Auroral Plasma Dynamics Revealed through Radio-Optical Sensor Fusion
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1 Auroral Plasma Dynamics Revealed through Radio-Optical Sensor Fusion Joshua Semeter Boston University Center for Space Physics Acknowledgements: Sebastijan Mrak, Brent Parham, Nithin Sivadas, John Swoboda, Michael Hirsch, Hassan Akbari, Chhavi Goenka, Matt Zettergren, Marcos Diaz
2 Solar wind - Magnetosphere Coupling: Energy Storage and Release B IMF! Magnetopause! Bow Shock! Solar Wind! Inductive energy is accumulated in the magnetotail via interaction with the solar wind. Stored energy is released impulsively into the atmosphere as heat, ionization, radiation, and bulk acceleration of gases.
3 Geospace multiscale mission 1 µa/m 2 Spherical harmonic expansion North
4 Incoherent Scatter Radar RISR EISCAT ESR PFISR Poker Flat Resolute Bay Sondrestrom ESR EISCAT Millstone Hill Jicamarca Arecibo Jicamarca Millstone Hill Arecibo Sondrestrom 4
5 Incoherent Scatter Radar Ion-acoustic s = C s k, si = 8 Langmuir C s = k B (T e +3T i )/m i 1 m e m i 2 + T e T i 3 2 exp T e 3 s 2T i 2 L = 2 pe +3k 2 v 2 the pe v the Dek 2, Li pe 3 1 exp 8 k 3 vthe 3 2 pe 2k 2 v 2 the 3 L 2 Te/Ti 700 area ~ Ne Altitude (km) 400 sti/mi Vi s Frequency (khz)! s! s! pe = s N e e 2 0 m e
6 Radar perspective All-sky 557.7nm, 100x real time S PFISR SNR (450MHz), 480us uncoded pulse satellite) o r) r) g) m).)) Coherent echoes from destabilized ion acoustic waves, 16-cm wavelength N 500 km E"region)impact)ioniza0on Akbari et al., 2013
7 Altitude (km) :05:26 Radar perspective PFISR SNR (450MHz), 480µs uncoded pulse satellite) Altitude (km) :05:32 r) r) g) m).)) Coherent echoes from destabilized ion acoustic waves, 16-cm wavelength :05:43 E"region)impact)ioniza0on Altitude (km) Frequency (khz) Candidate mechanisms: 1. Parametric decay of Langmuir turbulence (beam related) 2. ion-electron streaming instability (current related) Akbari et al., 2013
8 Optical manifestation of dispersive bursts 50 fps Radial keogram for event A A B Radial keogram for event B Altitude (km) Altitude (km) Seconds after 10:06:00 UT Emission profiles for event A 120 flaming vel: 80 km/s Seconds after 10:06:00 UT Altitude (km) 0.5 kev140 3 kev 150 X-32 DAHLGREN ET AL.: DISPERSIVE FIELD-ALIGNED AURORAL BU Altitude (km) x 104 Zenith brightness Seconds after 10:06:00 UT Emission profiles for event B Time after 10:06 UT (s) Seconds after 10:06:00 UT Average energy of primary electrons decreases Top panels: Radial keograms Figure for events 7. Top Field-aligned panel: A and Integrated bursts B. brightness are periodic The Dahlgren in radiala at et region ~2.4Hz al., JGRA of distan from 3keV to <500eV in 0.2-s. Brightness Power x 107 Power spectral density Frequency (Hz) 2.4 Hz Power spectral density
9 Time-energy dispersed electron... t... '... '7""'.'. i '. i... ;" > ";" "i' ' ' '-- : '" :' :'"" 40o!. [ i',,.'-'..-.':..'.: "...,:..--.':: : -" "- ""..,;.:! :. :; ; v.', : --:: e-", -:: ;:::' :.::il ',' I ' <',.,'; : :'.. :. ':::'-"' " "" ' ;:.4- ''" ""' '-- "½" ' "..'' '*' ' ' - kev "."-... ".....: ":.':'.. s : i "':.'- -' J... '!.::.,. '-. '. ;: :' ' ::.. -".-.- : '";'-.: ' :." -.'-};v'-. ":.,,-[? *-.:.': O.l... : 'ii!il Differential Number Flux Production Rate Flight Time (sec) Flight Time (see) Plasma Density a. b. c Arnoldy et al., 1999 J N ( cm 2 s 1 ev 1 ) ALTITUDE (km) s ENERGY (ev) ION PRODUCTION RATE ( m 3 s 1 ) ELECTRON DENSITY ( m 3 ) v Semeter et al., 2005
10 Mahali Experiment 67 Longitude Latitude Pankratius et al., IEEE Comm. Mag., 2016, Semeter et al., GRL 2017, Mrak et al JGRA 2017
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26 a) 06:18:24-35 b) 06:18:37-48 c) 06:18:49-00 d) 06:19: Geographic Latitude e) 06:19:14-25 f) 06:19:27-38 g) 06:19:39-50 h) 06:19:52-03 i) 06:20:04-15 j) 06:20:17-28 k) 06:20:29-40 l) 06:20: West Geographic Longitude Strong phase scintillation observed only along the trailing edge of the westward traveling surge Semeter et al., GRL 2017, Mrak et al JGRA 2017
27 Conclusion Dissipation of magnetospheric free energy occurs through a cascade of spatial scales, extending from ~100 km to ~10 cm. The role of small scale variability in modifying the energy dissipation process is poorly understood.
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