Janice Bishop

Last updated
Janice L. Bishop
Alma materBrown University
Scientific career
Thesis Spectroscopic analyses of chemically altered montmorillonites and applications to the soils on Mars  (1994)
Doctoral advisor John O. Edwards

Janice Bishop is a planetary scientist known for her research into the minerals found on Mars.

Contents

Education and career

In 1988, Bishop earned a B.S. in chemistry and an M.S. in Applied Earth Science from Stanford University. [1] She earned her Ph.D. from Brown University in 1994 and then was a postdoctoral associate at the German Aerospace Center in Berlin until 1997. From 1997 to 1999 she was a fellow at the National Aeronautics Space Agency (NASA) Ames Research Center before becoming a research scientist at the SETI Institute. [1] Starting in 2015 she joined the Science Council at the SETI Institute and is a contractor at the NASA Ames Research Center. [1]

In 2020 [2] she was elected a fellow of the American Geophysical Union for:

...enabling the discovery of phyllosilicates on Mars and for making critical discoveries regarding the climate history of Mars

Research

Bishop uses Raman spectroscopy to examine minerals that may be found on Mars [3] and examines minerals on Earth that serve as proxies for conditions on Mars. [4] Through this research Bishop has analyzed water in minerals such as montmorillonite [5] and used hyperspectral imaging to identify phyllosilicates on minerals from Earth. [6] On Mars, Bishop's research revealed these phyllosilicates are indicative of the presence of water. [7] In 2011, Bishop examined carbonate rocks in the Mojave Desert as an analogue for conditions that may occur on Mars [8] and her subsequent research revealed the wide-spread presence of rocks with carbonate on Mars [9] which could be indicative of potential life on Mars. [10] Using data from instruments on the Curiosity rover, Bishop and colleagues found presence of glauconitic clays which only form in bodies of water that remain still for long periods of time. [11] [12] In 2021, Bishop determined that dark streaks on Mars, called recurring slope lineae, can be the result of the interactions of sulfates and chlorine salts that absorb water, a condition that leads to landslides. [13] [14]

Selected publications

Awards and honors

Related Research Articles

<span class="mw-page-title-main">Noctis Labyrinthus</span> Labyrinthus on Mars

Noctis Labyrinthus is a region of Mars located in the Phoenicis Lacus quadrangle, between Valles Marineris and the Tharsis upland. The region is notable for its maze-like system of deep, steep-walled valleys. The valleys and canyons of this region formed by faulting and many show classic features of grabens, with the upland plain surface preserved on the valley floor. In some places the valley floors are rougher, disturbed by landslides, and there are places where the land appears to have sunk down into pit-like formations. It is thought that this faulting was triggered by volcanic activity in the Tharsis region. Research described in December 2009 found a variety of minerals, including clays, sulfates, and hydrated silicas, in some of the layers.

<span class="mw-page-title-main">Clay mineral</span> Fine-grained aluminium phyllosilicates

Clay minerals are hydrous aluminium phyllosilicates (e.g. kaolin, Al2Si2O5(OH)4), sometimes with variable amounts of iron, magnesium, alkali metals, alkaline earths, and other cations found on or near some planetary surfaces.

<span class="mw-page-title-main">Compact Reconnaissance Imaging Spectrometer for Mars</span> Visible-infrared spectrometer

The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) was a visible-infrared spectrometer aboard the Mars Reconnaissance Orbiter searching for mineralogic indications of past and present water on Mars. The CRISM instrument team comprised scientists from over ten universities and was led by principal investigator Scott Murchie. CRISM was designed, built, and tested by the Johns Hopkins University Applied Physics Laboratory.

<span class="mw-page-title-main">Isidis Planitia</span> Crater on Mars

Isidis Planitia is a plain located within a giant impact basin on Mars, located partly in the Syrtis Major quadrangle and partly in the Amenthes quadrangle. At approximately 1,500 km (930 mi) in diameter, it is the third-largest obvious impact structure on the planet, after the Hellas and Argyre basins. Isidis was likely the last major basin to be formed on Mars, having formed approximately 3.9 billion years ago during the Noachian period. Due to dust coverage, it typically appears bright in telescopic views, and was mapped as a classical albedo feature, Isidis Regio, visible by telescope in the pre-spacecraft era.

<span class="mw-page-title-main">Eberswalde (crater)</span> Crater on Mars

Eberswalde, formerly known as Holden NE, is a partially buried impact crater in Margaritifer Terra, Mars. Eberswalde crater lies just to the north of Holden, a large crater that may have been a lake. The 65.3-km-diameter crater, centered at 24°S, 33°W, is named after the German town of the same name, in accordance with the International Astronomical Union's rules for planetary nomenclature. It was one of the final four proposed landing sites for the Mars rover Mars Science Laboratory mission. This extraterrestrial geological feature lies situated within the Margaritifer Sinus quadrangle (MC-19) region of Mars. Although not chosen, it was considered a potential landing site for the Mars 2020 Perseverance rover, and in the second Mars 2020 Landing Site Workshop it survived the cut and was among the top eight sites still in the running.

