scholarly journals New data on the solar supercorona

1959 ◽  
Vol 9 ◽  
pp. 275-281
Author(s):  
V. V. Vitkevich
Keyword(s):  
Radio Emission ◽  
Solar Corona ◽  
Crab Nebula ◽  
New Method ◽  
Radio Waves ◽  
Pass Through ◽  
Academy Of Sciences ◽  
The Crab Nebula

1. This paper reports on the results of the investigation of the outermost regions of the solar corona (which for brevity I shall call the supercorona) that have been obtained during recent years.Seven years ago, in 1951, a new method of observation was published in Doklady of the Academy of Sciences of the U.S.S.R. The idea of the method, which at the present time is well known, is that the radio emission of the Crab nebula is received at the time when the source is covered by the solar corona. This original eclipse takes place yearly in the middle of June.By receiving the radio waves that pass through the solar corona regions, we can estimate the effects of attenuation, scattering and refraction and reach some conclusions about the structure of the supercorona.

scholarly journals 58. Results of observations of the scattering of radio waves by the electronic inhomogeneities of the solar corona

1957 ◽  
Vol 4 ◽  
pp. 313-317
Author(s):  
V. V. Vitkevitch
Keyword(s):  
Solar Corona ◽  
Radio Source ◽  
Crab Nebula ◽  
New Method ◽  
Radio Waves ◽  
The Crab Nebula

A new method for the investigation of the solar corona, suggested by us (Vitkevitch, 1951) [1], consists of observing the radio source identified with the Crab nebula (NGC 1952; α = 05h 31m 40s, δ = 22° 10′) when it is covered by the solar corona. This occurs every year on 14–15 June.

Multibaseline Observations of the Occultation of Crab Nebula by the Solar Corona at Decameter Wavelengths

2000 ◽  
Vol 179 ◽  
pp. 421-422
Author(s):  
K. R. Subramanian
Keyword(s):  
Refractive Index ◽  
Solar Corona ◽  
Radio Source ◽  
Crab Nebula ◽  
Angular Size ◽  
Radio Sources ◽  
Radio Waves ◽  
Apparent Increase ◽  
Pass Through ◽  
Point To Point

Extended abstractInformation about the outer solar corona can be obtained by observing the occultation of radio sources by the solar corona. As the radio waves pass through the corona they get scattered due to the fact that the electron density and consequently the refractive index varies from point to point. The effect of scattering is manifested by an apparent increase in the angular size of the radio source which can be measured by suitable interferometers. We present here multibaseline observations on the occultation of Crab Nebula at 34.5 MHz with baselines extending upto 4.9 km during June 1986 and 1987.

scholarly journals The scattering of radio waves in the solar corona

1959 ◽  
Vol 9 ◽  
pp. 268-273 ◽  
Author(s):  
A. Hewish
Keyword(s):  
Solar Corona ◽  
Crab Nebula ◽  
Angular Diameter ◽  
Radio Waves ◽  
The Crab Nebula ◽  
The Waves

The angular diameter of the Crab nebula is considerably increased when it is viewed through the solar corona. This effect is due to the scattering of the waves by coronal irregularities and its study gives some indication of the nature of the outermost corona. This paper is a summary of observations carried out each year at Cambridge for the period 1952 to 1958 inclusive.

scholarly journals Occupation of the Crab Nebula by the Solar Corona in June 1963

Nature ◽  
1963 ◽  
Vol 200 (4908) ◽  
pp. 766-766 ◽  
Author(s):  
J. D. WYNDHAM ◽  
B. G. CLARK
Keyword(s):  
Solar Corona ◽  
Crab Nebula ◽  
The Crab Nebula

scholarly journals 79. Radio emission from the moon and the nature of its surface

1957 ◽  
Vol 4 ◽  
pp. 406-407 ◽  
Author(s):  
V. S. Troitzky ◽  
S. E. Khaikin
Keyword(s):  
Radio Emission ◽  
Attenuation Coefficient ◽  
Wave Length ◽  
Degree Of Polarization ◽  
Lunar Phase ◽  
Radio Waves ◽  
The Moon ◽  
Subsolar Point ◽  
Image Position ◽  
Academy Of Sciences

A theoretical study of the integral radio emission of the moon, measured at the wave-length of 3·2 cm. (Zelinskaja and Troitzky[1]; Kajdanovsky, Turusbekov and Khaikin[2]), was carried out at the Gorky radio astronomical station ‘Zimenky’ and at the Physical Institute of the Academy of Sciences of the U.S.S.R. The following expression for the average radio temperature of the entire lunar disk, as a function of the lunar phase, Ωt, was obtained (Troitzky, 1954) [3]: Here tan ξ = δ/(1 + δ) and δ = β/κ, where β is the attenuation coefficient of the thermal wave, κ the power attenuation coefficient of the radio wave. Further, Tm = 374°K. is the temperature of the subsolar point, Tn is the temperature at the lunar midnight, Θ = Tm – Tn and k0 is the reflexion coefficient of radio waves for vertical incidence (k0 ≈ 0–1). The numerical coefficients in equation (1) were obtained as a result of averaging the Fresnel reflexion coefficients over the whole disk. The degree of polarization of the total radio emission was calculated and was found to be about 4 %.

scholarly journals Polarization of 10-cm radiation of the Crab nebula

1959 ◽  
Vol 9 ◽  
pp. 305-308
Author(s):  
A. D. Kuz'min ◽  
V. A. Udal'tsov
Keyword(s):  
Crab Nebula ◽  
Physical Institute ◽  
Academy Of Sciences ◽  
The Crab Nebula

In October and November 1957 at the Physical Institute of the Academy of Sciences of the U.S.S.R. a search was conducted to detect the plane polarization of the radiation from the Crab nebula at 9.6-cm wavelength [1].

scholarly journals Peculiar Differences in Radio and X-ray Synchrotron Radiation from Pulsar Wind Nebulae

2004 ◽  
Vol 218 ◽  
pp. 221-224
Author(s):  
John R. Dickel ◽  
Shiya Wang
Keyword(s):  
Synchrotron Radiation ◽  
Radio Emission ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Pulsar Wind Nebulae ◽  
X Ray ◽  
Pulsar Wind ◽  
The Crab Nebula

Several Crab-type supernova remnants appear to have very bright non-thermal X-ray cores just around the pulsar or expected pulsar. This X-ray brightness is often not matched by a corresponding increase in radio emission. The best example of this phenomenon is in N157B in the LMC. G21.5−0.9 and possibly 3C 58 also show it while the Crab Nebula and 0540−69.3 do not. Some method to enhance the higher energy particles must be present in these objects.

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