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Darwin Canyon Formation

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Journal Article
Published: 01 May 2010
Journal of Paleontology (2010) 84 (3): 529–537.
... and the Darwin Canyon Formation in California, Paraheritschioides fergusonensis n. sp. from the Ferguson Mountain and Bird Spring formations in Nevada, and Wendoverella arca n. gen. and n. sp., Permastraea nevadensis n. sp., and Pararachnastraea moormanensis n. sp. from the Pequop Formation in eastern Nevada...
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Composite measured section 2.3–2.4–2.5 across members 2–6 of the Darwin Hills Sequence and the lowest part of the Darwin Canyon Formation in the Darwin Hills. Lithocodes on the right of each column correspond to lithofacies described in Table 1. Stratigraphic abbreviations: Pdc—Permian Darwin Canyon Formation; PIPdh2–6—Pennsylvanian and Permian Darwin Hills Sequence Members 2–6. See Figure 4.2 for traverses. See File S1 (see text footnote 1) for clast count data. C—clay; vF—very fine sand; M—medium sand; vC—very coarse sand; P—pebble; B—boulder (see also Table 1).
Published: 12 April 2023
Figure 5. Composite measured section 2.3–2.4–2.5 across members 2–6 of the Darwin Hills Sequence and the lowest part of the Darwin Canyon Formation in the Darwin Hills. Lithocodes on the right of each column correspond to lithofacies described in Table 1 . Stratigraphic abbreviations: Pdc
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Fence diagram shows the Darwin Basin along the line indicated in the inset map (Fig. 2). Note the pronounced changes in thickness of the Osborne Canyon Formation across short distances and the absence of the unit in the Darwin Hills. Contact between tectonostratigraphic units α and β (see text discussion below) is indicated by a horizontal black line at the contact of the Darwin Canyon Formation with underlying units. Abbreviations: Fm.—Formation; Ls.—Limestone.
Published: 12 April 2023
Figure 8. Fence diagram shows the Darwin Basin along the line indicated in the inset map ( Fig. 2 ). Note the pronounced changes in thickness of the Osborne Canyon Formation across short distances and the absence of the unit in the Darwin Hills. Contact between tectonostratigraphic units α and β
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(A) Photograph shows thick bedded, very fine-grained sandstone turbidites interbedded with thin beds of carbonate mudstone. Panamint Springs Member of the Darwin Canyon Formation at Darwin Canyon. (B) Typical clast-supported calcirudite of the Osborne Canyon Formation contains pebble- to cobble-sized clasts of micrite and crinoid debris. Upper Osborne Canyon. (C) Structureless, coarse-grained calcarenite with outsized pebble-sized clasts of tan to gray carbonate mudstone. Darwin Hills Sequence Member 5, Darwin Hills. (D) Planar to wavy bedding in a fine-grained mixed siliciclastic-calciclastic sandstone was deposited via low-density turbidity current. Darwin Hills Sequence Member 6, Darwin Hills. (E) Thick intervals of nondescript gray, brown, or tan weathering of black carbonate mudstone makes up significant portions of the Osborne Canyon Formation pictured here at Panamint Springs Canyon. (F) Several-hundred meters of deep-marine strata of the Darwin Canyon (Pdc) and Osborne Canyon (Po) formations overlie shelf facies of the Bird Spring Formation (IPb) in an erosive and channelized disconformity at Marble Canyon. Note the black, laterally continuous calcirudite beds near the top of the Osborne Canyon Formation.
Published: 12 April 2023
Figure 9. (A) Photograph shows thick bedded, very fine-grained sandstone turbidites interbedded with thin beds of carbonate mudstone. Panamint Springs Member of the Darwin Canyon Formation at Darwin Canyon. (B) Typical clast-supported calcirudite of the Osborne Canyon Formation contains pebble
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Measured sections 4.1 and 4.2 at Panamint Springs Canyon (left) and section 6.1 at Marble Canyon. Sections traverse the uppermost part of the Tihvipah Limestone (IPt) at Panamint Springs Canyon or the Bird Spring Formation (IPb) at Marble Canyon, the Osborne Canyon Formation (Po), and the lowermost part of the Darwin Canyon Formation (Pdc). See Figures 4.4 and 4.6 for traverses and Figure 5 for legend. See File S1 (see text footnote 1) for clast count data. C—clay; vF—very fine sand; M—medium sand; vC—very coarse sand; P—pebble; B—boulder (see also Table 1).
