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Çelekli A, Zariç ÖE. Breathing life into Mars: Terraforming and the pivotal role of algae in atmospheric genesis. LIFE SCIENCES IN SPACE RESEARCH 2024; 41:181-190. [PMID: 38670646 DOI: 10.1016/j.lssr.2024.03.001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/20/2023] [Revised: 03/05/2024] [Accepted: 03/08/2024] [Indexed: 04/28/2024]
Abstract
The Martian environment, characterized by extreme aridity, frigid temperatures, and a lack of atmospheric oxygen, presents a formidable challenge for potential terraforming endeavors. This review article synthesizes current research on utilizing algae as biocatalysts in the proposed terraforming of Mars, assessing their capacity to facilitate Martian atmospheric conditions through photosynthetic bioengineering. We analyze the physiological and genetic traits of extremophile algae that equip them for survival in extreme habitats on Earth, which serve as analogs for Martian surface conditions. The potential for these organisms to mediate atmospheric change on Mars is evaluated, specifically their role in biogenic oxygen production and carbon dioxide sequestration. We discuss strategies for enhancing algal strains' resilience and metabolic efficiency, including genetic modification and the development of bioreactors for controlled growth in extraterrestrial environments. The integration of algal systems with existing mechanical and chemical terraforming proposals is also examined, proposing a synergistic approach for establishing a nascent Martian biosphere. Ethical and ecological considerations concerning introducing terrestrial life to extra-planetary bodies are critically appraised. This appraisal includes an examination of potential ecological feedback loops and inherent risks associated with biological terraforming. Biological terraforming is the theoretical process of deliberately altering a planet's atmosphere, temperature, and ecosystem to render it suitable for Earth-like life. The feasibility of a phased introduction of life, starting with microbial taxa and progressing to multicellular organisms, fosters a supportive atmosphere on Mars. By extending the frontier of biotechnological innovation into space, this work contributes to the foundational understanding necessary for one of humanity's most audacious goals-the terraforming of another planet.
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Affiliation(s)
- Abuzer Çelekli
- Gaziantep University, Faculty of Art and Science, Department of Biology, Gaziantep, Turkey; Gaziantep University, Environmental Research Center (GÜÇAMER), Gaziantep, Turkey.
| | - Özgür Eren Zariç
- Gaziantep University, Faculty of Art and Science, Department of Biology, Gaziantep, Turkey; Gaziantep University, Environmental Research Center (GÜÇAMER), Gaziantep, Turkey
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Lange L, Forget F, Banfield D, Wolff M, Spiga A, Millour E, Viúdez‐Moreiras D, Bierjon A, Piqueux S, Newman C, Pla‐García J, Banerdt WB. InSight Pressure Data Recalibration, and Its Application to the Study of Long-Term Pressure Changes on Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2022JE007190. [PMID: 35865505 PMCID: PMC9286347 DOI: 10.1029/2022je007190] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 01/15/2022] [Revised: 05/09/2022] [Accepted: 05/12/2022] [Indexed: 06/15/2023]
Abstract
Observations of the South Polar Residual Cap suggest a possible erosion of the cap, leading to an increase of the global mass of the atmosphere. We test this assumption by making the first comparison between Viking 1 and InSight surface pressure data, which were recorded 40 years apart. Such a comparison also allows us to determine changes in the dynamics of the seasonal ice caps between these two periods. To do so, we first had to recalibrate the InSight pressure data because of their unexpected sensitivity to the sensor temperature. Then, we had to design a procedure to compare distant pressure measurements. We propose two surface pressure interpolation methods at the local and global scale to do the comparison. The comparison of Viking and InSight seasonal surface pressure variations does not show changes larger than ±8 Pa in the CO2 cycle. Such conclusions are supported by an analysis of Mars Science Laboratory (MSL) pressure data. Further comparisons with images of the south seasonal cap taken by the Viking 2 orbiter and MARCI camera do not display significant changes in the dynamics of this cap over a 40 year period. Only a possible larger extension of the North Cap after the global storm of MY 34 is observed, but the physical mechanisms behind this anomaly are not well determined. Finally, the first comparison of MSL and InSight pressure data suggests a pressure deficit at Gale crater during southern summer, possibly resulting from a large presence of dust suspended within the crater.
