[ { "id": "authors:d9cc1-3zw74", "collection": "authors", "collection_id": "d9cc1-3zw74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190830-125811893", "type": "article", "title": "Phobos LIFE (Living Interplanetary Flight Experiment)", "author": [ { "family_name": "Betts", "given_name": "Bruce H.", "orcid": "0000-0002-4423-5800", "clpid": "Betts-B-H" }, { "family_name": "Warmflash", "given_name": "David", "clpid": "Warmflash-D" }, { "family_name": "Fraze", "given_name": "Raymond E.", "clpid": "Fraze-R-E" }, { "family_name": "Friedman", "given_name": "Louis", "clpid": "Friedman-L" }, { "family_name": "Vorobyova", "given_name": "Elena", "clpid": "Vorobyova-E" }, { "family_name": "Lilburn", "given_name": "Timothy G.", "clpid": "Lilburn-T-G" }, { "family_name": "Smith", "given_name": "Amy", "clpid": "Smith-Amy" }, { "family_name": "Rettberg", "given_name": "Petra", "orcid": "0000-0003-4439-2395", "clpid": "Rettberg-P" }, { "family_name": "J\u00f6nsson", "given_name": "K. Ingemar", "clpid": "J\u00f6nsson-K-I" }, { "family_name": "Ciftcioglu", "given_name": "Neva", "clpid": "Ciftcioglu-N" }, { "family_name": "Fox", "given_name": "George E.", "orcid": "0000-0001-7767-8387", "clpid": "Fox-G-E" }, { "family_name": "Svitek", "given_name": "Tomas", "clpid": "Svitek-T" }, { "family_name": "Kirschvink", "given_name": "Joseph L.", "orcid": "0000-0001-9486-6689", "clpid": "Kirschvink-J-L" }, { "family_name": "Moeller", "given_name": "Ralf", "clpid": "Moeller-R" }, { "family_name": "Wassmann", "given_name": "Marko", "clpid": "Wassmann-M" }, { "family_name": "Berger", "given_name": "Thomas", "clpid": "Berger-T" } ], "abstract": "The Planetary Society's Phobos Living Interplanetary Flight Experiment (Phobos LIFE) flew in the sample return capsule of the Russian Federal Space Agency's Phobos Grunt mission and was to have been a test of one aspect of the hypothesis that life can move between nearby planets within ejected rocks. Although the Phobos Grunt mission failed, we present here the scientific and engineering design and motivation of the Phobos LIFE experiment to assist with the scientific and engineering design of similar future experiments. Phobos LIFE flew selected organisms in a simulated meteoroid. The 34-month voyage would have been the first such test to occur in the high-radiation environment outside the protection of Earth's magnetosphere for more than a few days. The patented Phobos LIFE \"biomodule\" is an 88\u2009g cylinder consisting of a titanium outer shell, several types of redundant seals, and 31 individual Delrin sample containers. Phobos LIFE contained 10 different organisms, representing all three domains of life, and one soil sample. The organisms are all very well characterized, most with sequenced genomes. Most are extremophiles, and most have flown in low Earth orbit. Upon return from space, the health and characteristics of organisms were to have been compared with controls that remained on Earth and have not yet been opened.", "doi": "10.1089/ast.2018.1904", "issn": "1531-1074", "publisher": "Mary Ann Liebert", "publication": "Astrobiology", "publication_date": "2019-09", "series_number": "9", "volume": "19", "issue": "9", "pages": "1177-1185" }, { "id": "authors:f44ha-vxv06", "collection": "authors", "collection_id": "f44ha-vxv06", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140630-094825024", "type": "article", "title": "Thermal inertias in the upper millimeters of the Martian surface derived using Phobos' shadow", "author": [ { "family_name": "Betts", "given_name": "Bruce H.", "orcid": "0000-0002-4423-5800", "clpid": "Betts-B-H" }, { "family_name": "Murray", "given_name": "Bruce C.", "clpid": "Murray-B-C" }, { "family_name": "Sv\u00edtek", "given_name": "Tom\u00e1\u0161", "clpid": "Sv\u00edtek-T" } ], "abstract": "The first thermal images of Phobos' shadow on the surface of Mars, in addition to simultaneous visible images, were obtained by the Phobos '88 Termoskan instrument. The best observed shadow occurrence was on the flanks of Arsia Mons. For this occurrence, we combined the observed decrease in visible illumination of the surface with the observed decrease in brightness temperature to calculate thermal inertias of the Martian surface. The most realistic of our three models of eclipse cooling improves upon our preliminary model by including nonisothermal initial conditions and downward atmospheric flux. Most of our derived inertias fall within the range 38 to 59 J m^(\u22122) s^(\u22121)/2 K^(\u22121) (0.9 to 1.4 10\u22123 cal cm^(\u22122) s^(\u22121)/2 K^(\u22121)), corresponding to dust-sized particles (for a homogeneous surface), consistent with previous theories of Tharsis as a current area of dust deposition. Viking infrared thermal mapper (IRTM) inertias are diurnally derived and are sensitive to centimeter depths, whereas the shadow-derived inertias sample the upper tenths of a millimeter of the surface. The shadow-derived inertias are lower than those derived from Viking IRTM measurements (84 to 147), however, uncertainties in both sets of derived inertias make conclusions about layering tenuous. Thus, near-surface millimeter versus centimeter layering may exist in this region, but if it does, it is likely not very significant. Both eclipse and diurnal inertias appear to