Magnetic anomalies near Apollinaris Patera and the Medusae Fossae Formation in Lucus Planum, Mars

The nature of strong martian crustal field sources is investigated by mapping and modeling of Mars Global Surveyor magnetometer data near Apollinaris Patera, a previously proposed volcanic source, supplemented by large-scale correlative studies. Regional mapping yields evidence for positive correlations of orbital anomalies with both Apollinaris Patera and Lucus Planum, a nearby probable extrusive pyroclastic flow deposit that is mapped as part of the Medusae Fossae Formation. Iterative forward modeling of the Apollinaris Patera magnetic anomaly assuming a source model consisting of one or more uniformly magnetized near-surface disks indicates that the source is centered approximately on the construct with a scale size several times larger and comparable to that of the Apollinaris Patera free-air gravity anomaly. A significantly lower rms deviation is obtained using a two-disk model that favors a concentration of magnetization near the construct itself. Estimates for the dipole moment per unit area of the Lucus Planum source together with maximum thicknesses of ∼3 km based on topographic and radar sounding data lead to an estimated minimum magnetization intensity of ∼50 A/m within the pyroclastic deposits. Intensities of this magnitude are similar to those obtained experimentally for Fe-rich Mars analog basalts that cooled in an oxidizing (high fO₂) environment in the presence of a strong (?10 μT) surface field. Further evidence for the need for an oxidizing environment is provided by a broad spatial correlation of the locations of phyllosilicate exposures identified to date using Mars Express OMEGA data with areas containing strong crustal magnetic fields and valley networks in the Noachian-aged southern highlands. This indicates that the presence of liquid water, which is a major crustal oxidant, was an important factor in the formation of strong magnetic sources. The evidence discussed here for magnetic sources associated with relatively young volcanic units suggests that a martian dynamo existed during the late Noachian/early Hesperian, after the last major basin-forming impacts and the formation of the northern lowlands.     

Deep versus shallow origin of gravity anomalies, topography and volcanism on Earth, Venus and Mars

The relation between gravity anomalies, topography and volcanism can yield important insights about the internal dynamics of planets. From the power spectra of gravity and topography on Earth, Venus and Mars we infer that gravity anomalies have likely predominantly sources below the lithosphere up to about spherical harmonic degree l=30 for Earth, 40 for Venus and 5 for Mars. To interpret the low-degree part of the gravity spectrum in terms of possible sublithospheric density anomalies we derive radial mantle viscosity profiles consistent with mineral physics. For these viscosity profiles we then compute gravity and topography kernels, which indicate how much gravity anomaly and how much topography is caused by a density anomaly at a given depth. With these kernels, we firstly compute an expected gravity-topography ratio. Good agreement with the observed ratio indicates that for Venus, in contrast to Earth and Mars, long-wavelength topography is largely dynamically supported from the sublithospheric mantle. Secondly, we combine an empirical power spectrum of density anomalies inferred from seismic tomography in Earth’s mantle with gravity kernels to model the gravity power spectrum. We find a good match between modeled and observed gravity power spectrum for all three planets, except for 2?l?4 on Venus. Density anomalies in the Venusian mantle for these low degrees thus appear to be very small. We combine gravity kernels and the gravity field to derive radially averaged density anomaly models for the Martian and Venusian mantles. Gravity kernels for l?5 are very small on Venus below ≈800 km depth. Thus our inferences on Venusian mantle density are basically restricted to the upper 800 km. On Mars, gravity anomalies for 2?l?5 may originate from density anomalies anywhere within its mantle. For Mars as for Earth, inferred density anomalies are dominated by l=2 structure, but we cannot infer whether there are features in the lowermost mantle of Mars that correspond to Earth’s Large Low Shear Velocity Provinces (LLSVPs). We find that volcanism on Mars tends to occur primarily in regions above inferred low mantle density, but our model cannot distinguish whether or not there is a Martian analog for the finding that Earth’s Large Igneous Provinces mainly originate above the margins of LLSVPs.     

Formation of Jupiter using opacities based on detailed grain physics

Numerical simulations, based on the core-nucleated accretion model, are presented for the formation of Jupiter at 5.2 AU in three primordial disks with three different assumed values of the surface density of solid particles. The grain opacities in the envelope of the protoplanet are computed using a detailed model that includes settling and coagulation of grains and that incorporates a recalculation of the grain size distribution at each point in time and space. We generally find lower opacities than the 2% of interstellar values used in previous calculations (Hubickyj, O., Bodenheimer, P., Lissauer, J.J. [2005]. Icarus 179, 415-431; Lissauer, J.J., Hubickyj, O., D’Angelo, G., Bodenheimer, P. [2009]. Icarus 199, 338-350). These lower opacities result in more rapid heat loss from and more rapid contraction of the protoplanetary envelope. For a given surface density of solids, the new calculations result in a substantial speedup in formation time as compared with those previous calculations. Formation times are calculated to be 1.0, 1.9, and 4.0 Myr, and solid core masses are found to be 16.8, 8.9, and 4.7 M_⊕, for solid surface densities, σ, of 10, 6, and 4 g cm⁻², respectively. For σ = 10 and σ = 6 g cm⁻², respectively, these formation times are reduced by more than 50% and more than 80% compared with those in a previously published calculation with the old approximation to the opacity.     

论环境条件对航摄仪检定的影响

本文分析了航摄仪检定的环境条件(压力、温度)对内方位元素、畸变差的影响,并进行了不同环境压力和不同环境温度影响的检定实验。实验结果表明:环境压力和环境温度对航摄仪检定的影响是不容忽略的。本文针对国内目前航摄仪检定现状,提出了改进意见。     

渤海、黄海和东海的构造性质与演化

渤海、黄海、东海的性质与发展是不同的。渤海和黄海是内陆海,是由于地幔物质的上拱,地壳弯曲断裂而成。东海是一个边缘海,是由于 菲律宾海板块向亚洲板块之下插入,在大陆岩石圈的基础上形成的。它们现在的构造格局基本上是在晚上新世或早更新世奠定的。     

Wellsite,Laboratory, and Mathematical Techniques for Determining Sorbed Gas Content of Coals and Gas Shales Utilizing Well Cuttings

Drill cuttings can be used for desorption analyses but with more uncertainty than desorption analyses done with cores. Drill cuttings are not recommended to take the place of core, but in some circumstances, desorption work with cuttings can provide a timely and economic supplement to that of cores. The mixed lithologic nature of drill cuttings is primarily the source of uncertainty in their analysis for gas content, for it is unclear how to apportion the gas generated from both the coal and the dark-colored shale that is mixed in usually with the coal. In the Western Interior Basin Coal Basin in eastern Kansas (Pennsylvanian-age coals), dark-colored shales with normal (∼100 API units) gamma-ray levels seem to give off minimal amounts of gas on the order of less than five standard cubic feet per ton (scf/ton). In some cuttings analyses this rule of thumb for gas content of the shale is adequate for inferring the gas content of coals, but shales with high-gamma-ray values (>150 API units) may yield several times this amount of gas. The uncertainty in desorption analysis of drill cuttings can be depicted graphically on a diagram identified as a “lithologic component sensitivity analysis diagram.” Comparison of cuttings desorption results from nearby wells on this diagram, can sometimes yield an unique solution for the gas content of both a dark shale and coal mixed in a cuttings sample. A mathematical solution, based on equating the dry, ash-free gas-contents of the admixed coal and dark-colored shale, also yields results that are correlative to data from nearby cores.     