<span class="mw-page-title-main">Huygens (crater)</span> Crater on Mars

Huygens is an impact crater on Mars named in honour of the Dutch astronomer, mathematician and physicist Christiaan Huygens. It is the fifth largest recognizable impact crater on Mars after Utopia, Hellas, Argyre, and Isidis, and the largest one with a near intact rim.

<span class="mw-page-title-main">Carbonates on Mars</span> Overview of the presence of carbonates on Mars

Evidence for carbonates on Mars was first discovered in 2008. Previously, most remote sensing instruments such as OMEGA and THEMIS—sensitive to infrared emissivity spectral features of carbonates—had not suggested the presence of carbonate outcrops, at least at the 100 m or coarser spatial scales available from the returned data.

<span class="mw-page-title-main">Mawrth Vallis</span> Valley on Mars

Mawrth Vallis is a valley on Mars, located in the Oxia Palus quadrangle at 22.3°N, 343.5°E with an elevation approximately two kilometers below datum. Situated between the southern highlands and northern lowlands, the valley is a channel formed by massive flooding which occurred in Mars’ ancient past. It is an ancient water outflow channel with light-colored clay-rich rocks.

<span class="mw-page-title-main">Nili Fossae</span> Group of large, concentric grabens on Mars,

Nili Fossae is a group of large, concentric grabens on Mars, in the Syrtis Major quadrangle. They have been eroded and partly filled in by sediments and clay-rich ejecta from a nearby giant impact crater, the Isidis basin. It is at approximately 22°N, 75°E, and has an elevation of −0.6 km (−0.37 mi). Nili Fossae was on the list of potential landing sites of the Mars Science Laboratory, arriving in 2012, but was dropped before the final four sites were determined. Although not among the last finalists, in September 2015 it was selected as a potential landing site for the Mars 2020 rover, which will use the same design as Curiosity, but with a different payload focused on astrobiology. Nili Fossae is also considered ideal for future human exploration, with the prominent Gavin Crater at 21.43°N, 76.93°E considered the most likely landing zone in Nili Fossae.

<span class="mw-page-title-main">Jezero (crater)</span> Crater on Mars

Jezero is a crater on Mars in the Syrtis Major quadrangle, about 45.0 km (28.0 mi) in diameter. Thought to have once been flooded with water, the crater contains a fan-delta deposit rich in clays. The lake in the crater was present when valley networks were forming on Mars. Besides having a delta, the crater shows point bars and inverted channels. From a study of the delta and channels, it was concluded that the lake inside the crater probably formed during a period in which there was continual surface runoff.

<span class="mw-page-title-main">Columbus (crater)</span> Crater on Mars

Columbus is a crater in the Terra Sirenum of Mars. It is 119 km in diameter and was named after Christopher Columbus, Italian explorer (1451–1506). The discovery of sulfates and clay minerals in sediments within Columbus crater are strong evidence that a lake once existed in the crater. Research with an orbiting near-infrared spectrometer, which reveals the types of minerals present based on the wavelengths of light they absorb, found evidence of layers of both clay and sulfates in Columbus crater. This is exactly what would appear if a large lake had slowly evaporated. Moreover, because some layers contained gypsum, a sulfate which forms in relatively fresh water, life could have formed in the crater.

The mineralogy of Mars is the chemical composition of rocks and soil that encompass the surface of Mars. Various orbital crafts have used spectroscopic methods to identify the signature of some minerals. The planetary landers performed concrete chemical analysis of the soil in rocks to further identify and confirm the presence of other minerals. The only samples of Martian rocks that are on Earth are in the form of meteorites. The elemental and atmospheric composition along with planetary conditions is essential in knowing what minerals can be formed from these base parts.

<span class="mw-page-title-main">Groundwater on Mars</span> Water held in permeable ground

During past ages, there was rain and snow on Mars; especially in the Noachian and early Hesperian epochs. Some moisture entered the ground and formed aquifers. That is, the water went into the ground, seeped down until it reached a formation that would not allow it to penetrate further. Water then accumulated forming a saturated layer. Deep aquifers may still exist.

<span class="mw-page-title-main">Composition of Mars</span> Branch of the geology of Mars

The composition of Mars covers the branch of the geology of Mars that describes the make-up of the planet Mars.

<span class="mw-page-title-main">Flammarion (Martian crater)</span> Crater on Mars

Flammarion is an impact crater in the Syrtis Major quadrangle on Mars at 25.2 ° N and 48.3 ° E. It is 173.0 km in diameter. Its name was approved in 1973, and refers to French astronomer Camille Flammarion. There may have been a lake in the crater in the past because a channel is present on the northern rim, and sedimentary layers are present within the crater.

