反变色龙机制与致密星的质量极限
Inverse Chameleon Mechanism and Mass Limits for Compact Stars
摘要：
众所周知，致密星有各种质量极限。例如，不旋转的白矮星的最大质量是由著名的关于$1.4 M_\odot$（太阳质量）的克拉塞卡极限给出的。虽然中子星的质量极限到目前为止还不是很清楚，但一个被广泛接受的值是大约$2.1 M_\odot\,$。最近，出现了对这些质量限制的挑战。基于LIGO/Virgo在第三次（O3）观测中探测到的质量高达$2.4 \sim 2.8 M_\odot\,$的超Bracrasekhar质量白矮星和质量间隙（从$2.5 M_\odot$或$3 M_\odot$到$5 M_\odot$）中的致密天体（可能是中子星），我们重新考虑了致密星的质量极限。在不引入强磁场和奇异状态方程的情况下，我们试图在修正的引力理论中提高致密星的质量极限。本文提出了一种逆变色龙机制，并证明了标量场介导的第五种力可以避开地球、太阳系和宇宙中的严峻考验，而在白矮星和中子星等致密恒星中表现出来。在逆变色龙机制中，致密星的质量极限可以很容易地增加到$3 M_\odot\,$、$5 M_\odot$甚至更大。我们认为，逆变色龙机制可能会受到系外行星的观测，轨道紧凑的恒星（如白矮星和中子星），和引力波的最后阶段的致密双星合并。
英文摘要：
As is well known, there are various mass limits for compact stars. For example, the maximum mass for non-rotating white dwarfs is given by the famous Chandrasekhar limit about $1.4 M_\odot$ (solar masses). Although the mass limit for neutron stars is not so clear to date, one of the widely accepted values is about $2.1 M_\odot\,$. 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 mass gap (from $2.5 M_\odot$ or $3 M_\odot$ to $5 M_\odot$) inferred from gravitational waves detected by LIGO/Virgo in the third observing run (O3), we reconsider the mass limits for compact stars in the present work. Without invoking strong magnetic field and/or exotic equation of state (EOS), we try to increase the mass limits for compact stars in modified gravity theory. In this work, we propose an inverse chameleon mechanism, and show that the fifth-force mediated by the scalar field can evade the severe tests on earth, in solar system and universe, but manifest itself in compact stars such as white dwarfs and neutron stars. The mass limits for compact stars in the inverse chameleon mechanism 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 the observations of exoplanets orbiting compact stars (such as white dwarfs and neutron stars), and gravitational waves from the last stage of binary compact star coalescence.
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