Observations of the Quiet Sun with 6″ Resolution

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.

Download Full-text

Variation of Quiet Sun Radiation during Solar Cycles 23 and 24

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317007992 ◽

2017 ◽

Vol 13 (S335) ◽

pp. 11-13

Author(s):

Mahender Aroori ◽

G. Yellaiah ◽

K. Chenna Reddy

Keyword(s):

Radio Emission ◽

Brightness Temperature ◽

Statistical Method ◽

Solar Radio ◽

Solar Radio Emission ◽

Solar Cycles ◽

Quiet Sun ◽

Data Centre ◽

National Geophysical Data ◽

Using Data

AbstractRadio observations play a very important role in understanding the structure of the solar atmosphere. In this paper the quiet sun component of the solar radio emission has been investigated using data obtained from the Solar Indices Bulletin, National Geophysical Data Centre. By statistical method, the quiet sun component is estimated for 84 successive basic periods containing three solar rotations each using data obtained at different frequencies. From the quiet sun component we estimate the brightness temperature in each observing frequency.

Download Full-text

High Resolution Solar Observations at Three Frequencies: 1424 MHz, 696 MHz and 408 MHz

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000010456 ◽

1967 ◽

Vol 1 (2) ◽

pp. 45-46

Author(s):

D. G. Cole ◽

R. F. Mullaly ◽

A. Watkinson

Keyword(s):

High Resolution ◽

Radio Emission ◽

Solar Radio ◽

Solar Radio Emission ◽

The Sun ◽

Physical Mechanisms ◽

Solar Observations ◽

Source Structure ◽

East West

During the period 1966 July 12 to August 5 observations were made of the Sun at three radio observatories. The instruments used were the east-west arm of the Mills cross at Molonglo (408 MHz) and the Christiansen cross at Fleurs (696 MHz and 1424 MHz). The aim of these observations was to study the discrete sources of the slowly varying component of solar radio emission, while activity was comparatively quiet. The three frequencies enabled the variation of source structure with height of solar atmosphere to be studied. It has been pointed out by Swarup et al., and Christiansen et al. that the determination of the frequency dependence of these discrete sources is important for defining the physical mechanisms causing the radio emission.

Download Full-text

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

Astronomische Nachrichten ◽

10.1002/asna.2113110517 ◽

1990 ◽

Vol 311 (5) ◽

pp. 313-315 ◽

Cited By ~ 2

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

Download Full-text

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

International Astronomical Union Colloquium ◽

10.1017/s0252921100017541 ◽

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.

Download Full-text

Investigations of solar radio emission, solar wind and ionospheric disturbances with using Ukrainian decameter radio telescope system URAN and spacecrafts

Kosmìčna nauka ì tehnologìâ ◽

10.15407/knit2015.03.003 ◽

2015 ◽

Vol 21 (3(94)) ◽

pp. 3-8

Author(s):

N.N. Kalinichenko ◽

◽

A.A. Konovalenko ◽

Ya.S. Yatskiv ◽

L.N. Litvinenko ◽

...

Keyword(s):

Solar Wind ◽

Radio Emission ◽

Radio Telescope ◽

Solar Radio ◽

Solar Radio Emission ◽

Ionospheric Disturbances ◽

Decameter Radio ◽

Telescope System

Download Full-text

69. Disturbed radio emission from the sun as a sum of small monochromatic peaks

Symposium - International Astronomical Union ◽

10.1017/s0074180900049445 ◽

1957 ◽

Vol 4 ◽

pp. 363-365 ◽

Cited By ~ 1

Author(s):

V. V. Vitkevitch

Keyword(s):

Radio Emission ◽

Solar Radio ◽

Solar Radio Emission ◽

The Sun ◽

General Increase ◽

Quiet Sun ◽

Small Areas ◽

Physical Institute ◽

Academy Of Sciences

Observations of the radio emission from the sun carried out during recent years at the Crimean Station of the Physical Institute of the U.S.S.R. Academy of Sciences showed that the occurrence of spots appreciably increases the intensity of the solar radio emission in the range of metre wave-lengths. This increase of intensity has two components. The first (S-component) changes comparatively slowly with time. The second (P-component) consists of individual brief bursts (of the order of a second and less) of small amplitudes (10–100 % of the intensity of the quiet sun). The P-component is manifested most clearly in the emission connected with spots of small areas, when the general increase of the intensity is insignificant. Such a situation has been utilized for the study of the spectrum of individual small peaks.

Download Full-text

Observation of solar radio emission by the 22-m radio telescope at the Crimean Astrophysical Observatory at 2.25 mm and 8.15 mm wavelengths

Solar Physics ◽

10.1007/bf00155380 ◽

1969 ◽

Vol 8 (2) ◽

pp. 331-340 ◽

Cited By ~ 11

Author(s):

V. A. Efanov ◽

A. G. Kislyakov ◽

I. G. Moiseev ◽

A. I. Naumov

Keyword(s):

Radio Emission ◽

Radio Telescope ◽

Solar Radio ◽

Crimean Astrophysical Observatory ◽

Solar Radio Emission

Download Full-text

Properties of sources of the slowly varying component of 2 cm solar radio emission

Symposium - International Astronomical Union ◽

10.1017/s007418090002204x ◽

1968 ◽

Vol 35 ◽

pp. 575-580

Author(s):

V. G. Nagnibeda

Keyword(s):

High Resolution ◽

Radio Emission ◽

Radio Astronomy ◽

Solar Radio ◽

Emission Spectra ◽

Active Regions ◽

Solar Radio Emission ◽

Radio Sources ◽

Pulkovo Observatory ◽

Local Sources

To study the nature of the local sources of solar radio emission connected with active regions, it is important to investigate the structure of such sources and their emission spectra. These problems are being investigated in detail by a group of workers of the Radio Astronomy Department of the Pulkovo Observatory led by G.B. Gelfreikh. The Pulkovo large radio telescope used for the observations allows them to investigate the solar radio sources at the whole cm-wavelength range with a high resolution reaching 40 sec of arc at the 2-cm wave. Observations are taken at 2·0, 3·2, 4·4, 6·6, and 9-cm waves. The author observes at the 2-cm wave.

Download Full-text