increase near the eastern end of the shadow occurrence. We also analyzed a shadow occurrence near the crater Herschel that showed no observed cooling. This analysis was limited by cool morning temperatures and instrument sensitivity, but yielded a lower bound of 80 on eclipse inertias in that region. Based upon our results, we strongly recommend future spacecraft thermal observations of Phobos' shadow, and suggest that they will be most useful if they improve upon Termoskan's geographic and temporal coverage and its accuracy.", "doi": "10.1029/95JE00226", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "1995-03-25", "series_number": "E3", "volume": "100", "issue": "E3", "pages": "5285-5296" }, { "id": "authors:xqhtw-gax68", "collection": "authors", "collection_id": "xqhtw-gax68", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140415-090236800", "type": "article", "title": "Thermal studies of Martian channels and valleys using Termoskan data", "author": [ { "family_name": "Betts", "given_name": "Bruce H.", "orcid": "0000-0002-4423-5800", "clpid": "Betts-B-H" }, { "family_name": "Murray", "given_name": "Bruce C.", "clpid": "Murray-B-C" } ], "abstract": "The Termoskan instrument on board the Phobos '88 spacecraft acquired the highest spatial resolution thermal infrared emission data ever obtained for Mars. Included in the thermal images are 2 km/pixel, midday observations of several major channel and valley systems including significant portions of Shalbatana, Ravi, Al-Qahira, and Ma'adim Valles, the channel connecting Valles Marineris with Hydraotes Chaos, and channel material in Eos Chasma. Termoskan also observed small portions of the southern beginnings of Simud, Tiu, and Ares Valles and some channel material in Gangis Chasma. Simultaneous broadband visible reflectance data were obtained for all but Ma'adim Vallis. We find that most of the channels and valleys have higher thermal inertias than their surroundings, consistent with previous thermal studies. We show for the first time that the thermal inertia boundaries closely match flat channel floor boundaries. Also, buttes within channels have inertias similar to the plains surrounding the channels, suggesting the buttes are remnants of a contiguous plains surface. Lower bounds on typical channel thermal inertias range from 8.4 to 12.5 (10^(\u22123) cal cm^(\u22122) s^(\u22121/2) K^(\u22121)) (352 to 523 in SI units of J m^(\u22122) s^(\u22121/2) K^(\u22121)). Lower bounds on inertia differences with the surrounding heavily cratered plains range from 1.1 to 3.5 (46 to 147 SI). Atmospheric and geometric effects are not sufficient to cause the observed channel inertia enhancements. We favor nonaeolian explanations of the overall channel inertia enhancements based primarily upon the channel floors' thermal homogeneity and the strong correlation of thermal boundaries with floor boundaries. However, localized, dark regions within some channels are likely aeolian in nature as reported previously. Most channels with increased inertias have fretted morphologies such as flat floors with steep walls. Eastern Ravi and southern Ares Valles, the only major channel sections observed that have obvious catastrophic flood bedforms, do not have enhanced inertias. Therefore, we favor fretting processes over catastrophic flooding for explaining the inertia enhancements. We postulate that the inertia enhancements were caused either by the original fretting process or by a process involving the bonding of fines due to an increased availability of water, either initially or secondarily.", "doi": "10.1029/93JE03173", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "1994-01-25", "series_number": "E1", "volume": "99", "issue": "E1", "pages": "1983-1996" }, { "id": "authors:emmn9-bd143", "collection": "authors", "collection_id": "emmn9-bd143", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-152254992", "type": "article", "title": "Thermally distinct ejecta blankets from Martian craters", "author": [ { "family_name": "Betts", "given_name": "Bruce H.", "orcid": "0000-0002-4423-5800", "clpid": "Betts-B-H" }, { "family_name": "Murray", "given_name": "Bruce C.", "clpid": "Murray-B-C" } ], "abstract": "Utilizing the Termoskan data set of the Phobos '88 mission we have recognized a new feature on Mars: ejecta blanket distinct in the thermal infrared (EDITH). Virtually all of the more than 100 features discovered in the Termoskan data are located on the plains near Valles Marineris. EDITHs have a startlingly clear dependence upon terrains of Hesperian age, implying a spatial or temporal dependence on Hesperian terrains. Almost no thermally distinct ejecta blankets are associated with any of the thousands of craters within the data set that occur on the older Noachian units. EDITHs also do not appear on the portions of the younger Tharsis Amazonian units seen in the data. The Hesperian terrain dependence cannot be explained by either atmospheric or impactor variations; Noachian and Hesperian terrains must have experienced identical atmospheric and impactor conditions during Hesperian times. Thermally distinct ejecta blankets therefore reflect target material differences and/or secondary modification processes. Not all lobate ejecta blankets are thermally distinct, but all EDITHs