1
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Liu D, Jiang X, Wu Z, Sun X, Lu YB. Tolerance of Perovskite Solar Cells to Electrostatic Discharge in Martian Dust Activities. ACS OMEGA 2024; 9:25215-25222. [PMID: 38882146 PMCID: PMC11170748 DOI: 10.1021/acsomega.4c02887] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/25/2024] [Revised: 05/02/2024] [Accepted: 05/17/2024] [Indexed: 06/18/2024]
Abstract
In exploring the viability of perovskite solar cells (PSCs) for Mars missions, our study first delved into their temperature endurance in conditions mimicking the Martian climate, revealing remarkable thermal stability within the temperature range of 173-303 K. We then pioneered the examination of PSC resilience to electrostatic discharge (ESD), a critical factor given the frequent Martian dust activities. In a custom-built Martian simulation chamber, we discovered that ESD exposure dramatically reduced the power conversion efficiency of these devices by more than half (55.4%) in just 90 s. This groundbreaking research not only advances our understanding of the potential of PSCs for Mars exploration but also opens new avenues for optimizing solar technology in extreme environments.
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Affiliation(s)
- Dong Liu
- School of Space Science and Physics, Shandong University, Weihai 264209, China
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China
| | - Xianyuan Jiang
- School of Physical Science and Technology, ShanghaiTech University, Shanghai 201210, China
| | - Zhongchen Wu
- School of Space Science and Physics, Shandong University, Weihai 264209, China
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China
| | - Xianyang Sun
- School of Space Science and Physics, Shandong University, Weihai 264209, China
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China
| | - Ying-Bo Lu
- School of Space Science and Physics, Shandong University, Weihai 264209, China
- Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai 264209, China
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2
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Zhao H, Zhang Y, Han L, Qian W, Wang J, Wu H, Li J, Dai Y, Zhang Z, Bowen CR, Yang Y. Intelligent Recognition Using Ultralight Multifunctional Nano-Layered Carbon Aerogel Sensors with Human-Like Tactile Perception. NANO-MICRO LETTERS 2023; 16:11. [PMID: 37943399 PMCID: PMC10635924 DOI: 10.1007/s40820-023-01216-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/23/2023] [Accepted: 09/11/2023] [Indexed: 11/10/2023]
Abstract
Humans can perceive our complex world through multi-sensory fusion. Under limited visual conditions, people can sense a variety of tactile signals to identify objects accurately and rapidly. However, replicating this unique capability in robots remains a significant challenge. Here, we present a new form of ultralight multifunctional tactile nano-layered carbon aerogel sensor that provides pressure, temperature, material recognition and 3D location capabilities, which is combined with multimodal supervised learning algorithms for object recognition. The sensor exhibits human-like pressure (0.04-100 kPa) and temperature (21.5-66.2 °C) detection, millisecond response times (11 ms), a pressure sensitivity of 92.22 kPa-1 and triboelectric durability of over 6000 cycles. The devised algorithm has universality and can accommodate a range of application scenarios. The tactile system can identify common foods in a kitchen scene with 94.63% accuracy and explore the topographic and geomorphic features of a Mars scene with 100% accuracy. This sensing approach empowers robots with versatile tactile perception to advance future society toward heightened sensing, recognition and intelligence.
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Affiliation(s)
- Huiqi Zhao
- CAS Center for Excellence in Nanoscience, Beijing Key Laboratory of Micro-Nano Energy and Sensor, Beijing Institute of Nanoenergy and Nanosystems, Chinese Academy of Sciences, Beijing, 101400, People's Republic of China
- School of Nanoscience and Technology, University of Chinese Academy of Sciences, Beijing, 100049, People's Republic of China
| | - Yizheng Zhang
- Tencent Robotics X, Shenzhen, 518054, People's Republic of China
| | - Lei Han
- Tencent Robotics X, Shenzhen, 518054, People's Republic of China
| | - Weiqi Qian
- CAS Center for Excellence in Nanoscience, Beijing Key Laboratory of Micro-Nano Energy and Sensor, Beijing Institute of Nanoenergy and Nanosystems, Chinese Academy of Sciences, Beijing, 101400, People's Republic of China
- School of Nanoscience and Technology, University of Chinese Academy of Sciences, Beijing, 100049, People's Republic of China
| | - Jiabin Wang
- CAS Center for Excellence in Nanoscience, Beijing Key Laboratory of Micro-Nano Energy and Sensor, Beijing Institute of Nanoenergy and Nanosystems, Chinese Academy of Sciences, Beijing, 101400, People's Republic of China
- Center on Nanoenergy Research, School of Physical Science and Technology, Guangxi University, Nanning, 530004, People's Republic of China
| | - Heting Wu
- CAS Center for Excellence in Nanoscience, Beijing Key Laboratory of Micro-Nano Energy and Sensor, Beijing Institute of Nanoenergy and Nanosystems, Chinese Academy of Sciences, Beijing, 101400, People's Republic of China
| | - Jingchen Li
- Tencent Robotics X, Shenzhen, 518054, People's Republic of China
| | - Yuan Dai
- Tencent Robotics X, Shenzhen, 518054, People's Republic of China.
