scholarly journals Unconventional filling dynamics of a pit crater

2021 ◽  
Vol 576 ◽  
pp. 117230
Author(s):  
P.-Y. Burgi ◽  
S. Valade ◽  
D. Coppola ◽  
G. Boudoire ◽  
G. Mavonga ◽  
...  
Keyword(s):  
2015 ◽  
pp. 1575-1579
Author(s):  
Trudi Hoogenboom Hagen
Keyword(s):  

Mount Suswa is a low-lying Quaternary volcano in the Eastern Rift Valley of Kenya. It rises from the south-sloping floor of the Rift as an asymmetric, shield-shaped cone that covers an area of about 270 km2. The volcano consists of sodalite-bearing, phonolitic lava flows and subordinate proportions of pyroclastic rocks. The cone was built on a volcanic plateau composed of quartz-bearing, trachyte flood lavas (Plateau Trachyte Series; Baker 1958). The volcanic history of Mount Suswa can be divided into three major eruptive episodes: (1) formation of a primitive, shield-shaped volcano composed mainly of lava flows derived from central sources; (2) eruptions at the time of cauldron subsidence producing abundant pumice and thick lava flows, most of which issued from a ring-fracture zone outside, and concentric with, the caldera escarpment (‘ring-feeder’ lavas); (3) post-caldera lavas which partly filled the caldera and later built Ol Doinyo Nyukie volcano. Towards the end of the last eruptive episode an unusual collapse feature, in the form of a ‘ring graben’, was formed inside the older caldera. South of Mount Suswa a series of north-south linear faults transect the plateau basement of trachyte flood lavas. Near the southern periphery of Mount Suswa these faults die out, in some cases converging toward the centre of the volcano. Also in the south it is not always possible to distinguish between the quartz-bearing, trachyte flood lavas of the Rift floor and the sodalite-bearing flows from the central vents of Mount Suswa. (Sodalite-bearing flood lavas are known to be present.) The primitive volcano consists of lava flows, the earliest of which are the most voluminous. An unusual heterogeneous rock comprises the upper parts of the youngest primitive volcano flows. The rock consists principally of globules of lava moulded on to each other, each with a continuous glassy rim and a vesicular, crystalline core. The flows have been termed ‘globule-surface lavas' (Johnson 1968). Other heterogeneous glassy rocks on Mount Suswa resemble examples from the controversial 'froth flows’ described from various parts of Kenya (including Mount Suswa) by McCall (1965) and McCall & Bristow (1965). After a period of quiescence, a caldera was formed in the summit of the primitive volcano, the relationships between the caldera escarpment and the pumice and ring-feeder lavas on Mount Suswa are described in detail. These relationships are significant because they question the widely held assumption that, in calderas with thick pumice mantles, it is the rapid expulsion of pumice (producing a void in the magma chamber) that leads to the collapse of the magma chamber roof. This process, known widely as the ‘Krakataun’ mechanism (Williams 1941; after van Bemmelen 1929), is not applicable to Mount Suswa since the pumice and ring-feeder lavas mantle the caldera escarpment. Instead, as previously suggested by McCall (1963), a more likely process is that releases of pressure along the ring faults, formed during cauldron collapse, produce the explosive eruptions. In reviewing and discussing in detail the literature on calderas, it is concluded that many so-called ‘Krakatau-type’ calderas may have originated in the same way as the Mount Suswa caldera. Furthermore, it is emphasized that in the case of any one caldera great care must be taken in describing and interpreting the often ambiguous relations between cauldron subsidence and concomitant explosive eruptions. The post-caldera sequence of lavas on Mount Suswa is divided into two parts: an earlier group of generally non-porphyritic lavas; and a later group of distinctive, porphyritic lavas containing abundant anorthoclase phenocrysts. Most of the flows of the later group were erupted from a central vent in the southwest part of the caldera. They produced Ol Doinyo Nyukie volcano, at the summit of which is a pit crater. The second major collapse on Mount Suswa took place entirely within the older caldera and produced an annular trench, or ‘ring graben’. This unusual structure consists of two, more or less concentric, fault scarps bounding a steep-sided annular zone of subsidence. The ring graben truncates the pit crater of Ol Doinyo Nyukie and isolates a tilted, flat-topped, central island-block with a maximum diameter of 3.75 km. The island-block is inaccessible and its detailed structure is unknown. Consequently, the origin of the ring graben is still uncertain. However, three possible subsidence mechanisms are suggested. A fresh lava flow, similar to those of Ol Doinyo Nyukie volcano, partly covers the floor of the ring graben. This flow, and a similar one on the south flank of Mount Suswa, are the most recent eruptions of the volcano. Fumarolic activity persists at the present day.