湘赣地区中生代镁铁质岩浆作用与岩石圈伸展

综合分析了华南内部中生代 (178～ 80Ma)镁铁质岩石的年代学和元素同位素地球化学特征。研究表明区内主要发育 4期镁铁质岩浆活动 :2 2 0Ma± ,175Ma± ,12 0～ 15 0Ma ,80～ 90Ma ,其中 2 2 0Ma仅在道县发育辉长岩包体。地球化学上区内 175Ma左右的宁远太阳山和赣中项家碱性玄武岩和 80～ 90Ma的镁铁质岩石主要表现为Hawaii OIB玄武岩的元素同位素地球化学特征 ,而175Ma的其他镁铁质岩石表现为岩石圈地幔属性。 12 0～ 15 0Ma的镁铁质岩石则介于岩石圈地幔端员与软流圈地幔端员之间。时、空上表现为以郴州—临武断裂为界 ,西侧自 170Ma左右的EMI型为主向 80～ 90Ma的OIB型为主迁移演化 ,而东侧则自老而新自EMII型 (175Ma)为主演变为以OIB型 (80～ 90Ma)为主。上述资料暗示区内至少存在 4期强烈的岩石圈减薄作用 ,软流圈物质上涌和岩石圈伸展减薄是华南中生代岩浆作用形成的主要机制。但 2 2 0Ma左右的伸展减薄范围局限 ,而较大规模的岩石圈伸展减薄和软流圈上涌始于 178Ma ,其形成可能与华南印支造山作用的后造山 (或后碰撞 )拉张裂解地球动力学背景有关。同时也暗示郴州—临武断裂可能是界定中生代EMI型扬子岩石圈和EMII型华夏岩石圈地幔的重要边界。     

Planktic foraminiferal porosity: a water mass proxy for latest Cenomanian paleoceanography, Greenhorn Sea, Western Interior USA and Canada

Planktic foraminiferal porosity analyses can be used as a water mass proxy and were conducted on samples from above the latest Cenomanian Neocardioceras or B bentonite from the Western Interior Seaway of North America. This time slice provides a snapshot of water mass characteristics in this vast epicontinental sea during the early phase of Oceanic Anoxic Event 2. Mean sample porosity decreases northward and is interpreted as northward decrease in water temperature at the depth Hedbergella delrioensis (Carsey) calcified. Four water masses are defined by porosity, their boundaries are extremely similar to water mass boundaries previously identified by others using the distributions of macrofossils, microfossils and lithology. The boundary between the Subtropical–Tropical Water Mass and Central Subtropical Water Mass was located in southern Colorado. The boundary between the Central Subtropical Water Mass and the Northern Temperate Water Mass lay at approximately 48°N latitude. This boundary is displaced northward approximately 8° latitude as compared to the Holocene planktic foraminiferal temperate ocean province. Within-sample porosity variation suggests all water masses except the Temperate Water Mass were thermally stratified. Samples from the south indicate that the Subtropical–Tropical Water Mass was the most stratified. The porosity data support a previously published data-based paleoceanographic circulation of the southwestern seaway.     

Local scour and the laws of scour pit’s shape downstream of debris flow sabo dam

The erosion shape and the law of development of debris flow sabo dam downstream is a weak part in the study on debris flow erosion. The shape and development of scour pit have an important effect on the stability and safety of debris flow sabo dam, which determines the foundational depth of the dam and the design of protective measures downstream. Study on the scouring law of sabo dam downstream can evaluate the erosion range and reasonably arrange auxiliary protective engineering. Therefore, a series of flume experiments are carried out including different debris flow characteristics （density is varying from 1.5 t/m3 to 2.1 t/m~） and different gully longitudinal slopes. The result shows that the scour pit appears as an oval shape in a plane and deep in the middle while superficial at the ends in the longitudinal section, the position of the maximum depth point moves towards downstream with an increase of flume slope angle. The maximum depth of scour pit is mainly affected by the longitudinal slope of gully, density of debris flow, and the characteristics of gully composition （particle size and the viscosity of soil）. The result also indicates that the viscosity of soil will weaken the erosion extent. The interior slopes of scour pit are different between the upstream and the downstream, and the downstream slope is smaller than the upper one. For the viscous and non-viscous sands with the same distribution of gradation, the interior slope of non- viscous sand is smaller than the viscous sand.According to tbe regression analysis on the experimental data, the quantitative relationship between the interior slope of scour pit, slope of repose under water and the longitudinal slope of gully is established and it can be used to calculate the interior slope of scour pit. The results can provide the basis for the parameter design of the debris flow control engineering foundation.