<span class="mw-page-title-main">Lakes on Mars</span> Overview of the presence of lakes on Mars

In summer 1965, the first close-up images from Mars showed a cratered desert with no signs of water. However, over the decades, as more parts of the planet were imaged with better cameras on more sophisticated satellites, Mars showed evidence of past river valleys, lakes and present ice in glaciers and in the ground. It was discovered that the climate of Mars displays huge changes over geologic time because its axis is not stabilized by a large moon, as Earth's is. Also, some researchers maintain that surface liquid water could have existed for periods of time due to geothermal effects, chemical composition or asteroid impacts. This article describes some of the places that could have held large lakes.

<span class="mw-page-title-main">Northeast Syrtis</span>

Northeast Syrtis is a region of Mars once considered by NASA as a landing site for the Mars 2020 rover mission. This landing site failed in the competition with Jezero crater, another landing site dozens of kilometers away from Northeast Syrtis. It is located in the northern hemisphere of Mars at coordinates 18°N,77°E in the northeastern part of the Syrtis Major volcanic province, within the ring structure of Isidis impact basin as well. This region contains diverse morphological features and minerals, indicating that water once flowed here. It may be an ancient habitable environment; microbes could have developed and thrived here.

<span class="mw-page-title-main">Bethany Ehlmann</span> American planetary scientist

Bethany List Ehlmann is a professor of Planetary Science at California Institute of Technology and a Research Scientist at the Jet Propulsion Laboratory.

Astropedology is the study of very ancient paleosols and meteorites relevant to the origin of life and different planetary soil systems. It is a branch of soil science (pedology) concerned with soils of the distant geologic past and of other planetary bodies to understand our place in the universe. A geologic definition of soil is “a material at the surface of a planetary body modified in place by physical, chemical or biological processes”. Soils are sometimes defined by biological activity but can also be defined as planetary surfaces altered in place by biologic, chemical, or physical processes. By this definition, the question for Martian soils and paleosols becomes, were they alive? Astropedology symposia are a new focus for scientific meetings on soil science. Advancements in understanding the chemical and physical mechanisms of pedogenesis on other planetary bodies in part led the Soil Science Society of America (SSSA) in 2017 to update the definition of soil to: "The layer(s) of generally loose mineral and/or organic material that are affected by physical, chemical, and/or biological processes at or near the planetary surface and usually hold liquids, gases, and biota and support plants". Despite our meager understanding of extraterrestrial soils, their diversity may raise the question of how we might classify them, or formally compare them with our Earth-based soils. One option is to simply use our present soil classification schemes, in which case many extraterrestrial soils would be Entisols in the United States Soil Taxonomy (ST) or Regosols in the World Reference Base for Soil Resources (WRB). However, applying an Earth-based system to such dissimilar settings is debatable. Another option is to distinguish the (largely) biotic Earth from the abiotic Solar System, and include all non-Earth soils in a new Order or Reference Group, which might be tentatively called Astrosols.

<span class="mw-page-title-main">Spectroradiometry for Earth and planetary remote sensing</span>

Spectroradiometry is a technique in Earth and planetary remote sensing, which makes use of light behaviour, specifically how light energy is reflected, emitted, and scattered by substances in solid, liquid, or a gaseous states, in order to explore their properties in the electromagnetic (light) spectrum and identify or differentiate between substances. The interaction between light radiation and the surface of a given material determines the manner in which the radiation reflects back to a detector, i.e., a spectroradiometer. Combining the elements of spectroscopy and radiometry, spectroradiometry carries out precise measurements of electromagnetic radiation and associated parameters within different wavelength ranges. This technique forms the basis of multi- and hyperspectral imaging and reflectance spectroscopy, commonly applied across numerous geoscience disciplines, which evaluates the spectral properties exhibited by various materials found on Earth and planetary bodies.

