Helioseismic analysis of the solar flare-induced sunquake of 2005 January 15   总被引：1，自引：0，他引：1  

H. Moradi  A.-C. Donea  C. Lindsey  D. Besliu-Ionescu  P. S. Cally 《Monthly notices of the Royal Astronomical Society》2007,374(3):1155-1163

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Surficial properties in Gale Crater, Mars, from Mars Odyssey THEMIS data     

Shannon M Pelkey  Bruce M Jakosky  Philip R Christensen 《Icarus》2004,167(2):244-270

We examine the nature of the surface layer in Gale Crater as determined from high-resolution thermal and visible Mars Odyssey Thermal Emission Imaging System (THEMIS) data as well as how our conclusions compare to past analyses. At THEMIS resolution, the thermal surface structure is dominated by local control, thus providing us with detailed images that contain thermophysical information as well. Using these data sets we have created a map of the area, defining units based primarily on their geomorphology as determined from the daytime thermal and visible images and then using the nighttime thermal data to interpret the nature of the surface layer within each unit. Seven units have been defined: (i) partially blanketed knobby plateaus, (ii) crater walls with terrain similar to that on the plateaus on the upper half and exposed, rocky surfaces on the lower half, (iii)-(v) three floor units with varying combinations of bedrock and indurated and/or particulate deposits, (vi) sand sheets, and (vii) a central mound, consisting of indurated and/or rocky material forming layers, terraces, and slides, covered by particulate material that tapers in thickness downslope. Additionally, dozens of channels have been observed on the crater walls and central mound. The results indicate that aeolian processes have played a major role in shaping much of the present surface layer within Gale and may still be active today. Because of the dramatic size and structure of Gale, the winds are most likely controlled by the local topography. Additionally, the presence and frequency of channels within Gale bolster hypotheses involving aqueous episodes in the history of the crater.  相似文献   

Compressional and Shear Wave Velocities at Pressures to 10 Kilobars for Basalts from the East Pacific Rise     

Nikolas I. Christensen 《Geophysical Journal International》1972,28(5):425-429

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Special perturbations employing osculating reference states     

G. H. Born  E. J. Christensen  L. K. Seversike 《Celestial Mechanics and Dynamical Astronomy》1974,9(1):41-53

The concept of employing osculating reference position and velocity vectors in the numerical integration of the equations of motion of a satellite is examined. The choice of the reference point is shown to have a significant effect upon numerical efficiency and the class of trajectories described by the differential equations of motion. For example, when the position and velocity vectors on the osculating orbit at a fixed reference time are chosen, a universal formulation is yielded. For elliptical orbits, however, this formulation is unattractive for numerical integration purposes due to Poisson terms (mixed secular) appearing in the equations of motion. Other choices for the reference point eliminate this problem but usually at the expense of universality. A number of these formulations, including a universal one, are considered here. Comparisons of the numerical characteristics of these techniques with those of the Encke method are presented.  相似文献   

The state and future of Mars polar science and exploration.   总被引：1，自引：0，他引：1  

S M Clifford  D Crisp  D A Fisher  K E Herkenhoff  S E Smrekar  P C Thomas  D D Wynn-Williams  R W Zurek  J R Barnes  B G Bills  E W Blake  W M Calvin  J M Cameron  M H Carr  P R Christensen  B C Clark  G D Clow  J A Cutts  D Dahl-Jensen  W B Durham  F P Fanale  J D Farmer  F Forget  K Gotto-Azuma  H J Zwally 《Icarus》2000,144(2):210-242

As the planet's principal cold traps, the martian polar regions have accumulated extensive mantles of ice and dust that cover individual areas of approximately 10(6) km2 and total as much as 3-4 km thick. From the scarcity of superposed craters on their surface, these layered deposits are thought to be comparatively young--preserving a record of the seasonal and climatic cycling of atmospheric CO2, H2O, and dust over the past approximately 10(5)-10(8) years. For this reason, the martian polar deposits may serve as a Rosetta Stone for understanding the geologic and climatic history of the planet--documenting variations in insolation (due to quasiperiodic oscillations in the planet's obliquity and orbital elements), volatile mass balance, atmospheric composition, dust storm activity, volcanic eruptions, large impacts, catastrophic floods, solar luminosity, supernovae, and perhaps even a record of microbial life. Beyond their scientific value, the polar regions may soon prove important for another reason--providing a valuable and accessible reservoir of water to support the long-term human exploration of Mars. In this paper we assess the current state of Mars polar research, identify the key questions that motivate the exploration of the polar regions, discuss the extent to which current missions will address these questions, and speculate about what additional capabilities and investigations may be required to address the issues that remain outstanding.  相似文献   

Core flow inversion tested with numerical dynamo models     

Steffen Rau  Ulrich Christensen  rew Jackson  & Johannes Wicht 《Geophysical Journal International》2000,141(2):485-497

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Community Development Finance Institutions (CDFIs): Geographies of financial inclusion in the US and UK     

Lindsey Appleyard 《Geoforum》2011,42(2):250-258

The financial exclusion of enterprise is a concept that has been largely neglected by economic geographers. This is surprising given the attention dedicated to personal financial exclusion and alternative sources of finance. This paper compares financial inclusion policies in deprived areas of the United States (US) and United Kingdom (UK) through the example of Community Development Finance Institutions (CDFIs). CDFIs help overcome financial exclusion by providing local sources of loan finance to micro, small-and-medium-sized enterprises and social enterprises. Drawing upon interviews with key actors within the CDFI sector in the US and UK respectively, the paper aims to compare the CDFI landscape across the US and UK through the provision of finance for enterprise. This is in order to understand the geographies of finance that are being created by such alternative financial institutions thereby contributing to financial inclusion debates. The research concludes that although CDFIs do provide an important source of finance to excluded enterprises, policy initiatives have created uneven geographical coverage and market gaps leaving marked spaces of financial exclusion.  相似文献   

