HR: 0830h
AN: SP21B-06    [Abstracts]
TI: Imaging Type IIIdm Burst Trajectories
AU: * Liu, Z
EM: zl6@njit.edu
AF: The Center for Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Boulevard, 403 Tiernan Hall, Newark, NJ 07102 United States
AU: Gary, D E
EM: gary@adm.njit.edu
AF: The Center for Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Boulevard, 403 Tiernan Hall, Newark, NJ 07102 United States
AU: Nita, G M
EM: gnita@adm.njit.edu
AF: The Center for Solar-Terrestrial Research, New Jersey Institute of Technology, 323 Martin Luther King Boulevard, 403 Tiernan Hall, Newark, NJ 07102 United States
AU: White, S M
EM: white@astro.umd.edu
AF: Department of Astronomy, University of Maryland, Department of Astronomy, University of Maryland, College Park, MD 20742 United States
AU: Hurford, G J
EM: ghurford@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, Space Sciences Laboratory, University of California, Berkeley, CA 94720 United States
AB: Type IIIdm radio bursts are important diagnostics of the upward and downward directed beams of nonthermal electrons that originate in the energy release site. Because these bursts have a very high frequency drift rate ( |df/dt|=(0.09±0.03)× f^1.35±0.10, Melendez et al., 1999), high time and frequency resolution is a necessary for their observation. Since existing interferometers do not have this combination of spectral and time resolution in the decimetric range, we still do not have detailed information about the location and trajectory of Type IIIdm bursts. We are developing the new FASR Subsystem Testbed (FST) with three existing antennas of Owens Valley Solar Array (OVSA) that will permit imaging with high time and spectral resolution over the 1-9 GHz band. To accomplish this, the received signal is downconverted to 500 MHz bandwidth, then digitized with 1 GHz sampling rate, with digital correlation performed offline. With this three element interferometer, we have the ability to determine the centroid of simple source structures with very high time resolution (10 ms) and frequency resolution (<1 MHz). Such centroids as a function of frequency may outline the trajectories of nonthermal electron beams and so may show the magnetic topology at the energy release site. The FST is expected to be operational in early 2006. This poster presents the FST system configuration and the results of simulations of such trajectories, using a loop model with a simple magnetic geometry, density and temperature profiles given by hydrostatic equilibrium, for different loop heating functions (Aschwanden 2004, Physics of The Solar Corona, Chapter 3).
DE: 7500 SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly