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Höning D, Spohn T. Land Fraction Diversity on Earth-like Planets and Implications for Their Habitability. Astrobiology 2023; 23:372-394. [PMID: 36848252 DOI: 10.1089/ast.2022.0070] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/18/2023]
Abstract
A balanced ratio of ocean to land is believed to be essential for an Earth-like biosphere, and one may conjecture that plate-tectonics planets should be similar in geological properties. After all, the volume of continental crust evolves toward an equilibrium between production and erosion. If the interior thermal states of Earth-sized exoplanets are similar to those of Earth-a straightforward assumption due to the temperature dependence of mantle viscosity-one might expect a similar equilibrium between continental production and erosion to establish, and hence a similar land fraction. We show that this conjecture is not likely to be true. Positive feedback associated with the coupled mantle water-continental crust cycle may rather lead to a manifold of three possible planets, depending on their early history: a land planet, an ocean planet, and a balanced Earth-like planet. In addition, thermal blanketing of the interior by the continents enhances the sensitivity of continental growth to its history and, eventually, to initial conditions. Much of the blanketing effect is, however, compensated by mantle depletion in radioactive elements. A model of the long-term carbonate-silicate cycle shows the land and the ocean planets to differ by about 5 K in average surface temperature. A larger continental surface fraction results both in higher weathering rates and enhanced outgassing, partly compensating each other. Still, the land planet is expected to have a substantially dryer, colder, and harsher climate possibly with extended cold deserts in comparison with the ocean planet and with the present-day Earth. Using a model of balancing water availability and nutrients from continental crust weathering, we find the bioproductivity and the biomass of both the land and ocean planets to be reduced by a third to half of those of Earth. The biosphere on these planets might not be substantial enough to produce a supply of free oxygen.
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Affiliation(s)
- Dennis Höning
- Potsdam-Institute for Climate Impact Research, Potsdam, Germany
| | - Tilman Spohn
- International Space Science Institute, Bern, Switzerland
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2
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Spohn T, Hudson TL, Marteau E, Golombek M, Grott M, Wippermann T, Ali KS, Schmelzbach C, Kedar S, Hurst K, Trebi-Ollennu A, Ansan V, Garvin J, Knollenberg J, Müller N, Piqueux S, Lichtenheldt R, Krause C, Fantinati C, Brinkman N, Sollberger D, Delage P, Vrettos C, Reershemius S, Wisniewski L, Grygorczuk J, Robertsson J, Edme P, Andersson F, Krömer O, Lognonné P, Giardini D, Smrekar SE, Banerdt WB. The InSight HP 3 Penetrator (Mole) on Mars: Soil Properties Derived from the Penetration Attempts and Related Activities. Space Sci Rev 2022; 218:72. [PMID: 36514324 PMCID: PMC9734249 DOI: 10.1007/s11214-022-00941-z] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/03/2021] [Accepted: 11/26/2022] [Indexed: 06/17/2023]
Abstract
UNLABELLED The NASA InSight Lander on Mars includes the Heat Flow and Physical Properties Package HP3 to measure the surface heat flow of the planet. The package uses temperature sensors that would have been brought to the target depth of 3-5 m by a small penetrator, nicknamed the mole. The mole requiring friction on its hull to balance remaining recoil from its hammer mechanism did not penetrate to the targeted depth. Instead, by precessing about a point midway along its hull, it carved a 7 cm deep and 5-6 cm wide pit and reached a depth of initially 31 cm. The root cause of the failure - as was determined through an extensive, almost two years long campaign - was a lack of friction in an unexpectedly thick cohesive duricrust. During the campaign - described in detail in this paper - the mole penetrated further aided by friction applied using the scoop at the end of the robotic Instrument Deployment Arm and by direct support by the latter. The mole tip finally reached a depth of about 37 cm, bringing the mole back-end 1-2 cm below the surface. It reversed its downward motion twice during attempts to provide friction through pressure on the regolith instead of directly with the scoop to the mole hull. The penetration record of the mole was used to infer mechanical soil parameters such as the penetration resistance of the duricrust of 0.3-0.7 MPa and a penetration resistance of a deeper layer ( > 30 cm depth) of 4.9 ± 0.4 MPa . Using the mole's thermal sensors, thermal conductivity and diffusivity were measured. Applying cone penetration theory, the resistance of the duricrust was used to estimate a cohesion of the latter of 2-15 kPa depending on the internal friction angle of the duricrust. Pushing the scoop with its blade into the surface and chopping off a piece of duricrust provided another estimate of the cohesion of 5.8 kPa. The hammerings of the mole were recorded by the seismometer SEIS and the signals were used to derive P-wave and S-wave velocities representative of the topmost tens of cm of the regolith. Together with the density provided by a thermal conductivity and diffusivity measurement using the mole's thermal sensors, the elastic moduli were calculated from the seismic velocities. Using empirical correlations from terrestrial soil studies between the shear modulus and cohesion, the previous cohesion estimates were found to be consistent with the elastic moduli. The combined data were used to derive a model of the regolith that has an about 20 cm thick duricrust underneath a 1 cm thick unconsolidated layer of sand mixed with dust and above another 10 cm of unconsolidated sand. Underneath the latter, a layer more resistant to penetration and possibly containing debris from a small impact crater is inferred. The thermal conductivity increases from 14 mW/m K to 34 mW/m K through the 1 cm sand/dust layer, keeps the latter value in the duricrust and the sand layer underneath and then increases to 64 mW/m K in the sand/gravel layer below. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-022-00941-z.
