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Low-Frequency Turbulence in the Anisotropic Plasma Namig Dzhalilov

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Low-Frequency Turbulence in the Anisotropic Plasma Namig Dzhalilov Solar Wind: Low-frequency Turbulence in the Anisotropic Plasma Namig Dzhalilov Shamakhy Astrophysical Observatory, Azerbaijan 1 A g e n d a • Global structure of the heliosphere - general views • Solar wind measurements • The solar wind as a turbulence laboratory • MHD - Wave instability theory • Conclusions 2 3 The solar corona • Hot rarefied atmosphere above visible surface • Plasma beta <<1 in corona • magnetic field dominates • Closed magnetic field: plasma trapped • Open magnetic field: plasma can expand into interplanetary space 4 Eclipse: RED 1.1 106 K Iron X‐XI (RED) GREEN 2 106 K Iron XIII‐XIV (GREEN) This eclipse image shows the magnetic topology of the corona. 5 There is a clear separation of the high and low latitude solar wind. 6 This SOHO extreme ultraviolet (EIT) and scattered visible light (LASCO) composite image shows the outward streaming solar corona forming the supersonic solar wind 7 Expansion of the upper corona • Corona is very hot • Pressure is higher than ambient interstellar medium • Expands into interplanetary space (Parker, 1958): solar wind • Carves a cavity in interstellar medium: heliosphere • Nearly radial flow • Accelerates to full speed by ~20 solar radii SoHO coronagraph (LASCO) Artificial eclipse 8 9 What is the solar wind? • Collisionless, magnetised plasma • Continual, but variable, outflow from Sun’s corona • Blows a cavity in interstellar medium: heliosphere • Carries magnetic field, waves and turbulence from Sun’s corona • At edge of heliosphere, merges with interstellar medium • Interacts with planets and other bodies • Supersonic (super‐Alfvénic, …) • Hot: >105 K • Rarefied: few per cm3 at Earth • Complex due to solar variability, solar rotation, and in situ processes • Variable on all measured scales, from sub‐second centuries 10 What does the solar wind look like? • Very rarefied • Can’t usually see it • Near‐Sun solar wind is visible during eclipses 11 12 Aurora 13 Magnetic Storms, 10‐11 Sept 2018 14 Cosmic Missions 1959 Luna‐1 ‐ ilk dəfə bu Sover süni peykində G küləyinin sürəti ölçüldü 1961 Venera 1 1962 Mariner 2 – Veneraya uçuş 1965 Venera 2 1972 Pioner 10 1973 Pioner 11 1973 Mariner 10 – Merkuri səfəri => 85 R 1976 HELİOS => 0.29 a.e. = 64 R 1977 Voyager 1, Voyager 2 1990 SOHO (Solar and Heliospheric Observatory) 1990 Ulysses GK yüksək en dairələrindən asılılığını tədqiq etdi. 1997 ACE (Advanced Composition Explorer) 2008 STEREO 2012 Messenger 2015 Bepi‐Columbo 2018 SPP (Solar Probe Plus) => 8.5 R 15 16 Significant spacecrafts Wind, ACE (present) • Near‐Earth (L1). Good, modern instrumentation Helios (1975‐1984?) • Closest approach to the Sun (0.29 AU, 63 solar radii) Ulysses (1990‐2006) • Only measurements at high latitudes Voyager 1 &2 , Pioneer 10 & 11 (mid‐1970’s, some still operating) • Only outer heliosphere measurements (80+AU) we are here 17 18 19 Spacecraft particle measurements Measure: • Bulk distribution function, for ions and electrons Calculate: Moments of distribution function: velocity, temperature, density, etc. • Particle composition (protons, helium, oxygen, etc.) • Ion charge states • Time variations at sub- gyroperiod scales 20 Spacecraft magnetic and electric field measurements • Measure magnetic and electric field from DC up to ~Hz, as time series • Measure higher frequencies (can be up to MHz) using spectra Spacecraft measurements are difficult: • Very low fluxes and fields • Spacecraft contamination • Instrument effects • Low power and mass • Telemetry constraints 21 22 23 24 Histogram showing hourly average solar wind speeds measured by the spacecraft