1991 ◽  
Vol 47 (1-2) ◽  
pp. 89-104 ◽  
Author(s):  
Alfred Hirn ◽  
Jean-Claude Lépine ◽  
Martine Sapin ◽  
Hughes Delorme

2021 ◽  
Author(s):  
Craig Magee ◽  
Christopher A-L Jackson ◽  
Corbin L Kling ◽  
Paul K Byrne

<p>Pit craters are enigmatic sub-circular depressions observed on rocky and icy planetary bodies across the Solar System. These craters do not primarily form during catastrophic impact or the forcible eruption of subsurface materials, but likely due to collapse of subsurface cavities following fluid (e.g., magma) movement and/or extensional tectonics. Pit craters thus provide important surficial records of otherwise inaccessible subsurface processes. However, unlocking these pit crater archives is difficult because we do not know how their surface expression relates to their subsurface structure or driving mechanisms. As such, there is a variety of hypotheses concerning pit crater formation, which variously relate cavity collapse to: (i) opening of dilatational jogs during faulting; (ii) tensile fracturing; (iii) karst development; (iv) permafrost melting; (v) lava tube evacuation; (vi) volatile release from dyke tip process zones; (vii) pressure waning behind a propagating dike tip; (viii) migration of magma away from a reservoir; and/or (ix) hydrothermal fluid movement inducing host rock porosity collapse. Validating whether these proposed mechanisms can drive pit crater formation and, if so, identifying how the physical characteristics of pits can be used to infer their driving mechanisms, is critical to probing subsurface processes on Earth and other planetary bodies.</p><p>Here we use seismic reflection data from the North Carnarvon Basin offshore NW Australia, which provides ultra-sound like images of Earth’s subsurface, to characterize the subsurface structure of natural pit craters. We extracted geometrical data for 61 pits, and find that they are broadly cylindrical, with some displaying an inverted conical (trumpet-like) morphology at their tops. Fifty-six pit craters, which are sub-circular and have widths of ~150–740 m, extend down ~500 m to and are aligned in chains above the upper tips of dikes; crater depths are  ~12–225 m. These dike-related pit craters occur within long, linear graben interpreted to be bound by dyke-induced normal faults. Five pit craters, which are ~140–740 m wide and ~32–107 m deep, formed independent of dykes and are associated only with tectonic normal faults. Our preliminary data reveal a moderate, positive correlation between crater width and depth but there is no distinction between the depth and width trends of pit craters associated with dikes and those with tectonic normal faults. To test whether our quantitative data can be used to inform interpretation of pit craters observed on other planetary bodies, we compare their morphology to those imaged in Noctis Labyrinthus on Mars; there are >200 pit craters here, most of which occur in chains, with widths ranging from 369–11743 m and depths from 1–1858 m.</p><p>Overall, we show reflection seismology is a powerful tool for studying the three-dimensional geometry of pit craters, with which we can test pit crater formation mechanisms. We anticipate future seismic-based studies will improve our understanding of how the surface expressions of pit craters (either in subaerial or submarine settings) can be used to reconstruct subsurface structures and processes on other planetary bodies, where such subsurface information is not currently available.</p>


2013 ◽  
Vol 50 (1) ◽  
pp. 109-126 ◽  
Author(s):  
S.C. Davey ◽  
R.E. Ernst ◽  
C. Samson ◽  
E.B. Grosfils

Composed of a series of circular to elliptical bowl-shaped depressions, pit crater chains are common on the surface of many of our solar system’s terrestrial planets and moons. Using Magellan synthetic aperture radar (SAR) images, four areas of Venus are examined in which a total of 354 pit crater chains are found: Ganiki Planitia (180°E–210°E, 25°N–50°N), Ulfrun Regio (200°E–240°E, 0°N–25°N), Themis Regio (270°E–300°E, 25°S–40°S), and Idunn Mons (205°E–225°E, 35°S–55°S). A study of the distribution of these pit crater chains at regional and local scales reveals hierarchical clustering. On a regional scale, pit crater chain clusters are associated with graben–fissure systems that are radiating (associated with volcano-tectonic features), circumferential (associated with coronae), and linear (with uncertain volcano-tectonic genesis). At a local scale, pit crater chains are found with marked restriction to particular portions of graben–fissure systems. We conclude that this hierarchical clustering is an indication that both an extensional process and a lithological control contribute to the formation of pit crater chains. Specifically, we propose that pit crater chain formation on Venus occurs in poorly welded volcaniclastic material (e.g., shield plains material unit) that has been crosscut by graben–fissure system(s). Only portions of the shield plains material unit may have sufficient thickness of volcaniclastic material, thus explaining the lack of a co-extensive relationship. Additionally, pit crater chains in other map units may be explained by shallow burial of the volcaniclastic material.


Icarus ◽  
2012 ◽  
Vol 221 (2) ◽  
pp. 831-843 ◽  
Author(s):  
Catherine M. Elder ◽  
Veronica J. Bray ◽  
H. Jay Melosh
Keyword(s):  

2020 ◽  
Author(s):  
Koji Fujita ◽  
Hilal Karaca ◽  
Hiroki Nagai
Keyword(s):  

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