| | - Zhengyou Zhang
- Tencent Robotics X, Shenzhen, 518054, People's Republic of China
| | - Chris R Bowen
- Department of Mechanical Engineering, University of Bath, Bath, BA2 7AK, UK
| | - Ya Yang
- CAS Center for Excellence in Nanoscience, Beijing Key Laboratory of Micro-Nano Energy and Sensor, Beijing Institute of Nanoenergy and Nanosystems, Chinese Academy of Sciences, Beijing, 101400, People's Republic of China.
- School of Nanoscience and Technology, University of Chinese Academy of Sciences, Beijing, 100049, People's Republic of China.
- Center on Nanoenergy Research, School of Physical Science and Technology, Guangxi University, Nanning, 530004, People's Republic of China.
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3
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Liu J, Qin X, Ren X, Wang X, Sun Y, Zeng X, Wu H, Chen Z, Chen W, Chen Y, Wang C, Sun Z, Zhang R, Ouyang Z, Guo Z, Head JW, Li C. Martian dunes indicative of wind regime shift in line with end of ice age. Nature 2023; 620:303-309. [PMID: 37407822 PMCID: PMC10412455 DOI: 10.1038/s41586-023-06206-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/02/2022] [Accepted: 05/12/2023] [Indexed: 07/07/2023]
Abstract
Orbital observations suggest that Mars underwent a recent 'ice age' (roughly 0.4-2.1 million years ago), during which a latitude-dependent ice-dust mantle (LDM)1,2 was emplaced. A subsequent decrease in obliquity amplitude resulted in the emergence of an 'interglacial period'1,3 during which the lowermost latitude LDM ice4-6 was etched and removed, returning it to the polar cap. These observations are consistent with polar cap stratigraphy1,7, but lower- to mid-latitude in situ surface observations in support of a glacial-interglacial transition that can be reconciled with mesoscale and global atmospheric circulation models8 is lacking. Here we present a suite of measurements obtained by the Zhurong rover during its traverse across the southern LDM region in Utopia Planitia, Mars. We find evidence for a stratigraphic sequence involving initial barchan dune formation, indicative of north-easterly winds, cementation of dune sediments, followed by their erosion by north-westerly winds, eroding the barchan dunes and producing distinctive longitudinal dunes, with the transition in wind regime consistent with the end of the ice age. The results are compatible with the Martian polar stratigraphic record and will help improve our understanding of the ancient climate history of Mars9.
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Affiliation(s)
- Jianjun Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Xiaoguang Qin
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Xin Ren
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Xu Wang
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Yong Sun
- State Key Laboratory of Tibetan Plateau Earth System, Resources and Environment, Institute of Tibetan Plateau Research, Chinese Academy of Sciences, Beijing, China
| | - Xingguo Zeng
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Haibin Wu
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Zhaopeng Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Wangli Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Yuan Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Cheng Wang
- Beijing Aerospace Control Center, Beijing, China
| | - Zezhou Sun
- Beijing Institute of Spacecraft System Engineering, Beijing, China
| | - Rongqiao Zhang
- Lunar Exploration and Space Engineering Center, Beijing, China
| | - Ziyuan Ouyang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, China
| | - Zhengtang Guo
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China.
| | - James W Head
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI, USA.
| | - Chunlai Li
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
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4
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Qin X, Ren X, Wang X, Liu J, Wu H, Zeng X, Sun Y, Chen Z, Zhang S, Zhang Y, Chen W, Liu B, Liu D, Guo L, Li K, Zeng X, Huang H, Zhang Q, Yu S, Li C, Guo Z. Modern water at low latitudes on Mars: Potential evidence from dune surfaces. SCIENCE ADVANCES 2023; 9:eadd8868. [PMID: 37115933 PMCID: PMC10146874 DOI: 10.1126/sciadv.add8868] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Indexed: 05/03/2023]
Abstract
Landforms on the Martian surface are critical to understanding the nature of surface processes in the recent past. However, modern hydroclimatic conditions on Mars remain enigmatic, as explanations for the formation of observed landforms are ambiguous. We report crusts, cracks, aggregates, and bright polygonal ridges on the surfaces of hydrated salt-rich dunes of southern Utopia Planitia (~25°N) from in situ exploration by the Zhurong rover. These surface features were inferred to form after 1.4 to 0.4 million years ago. Wind and CO2 frost processes can be ruled out as potential mechanisms. Instead, involvement of saline water from thawed frost/snow is the most likely cause. This discovery sheds light on more humid conditions of the modern Martian climate and provides critical clues to future exploration missions searching for signs of extant life, particularly at low latitudes with comparatively warmer, more amenable surface temperatures.
