Interior Structure, Composition, and Mineralogy of the Terrestrial Planets

Sohl, F.; Schubert, G.

doi:10.1016/b978-0-444-53802-4.00166-4

Cited by 26 publications

(3 citation statements)

References 386 publications

(526 reference statements)

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“…This profile results in a core mass fraction CMF = CRF 2 = 1/3. Regarding the constituents, we consider a mass composition with a 2:1 ratio of silicates (MgSiO 3 ) to iron [150], with an iron core and a rocky mantle, which is representative of the Earth. Note, however, that the composition can be substantially different, including iron planets and ice satellites.…”

Section: Jcap05(2022)042mentioning

confidence: 99%

Evaporation of dark matter from celestial bodies

Garani

Palomares‐Ruiz

2022

J. Cosmol. Astropart. Phys.

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Scatterings of galactic dark matter (DM) particles with the constituents of celestial bodies could result in their accumulation within these objects. Nevertheless, the finite temperature of the medium sets a minimum mass, the evaporation mass, that DM particles must have in order to remain trapped. DM particles below this mass are very likely to scatter to speeds higher than the escape velocity, so they would be kicked out of the capturing object and escape. Here, we compute the DM evaporation mass for all spherical celestial bodies in hydrostatic equilibrium, spanning the mass range [10-10 - 102] M⊙, for constant scattering cross sections and s-wave annihilations. We illustrate the critical importance of the exponential tail of the evaporation rate, which has not always been appreciated in recent literature, and obtain a robust result: for the geometric value of the scattering cross section and for interactions with nucleons, at the local galactic position, the DM evaporation mass for all spherical celestial bodies in hydrostatic equilibrium is approximately given by Ec/Tχ ∼ 30, where Ec is the escape energy of DM particles at the core of the object and Tχ is their temperature. In that case, the minimum value of the DM evaporation mass is obtained for super-Jupiters and brown dwarfs, m evap ≃ 0.7 GeV. For other values of the scattering cross section, the DM evaporation mass only varies by a factor smaller than three within the range 10-41 cm2 ≤ σp ≤ 10-31 cm2, where σp is the spin-independent DM-nucleon scattering cross section. Its dependence on parameters such as the galactic DM density and velocity, or the scattering and annihilation cross sections is only logarithmic, and details on the density and temperature profiles of celestial bodies have also a small impact.

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Section: Jcap05(2022)042mentioning

confidence: 99%

Evaporation of dark matter from celestial bodies

Garani

Palomares‐Ruiz

2022

J. Cosmol. Astropart. Phys.

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show abstract

“…This profile results in a core mass fraction CMF = CRF 2 = 1/3. Regarding the constituents, we consider a mass composition with a 2:1 ratio of silicates (MgSiO 3 ) to iron [149], with an iron core and a rocky mantle, which is representative of the Earth. Note, however, that the composition can be substantially different, including iron planets and ice satellites.…”

Section: Iii2 Planetary Bodiesmentioning

confidence: 99%

Evaporation of dark matter from celestial bodies

Garani,

Palomares-Ruiz

2021

Preprint

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Scatterings of galactic dark matter (DM) particles with the constituents of celestial bodies could result in their accumulation within these objects. Nevertheless, the finite temperature of the medium sets a minimum mass, the evaporation mass, that DM particles must have in order to remain trapped. DM particles below this mass are very likely to scatter to speeds higher than the escape velocity, so they would be kicked out of the capturing object and escape. Here, we compute the DM evaporation mass for all spherical celestial bodies in hydrostatic equilibrium, spanning the mass range [10 −10 − 10 2 ] M . We illustrate the critical importance of the exponential tail of the evaporation rate, which has not always been appreciated in recent literature, and obtain a robust result: for the geometric value of the scattering cross section and for interactions with nucleons, the DM evaporation mass for all spherical celestial bodies in hydrostatic equilibrium is approximately given by Ec/Tχ ∼ 30, where Ec is the escape energy of DM particles at the core of the object and Tχ is the DM temperature. The minimum value of the DM evaporation mass is obtained for super-Jupiters and brown dwarfs, mevap 0.7 GeV. For other values of the scattering cross section, the DM evaporation mass only varies by a factor of two or less within the range 10 −41 cm 2 ≤ σp ≤ 10 −31 cm 2 , where σp is the spin-independent DM-nucleon scattering cross section. Its dependence on parameters such as the local galactic DM density and velocity, or the scattering and annihilation cross sections is only logarithmic.

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“…The cooling model solves the global energy, entropy and mass balance equations that describe the long-term evolution of the core (e.g., Breuer & Moore, 2015;Nimmo, 2015). The core comprises a snow layer on the liquidus above a vigorously convecting core.…”

Section: 1029/2020je006492mentioning

confidence: 99%

A Joint Experimental‐Modeling Investigation of the Effect of Light Elements on Dynamos in Small Planets and Moons

2020

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We present a joint experimental‐modeling investigation of core cooling in small terrestrial bodies. Significant amounts of light elements (S, O, Mg, Si) may compose the metallic cores of terrestrial planets and moons. However, the effect of multiple light elements on transport properties, in particular, electrical resistivity and thermal conductivity, is not well constrained. Electrical experiments were conducted at 10 GPa and up to 1850 K on high‐purity powder mixtures in the Fe‐S‐O(±Mg, ±Si) systems using the multianvil apparatus and the four‐electrode technique. The sample compositions contained 5 wt.% S, up to 3 wt.% O, up to 2 wt.% Mg, and up to 1 wt.% Si. We observe that above the eutectic temperature, electrical resistivity is significantly sensitive to the nature and amount of light elements. For each composition, thermal conductivity‐temperature equations were estimated using the experimental electrical results and a modified Wiedemann‐Franz law. These equations were implemented in a thermochemical core cooling model to study the evolution of the dynamo. Modeling results suggest that bulk chemistry significantly affects the entropy available to power dynamo action during core cooling. In the case of Mars, the presence of oxygen would delay the dynamo cessation by up to 1 Gyr compared to an O‐free, Fe‐S core. Models with 3 wt% O can be reconciled with the inferred cessation time of the Martian dynamo if the core‐mantle boundary heat flow falls from >2 TW to ~0.1 TW in the first 0.5 Gyr following core formation.

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Interior Structure, Composition, and Mineralogy of the Terrestrial Planets

Cited by 26 publications

References 386 publications

Evaporation of dark matter from celestial bodies

Evaporation of dark matter from celestial bodies

Evaporation of dark matter from celestial bodies

A Joint Experimental‐Modeling Investigation of the Effect of Light Elements on Dynamos in Small Planets and Moons

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