Volumetric changes of mud on Mars: evidence from laboratory simulations

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985530%3A_____%2F23%3A00579653" target="_blank" >RIV/67985530:_____/23:00579653 - isvavai.cz</a>

Alternative codes found

RIV/67985858:_____/23:00579653 RIV/00216208:11320/23:10473517

Result on the web

<a href="https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2023JE007950" target="_blank" >https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2023JE007950</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1029/2023JE007950" target="_blank" >10.1029/2023JE007950</a>

Result language

angličtina

Original language name

Volumetric changes of mud on Mars: evidence from laboratory simulations

Original language description

Subtle mounds have been discovered in the source areas of Martian kilometer-sized flows and on top of summit areas of domes. These features have been suggested to be related to subsurface sediment mobilization, opening questions regarding their formation mechanisms. Previous studies hypothesized that they mark the position of feeder vents through which mud was brought to the surface. Two theories have been proposed: (a) ascent of more viscous mud during the late stage of eruption and (b) expansion of mud within the conduit due to the instability of water under Martian conditions. Here, we present experiments performed inside a low-pressure chamber designed to investigate whether the volume of mud changes when exposed to a Martian atmospheric pressure. Depending on the mud viscosity, we observe a volumetric increase of up to 30% at the Martian average pressure of similar to 6 mbar. The reason is that the low pressure causes instability of the water within the mud, leading to the bubble formation that increases the volume of the mixture. This mechanism bears resemblance to the volumetric changes associated with the degassing of terrestrial lava or mud volcano eruptions caused by a rapid pressure drop. We conclude that the mounds associated with putative Martian sedimentary volcanoes might indeed be explained by volumetric changes in the mud. We also show that mud flows on Mars and elsewhere in the Solar System could behave differently to those found on Earth because mud dynamics are affected by the formation of bubbles in response to the different atmospheric pressures.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10505 - Geology

Project

<a href="/en/project/GA22-20388S" target="_blank" >GA22-20388S: Evolving Ice Shells - processes shaping planetary ice shells inferred from numerical modelling</a><br>

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2023

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Journal of Geophysical Research: Planets

ISSN

2169-9097

e-ISSN

2169-9100

Volume of the periodical

128

Issue of the periodical within the volume

12

Country of publishing house

US - UNITED STATES

Number of pages

16

Pages from-to

e2023JE007950

UT code for WoS article

001124248900001

EID of the result in the Scopus database

2-s2.0-85179692144