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57. Seasonal seismic activity on Mars

Author

Knapmeyer, Martin, Stähler, Simon Christian, Daubar, Ingrid J., Forget, François, Spiga, Aymeric, Pierron, T., van Driel, Martin, Banfield, Don, Hauber, Ernst, Grott, Matthias, Muller, N., Perrin, Clément, Jacob, Alice, Lucas, Antoine, Knapmeyer-Endrun, Brigitte, Newman, Claire, Panning, Mark P., Weber, Renee, Calef, Fred J., Böse, Maren, Ceylan, Savas, Charalambous, Constantinos, Clinton, John Francis, Dahmen, Nikolaj, Giardini, Domenico, Horleston, Anna, Kawamura, Taichi, Khan, Amir, Mainsant, Guénolé, Plasman, Matthieu, Lemmon, Mark, Lorenz, Ralph, Pike, W.T., Scholz, John‐Robert, Lognonne, Philippe, and Banerdt, Bruce

Subjects
Phobos, seasonal seismic activity, 13. Climate action, Elysium Planitia, Mars, InSight
Abstract

The rate of occurrence of High Frequency (HF) marsquakes, as recorded by InSight at Homestead Hollow, Elysium Planitia, increased after about Ls =33°, and ceased almost completely by Ls =187°, following an apparently seasonal variation with a peak rate near aphelion. We define seismic rate models based on the declination of the Sun, annual solar tides, and the annual CO2 cycle as measured by atmospheric pressure. Evaluation of Akaike weights and evidence ratios shows that the declination of the Sun is the most likely, and the CO2 cycle the least likely driver of this seismic activity, although the discrimination is weak, and the occurrence of a few events in August 2020 is in favor for a triggering by CO2 ice load. We also show that no periodicity related to Phobos' orbit is present in the HF event sequence. Event rate forecasts are presented to allow further discrimination of candidate mechanisms from future observations., Earth and Planetary Science Letters, 576, ISSN:0012-821X, ISSN:1385-013X

58. The atmosphere of Mars as observed by InSight

Author

Banfield, Don, Spiga, Aymeric, Newman, Claire, Forget, François, Lemmon, Mark, Lorenz, Ralph, Murdoch, Naomi, Viudez-Moreiras, Daniel, Pla-Garcia, Jorge, Garcia, Raphael F., Logonne, Philippe, Karatekin, Ozgur, Perrin, Clement, Martire, Leo, Teanby, Nicholas, Van Hove, Bart, Maki, Justin N., Kenda, Balthasar, Mueller, Nils T., Rodriguez, Sebastian, Kawamura, Taichi, McClean, John B., Stott, Alexander E., Charalambous, Constantinos, Millour, Ehouran, Johnson, Catherine L., Mittelholz, Anna, Maattanen, Anni, Lewis, Stephen, Clinton, John, Stahler, Simon C., Ceylan, Savas, Giardini, Domenico, Warren, Tristram, Pike, William T., Daubar, Ingrid, Golombek, Matthew, Rolland, Lucie, Widmer-Schnidrig, Rudolf, Mimoun, David, Beucler, Eric, Jacob, Alice, Lucas, Antoine, Baker, Mariah, Ansan, Veronique, Hurst, Kenneth, Mora-Sotomayor, Luis, Navarro, Sara, Torres, Josefina, Lepinette, Alain, Molina, Antonio, Marin-Jimenez, Mercedes, Gomez-Elvira, Javier, Peinado, Veronica, Rodriguez-Manfredi, Jose-Antonio, Carcich, Brian T., Sackett, Stephen, Russell, Christopher T., Spohn, Tilman, Smrekar, Suzanne E., Banerdt, W. Bruce, Banfield, Don, Spiga, Aymeric, Newman, Claire, Forget, François, Lemmon, Mark, Lorenz, Ralph, Murdoch, Naomi, Viudez-Moreiras, Daniel, Pla-Garcia, Jorge, Garcia, Raphael F., Logonne, Philippe, Karatekin, Ozgur, Perrin, Clement, Martire, Leo, Teanby, Nicholas, Van Hove, Bart, Maki, Justin N., Kenda, Balthasar, Mueller, Nils T., Rodriguez, Sebastian, Kawamura, Taichi, McClean, John B., Stott, Alexander E., Charalambous, Constantinos, Millour, Ehouran, Johnson, Catherine L., Mittelholz, Anna, Maattanen, Anni, Lewis, Stephen, Clinton, John, Stahler, Simon C., Ceylan, Savas, Giardini, Domenico, Warren, Tristram, Pike, William T., Daubar, Ingrid, Golombek, Matthew, Rolland, Lucie, Widmer-Schnidrig, Rudolf, Mimoun, David, Beucler, Eric, Jacob, Alice, Lucas, Antoine, Baker, Mariah, Ansan, Veronique, Hurst, Kenneth, Mora-Sotomayor, Luis, Navarro, Sara, Torres, Josefina, Lepinette, Alain, Molina, Antonio, Marin-Jimenez, Mercedes, Gomez-Elvira, Javier, Peinado, Veronica, Rodriguez-Manfredi, Jose-Antonio, Carcich, Brian T., Sackett, Stephen, Russell, Christopher T., Spohn, Tilman, Smrekar, Suzanne E., and Banerdt, W. Bruce