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Affiliation(s)
- T. Spohn
- International Space Science Institute, Hallerstrasse 6, 3012 Bern, Switzerland
- DLR Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany
| | - T. L. Hudson
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - E. Marteau
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - M. Golombek
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - M. Grott
- DLR Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany
| | - T. Wippermann
- DLR Institute of Space Systems, Robert-Hooke-Str. 7, 28359 Bremen, Germany
| | - K. S. Ali
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - C. Schmelzbach
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | - S. Kedar
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - K. Hurst
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - A. Trebi-Ollennu
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - V. Ansan
- Laboratoire de Planétologie et Géodynamique de Nantes, Université de Nantes, 44322 Nantes, France
| | - J. Garvin
- NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 USA
| | - J. Knollenberg
- DLR Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany
| | - N. Müller
- DLR Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany
| | - S. Piqueux
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - R. Lichtenheldt
- DLR Institute of System Dynamics and Control, Münchener Strasse 20, 82234 Wessling, Germany
| | - C. Krause
- DLR MUSC Space Operations and Astronaut Training, Linder Höhe, 51147 Köln, Germany
| | - C. Fantinati
- DLR MUSC Space Operations and Astronaut Training, Linder Höhe, 51147 Köln, Germany
| | - N. Brinkman
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | - D. Sollberger
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | - P. Delage
- École nationale des ponts et chaussées, Laboratoire Navier, Paris, France
| | - C. Vrettos
- Department of Civil Engineering, University of Kaiserslautern, Kaiserslautern, Germany
| | - S. Reershemius
- DLR Institute of Space Systems, Robert-Hooke-Str. 7, 28359 Bremen, Germany
| | - L. Wisniewski
- Astronika Sp. z o.o., ul. Bartycka 18, 00-716 Warszawa, Poland
| | - J. Grygorczuk
- Astronika Sp. z o.o., ul. Bartycka 18, 00-716 Warszawa, Poland
| | - J. Robertsson
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | - P. Edme
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | - F. Andersson
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | | | - P. Lognonné
- Institut du Physique du Globe Paris, CNRS, Université Paris Cité, Paris, France
| | - D. Giardini
- Department of Earth Sciences, ETH Zürich, Institute of Geophysics, CH-8092 Zürich, Switzerland
| | - S. E. Smrekar
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
| | - W. B. Banerdt
- Jet Propulsion Laboratory, California Institute of Technology, Oak Grove Drive, Pasadena, CA 91109 USA
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3
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Brinkman N, Schmelzbach C, Sollberger D, Pierick JT, Edme P, Haag T, Kedar S, Hudson T, Andersson F, van Driel M, Stähler S, Nicollier T, Robertsson J, Giardini D, Spohn T, Krause C, Grott M, Knollenberg J, Hurst K, Rochas L, Vallade J, Blandin S, Lognonné P, Pike WT, Banerdt WB. In Situ Regolith Seismic Velocity Measurement at the InSight Landing Site on Mars. J Geophys Res Planets 2022; 127:e2022JE007229. [PMID: 36582924 PMCID: PMC9787532 DOI: 10.1029/2022je007229] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 02/02/2022] [Revised: 07/15/2022] [Accepted: 09/15/2022] [Indexed: 06/17/2023]
Abstract
Interior exploration using Seismic Investigations, Geodesy and Heat Transport's (InSight) seismometer package Seismic Experiment for Interior Structure (SEIS) was placed on the surface of Mars at about 1.2 m distance from the thermal properties instrument Heat flow and Physical Properties Package (HP3) that includes a self-hammering probe. Recording the hammering noise with SEIS provided a unique opportunity to estimate the seismic wave velocities of the shallow regolith at the landing site. However, the value of studying the seismic signals of the hammering was only realized after critical hardware decisions were already taken. Furthermore, the design and nominal operation of both SEIS and HP3 are nonideal for such high-resolution seismic measurements. Therefore, a series of adaptations had to be implemented to operate the self-hammering probe as a controlled seismic source and SEIS as a high-frequency seismic receiver including the design of a high-precision timing and an innovative high-frequency sampling workflow. By interpreting the first-arriving seismic waves as a P-wave and identifying first-arriving S-waves by polarization analysis, we determined effective P- and S-wave velocities of v P = 11 9 - 21 + 45 m/s and v S = 6 3 - 7 + 11 m/s, respectively, from around 2,000 hammer stroke recordings. These velocities likely represent bulk estimates for the uppermost several 10s of cm of regolith. An analysis of the P-wave incidence angles provided an independent v P /v S ratio estimate of 1.8 4 - 0.35 + 0.89 that compares well with the traveltime based estimate of 1.8 6 - 0.25 + 0.42 . The low seismic velocities are consistent with those observed for low-density unconsolidated sands and are in agreement with estimates obtained by other methods.
