Synchrotron radiation from relativistic electrons in intense magnetic fields

1975 ◽  
Vol 18 (10) ◽  
pp. 1400-1405 ◽  
Author(s):  
A. A. Sokolov ◽  
A. V. Borisov ◽  
V. Ch. Zhukovskii
Keyword(s):  
Synchrotron Radiation ◽  
Magnetic Fields ◽  
Relativistic Electrons

scholarly journals Neutrino Pair Synchrotron Radiation from Relativistic Electrons in Strong Magnetic Fields

1995 ◽  
Vol 448 ◽  
pp. 264 ◽  
Author(s):  
A. Vidaurre ◽  
A. Perez ◽  
H. Sivak ◽  
J. Bernabeu ◽  
J. M. A. Ibanez
Keyword(s):  
Synchrotron Radiation ◽  
Magnetic Fields ◽  
Relativistic Electrons ◽  
Strong Magnetic Fields ◽  
Neutrino Pair

Radio Emission from Starspots on RSCVn Binary HR1099

1986 ◽  
Vol 6 (3) ◽  
pp. 316-319 ◽  
Author(s):  
John D. Bunton ◽  
R. T. Stewart ◽  
O. B. Slee ◽  
G. J. Nelson ◽  
Alan E. Wright ◽  
...  
Keyword(s):  
Synchrotron Radiation ◽  
Magnetic Fields ◽  
Radio Emission ◽  
Light Curve ◽  
Circular Polarization ◽  
Rotation Rate ◽  
Source Model ◽  
Microwave Emission ◽  
Relativistic Electrons ◽  
Synchrotron Source

AbstractProperties of the microwave emission from HR1099 are examined in an attempt to determine whether the emission arises as gyro-synchrotron radiation from mildly relativistic electrons trapped in magnetic fields above starspots on the active K subgiant component. It is shown that radio curves do not exhibit a systematic variation in phase with the rotation rate, as one might expect for emission from a source situated above a long-lived starspot. However, there is some evidence that the radio flaring occurs at two preferred longitude zones. Whether these zones agree with starspot locations remains to be determined by light curve modelling. What we can say with confidence is that the measured spectral index of the microwave emission does not fit a simple gyro-synchrotron source model, such as that proposed to explain the observed reversal with frequency of the sense of circular polarization.

scholarly journals 80 MHz Radioheliograph Evidence on Moving Type IV Bursts and Coronal Magnetic Fields

1971 ◽  
Vol 43 ◽  
pp. 616-641 ◽  
Author(s):  
S. F. Smerd ◽  
G. A. Dulk
Keyword(s):  
Magnetic Field ◽  
Synchrotron Radiation ◽  
Magnetic Fields ◽  
Magnetized Plasma ◽  
Relativistic Electrons ◽  
Radiation Mechanism ◽  
Type Iv ◽  
Coronal Magnetic Fields ◽  
Field Lines ◽  
Magnetic Arch

The characteristics of 12 moving type IV bursts observed with the 80 MHz radioheliograph at the Culgoora Observatory between February 1968 and April 1970 are summarized.Three classes of moving sources can be recognized; they are described as: (1) Expanding arch; (2) Advancing front; (3) Isolated source.The first class has been identified (Wild, 1969) with the expansion of a magnetic arch or loop; the second class is here identified with an advancing MHD disturbance which may accelerate the radiating electrons in situ when moving at greater than Alfvén speed; the third with solar ejecta in the form of magnetized plasma clouds, or plasmoids. In all cases the radiation mechanism is probably synchrotron radiation from mildly relativistic electrons; energies in the range ∼0.1 to ∼1 MeV could account for the observed strong circular polarizations.With an expanding magnetic arch, source and magnetic-field movement are inseparable; the field remains a closed loop throughout the event. The MHD front probably moves largely along and the plasmoids between the open magnetic-field lines of unipolar regions or helmet structures. In the latter case it is the internal magnetic field – possibly toroidal – of the moving plasmoid that determines the polarization of the synchrotron radiation. A preliminary comparison of moving type IV sources with Newkirk-Altschuler maps of coronal magnetic fields shows suitably located closed loops for 2 events identified as expanding magnetic arches and unipolar open field lines along the path of a moving source identified as a plasmoid.

Synchrotron radiation from single electrons gyrating in a magnetoactive plasma

1969 ◽  
Vol 47 (7) ◽  
pp. 757-768 ◽  
Author(s):  
P. C. W. Fung
Keyword(s):  
Synchrotron Radiation ◽  
Plasma Frequency ◽  
Radiation Power ◽  
Magnetoactive Plasma ◽  
Electron Plasma ◽  
Relativistic Electrons ◽  
Relative Importance ◽  
Numerical Examples ◽  
The Past ◽  
Single Electrons

In this paper, the incoherent synchrotron radiation power emitted by relativistic electrons gyrating in a cold magnetoactive plasma is rederived, correcting errors which have occurred in the past literature. One can specify the background plasma by the quantity A = ωp2/ωH2 (ωp is the angular electron plasma frequency and ωH is the angular electron gyro-frequency), i.e. the relative importance of the plasma frequency to the gyro-frequency. The general spectral features of synchrotron radiation from single electrons radiating in plasmas of large [Formula: see text] and small [Formula: see text] are discussed with the aid of a number of numerical examples.

Circularly Polarized Synchrotron Radiation in Dipolar Magnetic Fields with Application to the Planet Jupiter

1969 ◽  
Vol 1 (6) ◽  
pp. 274-276 ◽  
Author(s):  
L. J. Gleeson ◽  
M. P. C. Legg ◽  
K. C. Westfold
Keyword(s):  
Magnetic Field ◽  
Synchrotron Radiation ◽  
Magnetic Fields ◽  
Linear Polarization ◽  
Thin Shell ◽  
Total Radiation ◽  
Circularly Polarized ◽  
Preliminary Account ◽  
The Magnetic Field

This paper is a preliminary account of the calculation of the circularly polarized synchrotron radiation received from a distribution of electricallycharged particles confined to a thin shell in the magnetic field of a dipole. Calculations of the total radiation and the degree of linear polarization have previously been carried out, and these calculations are duplicated in part.

scholarly journals 8.4. Properties of synchrotron emission and magnetic fields in the central region of M31

1998 ◽  
Vol 184 ◽  
pp. 351-352 ◽  
Author(s):  
P. Hoernes ◽  
R. Beck ◽  
E.M. Berkhuijsen
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Spectral Index ◽  
Central Region ◽  
Relativistic Electrons ◽  
Synchrotron Emission ◽  
The Magnetic Field

At the centre of M31 the nonthermal spectral index between λ20 cm and λ6 cm is −0.2. It slowly decreases along the southern arm and the northern filaments visible in Hα, but perpendicular to these features it increases much faster. The magnetic field runs along the arm and the filaments. These phenomena suggest the existence of a mono-energetic source of relativistic electrons in the nucleus.

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