Abstract

The atmosphere of Mars is thin, although rich in dust aerosols, and covers a dry surface. As such, Mars provides an opportunity to expand our knowledge of atmospheres beyond that attainable from the atmosphere of the Earth. The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander is measuring Mars’s atmosphere with unprecedented continu- ity, accuracy and sampling frequency. Here we show that InSight unveils new atmospheric phenomena at Mars, especially in the higher-frequency range, and extends our understanding of Mars’s meteorology at all scales. InSight is uniquely sensitive to large- scale and regional weather and obtained detailed in situ coverage of a regional dust storm on Mars. Images have enabled high- altitude wind speeds to be measured and revealed airglow—faint emissions produced by photochemical reactions—in the middle atmosphere. InSight observations show a paradox of aeolian science on Mars: despite having the largest recorded Martian vortex activity and dust-devil tracks close to the lander, no visible dust devils have been seen. Meteorological measurements have pro- duced a catalogue of atmospheric gravity waves, which included bores (soliton-like waves). From these measurements, we have discovered Martian infrasound and unexpected similarities between atmospheric turbulence on Earth and Mars. We suggest that the observations of Mars’s atmosphere by InSight will be key for prediction capabilities and future exploration.

59. The atmosphere of Mars as observed by InSight

Author

Banfield, Don, Spiga, Aymeric, Newman, Claire, Forget, François, Lemmon, Mark, Lorenz, Ralph, Murdoch, Naomi, Viudez-Moreiras, Daniel, Pla-Garcia, Jorge, Garcia, Raphael F., Logonne, Philippe, Karatekin, Ozgur, Perrin, Clement, Martire, Leo, Teanby, Nicholas, Van Hove, Bart, Maki, Justin N., Kenda, Balthasar, Mueller, Nils T., Rodriguez, Sebastian, Kawamura, Taichi, McClean, John B., Stott, Alexander E., Charalambous, Constantinos, Millour, Ehouran, Johnson, Catherine L., Mittelholz, Anna, Maattanen, Anni, Lewis, Stephen, Clinton, John, Stahler, Simon C., Ceylan, Savas, Giardini, Domenico, Warren, Tristram, Pike, William T., Daubar, Ingrid, Golombek, Matthew, Rolland, Lucie, Widmer-Schnidrig, Rudolf, Mimoun, David, Beucler, Eric, Jacob, Alice, Lucas, Antoine, Baker, Mariah, Ansan, Veronique, Hurst, Kenneth, Mora-Sotomayor, Luis, Navarro, Sara, Torres, Josefina, Lepinette, Alain, Molina, Antonio, Marin-Jimenez, Mercedes, Gomez-Elvira, Javier, Peinado, Veronica, Rodriguez-Manfredi, Jose-Antonio, Carcich, Brian T., Sackett, Stephen, Russell, Christopher T., Spohn, Tilman, Smrekar, Suzanne E., Banerdt, W. Bruce, Banfield, Don, Spiga, Aymeric, Newman, Claire, Forget, François, Lemmon, Mark, Lorenz, Ralph, Murdoch, Naomi, Viudez-Moreiras, Daniel, Pla-Garcia, Jorge, Garcia, Raphael