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Affiliation(s)
| | | | | | | | - Pascal Edme
- Institute of GeophysicsETH ZürichZürichSwitzerland
| | - Thomas Haag
- Institute of GeophysicsETH ZürichZürichSwitzerland
| | - Sharon Kedar
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Troy Hudson
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | | | | | | | | | - Tilman Spohn
- Deutsches Zentrum für Luft‐ und Raumfahrt (DLR)BremenGermany
- International Space Science InstituteBernSwitzerland
| | | | - Matthias Grott
- Deutsches Zentrum für Luft‐ und Raumfahrt (DLR)BremenGermany
| | | | - Ken Hurst
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Ludovic Rochas
- Centre National des Études Spatiales (CNES)ToulouseFrance
| | - Julien Vallade
- Centre National des Études Spatiales (CNES)ToulouseFrance
| | - Steve Blandin
- Centre National des Études Spatiales (CNES)ToulouseFrance
| | - Philippe Lognonné
- Université Paris CitéInstitut de physique du globe de ParisCNRSParisFrance
| | | | - W. Bruce Banerdt
- NASA Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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4
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Sollberger D, Schmelzbach C, Andersson F, Robertsson JOA, Brinkman N, Kedar S, Banerdt WB, Clinton J, van Driel M, Garcia R, Giardini D, Grott M, Haag T, Hudson TL, Lognonné P, Pierick JT, Pike W, Spohn T, Stähler SC, Zweifel P. A Reconstruction Algorithm for Temporally Aliased Seismic Signals Recorded by the InSight Mars Lander. Earth Space Sci 2021; 8:e2020EA001234. [PMID: 34595325 PMCID: PMC8459272 DOI: 10.1029/2020ea001234] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/20/2020] [Revised: 05/31/2021] [Accepted: 06/18/2021] [Indexed: 06/13/2023]
Abstract
In December 2018, the NASA InSight lander successfully placed a seismometer on the surface of Mars. Alongside, a hammering device was deployed at the landing site that penetrated into the ground to attempt the first measurements of the planetary heat flow of Mars. The hammering of the heat probe generated repeated seismic signals that were registered by the seismometer and can potentially be used to image the shallow subsurface just below the lander. However, the broad frequency content of the seismic signals generated by the hammering extends beyond the Nyquist frequency governed by the seismometer's sampling rate of 100 samples per second. Here, we propose an algorithm to reconstruct the seismic signals beyond the classical sampling limits. We exploit the structure in the data due to thousands of repeated, only gradually varying hammering signals as the heat probe slowly penetrates into the ground. In addition, we make use of the fact that repeated hammering signals are sub-sampled differently due to the unsynchronized timing between the hammer strikes and the seismometer recordings. This allows us to reconstruct signals beyond the classical Nyquist frequency limit by enforcing a sparsity constraint on the signal in a modified Radon transform domain. In addition, the proposed method reduces uncorrelated noise in the recorded data. Using both synthetic data and actual data recorded on Mars, we show how the proposed algorithm can be used to reconstruct the high-frequency hammering signal at very high resolution.
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Affiliation(s)
| | | | | | | | | | - Sharon Kedar
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - William B. Banerdt
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - John Clinton
- Institute of GeophysicsETH ZürichZürichSwitzerland
| | | | - Raphael Garcia
- Institut Supérieur de l'Aéronautique et de l'Espace SUPAEROToulouseFrance
| | | | | | - Thomas Haag
- Institute of GeophysicsETH ZürichZürichSwitzerland
| | - Troy L. Hudson
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Philippe Lognonné
- Université de ParisInstitut de Physique du globe de ParisCNRSParisFrance
| | | | - William Pike
- Department of Electrical and Electronic EngineeringImperial College LondonSouth Kensington CampusLondonUK
| | - Tilman Spohn
- DLR Institute of Planetary ResearchBerlinGermany
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5
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Piqueux S, Müller N, Grott M, Siegler M, Millour E, Forget F, Lemmon M, Golombek M, Williams N, Grant J, Warner N, Ansan V, Daubar I, Knollenberg J, Maki J, Spiga A, Banfield D, Spohn T, Smrekar S, Banerdt B. Soil Thermophysical Properties Near the InSight Lander Derived From 50 Sols of Radiometer Measurements. J Geophys Res Planets 2021; 126:e2021JE006859. [PMID: 35845552 PMCID: PMC9285084 DOI: 10.1029/2021je006859] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/21/2021] [Revised: 04/12/2021] [Accepted: 04/19/2021] [Indexed: 06/11/2023]
Abstract
Measurements from the InSight lander radiometer acquired after landing are used to characterize the thermophysical properties of the Martian soil in Homestead hollow. This data set is unique as it stems from a high measurement cadence fixed platform studying a simple well-characterized surface, and it benefits from the environmental characterization provided by other instruments. We focus on observations acquired before the arrival of a regional dust storm (near Sol 50), on the furthest observed patch of soil (i.e., ∼3.5 m away from the edge of the lander deck) where temperatures are least impacted by the presence of the lander and where the soil has been least disrupted during landing. Diurnal temperature cycles are fit using a homogenous soil configuration with a thermal inertia of 183 ± 25 J m-2 K-1 s-1/2 and an albedo of 0.16, corresponding to very fine to fine sand with the vast majority of particles smaller than 140 μm. A pre-landing assessment leveraging orbital thermal infrared data is consistent with these results, but our analysis of the full diurnal temperature cycle acquired from the ground further indicates that near surface layers with different thermophysical properties must be thin (i.e., typically within the top few mm) and deep layering with different thermophysical properties must be at least below ∼4 cm. The low thermal inertia value indicates limited soil cementation within the upper one or two skin depths (i.e., ∼4-8 cm and more), with cement volumes <<1%, which is challenging to reconcile with visible images of overhangs in pits.