Published: 12 April 2023
), and the lowermost part of the Darwin Canyon Formation (Pdc). See Figures 4.4 and 4.6 for traverses and Figure 5 for legend. See File S1 (see text footnote 1 ) for clast count data. C—clay; vF—very fine sand; M—medium sand; vC—very coarse sand; P—pebble; B—boulder (see also Table 1 ).
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Measured sections 3.1 at upper Osborne Canyon and 1.1 and lower Osborne Canyon. Sections traverse the uppermost part of the Tihvipah Limestone (IPt), the Osborne Canyon Formation (Po), and the lowermost part of the Darwin Canyon Formation (Pdc). See Figure 4.1 and 4.3 for traverses and Figure 5 for legend. See File S1 (see text footnote 1) for clast count data. C—clay; vF—very fine sand; M—medium sand; vC—very coarse sand; P—pebble; B—boulder (see also Table 1).
Published: 12 April 2023
Figure 6. Measured sections 3.1 at upper Osborne Canyon and 1.1 and lower Osborne Canyon. Sections traverse the uppermost part of the Tihvipah Limestone (IPt), the Osborne Canyon Formation (Po), and the lowermost part of the Darwin Canyon Formation (Pdc). See Figure 4.1 and 4.3 for traverses
Journal Article
Journal: GSA Bulletin
Published: 12 April 2023
GSA Bulletin (2024) 136 (1-2): 234–260.
...Figure 5. Composite measured section 2.3–2.4–2.5 across members 2–6 of the Darwin Hills Sequence and the lowest part of the Darwin Canyon Formation in the Darwin Hills. Lithocodes on the right of each column correspond to lithofacies described in Table 1 . Stratigraphic abbreviations: Pdc...
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Journal Article
Journal: AAPG Bulletin
Published: 01 July 1984
AAPG Bulletin (1984) 68 (7): 932.
...K. Scott Barker ABSTRACT The Amsden Formation, named by N. H. Darton in 1904 during mapping of the Bighorn Mountains, Wyoming, consists of red shales, limestones, sandstones, and cherty beds. The Amsden was later subdivided into four members (in ascending order): the Darwin Sandstone (E...
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Schematic and speculative cross section of the Darwin Basin system is shown at three times in the evolution of the basin. Gzhelian–Asselian: flexural loading on the Last Chance Thrust begins to affect eastern California. Transient uplift from an inboard-migrating forebulge causes uplift, probably accommodated by minor forebulge faulting, of the Tihvipah Limestone and eventually the seaward margin of the Bird Spring Formation, resulting in submarine erosion, channelization, and the formation of a basin-wide, time-transgressive unconformity. Backbulge subsidence permits continuous deposition of shelf facies of the Bird Spring Formation on the eastern and southeastern margins of the basin. Sediment derived from submarine erosion of the Tihvipah Limestone, fault scarp, slump scars, slope collapses, and from the Bird Spring Shelf itself is mobilized downslope by sediment gravity flows and deposited in carbonate slope-apron depositional environments of the nascent Darwin Basin. These deposits are preserved today as the four lower members of the Darwin Hills Sequence and the unnamed turbidites in the Santa Rosa Hills. Dotted line denotes approximate sea level (S.L.) in all panels. Sakmarian: the Last Chance Allochthon (LCA) is emplaced on the northwestern margin of the basin by the Last Chance Thrust. Carbonate slope-apron facies of the Osborne Canyon Formation are deposited in the resulting foredeep, while unit 1 of the sedimentary rocks of Santa Rosa Flat (SRSRF) is deposited in a wedge-top setting, onlapping the Conglomerate Mesa Uplift (southeastern margin of Last Chance Allochthon). Paleocurrent data from the Osborne Canyon Formation in the Argus Range indicate that sediment was transported W–NW toward the axis of the basin and the Last Chance Allochthon. Abrupt lateral thickness and facies changes in the Osborne Canyon Formation are explained by onlapping of the previously uplifted forebulge and/or deposition on complex basin-floor bathymetry related to foreland faulting. Artinskian: slip on the Last Chance Thrust has ended, although subsidence and deposition within the Darwin Basin continue through at least this time. The entire basin system, from the Last Chance Allochthon to the coeval shelf edge exposed at Warm Spring Canyon, is buried under a minimum of 1.6 km of turbidites deposited in deep-marine basin-plain or submarine fan depositional environments. Paleocurrent data (Stevens et al., 1989) indicate that sediment gravity flows were directed to the southwest, toward the continental margin bounded by the California-Coahuila transform. Note tectonostratigraphic units α and β denoted on the Artinskian–Roadian panel. All strata depicted in the upper two panels belong to unit α.