References

  1. 1 2 3 "Bishop CV" (PDF). 2020.
  2. 1 2 "Bishop". Honors Program.
  3. ↑ Bishop, Janice L.; Murad, Enver (2004). "Characterization of minerals and biogeochemical markers on Mars: A Raman and IR spectroscopic study of montmorillonite". Journal of Raman Spectroscopy. 35 (6): 480–486. Bibcode:2004JRSp...35..480B. doi: 10.1002/jrs.1173 .
  4. ↑ Bishop, Janice L.; Murad, Enver (1 July 2005). "The visible and infrared spectral properties of jarosite and alunite". American Mineralogist. 90 (7): 1100–1107. Bibcode:2005AmMin..90.1100B. doi:10.2138/am.2005.1700. S2CID   11150685.
  5. ↑ Bishop, Janice L.; Pieters, Carlé M.; Edwards, John O. (1 December 1994). "Infrared Spectroscopic Analyses on the Nature of Water in Montmorillonite". Clays and Clay Minerals. 42 (6): 702–716. Bibcode:1994CCM....42..702B. doi:10.1346/CCMN.1994.0420606. S2CID   1748775.
  6. ↑ Bishop, J. L.; Lane, M. D.; Dyar, M. D.; Brown, A. J. (March 2008). "Reflectance and emission spectroscopy study of four groups of phyllosilicates: smectites, kaolinite-serpentines, chlorites and micas". Clay Minerals. 43 (1): 35–54. Bibcode:2008ClMin..43...35B. doi:10.1180/claymin.2008.043.1.03. S2CID   97373731.
  7. ↑ Bishop, J. L.; Dobrea, E. Z. N.; McKeown, N. K.; Parente, M.; Ehlmann, B. L.; Michalski, J. R.; Milliken, R. E.; Poulet, F.; Swayze, G. A.; Mustard, J. F.; Murchie, S. L.; Bibring, J.-P. (8 August 2008). "Phyllosilicate Diversity and Past Aqueous Activity Revealed at Mawrth Vallis, Mars". Science. 321 (5890): 830–833. Bibcode:2008Sci...321..830B. doi:10.1126/science.1159699. PMC   7007808 . PMID   18687963.
  8. ↑ Bishop, Janice L.; Schelble, Rachel T.; McKay, Christopher P.; Brown, Adrian J.; Perry, Kaysea A. (2011). "Carbonate rocks in the Mojave Desert as an analogue for Martian carbonates". International Journal of Astrobiology. 10 (4): 349–358. Bibcode:2011IJAsB..10..349B. doi:10.1017/S1473550411000206. ISSN   1473-5504. S2CID   122114343.
  9. ↑ Wray, James J.; Murchie, Scott L.; Bishop, Janice L.; Ehlmann, Bethany L.; Milliken, Ralph E.; Wilhelm, Mary Beth; Seelos, Kimberly D.; Chojnacki, Matthew (2016). "Orbital evidence for more widespread carbonate-bearing rocks on Mars". Journal of Geophysical Research: Planets. 121 (4): 652–677. Bibcode:2016JGRE..121..652W. doi: 10.1002/2015JE004972 . ISSN   2169-9100. S2CID   2327403.
  10. ↑ "Possible Dwellings of Early Life on Mars Identified". The Science Explorer. Retrieved 2021-07-13.
  11. ↑ Losa-Adams, Elisabeth; Gil-Lozano, Carolina; Fairén, Alberto G.; Bishop, Janice L.; Rampe, Elizabeth B.; Gago-Duport, Luis (2021-06-28). "Long-lasting habitable periods in Gale crater constrained by glauconitic clays". Nature Astronomy. 5 (9): 936–942. Bibcode:2021NatAs...5..936L. doi:10.1038/s41550-021-01397-x. ISSN   2397-3366. PMC   7611674 . PMID   34541329.
  12. ↑ "Could Clays Found in Ancient Gale Crater Lake on Mars Once Have Harbored Life?". SETI Institute. July 12, 2021.
  13. ↑ Bishop, J. L.; Yeşilbaş, M.; Hinman, N. W.; Burton, Z. F. M.; Englert, P. A. J.; Toner, J. D.; McEwen, A. S.; Gulick, V. C.; Gibson, E. K.; Koeberl, C. (February 2021). "Martian subsurface cryosalt expansion and collapse as trigger for landslides". Science Advances. 7 (6): eabe4459. Bibcode:2021SciA....7.4459B. doi:10.1126/sciadv.abe4459. PMC   7857681 . PMID   33536216.
  14. ↑ "Dark streaks on Mars may be caused by salts and melting ice | Space | EarthSky". earthsky.org. 2021-02-18. Retrieved 2021-07-13.
  15. ↑ "Janice Bishop". www.nasonline.org. Retrieved 2021-07-13.
  16. ↑ "Nine outstanding researchers receive Helmholtz International Fellow Awards". www.helmholtz.de. Retrieved 2021-07-13.
  17. ↑ "SETI's Dr. Janice Bishop Wins Award for Clay Science Research on Mars". May 25, 2016.
  18. ↑ "Marion L. and Chrystie M. Jackson Mid-Career Clay Scientist Award – The Clay Minerals Society".
  19. ↑ "GSA Fellowship". www.geosociety.org. Retrieved 2021-07-13.
  20. ↑ "MSA Fellows". www.minsocam.org. Retrieved 2021-07-13.
  21. ↑ "Janice Bishop Named AGU Fellow". November 18, 2020.
  22. ↑ "G. K. Gilbert Award - 2021". www.geosociety.org. Retrieved 2022-03-16.
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