On the role of domain size and resolution in the simulations with the HIRHAM region climate model     

Morten A. D. Larsen  Peter Thejll  Jens H. Christensen  Jens C. Refsgaard  Karsten H. Jensen 《Climate Dynamics》2013,40(11-12):2903-2918

We investigate the simulated temperature and precipitation of the HIRHAM regional climate model using systematic variations in domain size, resolution and detailed location in a total of eight simulations. HIRHAM was forced by ERA-Interim boundary data and the simulations focused on higher resolutions in the range of 5.5–12 km. HIRHAM outputs of seasonal precipitation and temperature were assessed by calculating distributed model errors against a higher resolution data set covering Denmark and a 0.25° resolution data set covering Europe. Furthermore the simulations were statistically tested against the Danish data set using bootstrap statistics. The results from the distributed validation of precipitation showed lower errors for the winter (DJF) season compared to the spring (MAM), fall (SON) and, in particular, summer (JJA) seasons for both validation data sets. For temperature, the pattern was in the opposite direction, with the lowest errors occurring for the JJA season. These seasonal patterns between precipitation and temperature are seen in the bootstrap analysis. It also showed that using a 4,000 × 2,800 km simulation with an 11 km resolution produced the highest significance levels. Also, the temperature errors were more highly significant than precipitation. In similarly sized domains, 12 of 16 combinations of variables, observation validation data and seasons showed better results for the highest resolution domain, but generally the most significant improvements were seen when varying the domain size.  相似文献   

Depletion of background galaxies owing to the cluster lens CL0024+1654: U- and R-band observations     

Ö. E. Rögnvaldsson  T. R. Greve  J. Hjorth  E. H. Gudmundsson  V. S. Sigmundsson  P. Jakobsson  A. O. Jaunsen  L. L. Christensen  E. van Kampen  A. N. Taylor 《Monthly notices of the Royal Astronomical Society》2001,322(1):131-140

We have obtained U - and R -band observations of the depletion of background galaxies resulting from the gravitational lensing of the galaxy cluster CL0024+1654 ( z =0.39). The radial depletion curves show a significant depletion in both bands within a radius of 40–70 arcsec from the cluster centre. This is the first time that depletion is detected in the U band. This gives independent evidence for a break in the slope of the U -band luminosity function at faint magnitudes. The radially averaged R -band depletion curve is broader and deeper than in the U band. The differences can be attributed to the wavelength dependence of the slope of the luminosity function and to the different redshift distribution of the objects probed in the two bands. We estimate the Einstein radius, r _E, of a singular isothermal sphere lens model using maximum-likelihood analysis. Adopting a slope of the number counts of α =0.2 and using the background density found beyond r =150 arcsec, we find r _E=17±3 and 25±3 arcsec in the U and R bands, respectively. When combined with the redshift of the single background galaxy at z =1.675 seen as four giant arcs around 30 arcsec from the cluster centre, these values indicate a median redshift in the range 〈 z _S〉≈0.7 to 1.1 for the U _AB≥24 mag and R _AB≥24 mag populations.  相似文献   

Eolian intracrater deposits on Mars: Physical properties and global distribution     

Philip R. Christensen 《Icarus》1983,56(3):496-518

An investigation of Martian intracrater materials has been made using their thermophysical properties as derived from Viking IRTM observations. Over one-fourth of all craters larger than 25 km in diameter between ?50°S and 50°N have localized deposits of coarse material on the floor which are associated with dark “splotches” seen visually. Assuming homogeneous, unconsolidated materials, the measured thermal inertias of these deposits ($\text{I = 0.003 × 10}{}^{\mathrm{?3}}\text{to}\text{0.026 × 10}{}^{\mathrm{?3}}\text{cal cm}{}^{\mathrm{?2}}\text{sec}{}^{\mathrm{<mtext>?</mtext><mtext>1</mtext><mtext>2</mtext>}}\text{°}\text{K}{}^{\mathrm{?1}}$) imply effective grain sizes ranging from 0.1 mm to 1 cm, with a modal value of 0.9 mm. These deposits are coarser and darker than the surrounding terrains and the majority of the Martian surface, but are not compositionally distinct from materials with similar albedos. They occur more frequently in the south, in regions of relatively coarse material (0.2 to 2 mm), and in relatively dark areas. These features most likely formed by entrapment of marginally mobile material which can be transported into, but not out of, crater depressions by the wind. Very few have recognizable dune forms: those that do have effective grain sizes less than 0.5 mm. The majority of the “splotch” deposits are coarser than the dune-forming materials found in the north polar region and inside extreme southern latitude craters and probably form low, broad zibar dunes or lag deposits. Intracrater deposits are noticeably lacking from the interior of the large, northern hemisphere low-inertia region of Arabia (?10°S to 30°N, 300° to 360°W), interpreted to be a sink for suspended dust, but do occur around the perimeter of this region. This distribution suggests that the intracrater features have been buried in the interior of Arabia and that the dust deposit is less extensive at the margins and may currently be expanding. The occurrence of regional dust deposits in the north may be related to the maximum wind activity currently occurring in the southern hemisphere and suggests that the location of regional sinks may migrate with time as the solar insolation maximum migrates.  相似文献