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Affiliation(s)
- Sylvain Piqueux
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Nils Müller
- DLR Institute for Planetary ResearchBerlinGermany
| | | | | | | | | | | | - Matthew Golombek
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Nathan Williams
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - John Grant
- National Air and Space MuseumSmithsonian InstitutionWashingtonDCUSA
| | | | | | | | | | - Justin Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | - Tilman Spohn
- DLR Institute for Planetary ResearchBerlinGermany
- International Space Science Institute ISSIBernSwitzerland
| | - Susan Smrekar
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Bruce Banerdt
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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6
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Khan A, Ceylan S, van Driel M, Giardini D, Lognonné P, Samuel H, Schmerr NC, Stähler SC, Duran AC, Huang Q, Kim D, Broquet A, Charalambous C, Clinton JF, Davis PM, Drilleau M, Karakostas F, Lekic V, McLennan SM, Maguire RR, Michaut C, Panning MP, Pike WT, Pinot B, Plasman M, Scholz JR, Widmer-Schnidrig R, Spohn T, Smrekar SE, Banerdt WB. Upper mantle structure of Mars from InSight seismic data. Science 2021; 373:434-438. [PMID: 34437116 DOI: 10.1126/science.abf2966] [Citation(s) in RCA: 54] [Impact Index Per Article: 18.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/21/2020] [Accepted: 05/14/2021] [Indexed: 11/03/2022]
Abstract
For 2 years, the InSight lander has been recording seismic data on Mars that are vital to constrain the structure and thermochemical state of the planet. We used observations of direct (P and S) and surface-reflected (PP, PPP, SS, and SSS) body-wave phases from eight low-frequency marsquakes to constrain the interior structure to a depth of 800 kilometers. We found a structure compatible with a low-velocity zone associated with a thermal lithosphere much thicker than on Earth that is possibly related to a weak S-wave shadow zone at teleseismic distances. By combining the seismic constraints with geodynamic models, we predict that, relative to the primitive mantle, the crust is more enriched in heat-producing elements by a factor of 13 to 20. This enrichment is greater than suggested by gamma-ray surface mapping and has a moderate-to-elevated surface heat flow.
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Affiliation(s)
- Amir Khan
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland. .,Physik-Institut, University of Zürich, Zürich, Switzerland
| | - Savas Ceylan
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland
| | - Martin van Driel
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland.,Mondaic AG, Zypressenstrasse 82, 8004 Zürich, Switzerland
| | | | - Philippe Lognonné
- Université de Paris, Institut de Physique du Globe de Paris, CNRS, Paris, France
| | - Henri Samuel
- Université de Paris, Institut de Physique du Globe de Paris, CNRS, Paris, France
| | | | | | - Andrea C Duran
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland
| | - Quancheng Huang
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Doyeon Kim
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Adrien Broquet
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.,Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France
| | | | - John F Clinton
- Swiss Seismological Service, ETH Zürich, Zürich, Switzerland
| | - Paul M Davis
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA, USA
| | - Mélanie Drilleau
- Institut Supérieur de l'Aéronautique et de l'Espace SUPAERO, Toulouse, France
| | - Foivos Karakostas
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Vedran Lekic
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Scott M McLennan
- Department of Geosciences, Stony Brook University, Stony Brook, NY, USA
| | - Ross R Maguire
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Chloé Michaut
- Institut Universitaire de France, Paris, France.,Laboratoire de Géologie, Terre, Planétes, Environnement, Lyon, France
| | - Mark P Panning
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - William T Pike
- Department of Electrical and Electronic Engineering, Imperial College London, London, UK
| | - Baptiste Pinot
- Institut Supérieur de l'Aéronautique et de l'Espace SUPAERO, Toulouse, France
| | - Matthieu Plasman
- Université de Paris, Institut de Physique du Globe de Paris, CNRS, Paris, France
| | | | | | - Tilman Spohn
- International Space Science Institute, Bern, Switzerland
| | - Suzanne E Smrekar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - William B Banerdt
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
