stephen white
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Gyroresonance emission in FORWARD & Developments in radio telescopes. Stephen White. Free-Free Opacity. Two different “modes,” or circular polarizations ( s =+1 o-mode, s = - 1 x-mode) - PowerPoint PPT PresentationTRANSCRIPT
Stephen White
Gyroresonance emission in FORWARD
&Developments in radio telescopes
Free-Free Opacity
• Two different “modes,” or circular polarizations (=+1 o-mode, =1 x-mode)
• X-mode has higher opacity, so becomes optically thick slightly higher in the chromosphere, while o-mode is optically thick slightly lower
• Polarization P = (TRTL)/(TR+TL) = 0 for isothermal atmosphere because temperature is same in both layers
• In “real” atmosphere get polarization due to temperature gradient
Gyroresonance emission
• Opacity results from electrons gyrating in coronal magnetic fields at fB = 2.8 106 B Hz: linear scaling of B with frequency.
• In the non-flare (non-relativistic) corona this produces narrow resonances, i.e. physically very thin layers (tens of km).
• Opacity n B/(B/l) (T/mc2 sin2)s-1 where s = 1, 2, 3, … is the harmonic
• Because T/mc2 is 1/3000, opacity drops by 3 orders of magnitude from one layer to the next
• Big difference in opacity of two polarizations of electromagnetic waves: extraordinary mode interacts more with electrons than ordinary mode
Gyroresonance opacity at low harmonics
Model sunspot gyroresonance layers
OVSA Expansion Project
Dale E. GaryProfessor, Physics, Center for Solar-Terrestrial Research
New Jersey Institute of Technology 7
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•09/24/2012•Prototype Review Meeting
•09/24/2012•Prototype Review Meeting
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LOFAR’s first solar image
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Murchison Widefield ArrayJoint US/Australian project located at the candidate SKA site in Western Australia (miles and miles from anywhere)US players are Haystack, Harvard/CfA, MITAustralian players are CSIRO/ATNF, Curtin University (WA) with a lot of support from Australian (federal) and West Australian (state) governmentsCovering the high-frequency end of the LOFAR range, same technique, same science goals.Using GPU units to do their data processing! 12
MWA station and 32T layout
Consortium with PAPER project in the future
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The Long Wavelength Array
US project involving Naval Research Laboratory, U. New Mexico, Los Alamos, Virginia Tech, U. Texas, NRAO, AFRL, …
“Zebra” patterns more common in flares
Unexpected fine structure above 60 MHz
“Wrigglers” at 10 millisecond resolution
“Type III” burst at RSTN (3 seconds, 0.15 MHz)
•At LWA1 resolution
Allen Telescope Array
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LOFAR’s first solar image
ATA solar image
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Siberian Solar Radio Telescope (SSRT)
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EVLA: better frequency, time coverage
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EVLA observation of the Sun at F10.7
ALMA
26
ALMA can observe the Sun! Will be wonderful for flares (but small FOV) and chromosphere studies IF we can get observing time … 27
Solar Submillimeter Telescope (Argentina/Brazil)
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The Sun
The Sun