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Affiliation(s)
- L. Lange
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - F. Forget
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - D. Banfield
- Cornell Center for Astrophysics and Planetary ScienceCornell UniversityIthacaNYUSA
| | - M. Wolff
- Space Science InstituteBoulderCOUSA
| | - A. Spiga
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
- Institut Universitaire de FranceParisFrance
| | - E. Millour
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - D. Viúdez‐Moreiras
- Centro de Astrobiología (CSIC‐INTA) and National Institute for Aerospace Technology (INTA)MadridSpain
| | - A. Bierjon
- Laboratoire de Météorologie Dynamique,Institut Pierre‐Simon Laplace (LMD/IPSL)Sorbonne UniversitéCentre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS)ParisFrance
| | - S. Piqueux
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - J. Pla‐García
- Centro de Astrobiología (CSIC‐INTA) and National Institute for Aerospace Technology (INTA)MadridSpain
- Southwest Research InstituteBoulderCOUSA
| | - W. B. Banerdt
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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Newman CE, de la Torre Juárez M, Pla-García J, Wilson RJ, Lewis SR, Neary L, Kahre MA, Forget F, Spiga A, Richardson MI, Daerden F, Bertrand T, Viúdez-Moreiras D, Sullivan R, Sánchez-Lavega A, Chide B, Rodriguez-Manfredi JA. Multi-model Meteorological and Aeolian Predictions for Mars 2020 and the Jezero Crater Region. SPACE SCIENCE REVIEWS 2021; 217:20. [PMID: 33583960 PMCID: PMC7868679 DOI: 10.1007/s11214-020-00788-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/20/2020] [Accepted: 12/26/2020] [Indexed: 05/27/2023]
Abstract
Nine simulations are used to predict the meteorology and aeolian activity of the Mars 2020 landing site region. Predicted seasonal variations of pressure and surface and atmospheric temperature generally agree. Minimum and maximum pressure is predicted at Ls ∼ 145 ∘ and 250 ∘ , respectively. Maximum and minimum surface and atmospheric temperature are predicted at Ls ∼ 180 ∘ and 270 ∘ , respectively; i.e., are warmest at northern fall equinox not summer solstice. Daily pressure cycles vary more between simulations, possibly due to differences in atmospheric dust distributions. Jezero crater sits inside and close to the NW rim of the huge Isidis basin, whose daytime upslope (∼east-southeasterly) and nighttime downslope (∼northwesterly) winds are predicted to dominate except around summer solstice, when the global circulation produces more southerly wind directions. Wind predictions vary hugely, with annual maximum speeds varying from 11 to 19 ms - 1 and daily mean wind speeds peaking in the first half of summer for most simulations but in the second half of the year for two. Most simulations predict net annual sand transport toward the WNW, which is generally consistent with aeolian observations, and peak sand fluxes in the first half of summer, with the weakest fluxes around winter solstice due to opposition between the global circulation and daytime upslope winds. However, one simulation predicts transport toward the NW, while another predicts fluxes peaking later and transport toward the WSW. Vortex activity is predicted to peak in summer and dip around winter solstice, and to be greater than at InSight and much greater than in Gale crater. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-020-00788-2.
