Estimation of surface temperatures on Mercury in preparation of the MERTIS experiment onboard BepiColombo

Bauch, Karin E.; Hiesinger, H.; Greenhagen, B. T.; Helbert, J.

doi:10.1016/j.icarus.2020.114083

Cited by 17 publications

(26 citation statements)

References 51 publications

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“…In fact, this is the first time that model temperatures on the complete polar MLA DTM are reported; this is especially of importance for temperatures at latitudes above ≈ 85 • N. In a previous study conducted during the ongoing MESSENGER mission, MLA tracks were still too sparse or they did not exist at these latitudes (Paige et al 2013). Other studies have concentrated on single craters or nonpolar regions (Hamill et al 2020;Bauch et al 2021). Due to the 3 : 2 spin-orbit resonance of Mercury, so-called hot (at 0 • E and 180 • E) and warm (at 90 • E and 270 • E) longitudes emerge (Siegler et al 2013).…”

Section: Resultsmentioning

confidence: 85%

Aspects of thermal modeling using digital terrain models

Gläser

2022

A&A

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Context. Our thermal model is adapted and extended in this study. Specifically the aspect of handling indirect radiation, the solar limb darkening effect, and depth profiles are addressed. Aims. Our goal is to improve the existing thermal model to handle terrain scattering and re-radiation in an adaptive way. In addition, we aim to change previously fixed and manually chosen discretization of the solar limb darkening effect and depth profile to be adaptive and applicable for various planets and purposes. Methods. The temperature was modeled based on digital terrain models (DTMs) using data of the Mercury Laser Altimeter (MLA). New implementations to handle terrain scattering and re-radiation were introduced using level-of-detail techniques. The solar disk was discretized into a variable number of rings and the depth profile was introduced as an exponential function for which the number of nodes and the maximum depth can be chosen. Results. We present results for the ideal window size and degree of level-of-detail for thermal studies of the Hermean north pole. Further we show that the previous discretization of the solar limb darkening effect proved insufficient for Mercury, and we updated the implementation accordingly. Similarly we improved the implementation for the depth profile. For the first time, we derived depthto-ice, as well as average and maximum temperature maps based on thermal modeling of the complete north polar MLA DTM.

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Section: Resultsmentioning

confidence: 85%

Aspects of thermal modeling using digital terrain models

Gläser

2022

A&A

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“…Global surface temperature maps were calculated based on initial data from MESSENGER MDIS albedo and topography data Becker et al 2016). Figure 13 shows the map of maximum surface temperatures superposed on the albedo map (Bauch et al 2020). The total range of temperatures in the covered latitude band is from 450 K to 700 K. Temperatures are highest at the equator at longitudes 0°W and 180°W.…”

Section: Thermal Modelingmentioning

confidence: 99%

“…Thus, the obtained spectral data are mixtures of these minerals and a non-linear deconvolution of the spectral data is necessary to quantify mineral abundances (Poulet and Erard 2004). First results with binary pyroxene and olivine mixtures show that it is possible to calculate the starting mixtures within a 3% deviation (Bauch et al , 2020Weber et al 2019.…”

Section: Data Deconvolutionmentioning

confidence: 99%

Studying the Composition and Mineralogy of the Hermean Surface with the Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) for the BepiColombo Mission: An Update

