共查询到20条相似文献，搜索用时 31 毫秒
1.
Norio Kaifu 《Astrophysics and Space Science》1989,160(1-2):27-29
The current achievements of the observational abilities of radio astronomy is briefly reviewed putting emphasis on the imaging capability. The new projects in radio astronomy are discussed in connection with the new generation of optical/IR telescope projects.Paper presented at the Symposium on the JNLT and Related Engineering Developments, Tokyo, November 29–December 1988. 相似文献
2.
Noah Brosch 《Astrophysics and Space Science》2009,320(1-3):207-215
After considering a number of historical but somewhat “forgotten” UV astronomy experiments, I discuss a number of ways of non-conventional astronomy in the ultraviolet that, on first considerations, could be viable alternatives and valuable complements to classical space observations. These are (a) UV astronomy from the Antarctic or the Arctic regions that take advantage of the “ozone hole”, (b) the use of high-altitude stratospheric balloon-borne telescopes, and (c) the operation of UV telescopes on the Moon. The advantages of these options are discussed and evaluated against the costs of each option and, one by one, are mostly rejected as not fully justifying the specific alternative. The possibility to achieve valuable (but limited) UV science, such as imaging at ～2000 Å, using long-duration stratospheric balloons is described. The option of lunar UV observatories is retained to be implemented for the case of a UV interferometer, where the stability of the lunar regolith is seen as a significant advantage in comparison to free-flying interferometers. A location beyond the main asteroid belt, where the background due zodiacal light may be negligible, is advocated as an ideal location for a UV observatory in the Solar System. 相似文献
3.
Following the detection of extraterrestrial radio waves in 1932 by Karl Jansky, radio astronomy developed quickly after World War II. It established itself soon as a new branch of astronomy with today's outstanding record in the detection of new phenomena in space. These have been honoured by a number of Nobel prizes. Radio astronomy largely depends on technical developments in receiver technology, antenna systems, electronics and computing power. Ever shorter wavelengths down to the submm‐wavelength range became accessible, resulting in new exciting discoveries. However, now and in future care must be taken, in particular for the lower frequency range, of harmful man‐made interferences, which might mask the weak signals from space. New international facilities with orders‐of‐magnitude higher sensitivity like ALMA and SKA are planned or under construction. Space‐borne observatories like PLANCK will detect weak fluctuations of the cosmic microwave background, which will constrain cosmological models with an unprecedented accuracy. 相似文献
4.
Robert W. Smith 《Experimental Astronomy》2009,26(1-3):149-161
The history of space astronomy is usually written from the perspective of the remarkable scientific findings garnered by space astronomers and the ways these findings have enriched and guided new views of the universe. This paper examines some aspects of the history of space astronomy in the early years of NASA, but takes patronage, management and control as its key issues. 相似文献
6.
G. H. Rieke 《Experimental Astronomy》2009,25(1-3):125-141
The first attempts to measure the infrared outputs of stars preceded by nearly a century the permanent establishment of infrared astronomy as an important aspect of the field. There were a number of false starts in that century, significant efforts that had little impact on the astronomical community at large. Why did these efforts fizzle out? What was different in the start that did not fizzle, in the 1960s? I suggest that the most important advances were the success of radio astronomy in demonstrating interesting phenomena outside of the optical regime, and the establishment virtually simultaneously in the United States of a number of research groups that could support each other and compete against one another in their approach to infrared astronomy. 相似文献
7.
T. G. Artemenko M. A. Balyshev I. B. Vavilova 《Kinematics and Physics of Celestial Bodies》2009,25(3):153-167
The impact of the Struve astronomical dynasty on the development of astronomy in Ukraine in the 19th–20th centuries is studied.
First of all, the role of F.G.W. Struve and O.V. Struve in the formation of astronomical research programs at the observatories
at the Kharkiv, Kyiv, Odesa, and Mykolayiv, in equipping the observatories with instruments, in practical training of astronomers
as well as in the organization of astronomy-geodetic expeditions (19th century). Particular attention is paid to the activity
of L.O. Struve as a director of the Astronomical observatory of Kharkiv University and his works conducted together with G.A.
