ or even larger.We argue that the inverse chameleon mechanism might be constrained by theobservations of exoplanets orbiting compact stars (such as white dwarfs andneutron stars), and gravitational waves from the last stage of binary compactstar coalescence.

Inverse Chameleon Mechanism and Mass Limits for Compact Stars