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Affiliation(s)
- Xiaoguang Qin
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Xin Ren
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Xu Wang
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Jianjun Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Haibin Wu
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing, China
| | - Xingguo Zeng
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Yong Sun
- Institute of Atmospheric Physics, Chinese Academy of Sciences, Beijing, China
| | - Zhaopeng Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Shihao Zhang
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Yizhong Zhang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Wangli Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Bin Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Dawei Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Lin Guo
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Kangkang Li
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Xiangzhao Zeng
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Hai Huang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Qing Zhang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Songzheng Yu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Chunlai Li
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Zhengtang Guo
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
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5
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Zhang S, Hu Y, Yang J, Li X, Kang W, Zhang J, Liu Y, Nie J. The Hadley circulation in the Pangea era. Sci Bull (Beijing) 2023:S2095-9273(23)00275-X. [PMID: 37179232 DOI: 10.1016/j.scib.2023.04.021] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/14/2023] [Revised: 03/30/2023] [Accepted: 04/04/2023] [Indexed: 05/15/2023]
Abstract
The Pangea era is an exceptional phase in Earth's history. It is characterized by its hothouse climate state and the latest supercontinent. Thus, it is expected that atmospheric circulation in the Pangea era was largely different from that of the modern world. Here, we study the Hadley circulation in the Pangea era and compare it with that of the present, by performing climate simulations. Our results show that the annual mean Hadley cells are about 20% and 45% weaker than that in the pre-industrial (PI) climate, and their poleward edges are about 2° wider in latitude. The austral winter cell is weakened by 27% and expanded by 2.6°, while the changes of the boreal winter cell are not significant. One distinctive feature is that the ascending branches of the boreal and austral winter cells shift to 23°S and 18°N, respectively, which are much more poleward than their present locations. Our analyses demonstrate that the weakening and widening of the Hadley circulation is due to increasing tropical and subtropical static stability, and that the poleward shifts of the ascending branches of the winter cells are associated with the geographic configuration of the supercontinent Pangea.
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Affiliation(s)
- Shiyan Zhang
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China
| | - Yongyun Hu
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China.
| | - Jun Yang
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China
| | - Xiang Li
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China
| | - Wanying Kang
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Jian Zhang
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China
| | - Yonggang Liu
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China
| | - Ji Nie
- Laboratory for Climate and Ocean-Atmosphere Studies, Department of Atmospheric and Oceanic Sciences, School of Physics, Peking University, Beijing 100871, China
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6
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Diurnal Variations of Water Ice in the Martian Atmosphere Observed by Mars Climate Sounder. REMOTE SENSING 2022. [DOI: 10.3390/rs14092235] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/05/2023]
Abstract
Simulation studies have proposed a significant thermal effect of water ice clouds on the Martian atmosphere and climate. However, previous studies focused more on seasonal variations but less on short-term changes. In this work, we used the MCS multi-local time data to investigate the water ice diurnal variations on Mars. We quantified its diurnal variations with amplitude and phase by applying the tidal fitting method to the water ice abundance. In addition, we found a close correlation (antiphase relation) between the thermal tide and water ice diurnal variations during the aphelion seasons that was not sensitive to both the background water ice and dust opacity but increased with the tidal amplitude. In the perihelion seasons, the antiphase relation was sensitive to the water ice and dust opacity, both affected by the dust storm activity. Finally, the statistic results suggested an unexpected low threshold of diurnal tide amplitude (2 to 3 K) for generating a relevant water ice diurnal variation, accounting for the ubiquitous water ice diurnal variations in the Martian atmosphere. These new observational results can help further understand the phase transition process between ice and vapor in the Martian atmosphere and better constrain the Martian global climate model in the future.