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7
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Boehnhardt H, Bibring JP, Apathy I, Auster HU, Ercoli Finzi A, Goesmann F, Klingelhöfer G, Knapmeyer M, Kofman W, Krüger H, Mottola S, Schmidt W, Seidensticker K, Spohn T, Wright I. The Philae lander mission and science overview. Philos Trans A Math Phys Eng Sci 2017; 375:rsta.2016.0248. [PMID: 28554970 PMCID: PMC5454222 DOI: 10.1098/rsta.2016.0248] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 01/12/2017] [Indexed: 05/25/2023]
Abstract
The Philae lander accomplished the first soft landing and the first scientific experiments of a human-made spacecraft on the surface of a comet. Planned, expected and unexpected activities and events happened during the descent, the touch-downs, the hopping across and the stay and operations on the surface. The key results were obtained during 12-14 November 2014, at 3 AU from the Sun, during the 63 h long period of the descent and of the first science sequence on the surface. Thereafter, Philae went into hibernation, waking up again in late April 2015 with subsequent communication periods with Earth (via the orbiter), too short to enable new scientific activities. The science return of the mission comes from eight of the 10 instruments on-board and focuses on morphological, thermal, mechanical and electrical properties of the surface as well as on the surface composition. It allows a first characterization of the local environment of the touch-down and landing sites. Unique conclusions on the organics in the cometary material, the nucleus interior, the comet formation and evolution became available through measurements of the Philae lander in the context of the Rosetta mission.This article is part of the themed issue 'Cometary science after Rosetta'.
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Affiliation(s)
- Hermann Boehnhardt
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | | | - Istvan Apathy
- Atomic Energy Research Institute, PO Box 49, 1525 Budapest, Hungary
| | - Hans Ulrich Auster
- Institute for Geophysics and Extraterrestrial Physics, Technical University Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany
| | | | - Fred Goesmann
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Göstar Klingelhöfer
- Institute for Inorganic and Analytical Chemistry, Johannes Gutenberg University, Staudinger Weg 9, 55099 Mainz, Germany
| | - Martin Knapmeyer
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstr. 2, 12489 Berlin, Germany
| | - Wlodek Kofman
- UGA-Grenoble CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble, UMR 5274, 38058 Grenoble, France
| | - Harald Krüger
- Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Stefano Mottola
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstr. 2, 12489 Berlin, Germany
| | - Walter Schmidt
- Space Research Division, Finnish Meteorological Institute, 00560 Helsinki, Finland
| | - Klaus Seidensticker
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstr. 2, 12489 Berlin, Germany
| | - Tilman Spohn
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstr. 2, 12489 Berlin, Germany
| | - Ian Wright
- Planetary and Space Science Research Institute, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
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Dehant V, Asael D, Baland RM, Baludikay BK, Beghin J, Belza J, Beuthe M, Breuer D, Chernonozhkin S, Claeys P, Cornet Y, Cornet L, Coyette A, Debaille V, Delvigne C, Deproost MH, De WInter N, Duchemin C, El Atrassi F, François C, De Keyser J, Gillmann C, Gloesener E, Goderis S, Hidaka Y, Höning D, Huber M, Hublet G, Javaux EJ, Karatekin Ö, Kodolanyi J, Revilla LL, Maes L, Maggiolo R, Mattielli N, Maurice M, McKibbin S, Morschhauser A, Neumann W, Noack L, Pham LBS, Pittarello L, Plesa AC, Rivoldini A, Robert S, Rosenblatt P, Spohn T, Storme JY, Tosi N, Trinh A, Valdes M, Vandaele AC, Vanhaecke F, Van Hoolst T, Van Roosbroek N, Wilquet V, Yseboodt M. PLANET TOPERS: Planets, Tracing the Transfer, Origin, Preservation, and Evolution of their ReservoirS. ORIGINS LIFE EVOL B 2016; 46:369-384. [PMID: 27337974 DOI: 10.1007/s11084-016-9488-z] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/15/2015] [Accepted: 01/21/2016] [Indexed: 11/25/2022]
Abstract
The Interuniversity Attraction Pole (IAP) 'PLANET TOPERS' (Planets: Tracing the Transfer, Origin, Preservation, and Evolution of their Reservoirs) addresses the fundamental understanding of the thermal and compositional evolution of the different reservoirs of planetary bodies (core, mantle, crust, atmosphere, hydrosphere, cryosphere, and space) considering interactions and feedback mechanisms. Here we present the first results after 2 years of project work.
