The ancient martian lithospheric structure at Isidis Planitia

Zhong, Zhang; Yan, Jianguo; Liu, Xuefei; Chen, Shiguo; Fan, Guangxue; Cheng, Yang; Pang, Lei; Barriot, Jean‐Pierre

doi:10.1016/j.icarus.2021.114741

Cited by 5 publications

(22 citation statements)

References 37 publications

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“…In Zhong et al. (2022) work, the negative load ratio indicates a positive density anomaly within the crust (Figure 10b in Zhong et al., 2022), which is similar to the modeling of the mantle plug in our work. In Zhong et al.…”

Section: Discussionsupporting

confidence: 89%

“…Zhong et al. (2022) suggest two values of T e for the Isidis basin: 110 km (with a load ratio of −0.418 and crustal density >2,900 kg/m 3 ) and 55 km (with a load ratio of −0.786 and crustal density ∼2,665 kg/m 3 ). The results obtained in this study show that the good‐fit models are with T e > 100 km ( f ∼ 0) and T e ∼ 30 km ( f ∼ 3).…”

Section: Discussionmentioning

confidence: 99%

“…(2005) and Zhong et al. (2022), a parameter that indicates the relationship between the initial topography loading ( h i ) and the density variation loading is introduced as follows:

f=-\frac{{\increment}\rho B}{{\rho }_{c}{h}_{i}}

Substituting Equations to Equation , we have the density variation (

{\increment}\rho

) and post‐deflection CrMB relief ( m ) as (in spherical harmonics):

{\increment}\rho =-\frac{{\rho }_{c}f}{B}\left(\frac{1+\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)+\alpha {g}_{1}{\rho }_{c}}{1+\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)+f\alpha {g}_{3}{\rho }_{c}}h+\frac{\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)}{1+\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)+f\alpha {g}_{3}{\rho }_{c}}{m}_{i}\right)

m = \frac{(f α g_{3} ρ_{c} - α g_{1} ρ_{c})}{1 + α g_{2} ()(, ρ_{m} - ρ_{c}) + f α g_{3} ρ_{c}} h + \frac{(1 + f α g_{3} ρ_{c})}{1 + α g_{2} ()(, ρ_{m} - ρ)}

…”

Section: Model Descriptionmentioning

confidence: 95%

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Lithospheric Loading Model for Large Impact Basins Where a Mantle Plug Is Present

Deng

Zhong

et al. 2023

JGR Planets

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The thin elastic shell lithospheric model is widely used in the geophysical studies of terrestrial bodies (Turcotte et al., 1981). This model assumes that the planetary lithosphere is an elastic shell that deflects when mass-related loads are imposed. The magnitude of deflection depends on the applied loads and the physical properties of the lithosphere (such as elastic thickness). If this deflection causes a change in the relief on a density interface, it will produce a gravity anomaly. Therefore, deflection measurements can be made using gravity and topography data. The elastic thickness can be used to characterize the physical properties of the lithosphere (Watts, 2001), which are mainly influenced by the temperature structure and are therefore closely related to the evolution of the entire planet.The interpretation of gravity and topography data is usually performed in the spherical harmonic (SH) domain. Degree-dependent correlation and admittance (transfer function) between gravity and topography contain information about loads in the lithosphere. Various types of loading models have been proposed. The simplest loading

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Section: Discussionsupporting

confidence: 89%

Section: Discussionmentioning

confidence: 99%

“…(2005) and Zhong et al. (2022), a parameter that indicates the relationship between the initial topography loading ( h i ) and the density variation loading is introduced as follows:

f=-\frac{{\increment}\rho B}{{\rho }_{c}{h}_{i}}

Substituting Equations to Equation , we have the density variation (

{\increment}\rho

) and post‐deflection CrMB relief ( m ) as (in spherical harmonics):

{\increment}\rho =-\frac{{\rho }_{c}f}{B}\left(\frac{1+\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)+\alpha {g}_{1}{\rho }_{c}}{1+\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)+f\alpha {g}_{3}{\rho }_{c}}h+\frac{\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)}{1+\alpha {g}_{2}\left({\rho }_{m}-{\rho }_{c}\right)+f\alpha {g}_{3}{\rho }_{c}}{m}_{i}\right)

m = \frac{(f α g_{3} ρ_{c} - α g_{1} ρ_{c})}{1 + α g_{2} ()(, ρ_{m} - ρ_{c}) + f α g_{3} ρ_{c}} h + \frac{(1 + f α g_{3} ρ_{c})}{1 + α g_{2} ()(, ρ_{m} - ρ)}

…”