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7
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Mapstone LJ, Leite MN, Purton S, Crawford IA, Dartnell L. Cyanobacteria and microalgae in supporting human habitation on Mars. Biotechnol Adv 2022; 59:107946. [DOI: 10.1016/j.biotechadv.2022.107946] [Citation(s) in RCA: 6] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/26/2021] [Revised: 02/21/2022] [Accepted: 03/15/2022] [Indexed: 12/16/2022]
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8
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Jin DW, Ko YJ, Ahn CW, Hur S, Lee TK, Jeong DG, Lee M, Kang CY, Jung JH. Polarization- and Electrode-Optimized Polyvinylidene Fluoride Films for Harsh Environmental Piezoelectric Nanogenerator Applications. SMALL (WEINHEIM AN DER BERGSTRASSE, GERMANY) 2021; 17:e2007289. [PMID: 33705597 DOI: 10.1002/smll.202007289] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/19/2020] [Revised: 01/20/2021] [Indexed: 06/12/2023]
Abstract
While piezoelectric nanogenerators have demonstrated the effective conversion of tiny mechanical vibrations to electricity, their performances are rarely examined under harsh environmental conditions. Here, a multilayered polyvinylidene fluoride (PVDF) film-based piezoelectric nanogenerator (ML-PENG) is demonstrated to generate considerable and stable power outputs even at extremely low temperatures and pressures, and under strong UV. Up-/down-polarized PVDF films are alternately stacked, and Ag electrodes are intercalated between the two adjacent films. At -266 °C and 10-5 Torr, the ML-PENG generates an open-circuit voltage of 1.1 V, a short-circuit current density of 8 nA cm-2 , and a power density of 4.4 nW cm-2 . The piezoelectric outputs are quite stable against prolonged illumination of UV, large temperature- and pressure-variations, and excessive mechanical vibrations. The piezoelectric power density is greatly enhanced above the freezing and glass transition temperatures of PVDF and recorded to be 10, 105, and 282 nW cm-2 at -73, 0, and 77 °C, respectively. The ML-PENG generates sufficient power to operate five light-emitting diodes by harvesting biomechanical energy under simulated Martian conditions. This work suggests that polarization- and electrode-optimized ML-PENG can serve as a reliable and economic power source in harsh and inaccessible environments like polar areas of Earth and extraterrestrial Mars.
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Affiliation(s)
- Da Woon Jin
- Department of Physics, Inha University, Incheon, 22212, Republic of Korea
| | - Young Joon Ko
- Department of Physics, Inha University, Incheon, 22212, Republic of Korea
| | - Chang Won Ahn
- Department of Physics and Energy Harvest-Storage Research Center, University of Ulsan, Ulsan, 44610, Republic of Korea
| | - Sunghoon Hur
- Center for Electronic Materials, Korea Institute of Science and Technology (KIST), Seoul, 02792, Republic of Korea
| | - Tae Kwon Lee
- Department of Physics, Inha University, Incheon, 22212, Republic of Korea
| | - Dong Geun Jeong
- Department of Physics, Inha University, Incheon, 22212, Republic of Korea
| | - Minbaek Lee
- Department of Physics, Inha University, Incheon, 22212, Republic of Korea
| | - Chong-Yun Kang
- Center for Electronic Materials, Korea Institute of Science and Technology (KIST), Seoul, 02792, Republic of Korea
- KU-KIST Graduate School of Converging Science and Technology, Korea University, Seoul, 02841, Republic of Korea
| | - Jong Hoon Jung
- Department of Physics, Inha University, Incheon, 22212, Republic of Korea
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9
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Sobrado JM. Mimicking the Martian Hydrological Cycle: A Set-Up to Introduce Liquid Water in Vacuum. SENSORS (BASEL, SWITZERLAND) 2020; 20:E6150. [PMID: 33138024 PMCID: PMC7662484 DOI: 10.3390/s20216150] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 09/24/2020] [Revised: 10/25/2020] [Accepted: 10/27/2020] [Indexed: 11/16/2022]
Abstract
Liquid water is well known as the life ingredient as a solvent. However, so far, it has only been found in liquid state on this planetary surface. The aim of this experiment and technological development was to test if a moss sample is capable of surviving in Martian conditions. We built a system that simulates the environmental conditions of the red planet including its hydrological cycle. This laboratory facility enables us to control the water cycle in its three phases through temperature, relative humidity, hydration, and pressure with a system that injects water droplets into a vacuum chamber. We successfully simulated the daytime and nighttime of Mars by recreating water condensation and created a layer of superficial ice that protects the sample against external radiation and minimizes the loss of humidity due to evaporation to maintain a moss sample in survival conditions in this extreme environment. We performed the simulations with the design and development of different tools that recreate Martian weather in the MARTE simulation chamber.