Shajn and B.P. Gerasimovich (20th century) as well as to the impact of his scientific and public activity, including one he
made as a President of IAC, on the development of astronomy in the Soviet Union and Ukraine. A range of important documents
from the archives of Russian Academy of Sciences, Institute of astronomy and State Archive of Ukraine are cited.
The article was translated by the authors. 相似文献
8.
9.
Minoru Oda 《Astrophysics and Space Science》1986,118(1-2):67-70
Japan's two X-ray astronomy satellites, HAKUCHO and TENMA, have been actively in operation leading to deeper understandings of the neutron star physics. Other satellite and balloon projects have been performed under international collaborators.Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984. 相似文献
10.
R. Seaman 《Astronomische Nachrichten》2008,329(3):237-240
Observational astronomy is the beneficiary of an ancient chain of apprenticeship. Kepler's laws required Tycho's data. As the pace of discoveries has increased over the centuries, so has the cadence of tutelage (literally, “watching over”). Naked eye astronomy is thousands of years old, the telescope hundreds, digital imaging a few decades, but today's undergraduates will use instrumentation yet unbuilt – and thus, unfamiliar to their professors – to complete their doctoral dissertations. Not only has the quickening cadence of astronomical data‐taking overrun the apprehension of the science within, but the contingent pace of experimental design threatens our capacity to learn new techniques and apply them productively. Virtual technologies are necessary to accelerate our human processes of perception and comprehension to keep up with astronomical instrumentation and pipelined dataflows. Necessary, but not sufficient. Computers can confuse us as efficiently as they illuminate. Rather, as with neural pathways evolved to meet competitive ecological challenges, astronomical software and data must become organized into ever more coherent ‘threads’ of execution. These are the same threaded constructs as understood by computer science. No datum is an island. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
11.
T. M. Palmieri 《Astrophysics and Space Science》1974,28(2):277-287
The Multiplex Advantage is defined and applied in considering various techniques presently used in X-ray astronomy. It is concluded that the multiplex advantage will be useful in evaluating future techniques to be used in X-ray astronomy. 相似文献
12.
Riccardo Giacconi 《Experimental Astronomy》2009,25(1-3):143-156
The development of X-ray telescopes over the last 45 years is briefly summarized. The first applications to the study of solar X-ray emission are described up to the 1973 Skylab mission. The rather convoluted path that led to the first stellar X-ray orbiting telescope Einstein (1978) and later to Chandra (1999) are discussed. During this 45 years period the angular resolution improved from 20 to 0.5 arc sec and the sensitivity by ten billions. X-ray observations have discovered new types of stellar systems (binary X-ray sources containing neutron stars and black holes) and intergalactic high temperature plasmas containing most of the baryonic mass of the universe. They have become an indispensable tool to study the role of energetic phenomena in the creation and dynamic evolution of cosmic structures. The methodology introduced by X-ray astronomy has influenced all of astronomy. 相似文献
13.
F.G. Smith 《Astronomische Nachrichten》2007,328(5):426-431
Radio astronomy started in Cambridge immediately after the hostilities of the World War II have ceased. Martin Ryle was the inspiring leader of a small group that started to develop interferometry techniques at the Cavendish Laboratory. From this development came the numerous Cambridge radio source surveys culminating in the Nobel prize awarded to Martin Ryle for invention of aperture synthesis. The history of this early development is the subject of the present paper. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
14.
V. Schnfelder 《Astronomische Nachrichten》2002,323(6):524-529
An overview of the history of gamma‐ray astronomy is given starting with predictions in the 1950s and first detections in the 1960s. Tremendous efforts have been made since then, with exciting discoveries, which finally culminated in the “Golden Age” of gamma‐ray astronomy which we are presently experiencing. 相似文献
15.
