Dr Jeff Tromp Air Vehicles Directorate AFRL/VA Air Force Research Laboratory
Stephen White Space Vehicles Directorate Air Force Research Laboratory
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Transcript of Stephen White Space Vehicles Directorate Air Force Research Laboratory
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Stephen White
Space Vehicles DirectorateAir Force Research Laboratory
Solar Radio Bursts with LWA-1:DRX Observations
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LW001: DRX data
X5 flare at 01 UT on 2012 March 7
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Post-flare loops: site of energy release(?)Locus of radio Type IV burst?
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Bright radio emission
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LW001
DRX setup:• Beam 1 on Sun: filter 5, 10-15 & 15-20 MHz• Beam 2 on Sun: filter 7, 15-34 & 34-52 MHz• Beam 3 off Sun: filter 7, 15-34 & 34-52 MHz• Beam 4 on Sun: filter 7, 52-70 & 70-88 MHz
3 2.2 TB + 0.4 TB (need 3 TB drives)Still learning …. but access time with LSL is fine
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245 MHz light curve into LWA morning
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Magnetic field distribution
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Summary plot: 10-15 MHz
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Summary plot: 15-20 MHz
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Summary plot: 15-34 MHz 45° above Sun
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Summary plot: 15-34 MHz on Sun
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Summary plot: 34-52 MHz off Sun
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Summary plot: 34-52 MHz on Sun
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Summary plot: 52-70 MHz
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Summary plot: 70-88 MHz
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RFI at 15 UT off Sun
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RFI at low elevation (solar beam)
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RFI at 20 UT off Sun
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RFI on Sun at local noon
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Typical noise storm feature: Type I bursts
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Low frequency emission: 34-52 MHz
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Unexpected fine structure above 60 MHz
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“Zebra” patterns more common in flares
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Issues at high frequencies: pointing?
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Wrigglers and zebra alternating
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“Wrigglers” at 10 millisecond resolution
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Wrigglers, Type I, broadband modulation
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Polarization properties: off Sun
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Polarization properties: on Sun
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Circular polarization spectrum
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Science with LWA-1 TBN data
• TBN data provide basically rapid sampling of the waveform at a fixed frequency
• Big push by the Sydney group (Cairns, Robinson, Li) to interpret low-frequency plasma emission with “stochastic growth theory” (SGT): electron beams are not uniformly saturated but are dominated by density fluctuations in the medium, results in marginally unstable beams with very bursty emission.
• SGT predicts a log-normal distribution of intensities when averaged, power-law at high time resolution
• Complicated for coronal work by large sources and multi-path propagation
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Science with LWA-1 TBW data
• TBW data provide snapshot spectra (60 msec) every minute: basically “luck” as to which portion of a burst you get
• What they do is confirm spectral structure that isn’t always “believable” in dynamic spectra
• Existing data already indicate interesting structure: need to interpret in terms of coronal inhomogeneity and electron beam properties.
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The