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10
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Wu Z, Li T, Zhang X, Li J, Cui J. Dust tides and rapid meridional motions in the Martian atmosphere during major dust storms. Nat Commun 2020; 11:614. [PMID: 32001703 PMCID: PMC6992627 DOI: 10.1038/s41467-020-14510-x] [Citation(s) in RCA: 14] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/27/2019] [Accepted: 01/09/2020] [Indexed: 11/08/2022] Open
Abstract
The atmosphere of Mars is strongly affected by the spatial and temporal variability of airborne dust. However, global dust variability within a sol (Martian day) is still poorly understood. Although short-term dynamic processes are crucial, detailed comparisons of simulated diurnal variations are limited by relatively sparse observations. Here, we report the discovery of ubiquitous, strong diurnal tides of dust in the Southern Hemisphere of Mars. Driven by the westward-propagating migrating diurnal thermal tide, zonally distributed dust fronts slosh back and forth in a wide latitudinal range of up to 40° within one sol during major dust storms. Dust tides-tidal transport of dust in this way-rapidly transport heat and constituents meridionally, allowing moist air near the summer pole to be rapidly transported to lower latitudes during the night, where it then can be lifted by daytime deep convection and contribute to hydrogen escape from Mars during global dust storms.
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Affiliation(s)
- Zhaopeng Wu
- School of Atmospheric Sciences, Sun Yat-sen University, Zhuhai, Guangdong, 519082, PR China.
- CAS Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, PR China.
- CAS Center for Excellence in Comparative Planetology, Hefei, Anhui, 230026, PR China.
| | - Tao Li
- CAS Center for Excellence in Comparative Planetology, Hefei, Anhui, 230026, PR China.
- CAS Key Laboratory of Geospace Environment, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui, 230026, PR China.
| | - Xi Zhang
- Department of Earth and Planetary Sciences, University of California Santa Cruz, Santa Cruz, CA, 95064, USA
| | - Jing Li
- School of Atmospheric Sciences, Sun Yat-sen University, Zhuhai, Guangdong, 519082, PR China
| | - Jun Cui
- School of Atmospheric Sciences, Sun Yat-sen University, Zhuhai, Guangdong, 519082, PR China
- CAS Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, PR China
- CAS Center for Excellence in Comparative Planetology, Hefei, Anhui, 230026, PR China
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11
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Hoffman PF, Abbot DS, Ashkenazy Y, Benn DI, Brocks JJ, Cohen PA, Cox GM, Creveling JR, Donnadieu Y, Erwin DH, Fairchild IJ, Ferreira D, Goodman JC, Halverson GP, Jansen MF, Le Hir G, Love GD, Macdonald FA, Maloof AC, Partin CA, Ramstein G, Rose BEJ, Rose CV, Sadler PM, Tziperman E, Voigt A, Warren SG. Snowball Earth climate dynamics and Cryogenian geology-geobiology. SCIENCE ADVANCES 2017; 3:e1600983. [PMID: 29134193 PMCID: PMC5677351 DOI: 10.1126/sciadv.1600983] [Citation(s) in RCA: 87] [Impact Index Per Article: 12.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/04/2016] [Accepted: 09/21/2017] [Indexed: 05/02/2023]
Abstract
Geological evidence indicates that grounded ice sheets reached sea level at all latitudes during two long-lived Cryogenian (58 and ≥5 My) glaciations. Combined uranium-lead and rhenium-osmium dating suggests that the older (Sturtian) glacial onset and both terminations were globally synchronous. Geochemical data imply that CO2 was 102 PAL (present atmospheric level) at the younger termination, consistent with a global ice cover. Sturtian glaciation followed breakup of a tropical supercontinent, and its onset coincided with the equatorial emplacement of a large igneous province. Modeling shows that the small thermal inertia of a globally frozen surface reverses the annual mean tropical atmospheric circulation, producing an equatorial desert and net snow and frost accumulation elsewhere. Oceanic ice thickens, forming a sea glacier that flows gravitationally toward the equator, sustained by the hydrologic cycle and by basal freezing and melting. Tropical ice sheets flow faster as CO2 rises but lose mass and become sensitive to orbital changes. Equatorial dust accumulation engenders supraglacial oligotrophic meltwater ecosystems, favorable for cyanobacteria and certain eukaryotes. Meltwater flushing through cracks enables organic burial and submarine deposition of airborne volcanic ash. The subglacial ocean is turbulent and well mixed, in response to geothermal heating and heat loss through the ice cover, increasing with latitude. Terminal carbonate deposits, unique to Cryogenian glaciations, are products of intense weathering and ocean stratification. Whole-ocean warming and collapsing peripheral bulges allow marine coastal flooding to continue long after ice-sheet disappearance. The evolutionary legacy of Snowball Earth is perceptible in fossils and living organisms.
