Selenophysical parameter inversion in the Lunar Southern Hemisphere Highland based on mutant particle swarm optimization

Zhong, Zhang; Yan, Jianguo; Jin, Shuanggen; Zhu, Min; Rodriguez, J. A. P.; Zhu, Huaqiang; Li, Yang

doi:10.1016/j.pepi.2019.05.001

Cited by 3 publications

(2 citation statements)

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“…It is important to note that Equation ( 8) is nonlinear, which can make parameter estimation challenging. The particle swarm optimization (PSO) method simulates the social behavior of birds, bees, or schools of fish, and performs well in solving nonlinear problems with multiple parameters [32]. We considered the PSO method to estimate the optimized parameters of Phobos.…”

Section: Theory and Methodsmentioning

confidence: 99%

The Mean Moment of Inertia for Irregularly Shaped Phobos and Its Application to the Constraint for the Two-Layer Interior Structure for the Martian Moon

et al. 2023

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The interior structure of Phobos has been the subject of debate in recent years, with the moment of inertia being a determining factor. To study this structure, we modeled Phobos with a two-layer structure and calculated its mean density and moment of inertia using updated gravity coefficients of degree-2 and forced libration amplitudes. By minimizing the misfit between modeled and derived moment of inertia, and observed and modeled mean density, we determined the frequency distribution for estimated parameters, including the core radius rc, core density ρc, and density ρm of the outer layer. Our results indicate that the optimized core radius is around 8.2 km for our models, along with a core density compromise of approximately 2500 kg·m−3, and an outer layer density of around 1400 kg·m−3. These values have remarkable sensitivity to the misfit function, implying a higher density likely inside Phobos compared to the outer layer. Given that the large core density was associated with ice content, it suggested that the fractional ice content in the outer layer is approximately 11% with a rock density of 2200 kg·m−3, while the content in the core is lower at 2.4% with a rock density of 3000 kg·m−3. The methodology introduced in this study can be further used to study the interior structure of irregularly shaped asteroids.

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Section: Theory and Methodsmentioning

confidence: 99%

The Mean Moment of Inertia for Irregularly Shaped Phobos and Its Application to the Constraint for the Two-Layer Interior Structure for the Martian Moon

et al. 2023

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“…Geometrically, the lunar crust is bounded by the high-resolution LOLA topography (Smith et al, 2010) and a crust-mantle interface (Wieczorek et al, 2013). Several regional (Liang et al, 2014;Jansen et al, 2017;Zhang et al, 2018;Zhao et al, 2019;Zhong et al, 2019) or global (Wieczorek et al, 2013;Han, 2013;Besserer et al, 2014;Wahl and Oberst, 2019) density maps have already been provided from LOLA and GRAIL. Here, we calculate independent bulk density for the lunar crust in three types of function: 1) a constant, 2) laterally variable, and 3) 3D spatially variable (assuming a linear change in the radial direction).…”

Section: Introductionmentioning

confidence: 99%