1 / 30

Reporter Review: Auroral Phenomena

Reporter Review: Auroral Phenomena. Clare E. J. Watt University of Alberta. Auroral Processes in the Magnetosphere. Aurora are caused when particles impact the upper atmosphere with sufficient energy to excite neutral atoms

giuseppe
Download Presentation

Reporter Review: Auroral Phenomena

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Reporter Review: Auroral Phenomena Clare E. J. Watt University of Alberta Reporter Review: Div III Auroral Processes C. E. J. Watt

  2. Auroral Processes in the Magnetosphere • Aurora are caused when particles impact the upper atmosphere with sufficient energy to excite neutral atoms • In order to precipitate, particles (electrons or protons) must have small enough pitch-angles to prevent trapping in the magnetic bottle created by the Earth’s magnetosphere. • This review will focus on recent advances in the study of magnetospheric processes which cause auroral particle precipitation. After Figure 3.1, Baumjohann and Treumann, [1997] Reporter Review: Div III Auroral Processes C. E. J. Watt

  3. www.phys.ualberta.ca/~cwatt/reporter_review • Papers selected were published between July 2007 and June 2009. • 214 articles from peer-reviewed sources: Reporter Review: Div III Auroral Processes C. E. J. Watt

  4. Structure of Review • Magnetospheric physics of auroral precipitation: • Quasi-static acceleration processes (upward & downward current) • Dynamic acceleration processes (e.g. Alfvén waves) • Consequences of auroral precipitation • Auroral Kilometric Radiation • Ion outflow from the ionosphere • Auroral phenomenology • Substorms • Solar-wind driven aurora • Aurora equatorward of auroral oval Figure 4.1 Paschmann et al., [SSR 2002] Reporter Review: Div III Auroral Processes C. E. J. Watt

  5. Quasi-static acceleration processes • Field-aligned acceleration • Field-aligned parallel electric field • Concentrated parallel electric fields; Transition layers; Double layers • Inverted-V electrons in situ Figure 1 [Partamies et al., AG, 2008] Shows typical inverted-V signature from in-situ FAST data Figure 2(b) [Ergun et al., GRL 2000] Concentrated potential drops/E|| Reporter Review: Div III Auroral Processes C. E. J. Watt

  6. Parallel electric fields: Double layers Earthward energy flux Anti-earthward flux electric potential Integrated study of Double Layers in downward current region: • FAST observations [Andersson et al., PoP 2008] • Vlasov simulations Newman et al., PoP, 2008a, 2008b] Figure 2, Andersson et al., PoP, 2008 0.26 s Reporter Review: Div III Auroral Processes C. E. J. Watt

  7. Control of Double Layers • Singh et al., [JGR 2009] show through self-consistent 2D PIC simulations how a potential drop manifests as a series of moving DLs and density cavities • Hwang et al., [JGR 2009a, 2009b] use FAST electron observations to deduce how the potential drop varies with magnetospheric and ionospheric parameters (tests previous analytical results: Cran-McGreehin and Wright, JGR 2005) Figure 2(b) [Ergun et al., GRL 2000] Concentrated potential drops/E|| Figure 8, Hwang et al., JGR 2009a Reporter Review: Div III Auroral Processes C. E. J. Watt

  8. Source & Structure of Upward Current • Haerendel, [JGR 2007, 2008, 2009] shows that in a static model, upward j|| can be driven by magnetic stress release in the near-Earth plasma sheet due to radial pressure gradients • Makes predictions which could be tested with sounding rockets or low-altitude spacecraft. Figure 3, Haerendel, JGR 2007 • Theory of stationary inertial Alfvén waves [orig. Knudsen JGR 1996; expanded by Finnegan et al., NPG 2008; PoP 2008; PPCF 2008] tested in the laboratory [Koepke et al., PPCF 2008] • can structure a large-scale current sheet into smaller perpendicular structures, without requiring a structured source Reporter Review: Div III Auroral Processes C. E. J. Watt

  9. Inverted-V electrons Occurrence vs MLT • Partamies et al., [AG 2008] show occurrence and characteristics of inverted-V electron signatures using 5 years of quicklook FAST data Scale size PC potential vs energy Figure 6 Figure 9 Figure 8 Red curve = occurrence of auroral arcs in MLT [Syrjäsuo and Donovan, AG 2004]. Black line = 3 x Energy Peak at 20-40km Reporter Review: Div III Auroral Processes C. E. J. Watt