F., Logonne, Philippe, Karatekin, Ozgur, Perrin, Clement, Martire, Leo, Teanby, Nicholas, Van Hove, Bart, Maki, Justin N., Kenda, Balthasar, Mueller, Nils T., Rodriguez, Sebastian, Kawamura, Taichi, McClean, John B., Stott, Alexander E., Charalambous, Constantinos, Millour, Ehouran, Johnson, Catherine L., Mittelholz, Anna, Maattanen, Anni, Lewis, Stephen, Clinton, John, Stahler, Simon C., Ceylan, Savas, Giardini, Domenico, Warren, Tristram, Pike, William T., Daubar, Ingrid, Golombek, Matthew, Rolland, Lucie, Widmer-Schnidrig, Rudolf, Mimoun, David, Beucler, Eric, Jacob, Alice, Lucas, Antoine, Baker, Mariah, Ansan, Veronique, Hurst, Kenneth, Mora-Sotomayor, Luis, Navarro, Sara, Torres, Josefina, Lepinette, Alain, Molina, Antonio, Marin-Jimenez, Mercedes, Gomez-Elvira, Javier, Peinado, Veronica, Rodriguez-Manfredi, Jose-Antonio, Carcich, Brian T., Sackett, Stephen, Russell, Christopher T., Spohn, Tilman, Smrekar, Suzanne E., and Banerdt, W. Bruce

Abstract

The atmosphere of Mars is thin, although rich in dust aerosols, and covers a dry surface. As such, Mars provides an opportunity to expand our knowledge of atmospheres beyond that attainable from the atmosphere of the Earth. The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander is measuring Mars’s atmosphere with unprecedented continu- ity, accuracy and sampling frequency. Here we show that InSight unveils new atmospheric phenomena at Mars, especially in the higher-frequency range, and extends our understanding of Mars’s meteorology at all scales. InSight is uniquely sensitive to large- scale and regional weather and obtained detailed in situ coverage of a regional dust storm on Mars. Images have enabled high- altitude wind speeds to be measured and revealed airglow—faint emissions produced by photochemical reactions—in the middle atmosphere. InSight observations show a paradox of aeolian science on Mars: despite having the largest recorded Martian vortex activity and dust-devil tracks close to the lander, no visible dust devils have been seen. Meteorological measurements have pro- duced a catalogue of atmospheric gravity waves, which included bores (soliton-like waves). From these measurements, we have discovered Martian infrasound and unexpected similarities between atmospheric turbulence on Earth and Mars. We suggest that the observations of Mars’s atmosphere by InSight will be key for prediction capabilities and future exploration.

62. Geometry and segmentation of the Cerberus Fossae fault system: implications on marsquake properties in Elysium Planitia, Mars.

Author

Perrin, Clément, Jacob, Alice, Lucas, Antoine, Batov, Alexey, Gudkova, Tamara, Rodriguez, Sébastien, Lognonné, Philippe, Drilleau, Mélanie, and Fuji, Nobuaki

Subjects
*MARS (Planet), *HIGH resolution imaging, *GEOLOGIC faults, *WIDTH measurement, *STRESS concentration, *DISCRETE element method
Abstract