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Affiliation(s)
- Paul F. Hoffman
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA
- School of Earth and Ocean Sciences, University of Victoria, Victoria, British Columbia V8P 5C2, Canada
| | - Dorian S. Abbot
- Department of Geophysical Sciences, University of Chicago, Chicago, IL 60637, USA
| | - Yosef Ashkenazy
- Department of Solar Energy and Environmental Physics, Ben-Gurion University of the Negev, Midreshet Ben-Gurion, 84990, Israel
| | - Douglas I. Benn
- School of Geography and Sustainable Development, University of St Andrews, St Andrews, Fife KY16 8YA, UK
| | - Jochen J. Brocks
- Research School of Earth Sciences, Australian National University, Canberra, Australian Capital Territory 2601, Australia
| | | | - Grant M. Cox
- Centre for Tectonics, Resources and Exploration (TRaX), Department of Earth Sciences, University of Adelaide, Adelaide, South Australia 5005, Australia
- Department of Applied Geology, Curtin University, Bentley, Western Australia 6845, Australia
| | - Jessica R. Creveling
- College of Earth, Ocean, and Atmospheric Sciences, Oregon State University, Corvallis, OR 97331–5503, USA
| | - Yannick Donnadieu
- Laboratoire des Sciences du Climat et de l’Environnement (LSCE), Institut Pierre Simon Laplace (IPSL), CEA-CNRS-UVSQ, Université Paris-Saclay, 91191 Gif-sur-Yvette, France
- Aix-Marseille Université, CNRS, L’Institut de recherche pour le développement (IRD), Centre Européen de Recherche et D’enseignement de Géosciences de L’environnement (CEREGE), 13545 Aix-en-Provence, France
| | - Douglas H. Erwin
- Department of Paleobiology, Smithsonian Institution, P.O. Box 37012, MRC 121, Washington, DC 20013–7012, USA
- Santa Fe Institute, 1399 Hyde Park Road, Santa Fe, NM 87501, USA
| | - Ian J. Fairchild
- School of Geography, Earth and Environmental Sciences, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
| | - David Ferreira
- Department of Meteorology, University of Reading, Reading, RG6 6BB, UK
| | - Jason C. Goodman
- Department of Environmental Science, Wheaton College, Norton, MA 02766, USA
| | - Galen P. Halverson
- Department of Earth and Planetary Sciences, McGill University, Montréal, Québec H3A 0E8, Canada
| | - Malte F. Jansen
- Department of Geophysical Sciences, University of Chicago, Chicago, IL 60637, USA
| | - Guillaume Le Hir
- Institut de Physique du Globe de Paris, 1, rue Jussieu, 75005 Paris, France
| | - Gordon D. Love
- Department of Earth Sciences, University of California, Riverside, Riverside, CA 92521, USA
| | - Francis A. Macdonald
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA
| | - Adam C. Maloof
- Department of Geosciences, Princeton University, Princeton, NJ 08544, USA
| | - Camille A. Partin
- Department of Geological Sciences, University of Saskatchewan, Saskatoon, Saskatchewan S7N 5E2, Canada
| | - Gilles Ramstein
- Laboratoire des Sciences du Climat et de l’Environnement (LSCE), Institut Pierre Simon Laplace (IPSL), CEA-CNRS-UVSQ, Université Paris-Saclay, 91191 Gif-sur-Yvette, France
| | - Brian E. J. Rose
- Department of Atmospheric and Environmental Sciences, University at Albany, Albany, NY 12222, USA
| | | | - Peter M. Sadler
- Department of Earth Sciences, University of California, Riverside, Riverside, CA 92521, USA
| | - Eli Tziperman
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138, USA
| | - Aiko Voigt
- Institute of Meteorology and Climate Research, Department of Troposphere Research, Karlsruhe Institute of Technology, Karlsruhe, Baden-Württemberg, Germany
- Lamont-Doherty Earth Observatory, Columbia University, P.O. Box 1000, Palisades, NY 10964–1000, USA
| | - Stephen G. Warren
- Department of Atmospheric Sciences, University of Washington, Seattle, WA 98195–1640, USA
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Kok JF, Parteli EJR, Michaels TI, Karam DB. The physics of wind-blown sand and dust. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2012; 75:106901. [PMID: 22982806 DOI: 10.1088/0034-4885/75/10/106901] [Citation(s) in RCA: 160] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/12/2023]
Abstract
The transport of sand and dust by wind is a potent erosional force, creates sand dunes and ripples, and loads the atmosphere with suspended dust aerosols. This paper presents an extensive review of the physics of wind-blown sand and dust on Earth and Mars. Specifically, we review the physics of aeolian saltation, the formation and development of sand dunes and ripples, the physics of dust aerosol emission, the weather phenomena that trigger dust storms, and the lifting of dust by dust devils and other small-scale vortices. We also discuss the physics of wind-blown sand and dune formation on Venus and Titan.
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Affiliation(s)
- Jasper F Kok
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY, USA.