  10. Dynamic acceleration processes • Shear Alfvén waves with small perpendicular extent can support time-varying and propagating E|| • Dynamic auroral displays • Generation of waves in magnetosphere • Cause of short perpendicular scales • Wave-particle interactions Reporter Review: Div III Auroral Processes C. E. J. Watt

  11. Generation of shear Alfvén waves which drive aurora Magnetotail driving • A mechanism for wave conversion from magnetosonic to shear Alfvén waves on very stretched or open field lines [Pilipenko et al., JGR 2008] • Wright and Allan [JGR 2008] use a simplified fluid model of the magnetotail to show how a plasmoid can drive Alfvénic disturbances with observed characteristics in both lobe and plasma sheet “Local” driving • Observational evidence for shear Alfvén waves driven by the shear flow in an inverted-V structure in Reimei data [Asamura et al., GRL 2009] Reporter Review: Div III Auroral Processes C. E. J. Watt

  12. Short perpendicular scales • Whatcausesshortperpendicularscales in shear Alfvén waves? • Chaston et al., [PRL 2008] show using FAST observations that Alfvénic aurora may be powered by a turbulent cascade • Conversion of large-scale shear Alfvén waves to small scale inertial Alfvén waves seen in 2.5D PIC simulation [Khazanov and Singh, PPCF 2008] requires small-scale density cavities • Ionospheric control of perpendicular scales [Streltsov, JGR 2007; Lysak and Song, GRL 2008; Sydorenko et al., JGR 2008] Figure 2, Chaston et al., PRL 2008 Reporter Review: Div III Auroral Processes C. E. J. Watt

  13. Characteristics of auroral SAW - modelling Inhomogeneous plasma • A dispersion relation for kinetic Alfvén waves in plasma with perpendicular plasma gradients [Lysak, PoP 2008] • cavities, boundaries between lobe/plasma sheet • Alfvénic solitons in inhomogeneous plasma supporting E||[Stasiewicz,PPCF 2007; Stasiewicz & Ekeburg, NPG 2008] Ionospheric feedback • Inclusion of ionospheric feedback important for SAW evolution • Conductivity evolution [Lu et al., JGR 2007, 2008] • Ionospheric heating [Streltsov., JGR 2008] • Ionospheric feedback instability characteristics different from FLR [Lu et al., JGR 2008] • Ionospheric feedback instability model provides new interpretation for localized e-m waves observed by Cluster at ~5RE in the PSBL [Streltsov & Karlsson, GRL 2008] Reporter Review: Div III Auroral Processes C. E. J. Watt

  14. Electron acceleration by shear Alfvén waves • Self-consistent model of electron acceleration by SAW in warm plasma: • Propagating SAW - Watt et al., PRL 2009 • Standing SAW - Rankin et al., GRL 2007 • c.f. Polar observations of SAW and electron acceleration at ~5RE in the PSBL [Wygant et al., JGR 2002] • Self-consistent simulations also show that acceleration by SAW can cause trapped magnetospheric populations and precipitation in the opposite ionosphere [Swift, JGR 2007] (top) Figure 2, Watt et al., PRL 2009 (bottom left) Figure 6(a) Wygant et al., JGR 2002 (bottom right) Figure 3(b) Watt et al., PRL 2009 Reporter Review: Div III Auroral Processes C. E. J. Watt

  15. Flickering/Pulsating Aurora • New instrumentation ideal for studying auroral processes with short temporal scales: • e.g. Reimei satellite, ASK, all-sky TV cameras, EMCCD detector • Stability and coherence of electron precipitation over different time scales using DMSP data [Boudouridis and Spence, JGR 2007] • Flickering aurora –spatial scales 50m-1km and frequencies 1-20Hz • Observations consistent with model of interfering electromagnetic waves [Whiter et al., GRL 2008; Gustavsson et al., JGR 2008] • Observations consistent with dispersive characteristics of Alfvén waves at ~6Hz [Semeter et al., JGR 2008] Figure 9, Semeter et al., JGR 2008 Reporter Review: Div III Auroral Processes C. E. J. Watt

