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10 results for “Interior Structure”
Carbon Dynamics Along a Permafrost Gradient at Caribou-Poker Creeks Research Watershed (CPCRW) in Interior Alaska: Forest stand structure in a 75x75m spatial domain along a permafrost and vegetation gradient.
This dataset includes forest stand structure. Project summary: Specific leaf area (SLA, leaf area per unit dry mass) is a key canopy structural characteristic, a measure of photosynthetic capacity, and an important input into many terrestrial process models. Although many studies have examined SLA variation, relatively few data exist from high latitude, climate-sensitive permafrost regions. We measured SLA and soil and topographic properties across a boreal forest permafrost transition, in which forest composition changed as permafrost deepened from 54 to >150 cm over 75 m hillslope transects in Caribou-Poker Creeks Research Watershed, Alaska. This is an exploratory study to begin understanding SLA variation and controls thereof in a non-contiguous permafrost system.
Text-fig. 9. Carpolithes (a–r). a–d: Carpolithes sp. 5. USNM PAL 772370. Scale bar = 5 mm, reflected light, palladium coated. a: Lateral view of seed, apex up, possible raphe descending from apex toward viewer. b: Lateral view of seed, apex up, possible raphe on right. c: Lateral view, opposite side, apex up, possible raphe on left. d: Apical view, note central pit with raphe descending towards bottom margin. e–h: Carpolithes sp. 6. USNM PAL 772371. Scale bar = 5 mm. e: Basal view illustrating depression and keel in plane of bisymmetry, reflected light, palladium coated. f–h: Micro-CT scan surface rendering. f: Lateral view showing relatively smooth rounded surface. g: Specimen rotated 180° from (f), surface partially eroded. h: Longitudinal view, showing median keel. i–m: Carpolithes sp. 7 USNM PAL 772372. Scale bar = 5 mm. i: View of intact face of globose fruit, possible apical constriction at top. j: Lateral view, intact surface to right, possible apical constriction at top, both micro-CT scan surface renderings. k: Apical view. l: Face view illustrating the mineral filling and the fine, radiating structure of the fruit wall on the left and right margins, both reflected light, palladium coated. m: Closeup of the cellular layer on the left of (l), micro-CT scan surface rendering. n–p: Carpolithes sp. 8. USNM PAL 772373. Scale bar = 3 mm, reflected light, palladium coated. n: Lateral view of pyrene-like structure, one ridge running vertically in the center of view, the other two forming the left and right margins. o: Lateral view of pyrene-like structure, ridge in (n) on the left. p: End-on view illustrating one convex, one concave, and one relatively flat to very slightly concave face. q, r: Carpolithes sp. 9 USNM PAL 772374. Scale bar = 5 mm, reflected light, palladium coated. q: Exterior of the smooth broken half-sphere. r: Interior of the broken half-sphere. in The Early Middle Eocene Wagon Bed Carpoflora Of Central Wyoming, U.S.A.
Text-fig. 9. Carpolithes (a–r). a–d: Carpolithes sp. 5. USNM PAL 772370. Scale bar = 5 mm, reflected light, palladium coated. a: Lateral view of seed, apex up, possible raphe descending from apex toward viewer. b: Lateral view of seed, apex up, possible raphe on right. c: Lateral view, opposite side, apex up, possible raphe on left. d: Apical view, note central pit with raphe descending towards bottom margin. e–h: Carpolithes sp. 6. USNM PAL 772371. Scale bar = 5 mm. e: Basal view illustrating depression and keel in plane of bisymmetry, reflected light, palladium coated. f–h: Micro-CT scan surface rendering. f: Lateral view showing relatively smooth rounded surface. g: Specimen rotated 180° from (f), surface partially eroded. h: Longitudinal view, showing median keel. i–m: Carpolithes sp. 7 USNM PAL 772372. Scale bar = 5 mm. i: View of intact face of globose fruit, possible apical constriction at top. j: Lateral view, intact surface to right, possible apical constriction at top, both micro-CT scan surface renderings. k: Apical view. l: Face view illustrating the mineral filling and the fine, radiating structure of the fruit wall on the left and right margins, both reflected light, palladium coated. m: Closeup of the cellular layer on the left of (l), micro-CT scan surface rendering. n–p: Carpolithes sp. 8. USNM PAL 772373. Scale bar = 3 mm, reflected light, palladium coated. n: Lateral view of pyrene-like structure, one ridge running vertically in the center of view, the other two forming the left and right margins. o: Lateral view of pyrene-like structure, ridge in (n) on the left. p: End-on view illustrating one convex, one concave, and one relatively flat to very slightly concave face. q, r: Carpolithes sp. 9 USNM PAL 772374. Scale bar = 5 mm, reflected light, palladium coated. q: Exterior of the smooth broken half-sphere. r: Interior of the broken half-sphere.
Data for Glacial isostatic adjustment reveals Mars' interior viscosity structure
<p>Present-day Martian interior models used in Broquet et al. (2024). All models use the following naming convention: Profile_NorthPole_Mars-TAYAK-dc-rho_south[-rho_north], where dc is the crustal thickness at the InSight landing site in km, rho_north and rho_south are the bulk density of the northern and southern hemisphere crust in g cm^-3. If added, XGRS provides the crustal heat producing element enrichment factor (X) with respect to the nominal Gamma Ray measured average of 49 pW kg^-1. </p> <p>Files with _60deg provide quantities averaged over the northern regions (>60°N) and _AVG give averages for the whole planet. Models with case numbers are from Plesa et al. (2018) [https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2018GL080728]. </p> <p>Data Columns:<br>------------------------------<br>Column 1: Radius [m]<br>Column 2: Temperature [K]<br>Column 3: Viscosity [Pa s]<br>Column 4: Shear Velocity [m/s]<br>Column 5: Density [kg/m3]<br>Column 6: Shear Modulus [Pa]</p>
Datasets for "Compositions and Interior Structures of the Large Moons of Uranus and Implications for Future Spacecraft Observations"
<p>Files used to build Figures 3, 4, 5, 7, 9, 10, 13 in manuscript entitled "Compositions and Interior Structures of the Large Moons of Uranus and Implications for Future Spacecraft Observations" submitted with JGR.</p>
Equation of State, Structure, and Transport Properties of Iron Hydride Melts at Planetary Interior Conditions dataset
<p>Datasets from <a href="https://doi.org/10.1029/2024JE008525">https://doi.org/10.1029/2024JE008525</a></p> <p>"Equation of State, Structure, and Transport Properties of Iron Hydride Melts at Planetary Interior Conditions"</p> <p>Emma R. Stoutenburg1, Razvan Caracas2, Natalia V. Solomatova3, and Andrew J. Campbell1</p> <p>1Department of the Geophysical Sciences, University of Chicago, Chicago, IL, USA, 2 Université Paris Cité, Institut de Physique du Globe de Paris, CNRS, 1 rue Jussieu, Paris, France, 3CNRS, Ecole Normale Supérieure de Lyon, Laboratoire de Géologie de Lyon LGLTPE UMR5276, Centre Blaise Pascal, Lyon, France</p> <p>--- </p> <p><em>Please make sure you download data from the 30 October, 2024 version. </em> </p> <p>--- </p> <p>ds01.xlsx</p> <p>Contains pressure, density, volume, and temperature of the main dataset discussed in the paper (10 and 100 GPa). Also included are the diffusivities of iron and hydrogen in units of m2/s, viscosity in units of Pa⋅s, average Fe-Fe and Fe-H coordination numbers and bond lengths, as well as the molecular hydrogen abundance and the average number of Fe in H1, H2, and H3 clusters. Nominal pressures, Pnom are provided as these data were generalized within the text; their actual pressure, Pavg, are provided as well. (v1 vs v2: viscosity columns ([visc_Pas, visc_std] were updated, as a typo was discovered in the calculation of viscosity and it was a factor of 1/3 too small; May 2024: added molecular hydrogen data; October 2024, viscosity updated to include a neglected factor of 1/2).</p> <p>ds02.xlsx</p> <p>Contains all the data used in fitting the equation of state (v1-2 vs May 2024: P<10 GPa added to equation of state fit). The first sheet includes the molar volume, temperature, pressure (P), the magnetism corrected pressure (P_magcor115), and the residuals from the equation of state fits (both Birch Murnaghan and Vinet). The second sheet includes the comparison of spin polarized and non-spin polarized pressure in the iron hydrides at ~1 GPa. The third sheet includes the comparison of spin polarized and non-spin polarized pressure in pure iron. </p> <p>FeH-EOS_XfromrhoPT.py</p> <p>added in Oct 2024 update, a simple python function that estimates the hydrogen content of an Fe-H melt with a given density, pressure, and temperature </p>