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Affiliation(s)
- V Dehant
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium.
| | - D Asael
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - R M Baland
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | | | - J Beghin
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - J Belza
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
- Universiteit Ghent (Ughent), Ghent, Belgium
| | - M Beuthe
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - D Breuer
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | | | - Ph Claeys
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - Y Cornet
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - L Cornet
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - A Coyette
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - V Debaille
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - C Delvigne
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - M H Deproost
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - N De WInter
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - C Duchemin
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - F El Atrassi
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - C François
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - J De Keyser
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - C Gillmann
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - E Gloesener
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - S Goderis
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - Y Hidaka
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - D Höning
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - M Huber
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - G Hublet
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - E J Javaux
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - Ö Karatekin
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - J Kodolanyi
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | | | - L Maes
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - R Maggiolo
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - N Mattielli
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - M Maurice
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - S McKibbin
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - A Morschhauser
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - W Neumann
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - L Noack
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - L B S Pham
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - L Pittarello
- Vrije Universiteit Brussel (VUB), Brussels, Belgium
| | - A C Plesa
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - A Rivoldini
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - S Robert
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - P Rosenblatt
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - T Spohn
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - J -Y Storme
- Université de Liège (Ulg), 4000, Liège 1, Belgium
| | - N Tosi
- Deutsche Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - A Trinh
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | - M Valdes
- Université Libre de Bruxelles (ULB), Brussels, Belgium
| | - A C Vandaele
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | | | - T Van Hoolst
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
| | | | - V Wilquet
- Belgian Institute for Space Aeronomy (BISA), Brussels, Belgium
| | - M Yseboodt
- Royal Observatory of Belgium (ROB), 3 Avenue Circulaire, B-1180, Brussels, Belgium
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Spohn T, Knollenberg J, Ball AJ, Banaszkiewicz M, Benkhoff J, Grott M, Grygorczuk J, Hüttig C, Hagermann A, Kargl G, Kaufmann E, Kömle N, Kührt E, Kossacki KJ, Marczewski W, Pelivan I, Schrödter R, Seiferlin K. COMETARY SCIENCE. Thermal and mechanical properties of the near-surface layers of comet 67P/Churyumov-Gerasimenko. Science 2015; 349:aab0464. [PMID: 26228152 DOI: 10.1126/science.aab0464] [Citation(s) in RCA: 145] [Impact Index Per Article: 16.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Thermal and mechanical material properties determine comet evolution and even solar system formation because comets are considered remnant volatile-rich planetesimals. Using data from the Multipurpose Sensors for Surface and Sub-Surface Science (MUPUS) instrument package gathered at the Philae landing site Abydos on comet 67P/Churyumov-Gerasimenko, we found the diurnal temperature to vary between 90 and 130 K. The surface emissivity was 0.97, and the local thermal inertia was 85 ± 35 J m(-2) K(-1)s(-1/2). The MUPUS thermal probe did not fully penetrate the near-surface layers, suggesting a local resistance of the ground to penetration of >4 megapascals, equivalent to >2 megapascal uniaxial compressive strength. A sintered near-surface microporous dust-ice layer with a porosity of 30 to 65% is consistent with the data.
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Affiliation(s)
- T Spohn
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany.
| | - J Knollenberg
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - A J Ball
- European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Noordwijk, Netherlands
| | | | - J Benkhoff
- European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Noordwijk, Netherlands
| | - M Grott
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | | | - C Hüttig
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - A Hagermann
- Department of Physical Sciences, The Open University, Milton Keynes, UK
| | - G Kargl
- Space Research Institute, Austrian Academy of Sciences Graz, Austria
| | - E Kaufmann
- Department of Physical Sciences, The Open University, Milton Keynes, UK
| | - N Kömle
- Space Research Institute, Austrian Academy of Sciences Graz, Austria
| | - E Kührt
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - K J Kossacki
- Faculty of Physics, University of Warsaw, Warsaw, Poland
| | | | - I Pelivan
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - R Schrödter
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - K Seiferlin
- Physics Institute, University of Berne, Berne, Switzerland
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Biele J, Ulamec S, Maibaum M, Roll R, Witte L, Jurado E, Muñoz P, Arnold W, Auster HU, Casas C, Faber C, Fantinati C, Finke F, Fischer HH, Geurts K, Güttler C, Heinisch P, Herique A, Hviid S, Kargl G, Knapmeyer M, Knollenberg J, Kofman W, Kömle N, Kührt E, Lommatsch V, Mottola S, Pardo de Santayana R, Remetean E, Scholten F, Seidensticker KJ, Sierks H, Spohn T. COMETARY SCIENCE. The landing(s) of Philae and inferences about comet surface mechanical properties. Science 2015; 349:aaa9816. [PMID: 26228158 DOI: 10.1126/science.aaa9816] [Citation(s) in RCA: 190] [Impact Index Per Article: 21.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Philae lander, part of the Rosetta mission to investigate comet 67P/Churyumov-Gerasimenko, was delivered to the cometary surface in November 2014. Here we report the precise circumstances of the multiple landings of Philae, including the bouncing trajectory and rebound parameters, based on engineering data in conjunction with operational instrument data. These data also provide information on the mechanical properties (strength and layering) of the comet surface. The first touchdown site, Agilkia, appears to have a granular soft surface (with a compressive strength of 1 kilopascal) at least ~20 cm thick, possibly on top of a more rigid layer. The final landing site, Abydos, has a hard surface.
