Thermal Radio Emission of the Moon at a Wave Length of 10 cm

1962 ◽  
Vol 14 ◽  
pp. 497-499
Author(s):  
V. N. Koshchenko ◽  
A. D. Kuzmin ◽  
A. E. Salomonovich
Keyword(s):  
Surface Layer ◽  
Radio Emission ◽  
Thermal Radiation ◽  
Wave Length ◽  
The Moon ◽  
Phase Dependence ◽  
Radio Range ◽  
Thermal Radio ◽  
Thermal Radio Emission

The investigations of intensity and phase dependence of the thermal radiation of the Moon at various wave lengths of the radio-range are very important for clarifying the properties and structure of the Moon's surface layer.

scholarly journals 42. Radio astronomy and the origin of cosmic rays

1957 ◽  
Vol 4 ◽  
pp. 238-240 ◽  
Author(s):  
A. Unsöld
Keyword(s):  
Cosmic Rays ◽  
Radio Emission ◽  
Thermal Radiation ◽  
Radio Astronomy ◽  
The Sun ◽  
Thermal Radio ◽  
Thermal Radio Emission

At present we can observe the origin of only the solar component of cosmic rays. The sun emits cosmic rays in connexion with flares and probably also continuously on a smaller scale. Thus the emission of cosmic rays appears to be connected much more closely with non-thermal radio emission than with thermal radiation of light and heat.

Thermal Radio Emission of the Moon and Certain Characteristics of its Surface Layer

1962 ◽  
Vol 14 ◽  
pp. 491-495 ◽  
Author(s):  
A. E. Salomonovich
Keyword(s):  
Surface Layer ◽  
Radio Emission ◽  
Additional Data ◽  
Optical Data ◽  
The Moon ◽  
Lunar Crust ◽  
Physics Institute ◽  
Thermal Radio Emission ◽  
Academy Of Sciences ◽  
Selection Of

In order to use the data on the radio emission of the Moon as a basis for conclusions regarding the characteristics of the surface layer of the lunar crust, additional data or assumptions about the properties of this layer are necessary. The use of high-resolution radio telescopes reduces to a certain extent the unavoidable arbitrariness in the selection of parameters. Observations with the 22-m radio telescope of the Physics Institute, Academy of Sciences, made it possible to evaluate certain characteristics of the surface layer without relying entirely on optical data.

scholarly journals Thermal Radio Emission from Normal Galaxies

1972 ◽  
Vol 44 ◽  
pp. 75-81 ◽  
Author(s):  
Yervant Terzian
Keyword(s):  
Radio Emission ◽  
Thermal Radiation ◽  
Spiral Galaxies ◽  
Hii Regions ◽  
Electron Densities ◽  
Normal Galaxies ◽  
Millimeter Wavelengths ◽  
Thermal Radio ◽  
Thermal Radio Emission ◽  
Normal Spiral

Thermal radiation from normal spiral galaxies may be detectable at centimeter and millimeter wavelengths. Predictions have been made assuming free-free radiation from Hii regions at Te = 7000 K, and a range of mean electron densities and radii.

Resonance effects in thermal radio emission of water surface

1986 ◽  
Vol 29 (4) ◽  
pp. 279-283 ◽  
Author(s):  
V. E. Gershenzon ◽  
V. G. Irisov ◽  
Yu. G. Trokhimovskii ◽  
V. S. �tkin
Keyword(s):  
Radio Emission ◽  
Water Surface ◽  
Resonance Effects ◽  
Thermal Radio ◽  
Thermal Radio Emission

scholarly journals Non-thermal radio emission from O-type stars

2007 ◽  
Vol 464 (2) ◽  
pp. 701-708 ◽  
Author(s):  
R. Blomme ◽  
M. De Becker ◽  
M. C. Runacres ◽  
S. Van Loo ◽  
D. Y. A. Setia Gunawan
Keyword(s):  
Radio Emission ◽  
Thermal Radio ◽  
Thermal Radio Emission

scholarly journals Erratum: Constraining the nature of DG Tau A's thermal and non-thermal radio emission

2018 ◽  
Vol 483 (3) ◽  
pp. 4085-4085
Author(s):  
S J D Purser ◽  
R E Ainsworth ◽  
T P Ray ◽  
D A Green ◽  
A M Taylor ◽  
...  
Keyword(s):  
Radio Emission ◽  
Thermal Radio ◽  
Thermal Radio Emission

scholarly journals Non-thermal radio emission in Wolf-Rayet stars: is binarity a pre-requisite?

1999 ◽  
Vol 193 ◽  
pp. 348-349
Author(s):  
Sean M. Dougherty
Keyword(s):  
Radio Emission ◽  
Spectral Index ◽  
Thermal Emission ◽  
Radio Observations ◽  
Thermal Radio ◽  
Thermal Radio Emission ◽  
Thermal Emitters

Radio observations of Wolf-Rayet stars currently available in the literature are examined to determine whether binarity is a common feature of WR systems with non-thermal emission. Among 24 stars with observed spectral index values, seven are definite non-thermal emitters, and six others possibly have composite thermal/non-thermal spectra. Stellar companions have been identified in 71% of the non-thermal emitters, strongly supporting a link between non-thermal emission and binarity.

scholarly journals The nearby extreme accretion and feedback system PDS 456: finding a complex radio-emitting nucleus

2020 ◽  
Vol 500 (2) ◽  
pp. 2620-2626
Author(s):  
Jun Yang ◽  
Zsolt Paragi ◽  
Emanuele Nardini ◽  
Willem A Baan ◽  
Lulu Fan ◽  
...  
Keyword(s):  
Black Hole ◽  
Radio Emission ◽  
High Speed ◽  
Feedback System ◽  
Emission Region ◽  
Starburst Galaxy ◽  
Massive Black Hole ◽  
Star Forming ◽  
Thermal Radio ◽  
Thermal Radio Emission

ABSTRACT When a black hole accretes close to the Eddington limit, the astrophysical jet is often accompanied by radiatively driven, wide-aperture and mildly relativistic winds. Powerful winds can produce significant non-thermal radio emission via shocks. Among the nearby critical accretion quasars, PDS 456 has a very massive black hole (about 1 billion solar masses), shows a significant star-forming activity (about 70 solar masses per year), and hosts exceptionally energetic X-ray winds (power up to 20 per cent of the Eddington luminosity). To probe the radio activity in this extreme accretion and feedback system, we performed very long baseline interferometric (VLBI) observations of PDS 456 at 1.66 GHz with the European VLBI Network and the enhanced Multi-Element Remotely Linked Interferometry Network. We find a rarely seen complex radio-emitting nucleus consisting of a collimated jet and an extended non-thermal radio emission region. The diffuse emission region has a size of about 360 pc and a radio luminosity about three times higher than that of the nearby extreme starburst galaxy Arp 220. The powerful nuclear radio activity could result either from a relic jet with a peculiar geometry (nearly along the line of sight) or more likely from diffuse shocks formed naturally by the existing high-speed winds impacting on high-density star-forming regions.

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