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Elastic Planetoids
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PRE
AI
DOI：doi:10.3847/1538-4357/ade8ef.png)
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Abstract
En 中文
Modeling the internal structure of self-gravitating solid and liquid bodies presents a challenge, as existing approaches are often limited to either overly simplistic constant-density approximations or more complex numerical equations of state (EOSs). We present a detailed analysis of a tractable and physically motivated model for perfectly elastic, spherically symmetric self-gravitating bodies in hydrostatic equilibrium. The model employs a logarithmic equation of state (often referred to as a logotropic EOS) with a nonzero initial density and constant bulk modulus. Importantly, the scaling properties of the model allow all solutions to be derived from a single, universal solution of an ordinary differential equation, resembling the Lane–Emden and Chandrasekhar models. The model provides new insights into stability issues and reveals oscillatory asymptotic behavior in the mass–radius relation, including the existence of both a maximum mass and a maximum radius. We derive useful, simple analytical approximations for key properties, such as central overdensity, moment of inertia, binding energy, and gravitational potential, applicable to small, metallic bodies like asteroids and moons. These new approximations could aid future research, including space mining and the scientific characterization of small solar system bodies.
Keywords:
logotropic equation of state
self-gravitating bodies
hydrostatic equilibrium
mass-radius relation
small solar system bodies
Journal
IF:
5.4
Papers:
8.3W
Citations:
32.0W
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