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Kok JF. Difference in the wind speeds required for initiation versus continuation of sand transport on mars: implications for dunes and dust storms. PHYSICAL REVIEW LETTERS 2010; 104:074502. [PMID: 20366891 DOI: 10.1103/physrevlett.104.074502] [Citation(s) in RCA: 14] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/30/2009] [Indexed: 05/16/2023]
Abstract
Much of the surface of Mars is covered by dunes, ripples, and other features formed by the blowing of sand by wind, known as saltation. In addition, saltation loads the atmosphere with dust aerosols, which dominate the Martian climate. We show here that saltation can be maintained on Mars by wind speeds an order of magnitude less than required to initiate it. We further show that this hysteresis effect causes saltation to occur for much lower wind speeds than previously thought. These findings have important implications for the formation of dust storms, sand dunes, and ripples on Mars.
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Affiliation(s)
- Jasper F Kok
- Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan 48109, USA.
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14
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Mata SA, Bottjer DJ. Development of lower Triassic wrinkle structures: implications for the search for life on other planets. ASTROBIOLOGY 2009; 9:895-906. [PMID: 19968465 DOI: 10.1089/ast.2008.0290] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/28/2023]
Abstract
Wrinkle structures are microbially mediated sedimentary structures that are a common feature of Proterozoic and earliest Phanerozoic siliciclastic seafloors on Earth and occur only rarely in post-Cambrian strata. These macroscopic microbially induced sedimentary structures are readily identifiable at the outcrop scale, and their recognition on other planetary bodies by landed missions may suggest the presence of past microbial life. Wrinkle structures of the Lower Triassic (Spathian) Virgin Limestone Member of the Moenkopi Formation in the western United States record an occurrence of widespread microbialite formation in the wake of the end-Permian mass extinction, the largest biotic crisis of the Phanerozoic. Wrinkle structures occur on proximal sandy tempestites deposited within the offshore transition. Storm layers appear to have been rapidly colonized by microbial mats and were subsequently buried by mud during fair-weather conditions. Wrinkle structures exhibit flat-topped crests and sinuous troughs, with associated mica grains oriented parallel to bedding, suggestive of trapping and binding activity. Although Lower Triassic wrinkle structures postdate the widespread occurrence of these features during the Proterozoic and Cambrian, they exhibit many of the same characteristics and environmental trends, which suggests a conservation of microbial formational and preservational processes in subtidal siliciclastic settings on Earth from the Precambrian into the Phanerozoic. In the search for extraterrestrial life, it may be these conservative characteristics that prove to be the most useful and robust for recognizing microbial features on other planetary bodies, and may add to an ever-growing foundation of knowledge for directing future explorations aimed at seeking out macroscopic microbial signatures.
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Affiliation(s)
- Scott A Mata
- Department of Earth Sciences, University of Southern California, Los Angeles, California 90089-0740, USA.
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Leblanc F, Langlais B, Fouchet T, Barabash S, Breuer D, Chassefière E, Coates A, Dehant V, Forget F, Lammer H, Lewis S, Lopez-Valverde M, Mandea M, Menvielle M, Pais A, Paetzold M, Read P, Sotin C, Tarits P, Vennerstrom S. Mars environment and magnetic orbiter scientific and measurement objectives. ASTROBIOLOGY 2009; 9:71-89. [PMID: 19317625 DOI: 10.1089/ast.2007.0222] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
In this paper, we summarize our present understanding of Mars' atmosphere, magnetic field, and surface and address past evolution of these features. Key scientific questions concerning Mars' surface, atmosphere, and magnetic field, along with the planet's interaction with solar wind, are discussed. We also define what key parameters and measurements should be performed and the main characteristics of a martian mission that would help to provide answers to these questions. Such a mission--Mars Environment and Magnetic Orbiter (MEMO)--was proposed as an answer to the Cosmic Vision Call of Opportunity as an M-class mission (corresponding to a total European Space Agency cost of less than 300 Meuro). MEMO was designed to study the strong interconnection between the planetary interior, atmosphere, and solar conditions, which is essential to our understanding of planetary evolution, the appearance of life, and its sustainability. The MEMO main platform combined remote sensing and in situ measurements of the atmosphere and the magnetic field during regular incursions into the martian upper atmosphere. The micro-satellite was designed to perform simultaneous in situ solar wind measurements. MEMO was defined to conduct: * Four-dimensional mapping of the martian atmosphere from the surface up to 120 km by measuring wind, temperature, water, and composition, all of which would provide a complete view of the martian climate and photochemical system; Mapping of the low-altitude magnetic field with unprecedented geographical, altitude, local time, and seasonal resolutions; A characterization of the simultaneous responses of the atmosphere, magnetic field, and near-Mars space to solar variability by means of in situ atmospheric and solar wind measurements.
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Affiliation(s)
- F Leblanc
- Service d'Aéronomie du CNRS/IPSL, Université Pierre et Marie Curie, France.
