scholarly journals 23rd Cycle of Solar Activity in the Light of 34 Years of Cracow Observations of Solar Radio Emission

1993 ◽  
Vol 137 ◽  
pp. 87-89
Author(s):  
Adam Michalec
Keyword(s):  
Solar Activity ◽  
Radio Emission ◽  
Radio Telescope ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
23Rd Cycle

Systematic daily observations of solar radio emission were started at the Fort Skała Observatory on 1st October 1957. The observations were made at the frequency of 810 MHz first with a 5m radio telescope - and since 1964 with a 7m one; at present they comprise already almost 70 thousand hours of observations (Michalec 1991). During that period there were two longer interruptions in the observations: from 23 September 1963 to 2 February 1964 - due to transferring the radio telescope’s antenna from the top of the Fort to a new site, and from 6 November 1973 to 11 March 1974 - connected with the reconstruction of the receiver. Other, fortunately short, interruptions in the course of observations had no influence on the homogeneity of the series.

scholarly journals Observations of the Quiet Sun with 6″ Resolution

1980 ◽  
Vol 86 ◽  
pp. 53-55
Author(s):  
M. R. Kundu ◽  
A. P. Rao ◽  
F. T. Erskine ◽  
J. D. Bregman
Keyword(s):  
High Resolution ◽  
Radio Emission ◽  
Transition Region ◽  
Spatial Resolution ◽  
Radio Telescope ◽  
Solar Radio ◽  
High Spatial Resolution ◽  
Solar Radio Emission ◽  
Quiet Sun ◽  
Millimeter Wavelengths

Solar radio emission at centimeter and millimeter wavelengths originates in the chromosphere and transition region and is a useful probe for the temperature and density in these regions. High spatial resolution observations of the quiet sun provide valuable information on the structure of the solar atmosphere. We have performed high resolution (~ 6″ (E-W) x 15″ (N-S)) observations at 6 cm with the Westerbork Synthesis Radio Telescope (WSRT) in June 1976 in order to search for the radio analog of the supergranulation network and to study the extent and symmetry of limb brightening. The use of the WSRT for high spatial resolution solar mapping has been described by Bregman and Felli (1976), Kundu et al. (1977), and others.

Some results of solar radio emission observations at the Siberian Solar Radio Telescope

1990 ◽  
Vol 311 (5) ◽  
pp. 313-315 ◽  
Author(s):  
G. N. Zubkova ◽  
N. N. Kardapolova ◽  
B. I. Lubyshev ◽  
V. P. Nefedyev ◽  
G. Ya. Smolkov ◽  
...  
Keyword(s):  
Radio Emission ◽  
Radio Telescope ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Siberian Solar Radio Telescope

scholarly journals Structural and Evolutionary Features of Flare-Producing Active Regions During 1988-1990

1993 ◽  
Vol 141 ◽  
pp. 388-390
Author(s):  
A. A. Golovko
Keyword(s):  
Solar Activity ◽  
Radio Emission ◽  
Solar Radio ◽  
Active Regions ◽  
Magnetic Activity ◽  
High Solar Activity ◽  
Solar Radio Emission ◽  
Evolutionary Features ◽  
Siberian Solar Radio Telescope ◽  
Flare Productivity

During the period of high solar activity (1988-1990) the Sayan and Baikal Observatories of the ISTP carried out observations of the chromosphere in the H-alpha line, the photosphere and of sunspot magnetic fields; at the Siberian Solar Radio Telescope, solar radio emission observations at 5.2 cm wavelength were made. Using those observations a study is made of the evolution of “centers of magnetic activity” (Bumba, 1986) in nine active regions with different flare productivity, for which the most complete observations were available. In three cases (NOAA Nos. 5229, 5643 and 5669) they were the targets of the cooperative international Max’91 program.

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.

Mid-term Periodicities in Solar Radio Emission Corresponding to Sunspot Number During Solar Cycle 23

Solar Physics ◽  
2021 ◽  
Vol 296 (3) ◽  
Author(s):  
Mahender Aroori ◽  
Panditi Vemareddy ◽  
Partha Chowdhury ◽  
Ganji Yellaiah
Keyword(s):  
Solar Cycle ◽  
Radio Emission ◽  
Sunspot Number ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Solar Cycle 23

Flare-plasma diagnostics from millisecond pulsations of the solar radio emission

2002 ◽  
Vol 46 (6) ◽  
pp. 497-514 ◽  
Author(s):  
V. F. Melnikov ◽  
G. D. Fleishman ◽  
Q. J. Fu ◽  
G.-L. Huang
Keyword(s):  
Radio Emission ◽  
Plasma Diagnostics ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Flare Plasma
Sign in / Sign up

Export Citation Format

Share Document