R. Bharat 《Experimental Astronomy》1994,3(1-4):219-225
An overview of the three major types of impurity band conduction (IBC) detectors — Blocked Impurity Band (BIB) detector, Solid State Photomultiplier (SSPM) and Visible Light Photon Counter (VLPC) - pioneered by Rockwell is presented. Key functional features, level of developmental maturity and applications to astronomy are described. 相似文献
16.
The increasing array size of radio astronomy interferometers is causing the associated computation to scale quadratically with the number of array signals. Consequently, efficient usage of alternate processing architectures should be explored in order to meet this computational challenge. Affordable parallel processors have been made available to the general scientific community in the form of the commodity graphics card. This work investigates the use of the Graphics Processing Unit in the parallelisation of the combined conjugate multiply and accumulation stage of a correlator for a radio astronomy array. Using NVIDIA’s Compute Unified Device Architecture, our testing shows processing speeds from one to two orders of magnitude faster than a Central Processing Unit approach. 相似文献
17.
H. Inoue 《Experimental Astronomy》1993,4(1):1-10
ASCA (ASTRO-D), the fourth X-ray astronomy satellite of ISAS, was successfully launched on February 20, 1993. It carries nested thin-foil X-ray mirrors providing a large effective area over a wide energy range up to 12 keV. A set of CCD cameras and imaging gas scintillation proportional counters are placed on the focal plane.ASCA is a high-throughput imaging and spectroscopic X-ray observatory with these instruments. 相似文献
18.
Considerable progress has been made in the last half-decade in the field of very high energy (VHE) gamma-ray astronomy (photons with energies between 1011 and 1013 eV). The high background level due to the isotropic cosmic ray flux which has bedevilled the field since its inception in the early 1960's can now be reduced to such a degree that significant gamma-ray signals from several sources become visible within a few hours of observation. The instrumentation and methodologies which have made this possible are reviewed. A brief historical introduction is followed by a summary of the salient properties of the atmospheric Cherenkov flash associated with VHE gamma-ray events. The major components of a VHE gamma-ray astronomy telescope are then reviewed. This is followed by a discussion of the different methodologies currently being used to discriminate against the cosmic ray background. Properties of several specific installations are then summarized, and possible future developments in VHE instrumentation are briefly discussed. 相似文献
19.
Jeffrey L. Linsky 《Astrophysics and Space Science》2018,363(5):101
Astronomers have long recognized the critical need for ultraviolet imaging, photometry and spectroscopy of stars, planets, and galaxies, but this need could not be satisfied without access to space and the development of efficient instrumentation. When UV measurements became feasible, first with rockets and then with satellites, major discoveries came rapidly. It is true in the UV spectral region as in all others, that significant increases in sensitivity, spectral resolution, and time domain coverage have led to significant new understanding of astrophysical phenomena. I will describe a selection of these discoveries made in each of three eras: (1) the early history of rocket instrumentation and Copernicus, the first UV satellite, (2) the discovery phase pioneered by the IUE, FUSE and EUVE satellites, and (3) the full flowering of UV astronomy with the successful operation of HST and its many instruments. I will also mention a few areas where future UV instrumentation could lead to new discoveries. This review concentrates on developments in stellar and interstellar UV spectroscopy; the major discoveries in galactic, extragalactic, and solar system research are beyond the scope of this review. The important topic of UV technologies and detectors, which enable the remarkable advances in UV astronomy are also not included in this review. 相似文献
20.
It is suggested that the development of the SKA will drastically change the face of radio astronomy in the 21st Century. A
FAST-style SKA would admit observations of low contrast features, and would be the best design for studying the `dark ages'
of the Universe (x≫ 1) where sub-arcmin total power instruments can usefully be employed. To date there have been no proposals for post-SKA,
billion square-metra instruments; we speculate that mobile communication systems can be used. In the very distant future,
SKA multi-beam systems could be used to collect signals reflected by Solar system bodies such as the asteroid belt.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献