  16. Reimei satellite (ISAS) Name REIMEI Objectives Demonstration of next-generation advanced satellite technologies in orbit Realization of small-scale, frequent scientific observation missions Launch Date 06:10, August 24, 2005 (JST) Location Republic of Kazakhstan Launch Vehicle Dnepr (launched together with OICETS satellite) Configuration Weight Approx. 60 kg Dimensions 60 × 60 × 70 cmOrbit Altitude: Perigee 610 km, Apogee 654 km Inclination 97.8° Type of Orbit Near-circular orbit Period 97 min Scientific Instruments Star tracker Spin/non-spin type solar sensors (SSAS/NSAS) Geomagnetic Aspect sensor (GAS) Three-axis optical fiber gyro (FOG) Reaction wheel (RW) and magnetic torquer (MTQ) as actuators Multi-spectral Auroral Camera (MAC) Aurora particle observation instrument (Electron/Ion Spectrum Analyzer: ESA/ISA) Still operational on May 23rd 2008 Reporter Review: Div III Auroral Processes C. E. J. Watt

  17. Consequences of Auroral Acceleration • Auroral Kilometric Radiation • Earth’s natural radio wave source • Frequency ~ electron cyclotron frequency • Current model: field-aligned beams of electrons form unstable distribution functions due to magnetic field convergence and mirror force Reporter Review: Div III Auroral Processes C. E. J. Watt

  18. AKR and radio emissions • Laboratory experiments have confirmed that electrons travelling into a converging magnetic field form a horseshoe distribution function which is unstable to radio emissions near the electron cyclotron frequency [McConville et al., PPCF 2008; Ronald et al., PoP 2008] • Results consistent with 3D PIC simulations [Gillespie et al., PPCF 2008] • NB: no background plasma in lab • Active experiments have artificially triggered AKR and observed significant density depletions [Wong et al., PRL 2009] Figure 1, McConville et al., PPCF 2008 fce = 4.42GHz Figure 8(b), McConville et al., PPCF 2008 Reporter Review: Div III Auroral Processes C. E. J. Watt

  19. AKR fine structure FAST data: Figure 1e, Su et al., [JGR 2008]: Alfvén waves Cluster data: Figure 1, Hanasz et al., GRL 2008]: Alfvén waves FAST & Cluster data: Figures 2&5, Pottelette & Pickett, [NPG 2007]: Phase space holes Reporter Review: Div III Auroral Processes C. E. J. Watt

  20. Location of AKR • Morioka et al., [JGR 2008; AG 2009] use frequency of AKR to infer source altitude • Modelling [Savilov et al., PoP 2007] suggests that AKR could present with multiple frequencies • not just Ωce • J||↑, frequencies change • Better to use multiple spacecraft and ray-tracing to deduce the source location of AKR [Mogilevsky et al., JETP 2007; Mutel et al., GRL 2008] • Lab experiments also available • Can frequency alone determine source altitude? Figure 1, Morioka et al., [AG 2009] Reporter Review: Div III Auroral Processes C. E. J. Watt

  21. Consequences of Auroral Acceleration • Ion Outflow and Upflow • Wave-driven (shear Alfvén waves) • Electron precipitation and electromagnetic Poynting flux • Ion heating (“pressure-cooker” effect) Reporter Review: Div III Auroral Processes C. E. J. Watt

  22. Ion outflow and shear Alfvén waves • Models of interaction between Alfvén waves and plasma which result in density cavities and upflowing ions: • Steepening nonlinear inertial Alfvén waves → ion cyclotron and ion acoustic waves → ion heating → upflow [Seyler & Liu, JGR 2007] • Ponderomotive force in the Ionospheric Alfvén Resonator [Sydorenko et al., JGR 2008] • Active ionospheric feedback and ponderomotive force [Streltsov & Lotko, JGR 2008] t=0 t=40s t=0 t=3min Figure 5, Streltsov & Lotko, [JGR 2008] Figure 7(e), Sydorenko et al., [JGR 2008] Reporter Review: Div III Auroral Processes C. E. J. Watt

  23. Ion upflow and outflow Ionospheric plasma parameters and model: Figure 10, Zettergren et al., JGR 2008 • Modelling of ion upflow/outflow, including electron precipitation, wave-particle interactions, heating, etc: • fluid kinetic model [Zettergren et al., JGR 2007] • dynamic fluid kinetic [Horwitz and Zeng, JGR 2009] • wave-particle interactions [Barghouthi et al., JASTP 2008; Barghouthi, JGR 2008] • Detailed observations: • SIERRA rocket [Lynch et al., AG 2007] • Incoherent scatter radar [Zettergren et al., JGR 2008] pitch angle time (s) Figure 6, Lynch et al., AG 2007 Reporter Review: Div III Auroral Processes C. E. J. Watt