The NASA InSight mission to Mars successfully landed on November 26th, 2018 in Elysium Planitia. It aims to characterize the seismic activity and the internal structure of Mars. In this study we focus on the Cerberus Fossae fault system, which is the closest and largest tectonic structure (~1200 km long) near the landing site of the InSight mission. It is formed by four to five main grabens located on the Southeast of the Elysium Mons volcanic rise. The faults tectonic activity is expected to generate medium-sized marsquakes (Mw > 3) during the nominal mission. In order to better constrain these potential seismic sources, we performed a detailed mapping of the entire fault system based on high resolution satellite images (e.g. CTX, HiRISE) and calculated DEMs. The refined cartography presents a wide range of fault and fracture patterns. Graben widths measurements show a strong correlation with existing fault throws measurements. Altogether they give some insights on the direction of long-term propagation of the fault system but also on fault dips at depth and how the grabens are rooted in the shallow part of the crust. Moreover, the exceptional preservation of the grabens allows to detect up to four scales of segmentation, each formed by a similar number of 3-4 segments/subsegments. This generic distribution of the number of segments is comparable to continental faults on Earth. Fault segmentation can be used to highlight local stress concentrations along the fault and thus anticipate locations of potential marsquakes. We finally compare our surface analysis of fault traces with numerical simulations of the regional crustal stress field of the Elysium Planitia area using joint analysis of gravity and topographic data truncated to spherical harmonic models. [ABSTRACT FROM AUTHOR]

Published
2019

63. Predicting The Meteorological And Seismic Signals Of Martian Dust-Devil Vortices As Observed On The Insight Lander.

Author

Murdoch, Naomi, Lorenz, Ralph, Spiga, Aymeric, Garcia, Raphael, Mimoun, David, Warren, Tristam, Pike, William T., McClean, John B., Stott, Alexander, Charalambous, Constantinos, Widmer-Schnidrig, Rudolph, Kedar, Sharon, Kenda, Balthazar, Kawamura, Taichi, Lognonné, Phillipe, Perrin, Clement, Jacob, Alice, Lucas, Antoine, Rodriguez, Sebastien, and Newman, Claire

Published
2019

66. [Changed taste perception in patients with eating disorders].

Author

Wöckel L, Hummel T, Zepf FD, Jacob A, and Poustka F

Subjects
Adolescent, Adult, Anorexia Nervosa diagnosis, Anorexia Nervosa pathology, Anorexia Nervosa psychology, Body Mass Index, Bulimia Nervosa diagnosis, Bulimia Nervosa pathology, Bulimia Nervosa psychology, Female, Humans, Image Processing, Computer-Assisted, Photography, Pilot Projects, Propylthiouracil, Reference Values, Sensory Thresholds physiology, Anorexia Nervosa physiopathology, Bulimia Nervosa physiopathology, Taste physiology, Taste Buds pathology
Abstract

Objective: Taste is a hereditary trait and affects eating and dietary behavior. The tongue's papillae represent the first line of the gustatory apparatus to provide information about taste. The aim of the present investigation was to evaluate the number of fungiform papillae (fPap) in relationship with 6-n-propylthiouracil (PROP) sensitivity and body mass index (BMI) in patients with eating disorders., Methods: 18 female patients with eating disorders (anorexia or bulimia nervosa; age 14-20 yrs.) and 15 age-matched female controls were included. The number of fPap was quantified. Bitter taste was probed with PROP. Different BMIs (e.g. minimal BMI, maximal BMI) were calculated., Results: As regards non-tasters (PROP negative), anorectic patients showed a significant reduction in the number of fPap compared to both PROP negative healthy controls and also bulimic patients. The number of fPap did not differ significantly between tasters and non-tasters within controls and eating disorder groups. There was a trend of higher BMI's in bulimic and healthy non-tasters., Conclusions: In anorectic patients a reduced number of fPap was associated with a decreased PROP sensitivity, which is a new finding. The data of the present study support the notion that the variation of fPap number and PROP sensitivity influences the pathophysiology of eating behavior and taste perception, and following this are involved in the development of eating disorders.

Published
2007
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