Multiband exciters for Solar Radio Telescopes

1973 ◽  
Vol 16 (12) ◽  
pp. 1479-1481
Author(s):  
V. M. Vyatkina ◽  
V. G. Ioganson
Keyword(s):  
Solar Radio ◽  
Radio Telescopes

scholarly journals Solar Radio Burst (Type III)

1996 ◽  
Vol 154 ◽  
pp. 251-254
Author(s):  
Hari Om Vats ◽  
M.R. Deshpande ◽  
K.N. Iyer ◽  
Tetsuro Kondo ◽  
Takeshi Isobe
Keyword(s):  
Radio Burst ◽  
Solar Radio ◽  
Solar Radio Burst ◽  
Radio Telescopes ◽  
Fall Time ◽  
Type Iii

AbstractThis article describes the observations of a type III radio burst observed at 103 MHz simultaneously by the two radio telescopes situated at Rajkot (22.3°N, 70.7°E) and Thaltej (23°N, 72.4°E). This event occurred on September 30, 1993 at about 0430 UT and lasted for only half a minute. The event consisted of several sharp spikes in a group. The rise and fall time of these are comparable, however the peaks of individual spikes varied by a factor of four. The comparison of these observations with the data of solar radio spectrograph HiRAS indicates that this was a metric radio burst giving highest emission at about 103 MHz.

scholarly journals Small-sized radio telescopes for monitoring and studies of solar radio emission at meter and decameter wavelengths

2019 ◽  
Author(s):  
Sergei Yerin ◽  
Alexander Stanislavsky ◽  
I. Bubnov ◽  
A. Konovalenko ◽  
P. Tokarsky ◽  
...  
Keyword(s):  
Radio Emission ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Radio Telescopes

Measurements of Radio Interference at Solar Radio Stations in Beijing

2001 ◽  
Vol 196 ◽  
pp. 311-314 ◽  
Author(s):  
Yihua Yan ◽  
Qijun Fu ◽  
Yuying Liu ◽  
Zhijun Chen
Keyword(s):  
Solar Radio ◽  
Radio Interference ◽  
Radio Telescopes ◽  
Radio Stations ◽  
Working Frequency

Shahe Station of our Solar Radio Group has suffered from radio interference in recent years, so we decided to move our solar radio telescopes to Huairou Station of BAO. We measured radio interference at both sites recently and found that the radio interference is more serious in Shahe than in Huairou. Although the interference is low at the single working frequency, we do find some radio interference within the working band at Shahe. It is comparatively radio quiet at Huairou and suitable for placement of the solar radio instruments there.

scholarly journals 45. The quiet and active sun: Introductory Lecture

1957 ◽  
Vol 4 ◽  
pp. 253-262 ◽  
Author(s):  
C. W. Allen
Keyword(s):  
Solar Activity ◽  
Radio Emission ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Radio Telescopes ◽  
Variable Part ◽  
Introductory Lecture

It is both convenient and realistic to regard the solar radio-emission as being composed of a quiet permanent part coming from the whole of the sun's surface, together with a superimposed variable part emitted from centres of activity. The variable part can be further subdivided into various components to which separate reference will be made. The components are almost independent and add to one another to give the solar emission recorded by radio telescopes. For our understanding of the phenomena it would be a great advantage if the components could be completely and reliably segregated but this is not always possible. The results from a wide network of observational stations are recorded in theQuarterly Bulletin of Solar Activity, from which the intensities and characteristics of most of the components may be extracted.

Type II Solar Radio Bursts over Solar Cycle 21

1994 ◽  
Vol 144 ◽  
pp. 283-284
Author(s):  
G. Maris ◽  
E. Tifrea
Keyword(s):  
Solar Radio ◽  
Interplanetary Space ◽  
Impulsive Phase ◽  
Radio Bursts ◽  
Type Ii ◽  
Solar Radio Bursts ◽  
Strong Energy ◽  
Mass Ejection ◽  
Geophysical Effect ◽  
Radio Event

The type II solar radio bursts produced by a shock wave passing through the solar corona are one of the most frequently studied solar activity phenomena. The scientific interest in this type of phenomenon is due to the fact that the presence of this radio event in a solar flare is an almost certain indicator of a future geophysical effect. The origin of the shock waves which produce these bursts is not at all simple; besides the shocks which are generated as a result of a strong energy release during the impulsive phase of a flare, there are also the shocks generated by a coronal mass ejection or the shocks which appear in the interplanetary space due to the supplementary acceleration of the solar particles.

The Role of VLBI in the Establishment of Coordinate Systems

1975 ◽  
Vol 26 ◽  
pp. 293-295 ◽  
Author(s):  
I. Zhongolovitch
Keyword(s):  
General Solution ◽  
Future Development ◽  
Rational Approach ◽  
Radio Telescopes ◽  
Coordinate Systems ◽  
Tectonic Plates ◽  
Astronomical Observations ◽  
Optical Instruments ◽  
Fundamental Polyhedron

Considering the future development and general solution of the problem under consideration and also the high precision attainable by astronomical observations, the following procedure may be the most rational approach:1. On the main tectonic plates of the Earth’s crust, powerful movable radio telescopes should be mounted at the same points where standard optical instruments are installed. There should be two stations separated by a distance of about 6 to 8000 kilometers on each plate. Thus, we obtain a fundamental polyhedron embracing the whole Earth with about 10 to 12 apexes, and with its sides represented by VLBI.

The Current Situation in Chemical Stabilization of Biological Materials

1972 ◽  
Vol 30 ◽  
pp. 132-133
Author(s):  
John H. Luft
Keyword(s):  
Electron Microscopy ◽  
Electron Microscope ◽  
Osmium Tetroxide ◽  
Molecular Level ◽  
Cross Linking ◽  
Chemical Stabilization ◽  
Specimen Preparation ◽  
Sufficient Condition ◽  
Radio Telescopes

With information processing devices such as radio telescopes, microscopes or hi-fi systems, the quality of the output often is limited by distortion or noise introduced at the input stage of the device. This analogy can be extended usefully to specimen preparation for the electron microscope; fixation, which initiates the processing sequence, is the single most important step and, unfortunately, is the least well understood. Although there is an abundance of fixation mixtures recommended in the light microscopy literature, osmium tetroxide and glutaraldehyde are favored for electron microscopy. These fixatives react vigorously with proteins at the molecular level. There is clear evidence for the cross-linking of proteins both by osmium tetroxide and glutaraldehyde and cross-linking may be a necessary if not sufficient condition to define fixatives as a class.

One Step Short of Life

2018 ◽  
Author(s):  
Karel Schrijver
Keyword(s):  
Liquid Water ◽  
Radio Telescopes ◽  
Speed Of Light ◽  
Extraterrestrial Life ◽  
True Nature ◽  
One Step ◽  
New Strategies ◽  
Present Focus

This chapter briefly reviews some the challenges encountered in the search for extraterrestrial life. So far, no signs of extraterrestrial life have been found. The search started with radio telescopes, looking for technology-based civilizations, but new strategies have emerged that take on the primary challenges in this search: the enormous distances to exoplanets and the question of the true nature of life. The author outlines the development of new tools for the search, and why the present focus is on Earth-sized exoplanets with a potential for liquid water on their surfaces. Not having been visited by an alien civilization presents us with a paradox: if life develops as quickly elsewhere as on Earth, then why have we not been contacted? Is the speed of light too slow to cross interstellar distances, is life intrinsically rare, or should we conclude that civilizations are intrinsically short-lived?

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