Published: 12 April 2023
and facies changes in the Osborne Canyon Formation are explained by onlapping of the previously uplifted forebulge and/or deposition on complex basin-floor bathymetry related to foreland faulting. Artinskian: slip on the Last Chance Thrust has ended, although subsidence and deposition within the Darwin Basin
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Paleogeography of the Darwin Basin system is shown. Pennsylvanian (Pre-Gzhelian): the Bird Spring Shelf is flanked by the Tihvipah Ramp and the Keeler Basin. Gzhelian: the Darwin Basin forms after the southwestern portion of the Tihvipah Ramp subsides (Stevens et al., 2015c). The boundary between the Keeler Basin and Darwin Basin is defined by the former Mississippian shelf edge, where rocks of the Darwin Basin overlie Mississippian shelf carbonates and rocks of the Keeler Basin overlie Mississippian basinal rocks (Stevens et al., 2015b). Sakmarian: further subsidence of the Tihvipah Ramp and the Bird Spring Shelf leads to areal expansion of the Darwin Basin and retrogradation of the carbonate apron depositional system onto the shelf and slope. Emplacement of the Last Chance Allochthon by the Last Chance Thrust (LCT) to the northwest forms a bathymetric high referred to as the Conglomerate Mesa Uplift (CMU), which represents the toe of this allochthon. The Keeler Basin was succeeded by the Lone Pine Basin during this time (Stone et al., 2000; Stevens et al., 2001; Stevens et al., 2015b). Artinskian: basin-plain facies of the Darwin Canyon and Lone Pine formations prevail across the entire region after complete subsidence of the Bird Spring Shelf and Tihvipah Ramp in this area (Stevens et al., 2015b). Adapted from Stevens et al. (2015a).
Published: 12 April 2023
to as the Conglomerate Mesa Uplift (CMU), which represents the toe of this allochthon. The Keeler Basin was succeeded by the Lone Pine Basin during this time ( Stone et al., 2000 ; Stevens et al., 2001 ; Stevens et al., 2015b ). Artinskian: basin-plain facies of the Darwin Canyon and Lone Pine formations prevail
Journal Article
Journal: AAPG Bulletin
Published: 01 March 1973
AAPG Bulletin (1973) 57 (3): 498–509.
... and a Pennsylvanian fauna about 52 m above the Darwin Member in Wiggins Fork Canyon. A debate followed concerning the age of the lower Amsden fauna, the stratigraphic position of the Darwin Member, and the age and stratigraphic position of the Sacajawea Formation ( Branson, 1939 ; Baker, 1946 ; Scott and Wilson...
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Journal Article
Journal: AAPG Bulletin
Published: 01 April 1967
AAPG Bulletin (1967) 51 (4): 529–557.
... filled with sandstone derived from above during deposition of the Darwin Sandstone Member. Sinkhole .—A sinkhole filled by the Darwin and extending at least 20 feet deep into the Madison was found at the top of the formation in the Dinwoody Canyon section. Shattered zones .—Intervals in which...
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Journal Article
Journal: Lithosphere
Publisher: GSW
Published: 16 December 2020
Lithosphere (2020) 2020 (1): 9406113.
... folds at several stratigraphic levels in the Darwin Basin section [ 17 ]. The Pennsylvanian to Early Permian Keeler Canyon Formation [ 28 , 29 ] underlies both basins and is exposed at the crest of the uplift, where it is unconformably overlain by the Union Wash Formation [ 17 ]. Sakmarian fusulinids...
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Journal Article
Journal: GSA Bulletin
Published: 13 October 2020
GSA Bulletin (2021) 133 (5-6): 1105–1127.
