First Solar Results with the FASR Subsystem Testbed

Details First Solar Results with the FASR Subsystem Testbed First Solar Results with the FASR Subsystem Testbed

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2502g&link_type=abstract

American Astronomical Society, SPD meeting #37, #25.02; Bulletin of the American Astronomical Society, Vol. 38, p.252

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The Frequency Agile Solar Radiotelescope (FASR) Subsystem Testbed (FST) is a new, three-element interferometer, utilizing three antennas of the Owens Valley Solar Array. FST is the first radio instrument capable of measuring solar burst locations with spectrograph-like time and frequency resolution. Operating with 500 MHz instantaneous bandwidth, tunable anywhere in the 1-9 GHz range, FST can measure centroid locations of typical bursts on millisecond timescales and MHz frequency resolution. The system is designed as a prototype for FASR, for several purposes including the study of radio frequency interference (RFI) mitigation techniques, a testbed for the design of FASR's digitial signal processing, and investigating use of satellite signals for calibration. In addition, however, FST is unique in its ability to locate solar bursts on the extremely fine frequency and time scales on which their emission varies.A technical description of the instrument can be found in an accompanying poster (Liu et al.), along with first results on the several topics mentioned above. In this talk we focus on the solar applications of FST. We describe the operation of the system for solar observations, the science goals of the instrument, and some first results of observations of solar bursts. The first recorded burst, obtained on the first day of solar observations, was a group of type III bursts associated with a B5.1 X-ray burst, also observed with RHESSI. Individual type IIIs show downward propagation (reverse-frequency slope), with significant positional differences from one type III to another, while within a type III are seen smaller positional changes as a function of frequency. This suggests smooth trajectories for individual bursts, but widely diverging locations for separate bursts. We describe joint RHESSI/FST observations and findings for those bursts observed so far. This work is supported by NSF grant AST-0352915 to NJIT.

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