Data from: Influence of drift and admixture on population structure of American black bears (Ursus americanus) in the Central Interior Highlands, U.S.A. 50 years after translocation
Bottlenecks, founder events, and genetic drift often result in decreased genetic diversity and increased population differentiation. These events may follow abundance declines due to natural or anthropogenic perturbations, where translocations may be an effective conservation strategy to increase population size. American black bears (Ursus americanus) were nearly extirpated from the Central Interior Highlands, USA by 1920. In an effort to restore bears, 254 individuals were translocated from Minnesota, USA and Manitoba, Canada, into the Ouachita and Ozark Mountains from 1958 to 1968. Using 15 microsatellites and mitochondrial haplotypes, we observed contemporary genetic diversity and differentiation between the source and supplemented populations. We inferred four genetic clusters: Source, Ouachitas, Ozarks, and a cluster in Missouri where no individuals were translocated. Coalescent models using approximate Bayesian computation identified an admixture model as having the highest posterior probability (0.942) over models where the translocation was unsuccessful or acted as a founder event. Nuclear genetic diversity was highest in the source (A = 9.11) and significantly lower in the translocated populations (A = 7.07 - 7.34; P = 0.004). The Missouri cluster had the lowest genetic diversity (A = 5.48) and served as a natural experiment showing the utility of translocations to increase genetic diversity following demographic bottlenecks. Differentiation was greater between the two admixed populations than between the source, suggesting that genetic drift acted strongly over the eight generations since the translocation. The Ouachitas and Missouri were previously hypothesized to be remnant lineages. We observed a pre-translocation remnant signature in Missouri but not in the Ouachitas.
Supporting material for Petricca et al. (2024), "Gravity and Radio Science Investigation at the Moons of Uranus to Reveal Subsurface Oceans and Characterize Interior Structures", JGR: Planets
<p>This archive contains the supplementary material for the paper "Gravity and Radio Science Investigation at the Moons of Uranus to Reveal Subsurface Oceans and Characterize Interior Structures", JGR: Planets</p> <p>Content of the dataset:</p> <ol> <li>Synthetic gravity fields for Ariel and Titania generated in the study</li> <li>SPICE kernels of the trajectory of the Uranus Orbiter and Probe designed at JPL</li> </ol> <p> </p> <p>---------------------------------------------------------------</p> <p>Synthetic gravity fields</p> <p>---------------------------------------------------------------</p> <p>The gravity fields are generated following the procedures described in Section 2.1.2 of the main paper. The hydrosphere thickness is assumed to be 190 km and 220 km for Ariel and Titania, respectively. The ocean density is fixed at 1050 kg/m^3. The syntethic topography is generated with pyshtools (Wieczorek and Meschede, 2018). The label of the file indicates the amplitude of the topography of each interface (ice shell or ocean floor) and the maximum degree of the spherical harmonics expansion. The files are formatted according to the Spherical Harmonics ASCII Data Record (SHADR) standard.</p> <p>The header of each file contains: reference radius (km), GM (km^3 / s^2), uncertatinty in the GM (not used and set to zero), maximum degree <em>l </em>of the<em> </em>expansion, maximum order<em> m </em>of the expansion, normalization (0 for unnormalized, 1 for 4pi normalization), reference latitude, reference longitude</p> <p>The columns contain: degree <em>l</em>, order <em>m</em>, coefficient C_<em>lm</em>, coefficient S_<em>lm</em></p> <p>---------------------------------------------------------------</p> <p>UOP trajectories</p> <p>---------------------------------------------------------------</p> <p>The reference positions and velocities of the UOP were generated by Damon Landau (JPL) as part of an internal study at JPL. These initial positions and velocities were numerically integrated by Flavio Petricca (JPL) using the dynamical models described in the main paper. For this reason, the trajectories only cover +- 8 hours from closest approach with each moon and not the entire tour.