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Whiteway J, Daly M, Carswell A, Duck T, Dickinson C, Komguem L, Cook C. Lidar on the Phoenix mission to Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003002] [Citation(s) in RCA: 51] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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McCleese DJ, Schofield JT, Taylor FW, Calcutt SB, Foote MC, Kass DM, Leovy CB, Paige DA, Read PL, Zurek RW. Mars Climate Sounder: An investigation of thermal and water vapor structure, dust and condensate distributions in the atmosphere, and energy balance of the polar regions. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002790] [Citation(s) in RCA: 184] [Impact Index Per Article: 10.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Urban J, Dassas K, Forget F, Ricaud P. Retrieval of vertical constituents and temperature profiles from passive submillimeter wave limb observations of the Martian atmosphere: a feasibility study. APPLIED OPTICS 2005; 44:2438-2455. [PMID: 15861854 DOI: 10.1364/ao.44.002438] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/24/2023]
Abstract
The investigation of the Martian atmosphere is of key importance for an understanding of the planets present and past. Passive limb observations of thermal radiation at submillimeter wavelengths in the 320-350-GHz range by use of a state-of-the-art satellite receiver on a low Mars orbit allow important parameters such as the mixing ratios of H2O, HDO, 12CO, 13CO, O3, and H2O2 as well as the thermal profile to be retrieved with high precision and unprecedented vertical range and resolution, providing valuable information for better understanding of the planet's water cycle, atmospheric dynamics, and photochemistry. The feasibility of these kinds of measurement is demonstrated by means of model simulations based on realistic atmospheric, spectroscopic, and instrumental parameters. Temperature can be retrieved to approximately 90 km with half-scale height vertical resolution from single-scan measurements of emission lines of the long-lived species 12CO and 13CO. The global water-vapor distribution can be measured even under dry or wet conditions with good vertical resolution from the surface to approximately 45 km, and simultaneous observations of HDO allow useful information on the D/H ratio up to an altitude of approximately 30 km to be derived. The sensitivity of the limb-sounding technique also permits information on the photochemically important minor species O3, and H2O2 to be obtained. It is shown that spectral averaging may improve precision, altitude range, and resolution of the retrieved profiles. Other frequency bands are explored, and the 435-465-GHz range is suggested as a possible alternative to the 320-350-GHz range.
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Affiliation(s)
- Joachim Urban
- Observatoire Aquitain des Sciences de l'Univers, 2, Rue de l'Observatoire, B.P. 89, 33270 Floirac, France.
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Head JW, Mustard JF, Kreslavsky MA, Milliken RE, Marchant DR. Recent ice ages on Mars. Nature 2003; 426:797-802. [PMID: 14685228 DOI: 10.1038/nature02114] [Citation(s) in RCA: 606] [Impact Index Per Article: 28.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/16/2003] [Accepted: 10/08/2003] [Indexed: 11/09/2022]
Abstract
A key pacemaker of ice ages on the Earth is climatic forcing due to variations in planetary orbital parameters. Recent Mars exploration has revealed dusty, water-ice-rich mantling deposits that are layered, metres thick and latitude dependent, occurring in both hemispheres from mid-latitudes to the poles. Here we show evidence that these deposits formed during a geologically recent ice age that occurred from about 2.1 to 0.4 Myr ago. The deposits were emplaced symmetrically down to latitudes of approximately 30 degrees--equivalent to Saudi Arabia and the southern United States on the Earth--in response to the changing stability of water ice and dust during variations in obliquity (the angle between Mars' pole of rotation and the ecliptic plane) reaching 30-35 degrees. Mars is at present in an 'interglacial' period, and the ice-rich deposits are undergoing reworking, degradation and retreat in response to the current instability of near-surface ice. Unlike the Earth, martian ice ages are characterized by warmer polar climates and enhanced equatorward transport of atmospheric water and dust to produce widespread smooth deposits down to mid-latitudes.
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Affiliation(s)
- James W Head
- Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA.
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Abstract
During thermal cycling, organisms could live on thermosynthesis, a theoretical mechanism applicable to the origin of life and the early evolution of biological energy conversion. All extraterrestrial ice may be a repository for frozen dead or dormant organisms from earlier stages of evolution. In the presence of a thermal gradient within the ice, organisms might still be harvesting energy from thermosynthesis. Possible habitats for thermosynthesizers can be found throughout the Solar System, particularly in the cold traps on Mercury and the Moon, convecting waters on Mars, the oceans on moons in the outer Solar System, and smaller bodies rotating in the sunlight such as cosmic dust, meteorites, asteroids, and comets. A general strategy for detecting thermosynthetic organisms on Earth is offered, and highlights of current and upcoming robotic exploratory missions relevant to the detection of thermosynthesis are reviewed.
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