et al. 2020

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Launched onboard the BepiColombo Mercury Planetary Orbiter (MPO) in October 2018, the Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) is on its way to planet Mercury. MERTIS consists of a push-broom IR-spectrometer (TIS) and a radiometer (TIR), which operate in the wavelength regions of 7-14 μm and 7-40 μm, respectively. This wavelength region is characterized by several diagnostic spectral signatures: the Christiansen feature (CF), Reststrahlen bands (RB), and the Transparency feature (TF), which will allow us to identify and map rock-forming silicates, sulfides as well as other minerals. Thus, the instrument is particularly well-suited to study the mineralogy and composition of the hermean surface at a spatial resolution of about 500 m globally and better than 500 m for approximately 5-10% of the surface. The instrument is fully functional onboard the BepiColombo spacecraft and exceeds all requirements (e.g., mass, power, performance). To prepare for the science phase at Mercury, the team developed an innovative operations plan to maximize the scientific output while at the same time saving spacecraft resources (e.g., data downlink). The upcoming fly-bys will be excellent opportunities to further test and adapt our software and operational procedures. In summary, the team is undertaking action at multiple levels, including performing a comprehensive suite of spectroscopic measurements in our laboratories on relevant analog materials, performing extensive spectral modeling, examining space weathering effects, and modeling the thermal behavior of the hermean surface.

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“…at Aphelion. A special feature of Mercury is that the angular velocity of the orbit near the Perihelion slightly exceeds that of the rotation, which leads to a secondary sunrise (e.g., [66,68,70,71]). Against this background, the Moon is preferable for testing the plausibility of the thought model of an Earth in absence of its atmosphere.…”

Section: Me E ≅mentioning

confidence: 99%

“…It is therefore essential to expand the concept of solar climate in such a way that such a model artifact is generally excluded. Consequently, the soil heat flux has to be considered as well, as done, for instance, by Wesselink [62], Jaeger [63], Cremers et al [64], Mitchell and de Pater [65], Vasavada et al [58,66], Bauch et al [67,68], Hu et al [69], and Kramm et al [29].…”

Section: Introductionmentioning

confidence: 99%

On the Solar Climate of the Moon and the Resulting Surface Temperature Distribution

Kramm¹,

Mölders²,

Berger³

et al. 2022

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The solar climate of our Moon is analyzed using the results of numerical simulations and the recently released data of the Diviner Lunar Radiometer Experiment (DLRE) to assess (a) the resulting distribution of the surface temperature, (b) the related global mean surface temperature s T , and (c) the effective radiation temperature e T often considered as a proxy for s T of rocky planets and/or their natural satellites, where e T is based on the global radiation budget of the well-known "thought model" of the Earth in the absence of its atmosphere. Because the Moon consists of similar rocky material like the Earth, it comes close to this thought model. However, the Moon's astronomical features (e.g., obliquity, angular velocity of rotation, position relative to the disc of the solar system) differ from that of the Earth. Being tidally locked to the Earth, the Moon's orbit around the Sun shows additional variation as compared to the Earth's orbit. Since the astronomical parameters affect the solar climate, we predicted the Moon's orbit coordinates both relative to the Sun and the Earth for a period of 20 lunations starting May 24, 2009, 00:00 UT1 with the planetary and lunar ephemeris DE430 of the Jet Propulsion Laboratory of the California Institute of Technology. The results revealed a mean heliocentric distance for the Moon and Earth of 1.00124279 AU and 1.00166376 AU, respectively. The mean geocentric distance of the Moon was 384792 km. The synodic and draconic months deviated from their respective means in a range of −5.7 h to 6.9 h and ±3.4 h, respectively. The deviations of the anomalistic months from their mean range between −2.83 d and 0.97 d with the largest negative deviations occurring around the points of inflection in the curve that represents the departure of the Open Access slab e M T T , 0.743 ≅. The DLRE observations suggest that in the case of rocky planets and their natural satellites, the globally averaged surface temperature is notably lower than the effective radiation temperature. They differ by a factor that depends on the astronomical parameters especially on the angular velocity of rotation.

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Estimation of surface temperatures on Mercury in preparation of the MERTIS experiment onboard BepiColombo

Cited by 17 publications

References 51 publications

Aspects of thermal modeling using digital terrain models

Aspects of thermal modeling using digital terrain models

Studying the Composition and Mineralogy of the Hermean Surface with the Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) for the BepiColombo Mission: An Update

On the Solar Climate of the Moon and the Resulting Surface Temperature Distribution

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