</p> <p>The ID of the spacecraft is set to -999. The simple text kernel provided here (id_name_map.txt) can be loaded in the kernel pool to associate the ID code with the SPICE names 'URANUS ORBITER PROBE' and 'UOP' for a more explicit and user-friendly access to the trajectories.</p>
Data from: Influence of drift and admixture on population structure of American black bears (Ursus americanus) in the Central Interior Highlands, U.S.A. 50 years after translocation
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The librations, tides, and interior structure of Io
<p>The librations, tides, and interior structure of Io </p> <p>Tim Van Hoolst, Rose-Marie Baland, Antony Trinh, Marie Yseboodt, and Francis Nimmo</p> <p>For each of the 574 lines of the file Iomodels_results, corresponding to different interior structure models of Io, values of the following quantities are given:</p> <ul> <li>Thickness of the crust [km]</li> <li>Thickness of the magma ocean or asthenosphere [km]</li> <li>Radius of the core [km]</li> <li>Density of the mantle (equal to that of the crust and asthenosphere of magma ocean) [kg/m<sup>3</sup>]</li> <li>Density of the core [kg/m<sup>3</sup>]</li> <li>Polar flattening of the surface (defined as the relative difference between the mean equatorial and polar radii)</li> <li>Polar flattening of the outer surface of the magma ocean or asthenosphere</li> <li>Polar flattening of the outer surface of the mantle</li> <li>Polar flattening of the core</li> <li>Equatorial flattening of the surface (defined as the relative difference between the largest and smallest equatorial radii)</li> <li>Equatorial flattening of the outer surface of the magma ocean or asthenosphere</li> <li>Equatorial flattening of the outer surface of the mantle</li> <li>Equatorial flattening of the core</li> <li>Rigidity of the crust [GPa]</li> <li>Rigidity of the asthenosphere [GPa]</li> <li>Rigidity of the mantle [GPa]</li> <li>Rigidity of the core [GPa]</li> <li>Love number of the model with asthenosphere and liquid core</li> <li>Libration amplitude of the model with asthenosphere and liquid core, without deformation [m]</li> <li>Libration amplitude of the model with asthenosphere and liquid core, with deformation [m]</li> <li>Love number of the model with magma ocean</li> <li>Period of the out-of-phase eigenmode, without deformation [days]</li> <li>Period of the out-of-phase eigenmode, with deformation [days]</li> <li>Period of the in-phase eigenmode, without deformation [days]</li> <li>Period of the in-phase eigenmode, with deformation [days]</li> <li>Libration amplitude of the model with magma ocean, without deformation [m]</li> <li>Libration amplitude of the model with magma ocean, with deformation [m]</li> <li>Libration amplitude of the mantle below the magma ocean, without deformation [m]</li> <li>Libration amplitude of the mantle below the magma ocean, with deformation [m]</li> </ul> <p> </p>
supplementary data to 'Mercury's Interior Structure constrained by Density and P-wave Velocity Measurements of Liquid Fe-Si-C Alloys'
<p>This zipfile contain raw experimental data, the matlab code used for data-analysis, and the interior structure models of Mercury that are used in the paper 'Mercury’s Interior Structure constrained by Density and P-wave Velocity Measurements of Liquid Fe-Si-C Alloys', which is authored by Knibbe et al.</p>
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