... Ordovician strata over the Permian Darwin Canyon Formation ( Fig. 2 ; Snow, 1992 ; Stone et al., 2014 ). The Lemoigne thrust is geometrically similar to the Marble Canyon thrust, and it places the Middle Cambrian Bonanza King Formation over the Darwin Canyon Formation ( Fig. 2 ; Snow, 1992 ; Stevens...
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Journal Article
Journal: AAPG Bulletin
Published: 01 April 1954
AAPG Bulletin (1954) 38 (4): 508–583.
.... Branson (1939) also reported Desmoinesian fusulinids 175 feet below the top of the Tensleep at Wind River Canyon. J. D. Love (1939, p. 26) divided the Amsden formation of the Absaroka Range into an upper Amsden and lower Darwin sandstone member. The name Darwin, first used by Blackwelder (1918 , p...
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... turbidite basins in which the Pennsylvanian to Early Permian Keeler Canyon Formation (Keeler Basin of Stevens et al., 2001 ) and the Early Permian Osborne Canyon and Darwin Canyon Formations of the Owens Valley Group (herein called the Darwin Basin) accumulated ( Stone and Stevens, 1988 ; Stevens, 1991b...
Journal Article
Journal: GSA Bulletin
Published: 20 December 2022
GSA Bulletin (2023) 135 (9-10): 2296–2314.
... ), within the Nova Formation conglomerates. Geochemical data indicate that the volcanic flows erupted from the Darwin Plateau volcanic field in the Argus Range west of Panamint Valley (path N in Fig. 2 ; Coleman and Walker, 1990 ). Figure 8. Left: Geologic map of the northern Panamint Valley–Towne...
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Tectonostratigraphic chart for the Death Valley area. To accommodate as many events as possible, the time scale (from Gradstein et al., 2004) is shown with a variable vertical scale, logarithmic from 1000 yr to 1 m.y., then a linear scale from 1 to 5 m.y. and a different linear scale from 5 to 25 m.y. From the left, the columns show the igneous events, stratigraphy, tectonic events, and regional tectonic regime. See Table 1 for data and explanations of abbreviations used. The stratigraphic column illustrates age ranges of named sedimentary formations, with different patterns indicating whether or not formations have been interpreted as syntectonic (Snow and Lux, 1999). The Artist Drive Formation is shown by a different symbol as these rocks in their northern Black Mountains type area are primarily lava flows or volcaniclastics. The naming convention for sedimentary formations follows that established by Hunt and Mabey (1966) and subsequently modified by Snow and Lux (1999) and Knott et al. (2005). Also shown are the three Quaternary pluvial Lake Manly events when Death Valley was flooded (Anderson and Wells, 2003). In the stratigraphic column, formations from the north and west of the area are on the left so that left to right is equivalent to north and west to south and east. DP—Darwin Plateau (Snyder and Hodges, 2000); WSP—Willow Springs Pluton (Calzia nd Rämö, 2000); SMG—Smith Mountain Granite (Miller and Pavlis, 2005); MSG—granite of Miller Spring (Calzia and Rämö, 2000); SWNVF—Southwest Nevada Volcanic Field (Sawyer et al., 1994); TC+RT—Trail Canyon volcanics and Rhodes Tuff/Sheepshead andesite (McKenna and Hodges, 1990).
Published: 01 February 2011
from 5 to 25 m.y. From the left, the columns show the igneous events, stratigraphy, tectonic events, and regional tectonic regime. See Table 1 for data and explanations of abbreviations used. The stratigraphic column illustrates age ranges of named sedimentary formations, with different patterns
Journal Article
Journal: AAPG Bulletin
Published: 01 July 1964
AAPG Bulletin (1964) 48 (7): 1063–1090.
... arid conditions during regression. A mixture of strongly altered feldspar grains with moderately altered grains is characteristic of the Darwin Member (sandstone) of the Sacajawea Formation. In contrast, Tensleep feldspar is more uniformly weathered. This suggests moderate topographic relief...
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Journal Article
Journal: AAPG Bulletin
Published: 01 September 1947
AAPG Bulletin (1947) 31 (9): 1537–1593.
... the name Boysen formation. The type locality for the Boysen is in Wind River Canyon. Although some recent writers have not recognized this change, the name Boysen formation is used for the uppermost Cambrian formation in this paper because Miller 13 and others have shown that it is correlative...
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