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Affiliation(s)
- Jens Biele
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Stephan Ulamec
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Michael Maibaum
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Reinhard Roll
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Lars Witte
- DLR/Institut für Raumfahrtsysteme, Robert Hooke-Straße 7, 28359 Bremen, Germany
| | - Eric Jurado
- Centre National d'Études Spatiales, 18 Avenue Édouard Belin, 31400 Toulouse, France
| | - Pablo Muñoz
- European Space Agency/European Space Operations Centre (ESA/ESOC), Robert-Bosch-Straße 5, 64293 Darmstadt, Germany. Grupo Mecánica de Vuelo at ESA/ESOC - GMV Robert-Bosch-Straße 5, 64293 Darmstadt, Germany
| | - Walter Arnold
- 1. Physikalisches Institut, Georg August Universität, 37077 Göttingen, Germany; permanent address: Department of Materials Science, Saarland University, 66123 Saarbrücken, Germany
| | - Hans-Ulrich Auster
- Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig Mendelssohnstrasse 3, 38106 Braunschweig, Germany
| | - Carlos Casas
- European Space Agency/European Space Operations Centre (ESA/ESOC), Robert-Bosch-Straße 5, 64293 Darmstadt, Germany. Grupo Mecánica de Vuelo at ESA/ESOC - GMV Robert-Bosch-Straße 5, 64293 Darmstadt, Germany
| | - Claudia Faber
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Cinzia Fantinati
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Felix Finke
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Hans-Herbert Fischer
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Koen Geurts
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Carsten Güttler
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Philip Heinisch
- Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig Mendelssohnstrasse 3, 38106 Braunschweig, Germany
| | - Alain Herique
- Université Grenoble Alpes and CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, F-38000 Grenoble, France
| | - Stubbe Hviid
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Günter Kargl
- Institut für Weltraumforschung (IWF) Graz, Austria Austrian Academy of Sciences, Space Research Institute, Schmiedlstraße 6, 8042 Graz, Austria
| | - Martin Knapmeyer
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Jörg Knollenberg
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Wlodek Kofman
- Université Grenoble Alpes and CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, F-38000 Grenoble, France
| | - Norbert Kömle
- Institut für Weltraumforschung (IWF) Graz, Austria Austrian Academy of Sciences, Space Research Institute, Schmiedlstraße 6, 8042 Graz, Austria
| | - Ekkehard Kührt
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Valentina Lommatsch
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)/Raumflugbetrieb und Astronautentraining, Microgravity User Support Center (MUSC), Linder Höhe 1, 51147 Cologne, Germany
| | - Stefano Mottola
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | - Ramon Pardo de Santayana
- European Space Agency/European Space Operations Centre (ESA/ESOC), Robert-Bosch-Straße 5, 64293 Darmstadt, Germany. Grupo Mecánica de Vuelo at ESA/ESOC - GMV Robert-Bosch-Straße 5, 64293 Darmstadt, Germany
| | - Emile Remetean
- Centre National d'Études Spatiales, 18 Avenue Édouard Belin, 31400 Toulouse, France
| | - Frank Scholten
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
| | | | - Holger Sierks
- Max-Planck-Institut für Sonnensystemforschung (MPS), Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Tilman Spohn
- DLR/Institut für Planetenforschung Rutherfordstraße 2, 12489 Berlin, Germany
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Bibring JP, Taylor MGGT, Alexander C, Auster U, Biele J, Finzi AE, Goesmann F, Klingelhoefer G, Kofman W, Mottola S, Seidensticker KJ, Spohn T, Wright I. Philae's first look. Philae's First Days on the Comet. Introduction. Science 2015; 349:493. [PMID: 26228139 DOI: 10.1126/science.aac5116] [Citation(s) in RCA: 37] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- J-P Bibring
- Institut d'Astrophysique Spatiale, Orsay, France
| | - M G G T Taylor
- European Space Research and Technology Centre, Noordwijk, Netherlands
| | - C Alexander
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, deceased
| | - U Auster
- Institute for Geophysics and Extraterrestrial Physics, TU-Braunschweig, Germany
| | - J Biele
- DLR RB-MUSC, Cologne, Germany
| | | | - F Goesmann
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | | | - W Kofman
- Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - S Mottola
- DLR, Institute of Planetary Research, Berlin, Germany
| | | | - T Spohn
- DLR, Institute of Planetary Research, Berlin, Germany
| | - I Wright
- Open University, Milton Keynes, UK
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Spohn T, Hort M, Fischer H. Numerical simulation of the crystallization of multicomponent melts in thin dikes or sills: 1. The liquidus phase. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb093ib05p04880] [Citation(s) in RCA: 39] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Kömle NI, Hütter ES, Macher W, Kaufmann E, Kargl G, Knollenberg J, Grott M, Spohn T, Wawrzaszek R, Banaszkiewicz M, Seweryn K, Hagermann A. In situ methods for measuring thermal properties and heat flux on planetary bodies. Planet Space Sci 2011; 59:639-660. [PMID: 21760643 PMCID: PMC3089965 DOI: 10.1016/j.pss.2011.03.004] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/21/2010] [Revised: 03/10/2011] [Accepted: 03/11/2011] [Indexed: 05/31/2023]
Abstract
The thermo-mechanical properties of planetary surface and subsurface layers control to a high extent in which way a body interacts with its environment, in particular how it responds to solar irradiation and how it interacts with a potentially existing atmosphere. Furthermore, if the natural temperature profile over a certain depth can be measured in situ, this gives important information about the heat flux from the interior and thus about the thermal evolution of the body. Therefore, in most of the recent and planned planetary lander missions experiment packages for determining thermo-mechanical properties are part of the payload. Examples are the experiment MUPUS on Rosetta's comet lander Philae, the TECP instrument aboard NASA's Mars polar lander Phoenix, and the mole-type instrument HP(3) currently developed for use on upcoming lunar and Mars missions. In this review we describe several methods applied for measuring thermal conductivity and heat flux and discuss the particular difficulties faced when these properties have to be measured in a low pressure and low temperature environment. We point out the abilities and disadvantages of the different instruments and outline the evaluation procedures necessary to extract reliable thermal conductivity and heat flux data from in situ measurements.
