Solar Type III Radio Bursts: Directivity Characteristics

14th Annual International Astrophysics Conference: Linear and Nonlinear Particle Energization throughout the Heliosphere and Beyond

物理学;天文学

Thejappa, G.^1 ; MacDowall, R.J.^2

Department of Astronomy, University of Maryland, College Park

MD

20742, United States^1

NASA, Goddard Space Flight Center, Greenbelt

MD

20771, United States^2

关键词: Directivity factor;    Electron plasma frequency;    Harmonic emissions;    Magnetic field direction;    Magnetic field line;    Ray trajectories;    Second harmonics;    Simultaneous observation;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/642/1/012028/pdf
DOI  :  10.1088/1742-6596/642/1/012028

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

Type III radio bursts are a group of fast drifting radio emissions associated with solar flares. These radio emissions are believed to be excited at the fundamental and second harmonic of the electron plasma frequency, fpeby the electron beam excited Langmuir waves through a mechanism called the plasma mechanism. This mechanism attributes the dipole and quadrupole beam patterns for the fundamental and harmonic emissions. To verify these predictions, we analyze the simultaneous observations of type III radio bursts by the STEREO A, B and Wind spacecraft located at different vantage points in the ecliptic plane, and determine their normalized peak intensities (directivity factors) at each spacecraft using their time profiles. Assuming that the sources of these bursts are located on the Parker spiral magnetic field lines emerging from the associated active regions, we estimate the angles between the magnetic field directions and the lines connecting the sources to the spacecraft (viewing angles). Based on the plots of the directivity factors versus the viewing angles, one can divide these bursts into (1) intense bursts emitted into a narrow cone centered around the tangent to the magnetic field, and (2) relatively weaker bursts emitting into a wider cone centered around the tangent to the magnetic field. We compute the distributions of ray trajectories emitted by an isotropic point source and show that the refraction focuses the fundamental and harmonic emissions into narrow and wider cones, respectively. The comparison of these distributions with observations indicates that the intense bursts visible to a narrow range of angles around the tangent to the magnetic field probably correspond to the fundamental, and the relatively weaker bursts visible to a wide range of angles probably are the harmonic emissions.