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Affiliation(s)
| | - M. de la Torre Juárez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91001 USA
| | - J. Pla-García
- Centro de Astrobiología (CSIC-INTA), 28850 Madrid, Spain
- Space Science Institute, Boulder, CO 80301 USA
| | | | | | - L. Neary
- Belgian Institute for Space Aeronomy, Brussels, Belgium
| | | | - F. Forget
- Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), 75005 Paris, France
| | - A. Spiga
- Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), 75005 Paris, France
- Institut Universitaire de France, 75005 Paris, France
| | | | - F. Daerden
- Belgian Institute for Space Aeronomy, Brussels, Belgium
| | - T. Bertrand
- Ames Research Center, Mountain View, CA USA
- LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
| | | | - R. Sullivan
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853 USA
| | | | - B. Chide
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE), Toulouse, France
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Korablev OI, Dobrolensky Y, Evdokimova N, Fedorova AA, Kuzmin RO, Mantsevich SN, Cloutis EA, Carter J, Poulet F, Flahaut J, Griffiths A, Gunn M, Schmitz N, Martín-Torres J, Zorzano MP, Rodionov DS, Vago JL, Stepanov AV, Titov AY, Vyazovetsky NA, Trokhimovskiy AY, Sapgir AG, Kalinnikov YK, Ivanov YS, Shapkin AA, Ivanov AY. Infrared Spectrometer for ExoMars: A Mast-Mounted Instrument for the Rover. ASTROBIOLOGY 2017; 17:542-564. [PMID: 28731817 DOI: 10.1089/ast.2016.1543] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
ISEM (Infrared Spectrometer for ExoMars) is a pencil-beam infrared spectrometer that will measure reflected solar radiation in the near infrared range for context assessment of the surface mineralogy in the vicinity of the ExoMars rover. The instrument will be accommodated on the mast of the rover and will be operated together with the panoramic camera (PanCam), high-resolution camera (HRC). ISEM will study the mineralogical and petrographic composition of the martian surface in the vicinity of the rover, and in combination with the other remote sensing instruments, it will aid in the selection of potential targets for close-up investigations and drilling sites. Of particular scientific interest are water-bearing minerals, such as phyllosilicates, sulfates, carbonates, and minerals indicative of astrobiological potential, such as borates, nitrates, and ammonium-bearing minerals. The instrument has an ∼1° field of view and covers the spectral range between 1.15 and 3.30 μm with a spectral resolution varying from 3.3 nm at 1.15 μm to 28 nm at 3.30 μm. The ISEM optical head is mounted on the mast, and its electronics box is located inside the rover's body. The spectrometer uses an acousto-optic tunable filter and a Peltier-cooled InAs detector. The mass of ISEM is 1.74 kg, including the electronics and harness. The science objectives of the experiment, the instrument design, and operational scenarios are described. Key Words: ExoMars-ISEM-Mars-Surface-Mineralogy-Spectroscopy-AOTF-Infrared. Astrobiology 17, 542-564.
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Affiliation(s)
| | | | | | | | - Ruslan O Kuzmin
- 1 Space Research Institute IKI , Moscow, Russia
- 2 Vernadsky Institute of Geochemistry and Analytical Chemistry GEOKHI , Moscow, Russia
| | - Sergei N Mantsevich
- 1 Space Research Institute IKI , Moscow, Russia
- 3 Department of Physics, Lomonosov Moscow State University , Russia
| | | | - John Carter
- 5 Institut d'Astrophysique Spatiale IAS-CNRS/Université Paris Sud , Orsay, France
| | - Francois Poulet
- 5 Institut d'Astrophysique Spatiale IAS-CNRS/Université Paris Sud , Orsay, France
| | - Jessica Flahaut
- 6 Université Lyon 1 , ENS-Lyon, CNRS, UMR 5276 LGL-TPE, Villeurbanne, France
| | - Andrew Griffiths
- 7 Mullard Space Science Laboratory, University College London , Dorking, United Kingdom
| | - Matthew Gunn
- 8 Department of Physics, Aberystwyth University , Aberystwyth, United Kingdom
| | | | - Javier Martín-Torres
- 10 Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology , Kiruna, Sweden
- 11 Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR) , Granada, Spain
| | - Maria-Paz Zorzano
- 10 Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology , Kiruna, Sweden
- 12 Centro de Astrobiología (INTA-CSIC) , Madrid, Spain
| | | | | | - Alexander V Stepanov
- 1 Space Research Institute IKI , Moscow, Russia
- 3 Department of Physics, Lomonosov Moscow State University , Russia
| | | | | | | | | | - Yurii K Kalinnikov
- 14 National Research Institute for Physicotechnical and Radio Engineering Measurements VNIIFTRI , Mendeleevo, Russia