correlated with visibly discernible ejecta blankets are associated with lobate ejecta blankets. The boundaries of the thermally distinct areas usually follow closely the termini of the fluidized lobate ejecta blankets, even when the ejecta blankets show a high degree of sinuosity. Thus, the thermally distinct nature of EDITHs must be due to the primary ejecta formation process. The coupling of these thermal anomalies to morphology is unlike most sharp Martian inertia variations which are decoupled from observed surface morphology. Some thermally distinct ejecta blankets occur near otherwise similar craters that do not have thermally distinct ejecta blankets. Thus, wind patterns or locally available aeolian material cannot provide a single overall explanation for the observed variations. We compiled a data base of 110 EDITH and non-EDITH craters ranging in diameter from 4.2 km to 90.6 km. There are almost no correlations within the data base other than occurrence on Hesperian terrains. We postulate that most of the observed EDITHs are due to excavation of thermally distinctive Noachian age material from beneath a relatively thin layer of younger, more consolidated Hesperian volcanic material. The plausibility of this theory is supported by much geological evidence for relatively thin near-surface Hesperian deposits overlying massive Noachian megabreccias on the EDITH-rich plains units. We suggest that absence of thermally distinct ejecta blankets on Noachian and Amazonian terrains is due to absences of distinctive near-surface layering. Thermally distinct ejecta blankets are excellent locations for future landers and remote sensing because of relatively dust free surface exposures of material excavated from depth.", "doi": "10.1029/93JE00107", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research E", "publication_date": "1993-06-25", "series_number": "E6", "volume": "98", "issue": "E6", "pages": "11043-11059" }, { "id": "authors:ge93n-nft13", "collection": "authors", "collection_id": "ge93n-nft13", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140410-092259617", "type": "article", "title": "Preliminary assessment of Termoskan observations of Mars", "author": [ { "family_name": "Murray", "given_name": "B.", "clpid": "Murray-B-C" }, { "family_name": "Naraeva", "given_name": "M. K.", "clpid": "Naraeva-M-K" }, { "family_name": "Selivanov", "given_name": "A. S.", "clpid": "Selivanov-A-S" }, { "family_name": "Betts", "given_name": "B. H.", "orcid": "0000-0002-4423-5800", "clpid": "Betts-B-H" }, { "family_name": "Svitek", "given_name": "T.", "clpid": "Svitek-T" }, { "family_name": "Kharlamov", "given_name": "V. D.", "clpid": "Kharlamov-V-D" }, { "family_name": "Romanov", "given_name": "A. V.", "clpid": "Romanov-A-V" }, { "family_name": "Santee", "given_name": "M. L.", "clpid": "Santee-M-L" }, { "family_name": "Gektin", "given_name": "Y. M.", "clpid": "Gektin-Y-M" }, { "family_name": "Fomin", "given_name": "D. A.", "clpid": "Fomin-D-A" }, { "family_name": "Paige", "given_name": "D. A.", "clpid": "Paige-D-A" }, { "family_name": "Panfilov", "given_name": "A. S.", "clpid": "Panfilov-A-S" }, { "family_name": "Crisp", "given_name": "D.", "orcid": "0000-0002-4573-9998", "clpid": "Crisp-D" }, { "family_name": "Head", "given_name": "J. W.", "orcid": "0000-0003-2013-560X", "clpid": "Head-J-W" }, { "family_name": "Murchie", "given_name": "S. L.", "orcid": "0000-0002-1616-8751", "clpid": "Murchie-S-L" }, { "family_name": "Martin", "given_name": "T. Z.", "clpid": "Martin-T-Z" } ], "abstract": "In February and March, 1989, the Termoskan instrument onboard the Phobos '88 spacecraft acquired a limited set of very high resolution observations of the 8\u201312 \u03bcm thermal emission from Mars' equatorial regions. Simultaneous and coincident observations were acquired in the 0.5 to 1.0 \u03bcm region also. We have evaluated quantitatively about 25% of those data and find close agreement with the lower-resolution Viking Orbiter Infrared Thermal Mapper (IRTM) observations, demonstrating the accuracy of the Termoskan system. Termoskan's thermal emission panoramas display limb brightening at the morning limb, which we interpret as arising from the presence of a diurnal ice crystal haze there. Detached hazes at high altitude also are evident in the visible panorama of the evening limb. The Phobos '88 orbit enabled Termoskan to record the visible shadow from the Martian moonlet Phobos and to measure the surface thermal response to that shadow's passage. Analysis of one such data set shows that the uppermost fraction of a millimeter is two to four times more insulating than the uppermost centimeters sensed by the IRTM experiment. The Termoskan data are of direct importance to the planning and execution of the PMIRR and TES experiments of the U.S. Mars Observer mission to be launched in 1992. An improved version of Termoskan is planned for the Mars '94 mission of the U.S.S.R. Those data will be of still higher surface resolution and, thus, complement well the expected PMIRR and TES global data sets.", "doi": "10.1016/0032-0633(91)90147-3", "issn": "0032-0633", "publisher": "Elsevier", "publication": "Planetary and Space Science", "publication_date": "1991-01", "series_number": "1-2", "volume": "39", "issue": "1-2", "pages": "237-265" } ]