Section: Model Descriptionmentioning

confidence: 95%

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Lithospheric Loading Model for Large Impact Basins Where a Mantle Plug Is Present

Deng

Zhong

et al. 2023

JGR Planets

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“…The load ratio is sampled with an interval of 0.01 from −1 to 1. The normalized misfit (

\sigma

) for each parameter set is expressed with chi‐squared function (Ding et al., 2019; Zhong et al., 2022):

{\sigma }^{2}=\frac{1}{{L}_{\mathrm{max}}-{L}_{\mathrm{w}\mathrm{i}\mathrm{n}}+1}\sum\limits _{l={L}_{\mathrm{w}\mathrm{i}\mathrm{n}}}^{{L}_{\mathrm{max}}}{\left[\frac{{z}^{\mathrm{o}\mathrm{b}\mathrm{s}}(l)-{z}^{\mathrm{mod}}(l)}{{\sigma }_{z}(l)}\right]}^{2}

in which L max denotes the maximum degree to fit the admittance spectrum, and L win is the localized bandwidth ( L win = 10).

{z}^{\mathrm{o}\mathrm{b}\mathrm{s}}(l)

is the admittance function calculated by the gravity field model and topography data, and

{z}^{\mathrm{mod}}(l)

is the admittance function from the loading model.…”

Section: Methodsmentioning

confidence: 99%

Lithospheric Elastic Thickness Beneath the Caloris Basin: Implications for the Thermal Structure of Mercury

Deng

Zhong

et al. 2023

JGR Planets

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The basin interior is covered by the Caloris interior plains (CIP) that have been deformed by complex tectonic features (Denevi et al., 2018), including concentric ridges and tensional grabens that exhibit both radial and tangential strikes (Byrne et al., 2018). Both the northern and southern parts of the basin floor have been significantly uplifted to heights that exceed the basin rim (Figure 1c), and the two mountain belts have a trend that is more-or-less parallel to the east-northeast to west-southwest direction (Byrne et al., 2014).

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“…当前, 火星主要高阶重力场是JGMRO120d [8] 和GMM3-120 [7] , 这两个模型的最大展开阶次均为120阶次. 其中, JGMRO120d主要依据MRO 以及部分MGS的轨道跟踪数据求解而来, 被广泛应用于后续科学研究中 [15,16] , 目前数据更新后的模型为JGMRO120f [17] . GMM3-120除了参考MRO 和MGS的轨道跟踪数据外, 还参考了ODY的轨道跟踪数据.…”

Section: 火星平均密度和平均惯性矩因子unclassified

Constraining the size and density composition of the Martian core by using second-order potential coefficient and recent precession rate of gravity field model

Zhong¹,

Qi-Lin²,

Jiang³

2023

Acta Phys. Sin.

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Recently, it is yet difficult to detect the existence of Martian solid inner core merely based on Mars seismic InSight data. To deal with this problem, our study intends to use the mean density and mean moment of inertia factor to constrain the size and density of Martian solid inner core. Using Mars high-degree gravity field models JGMRO120f and GMM3-120, and considering the recent precession rate, we obtained the mean density and mean moment of inertia factor, which are treated as observed values. Referring to the 4-layers internal structure model of Mars, and considering the 4 parameters including crustal density, mantle density, density of outer core, size and density of inner core, we calculated the modeled values of the Martian mean density and the mean moment of inertia factor. From the minimum residuals between observed and modeled values of mean density as well as that of mean moment of inertia factor, it is found that the two gravity fields models have the same result of distribution of free parameters. As to the optimized values of the free parameters, the two gravity field models even have the same results. Furthermore, the optimized crustal density, mantel density and density of outer core approach other studies, indicating the dependence of our results. Finally, our result demonstrates that Mars likely has a solid inner core with a size close to 840 km, and the density of inner core is near to 6950 kg·m<sup>-3</sup>. Our result implies that Mars has an inner core not fully composed of pure iron, which is consistent with the recent study that Mars requires a substantial complement of light elements in Martian core. However, it is further needed to constrain the size and composition of Martian inner core due to the non-uniqueness of inversion results. With the improvement of processing technology on the InSight data, it can be further constrained for the size and composition of Martian inner core.

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The ancient martian lithospheric structure at Isidis Planitia

Cited by 5 publications

References 37 publications

Lithospheric Loading Model for Large Impact Basins Where a Mantle Plug Is Present

Lithospheric Loading Model for Large Impact Basins Where a Mantle Plug Is Present

Lithospheric Elastic Thickness Beneath the Caloris Basin: Implications for the Thermal Structure of Mercury

Constraining the size and density composition of the Martian core by using second-order potential coefficient and recent precession rate of gravity field model

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