Radio Astronomy Antennas by the Thousands     

Roger Schultz 《Experimental Astronomy》2004,17(1-3):119-139

Large number of microwave antennas of size and surface accuracy appropriate for the Square Kilometre Array (SKA) have not been manufactured previously. To minimize total cost, the design needs to be much more carefully considered and optimized than would be affordable for a small number of antennas. The required surface area requires new methods of manufacture and production-line type assembly to be considered. A blend of past antenna construction technology, creativity, and new technology is needed to provide the best possible telescope for the proposed SKA science goals. The following key concepts will be discussed with respect to reflector antennas and many supporting photographs, figures and drawings will be included.

Surface and supporting structure – comparison of panels with a one-piece shell as produced by hydroforming.

Combined reflector and mount geometry – performance/cost materially governed by this geometry which must be optimized for SKA requirements which are significantly different from typical communications antennas

Types of fully steerable mounts – king post, turntable bearing and wheel and track

Pointing accuracy – factors effecting cost, non-repeatable and repeatable errors

Axis drive concepts – traction devices, gears, screws, etc.

Life cycle costs – maintenance and power costs must be considered

Synergistic design – all of the above factors must be considered together with the wideband feed and receiver system to optimize the whole system

  相似文献   

Rings in the Planetesimal Disk of beta Pictoris     

Kalas P  Larwood J  Smith BA  Schultz A 《The Astrophysical journal》2000,530(2):L133-L137

The nearby main-sequence star beta Pictoris is surrounded by an edge-on disk of dust produced by the collisional erosion of larger planetesimals. Here we report the discovery of substructure within the northeast extension of the disk midplane that may represent an asymmetric ring system around beta Pic. We present a dynamical model showing that a close stellar flyby with a quiescent disk of planetesimals can create such rings, along with previously unexplained disk asymmetries. Thus we infer that beta Pic's planetesimal disk was highly disrupted by a stellar encounter in the last hundred thousand years.  相似文献   

Introduction to the Special Issue on faulting and fault-related processes on planetary surfaces     

Richard Schultz  Robert T. Pappalardo  David A. Ferrill   《Journal of Structural Geology》2006,28(12):2121-2122

Faults have been documented on nearly every solid surface in the solar system, from asteroids to moons to planets, and they provide a remarkable suite of data sets and critical problems for investigation and analysis by structural geologists. The lack of significant atmospheres on Mercury, the Moon, and most outer planet satellites, along with slow erosion rates and a lack of crustal recycling and Earth-like plate tectonics on most planetary bodies, allows for excellent preservation of fault scarp morphologies for study of fault populations and developmental sequences.  相似文献   

Assessing the spatial variability of the ~3 μm OH/H2O absorption feature in CM2 carbonaceous chondrites     

Cody Schultz  Brendan A. Anzures  Ralph E. Milliken  Taki Hiroi  Kevin Robertson 《Meteoritics & planetary science》2023,58(2):170-194

H₂O and OH are readily detected in hydrated minerals in CM chondrites via reflectance spectroscopy due to their characteristic vibration absorptions at infrared wavelengths. Previous spectroscopic work on bulk powdered CM chondrites has shown that spectral parameters, like the wavelength position of the “3 μm absorption feature,” vary systematically with the extent to which the samples have been aqueously altered. However, it is yet unclear how these spectral features may vary across an intact meteorite chip when measured at spatial scales smaller than that of the individual components of the meteorite. Here, we explore the spatial variability of this spectral feature and others on intact CM2 chips which, unlike powders, retain their petrologic and textural characteristics. We also model the modal mineralogy of the bulk meteorite powders and correlate this with key spectral features, demonstrating that microscope Fourier transform infrared spectroscopic mapping provides a powerful, rapid, and non-destructive technique for assessing compositional diversity and variations in water–rock interactions in chondritic planetary materials. In all CM2 chondrites studied here, we find that variations in the position, shape, and strength of the 3 μm absorption feature reveal a single chondrite can exhibit as much spectral variation as the entire suite of CM2 chondrites. The observed variations in the position and shape of the 3 μm feature within individual CM2 chondrite chips suggest a range of alteration products (e.g., Mg-rich to Fe-rich phyllosilicates) are present and record sub-mm scale variations in the amount and/or chemistry of the altering fluids. The samples having experienced the most progressive aqueous alteration show the least amount of variability in features like the 3 μm absorption band minimum position, whereas the least altered samples exhibit the most variability. We also find that the bulk spectral signatures in the least altered samples appear to be biased toward the spectral signatures of clasts versus matrix. By extension, asteroid reflectance spectra exhibiting 3 μm absorption features consistent with those measured here may be interpreted in a similar framework in which the spectrum of what may appear to be the least altered asteroids represents an average that belies the true diversity of mineralogy and chemistry of the body.  相似文献   

利用卫星图像分析南京信息工程大学校园变化特征     

李旭辉  赵佳玉  Natalie Schultz  肖薇  刘寿东 《南京气象学院学报》2020,12(1):7-21

本文主要目的是利用卫星图像资料分析南京信息工程大学（Nanjing University of Information Science and Technology,NUIST）建校之初至今校园的变化特征.共分析了1964年11月至1970年12月之间的5幅无云的美国侦察卫星图像（1995年解密）,地理配准后图像的位置精度为4.8至7.8 m,图像中的建筑物、道路和水体都清晰可见.通过对比这些黑白的侦察卫星图像与2006—2018年的Google Earth彩色图像,发现现在校园面积远远大于旧校园;旧图像里中苑老操场跑道长度为298 m,2006年Google Earth图像中为406.5 m,操场中心点向东移动了9 m,向南移动了47 m.侦察卫星图像和Google Earth图像都是以统一坐标系做地理位置校正,相关图像见附件.  相似文献