| | - Yurii S Ivanov
- 15 Main Astronomical Observatory MAO NASU , Kyiv, Ukraine
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Misra A, Meadows V, Claire M, Crisp D. Using dimers to measure biosignatures and atmospheric pressure for terrestrial exoplanets. ASTROBIOLOGY 2014; 14:67-86. [PMID: 24432758 PMCID: PMC3928785 DOI: 10.1089/ast.2013.0990] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/04/2023]
Abstract
We present a new method to probe atmospheric pressure on Earth-like planets using (O2-O2) dimers in the near-infrared. We also show that dimer features could be the most readily detectable biosignatures for Earth-like atmospheres and may even be detectable in transit transmission with the James Webb Space Telescope (JWST). The absorption by dimers changes more rapidly with pressure and density than that of monomers and can therefore provide additional information about atmospheric pressures. By comparing the absorption strengths of rotational and vibrational features to the absorption strengths of dimer features, we show that in some cases it may be possible to estimate the pressure at the reflecting surface of a planet. This method is demonstrated by using the O2 A band and the 1.06 μm dimer feature, either in transmission or reflected spectra. It works best for planets around M dwarfs with atmospheric pressures between 0.1 and 10 bar and for O2 volume mixing ratios above 50% of Earth's present-day level. Furthermore, unlike observations of Rayleigh scattering, this method can be used at wavelengths longer than 0.6 μm and is therefore potentially applicable, although challenging, to near-term planet characterization missions such as JWST. We also performed detectability studies for JWST transit transmission spectroscopy and found that the 1.06 and 1.27 μm dimer features could be detectable (SNR>3) for an Earth analogue orbiting an M5V star at a distance of 5 pc. The detection of these features could provide a constraint on the atmospheric pressure of an exoplanet and serve as biosignatures for oxygenic photosynthesis. We calculated the required signal-to-noise ratios to detect and characterize O2 monomer and dimer features in direct imaging-reflected spectra and found that signal-to-noise ratios greater than 10 at a spectral resolving power of R=100 would be required.
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Affiliation(s)
- Amit Misra
- University of Washington Astronomy Department, Seattle, Washington, USA
- NAI Virtual Planetary Laboratory, Seattle, Washington, USA
- University of Washington Astrobiology Program, Seattle, Washington, USA
| | - Victoria Meadows
- University of Washington Astronomy Department, Seattle, Washington, USA
- NAI Virtual Planetary Laboratory, Seattle, Washington, USA
- University of Washington Astrobiology Program, Seattle, Washington, USA
| | - Mark Claire
- NAI Virtual Planetary Laboratory, Seattle, Washington, USA
- Department of Earth and Environmental Sciences, University of St Andrews, Fife, Scotland
- Blue Marble Space Institute of Science, Seattle, Washington, USA
| | - Dave Crisp
- NAI Virtual Planetary Laboratory, Seattle, Washington, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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Sprague AL, Boynton WV, Forget F, Lian Y, Richardson M, Starr R, Metzger AE, Hamara D, Economou T. Interannual similarity and variation in seasonal circulation of Mars' atmospheric Ar as seen by the Gamma Ray Spectrometer on Mars Odyssey. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003873] [Citation(s) in RCA: 36] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Inada A, Garcia-Comas M, Altieri F, Gwinner K, Poulet F, Bellucci G, Keller HU, Markiewicz WJ, Richardson MI, Hoekzema N, Neukum G, Bibring JP. Dust haze in Valles Marineris observed by HRSC and OMEGA on board Mars Express. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002893] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Spiga A, Forget F, Dolla B, Vinatier S, Melchiorri R, Drossart P, Gendrin A, Bibring JP, Langevin Y, Gondet B. Remote sensing of surface pressure on Mars with the Mars Express/OMEGA spectrometer: 2. Meteorological maps. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002870] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Aymeric Spiga
- Laboratoire de Météorologie Dynamique; Institut Pierre-Simon Laplace; Paris France
| | - François Forget
- Laboratoire de Météorologie Dynamique; Institut Pierre-Simon Laplace; Paris France
| | - Bastien Dolla
- Laboratoire de Météorologie Dynamique; Institut Pierre-Simon Laplace; Paris France
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