Techniques for identifying dust devils in Mars Pathfinder images

2000 ◽  
Vol 38 (2) ◽  
pp. 870-876 ◽  
Author(s):  
S.M. Metzger ◽  
J.R. Carr ◽  
J.R. Johnson ◽  
T.J. Parker ◽  
M.T. Lemmon
Keyword(s):  
Dust Devils ◽  
Mars Pathfinder

scholarly journals Dust devils as observed by Mars Pathfinder

2003 ◽  
Vol 108 (E12) ◽  
Author(s):  
Francesca Ferri ◽  
Peter H. Smith ◽  
Mark Lemmon ◽  
Nilton O. Rennó
Keyword(s):  
Dust Devils ◽  
Mars Pathfinder

Dust devils: Characteristics of the forward motion from a Saharan survey

2021 ◽  
Vol 50 ◽  
pp. 100678
Author(s):  
Gabriele Franzese ◽  
Simone Silvestro ◽  
David A. Vaz ◽  
Ciprian Ionut Popa ◽  
Fabio Cozzolino ◽  
...  
Keyword(s):  
Dust Devils ◽  
Forward Motion

Observations of Phobos, Deimos, and bright stars with the Imager for Mars Pathfinder

1999 ◽  
Vol 104 (E4) ◽  
pp. 9055-9068 ◽  
Author(s):  
N. Thomas ◽  
D. T. Britt ◽  
K. E. Herkenhoff ◽  
S. L. Murchie ◽  
B. Semenov ◽  
...  
Keyword(s):  
Mars Pathfinder

scholarly journals Whirlwinds and Hairpins in the Atmospheric Surface Layer

2016 ◽  
Vol 73 (12) ◽  
pp. 4927-4943 ◽  
Author(s):  
Steven P. Oncley ◽  
Oscar Hartogensis ◽  
Chenning Tong
Keyword(s):  
Surface Layer ◽  
Atmospheric Surface Layer ◽  
Dust Devils ◽  
Hairpin Vortices ◽  
Structure And Dynamics ◽  
Fixed Array ◽  
Visual Observations

Abstract Vortices in the atmospheric surface layer are characterized using observations at unprecedented resolution from a fixed array of 31 turbulence sensors. During the day, these vortices likely are dust devils, though no visual observations are available for confirmation. At night, hairpin vortices appear to have been observed. The structure and dynamics of several types of vortices are described and related to other vortex investigations, including tornadoes and hurricanes.

Mars Pathfinder project progress report

1996 ◽  
Vol 39 (1-4) ◽  
pp. 91-99 ◽  
Author(s):  
Anthony J. Spear ◽  
Matthew P. Golombek
Keyword(s):  
Progress Report ◽  
Mars Pathfinder

General geology and geomorphology of the Mars Pathfinder landing site

1999 ◽  
Vol 104 (E4) ◽  
pp. 8555-8571 ◽  
Author(s):  
A. W. Ward ◽  
L. R. Gaddis ◽  
R. L. Kirk ◽  
L. A. Soderblom ◽  
K. L. Tanaka ◽  
...  
Keyword(s):  
Landing Site ◽  
General Geology ◽  
Mars Pathfinder

Exploration of Characteristics Governing Dynamics of Whirlwinds: Application to Dust Devils

2017 ◽  
Vol 72 (8) ◽  
pp. 763-778
Author(s):  
Sanjay Kumar Pandey ◽  
Jagdish Prasad Maurya
Keyword(s):  
Physical Phenomenon ◽  
Radial Pressure ◽  
Buffer Zone ◽  
Vertical Gradient ◽  
Azimuthal Velocity ◽  
Low Pressure ◽  
Dust Devils ◽  
Growth And Survival ◽  
Pressure Region ◽  
Upward Direction

AbstractIt is intended to model mathematically an ideal whirlwind which characterises this geo-physical phenomenon and eventually helps us decode the inherent dynamics. A dense cylindrical aerial mass is taken into consideration surrounding a rarer aerial region in order to keep a radial favourable gradient of pressure to sustain a rotational motion. It has been concluded that the whirlwind will survive as long as the low pressure region exists. The vertical pressure gradient also plays an equally important role. Since it is not connected to any cloud and the axial velocity is in the vertically upward direction, the momentary vertical gradient of pressure is required for its growth and survival. Horizontal ambient winds that rush towards low pressure zone, crush the air in the buffer zone, and turn vertically upward may also take the dust carried with them visibly to some height. It is considered that the angular azimuthal velocity varies within the annulus. An inference is that no whirlwind without a low pressure region within it can survive. This may be termed as the fundamental characteristic of whirlwind. It is further concluded that if the radial pressure difference between the outermost and innermost layers is larger, the whirlwind is thicker and consequently, it will last longer. Moreover, another conclusion arrived at is that the angular velocity will vanish if the inner radius is zero.

The Site Tilt and Lander Transfer Function from the Short-Period Seismometer of InSight on Mars

2021 ◽  
Author(s):  
Alexander E. Stott ◽  
Constantinos Charalambous ◽  
Tristram J. Warren ◽  
William T. Pike ◽  
Robert Myhill ◽  
...  
Keyword(s):  
Young’S Modulus ◽  
Young's Modulus ◽  
Dust Devils ◽  
Total Change ◽  
Noise Sources ◽  
Element Analysis ◽  
Near Surface ◽  
Seismic Experiment ◽  
Short Period ◽  
Sensitivity Changes

ABSTRACT The National Aeronautics and Space Administration InSight mission has deployed the seismic experiment, SEIS, on the surface of Mars, and has recorded a variety of signals including marsquakes and dust devils. This work presents results on the tilt and local noise sources, which provide context to aid interpretation of the observed signals and allow an examination of the near-surface properties. Our analysis uses data recorded by the short-period sensors on the deck, throughout deployment and in the final configuration. We use thermal decorrelation to provide an estimate of the sol-to-sol tilt. This tilt is examined across deployment and over a Martian year. After each modification to the site, the tilt is seen to stabilize over 3–20 sols depending on the action, and the total change in tilt is <0.035°. Long-term tilt over a Martian year is limited to <0.007°. We also investigate the attenuation of lander-induced vibrations between the lander and SEIS. Robotic arm motions provide a known lander source in the 5–9 Hz bandwidth, yielding an amplitude attenuation of lander signals between 100 and 1000 times. The attenuation of wind sensitivity from the deck to ground presents a similar value in the 1.5–9 Hz range, thus favoring a noise dominated by lander vibrations induced by the wind. Wind sensitivities outside this bandwidth exhibit different sensitivity changes, indicating a change in the coupling. The results are interpreted through a finite-element analysis of the regolith with a depth-dependent Young’s modulus. We argue that discrepancies between this model and the observations are due to local compaction beneath the lander legs and/or anelasticity. An estimate for the effective Young’s modulus is obtained as 62–81 MPa, corroborating previous estimates for the top layer duricrust.

scholarly journals Chemical, multispectral, and textural constraints on the composition and origin of rocks at the Mars Pathfinder landing site

1999 ◽  
Vol 104 (E4) ◽  
pp. 8679-8715 ◽  
Author(s):  
H. Y. McSween ◽  
S. L. Murchie ◽  
J. A. Crisp ◽  
N. T. Bridges ◽  
R. C. Anderson ◽  
...  
Keyword(s):  
Landing Site ◽  
Mars Pathfinder
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