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Affiliation(s)
- Norbert I. Kömle
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Erika S. Hütter
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Wolfgang Macher
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Erika Kaufmann
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Günter Kargl
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | | | - Tilman Spohn
- DLR Insitut für Planetenforschung, Berlin, Germany
| | - Roman Wawrzaszek
- Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
| | | | - Karoly Seweryn
- Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
| | - Axel Hagermann
- Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR), Open University, Milton Keynes, UK
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Spohn T, Breuer D. How would life factor in the evolution of planetary interiors? Comment on "Life, hierarchy, and the thermodynamic machinery of planet Earth" by A. Kleidon. Phys Life Rev 2010; 7:471-2; discussion 473-6. [PMID: 21071292 DOI: 10.1016/j.plrev.2010.11.002] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Affiliation(s)
- Tilman Spohn
- Institute of Planetary Research, DLR, Rutherfordstrasse 2, 12489 Berlin, Germany.
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Lammer H, Selsis F, Chassefière E, Breuer D, Griessmeier JM, Kulikov YN, Erkaev NV, Khodachenko ML, Biernat HK, Leblanc F, Kallio E, Lundin R, Westall F, Bauer SJ, Beichman C, Danchi W, Eiroa C, Fridlund M, Gröller H, Hanslmeier A, Hausleitner W, Henning T, Herbst T, Kaltenegger L, Léger A, Leitzinger M, Lichtenegger HIM, Liseau R, Lunine J, Motschmann U, Odert P, Paresce F, Parnell J, Penny A, Quirrenbach A, Rauer H, Röttgering H, Schneider J, Spohn T, Stadelmann A, Stangl G, Stam D, Tinetti G, White GJ. Geophysical and atmospheric evolution of habitable planets. Astrobiology 2010; 10:45-68. [PMID: 20307182 DOI: 10.1089/ast.2009.0368] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
The evolution of Earth-like habitable planets is a complex process that depends on the geodynamical and geophysical environments. In particular, it is necessary that plate tectonics remain active over billions of years. These geophysically active environments are strongly coupled to a planet's host star parameters, such as mass, luminosity and activity, orbit location of the habitable zone, and the planet's initial water inventory. Depending on the host star's radiation and particle flux evolution, the composition in the thermosphere, and the availability of an active magnetic dynamo, the atmospheres of Earth-like planets within their habitable zones are differently affected due to thermal and nonthermal escape processes. For some planets, strong atmospheric escape could even effect the stability of the atmosphere.
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Affiliation(s)
- Helmut Lammer
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria.
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Affiliation(s)
- F. Sohl
- Institut für Planetologie; Westfälische Wilhelms-Universität; Münster Germany
| | - H. Hussmann
- Institut für Planetologie; Westfälische Wilhelms-Universität; Münster Germany
| | - B. Schwentker
- Institut für Planetologie; Westfälische Wilhelms-Universität; Münster Germany
| | - T. Spohn
- Institut für Planetologie; Westfälische Wilhelms-Universität; Münster Germany
| | - R. D. Lorenz
- Lunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
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Breuer D, Zhou H, Yuen DA, Spohn T. Phase transitions in the Martian mantle: Implications for the planet's volcanic history. ACTA ACUST UNITED AC 1996. [DOI: 10.1029/96je00117] [Citation(s) in RCA: 31] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hort M, Spohn T. Numerical simulation of the crystallization of multicomponent melts in thin dikes or sills: 2. Effects of heterocatalytic nucleation and composition. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/90jb01896] [Citation(s) in RCA: 20] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Spohn T. Liability insurance is essential to professional security. J Post Anesth Nurs 1988; 3:423-4. [PMID: 2462644] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [MESH Headings] [Subscribe] [Scholar Register] [Indexed: 01/01/2023]
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