  24. Substorm aurora: Large scale/low frequency undulations • All the physical processes discussed previously apply to substorm aurora • Many repeatable features of substorm aurora that deserve particular study. Figure 3, Keiling et al., [GRL 2008]. Variations in large-scale brightening (21-24MLT) with same period as ion injection, ground Pi2 [Keiling et al., GRL 2008] and boundary oscillation in space [Keiling et al., JGR 2008] in-situ energetic ions auroral photon flux Periodic bright spots related to an instability? Figure 2, Henderson [AG 2009] Reporter Review: Div III Auroral Processes C. E. J. Watt

  25. raw difference Substorm aurora: Expansion phase onset Figure 2, Sakaguchi et al., AG 2009 All-sky TV camera (30Hz); 1s images Figure 1, Liang et al., GRL 2008 THEMIS ASI: 3s images Reporter Review: Div III Auroral Processes C. E. J. Watt

  26. Substorm aurora: Pi1/Pi2 waves and auroral onset Figure 6, Rae et al., JGR 2009 • Substorm onset can manifest as undulations in aurora (λ~10s of km) • Both undulations and large-scale auroral onset location are linked to magnetic perturbations in the Pi1/Pi2 wave bands raw difference Figure 6, Murphy et al., JGR 2009 Reporter Review: Div III Auroral Processes C. E. J. Watt

  27. electron aurora Solar-wind driven aurora dawn proton aurora dusk • Proton and electron aurora show prompt and persistent response to high SW dynamic pressure [Liou et al., JGR 2007; Laundal & Østgaard, JGR 2008]. • Compression of magnetosphere → changing mirror ratio → precipitaton • Dawn-dusk asymmetry suggests that gradient & curvature drift play a role Figure 2, Liou et al., JGR 2007 Figure 1 (a), Laundal & Østgaard, JGR 2007 Reporter Review: Div III Auroral Processes C. E. J. Watt

  28. Aurora equatorward of traditional oval • Isolated arcs equatorward of main auroral oval due to particle scattering by EMIC waves: • Protons: tens of keV[Yahnin et al., JGR 2007; Yahnina et al., JGR 2008; Sakaguchi et al., JGR 2008] • Electrons: MeV[Miyoshi et al., GRL 2008] • All associated with ground-based wave observations in Pc1 band • Sandanger et al., [JGR 2007] show that structure in the relativistic electron precipitation match structures in the anisotropic proton flux → EMIC wave precipitation • Jordanova et al., [JGR 2007] present simulations of sub-auroral arcs due to EMIC waves which compare favourably with observations. Reporter Review: Div III Auroral Processes C. E. J. Watt

  29. Advances in Auroral Science methods • Observations: • High temporal resolution ground-based imagers • Coverage over northern latitudes and many hours of MLT • High temporal resolution imagers with spectral resolution • Low-altitude spacecraft with imager & particle detection • Multi-spacecraft missions • Theory/simulation: • Generation and evolution of parallel electric fields • Non-uniform, non-periodic models • Active magnetosphere-ionosphere coupling • Active experiments: • Laboratory • Ionosphere/Magnetosphere Reporter Review: Div III Auroral Processes C. E. J. Watt

  30. Further information • Reviews published 2007-2009 • Shear Alfvén waves in the magnetosphere [Keiling, SSR 2009] • Downward current region physics [Marklund, SSR 2009] • Laboratory experiments and space physics [Koepke, RG 2008] • Current-voltage relationship [Pierrard et al., JASTP 2007] • Fine structure of aurora [Sandahl et al., JASTP 2008] • Polar cap aurora [Newell et al., JASTP 2009] • EMIC waves and proton precipitation [Yahnin & Yahnina, JASTP 2007] • Artificial stimulation of IAR [Yeoman et al., ASR 2008] • Importance of auroral physics in the Universe [Hultqvist, JASTP 2008] • This review, and the bibliography, is available at: http://www.phys.ualberta.ca/~cwatt/reporter_review Reporter Review: Div III Auroral Processes C. E. J. Watt

More Related