ACE (green) and Ulysses (blue). The vertical dashed black and red lines show typical slow and fast wind velocities respectively. We have only considered Ulysses measurements from when te spacecraft was less than 2.5 AU from the Sun. The distributions from the two spacecraft are different because they probed the solar wind at different latitudes. The orbit of ACE is in the equatorial plane, and therefore ACE measured mostly the slow component of the solar wind. The orbit of Ulysses is almost perpendicular to the equatorial plane, and therefore Ulysses measured both the slow and fast components of the solar wind. 25 26 Composition of the solar wind H He 27 28 Global structure of the solar wind • Source in the corona • Relation to coronal structure • Effect of solar rotation • Solar cycle dependence • Transient events • Interaction with the interstellar medium 29 Magnetic field: the Parker spiral • Solar rotation drags out solar wind magnetic field into Archimedian spiral • Predicted by Gene Parker • Parker spiral • Winding angle depends on wind speed, but: • ~45º at Earth • ~90º by 10 AU Magnetic field is frozen in plasma! 30 IMF Sector Structure The heliospheric current sheet is the surface where the polarity of the Sun’s magnetic field changes sign. This field extends throu‐ ghout the Sun's equatorial plane in the heliosphere. A small electrical current flows within the sheet, about 10−10 A/m². The thickness of the current sheet is about 10,000 km near the orbit of the Earth. In Out 31 The heliospheric current sheet, the largest coherent structure in the solar system, is a wavy sheet, resembling a ballerina skirt, due to the fact that the Sun’s magnetic dipole is tilted by different amounts, depending on the phase of the solar cycle, from its rotation axis. 32 Corotating Interaction Regions 33 Corotating Interaction Regions 34 The heliosphere Cosmic rays Heliopause • Solar wind blows bubble in interstellar medium • Probably around 100 AU from Sun at Solar the nose wind Interstellar medium • Cosmic rays enter heliosphere: motion controlled by turbulent magnetic field Termination shock 35 The Heliosphere 36 Interstellar bowshocks • Shocks also form between stellar winds and interstellar medium • General shape is probably similar to the Sun’s bow shock NASA and The Hubble Heritage Team (STScI/AURA) 37 Pickup Ions can heat the Solar Wind? 38 The magnetosphere • Interaction of solar wind with Earth’s magnetic field • Bowshock: high Mach number shock • Magnetosheath: shocked solar wind plasma • Magnetosphere: very low beta plasma Good: Many spacecraft Bad: High data rate Very complicated 39 40 Solar Wind Flow Near Sun 41 Temperature Gradients R < 1 AU In the range 0.3 < R < 1.0 AU, Helios observations demonstrate the following: For V < 300 km/s, T ~ R ‐1.3 0.13 SW Adiabatic expansion ‐1.2 0.09 ‐4/3 300 < VSW < 400 km/s, T ~ R yields T ~ R . ‐1.0 0.10 400 < VSW < 500 km/s, T ~ R Low speed wind ‐0.8 0.10 500 < VSW < 600 km/s, T ~ R expands without in ‐0.8 0.09 situ heating!? 600 < VSW < 700 km/s, T ~ R ‐0.8 0.17 High speed wind is 700 < VSW < 800 km/s, T ~ R heated as it expands. Why is this? It seems distinct from the high‐latitude observations. We can look to explain this through theory and link it to observations of the dissipation range and inferred spectral cascade rates. 42 Turbulence 43 Importance of waves and turbulence Energetic particle transport • Controls cosmic rays throughout the solar system Effect on the Earth • Can trigger reconnection, substorms, aurorae, … Understanding solar processes • Signature of coronal heating, etc. Application to astrophysical plasmas • Turbulence is pervasive Turbulence as a universal phenomenon • Comparison with hydrodynamics 44 Solar wind as a turbulence laboratory • Characteristics – Collisionless plasma – Variety of parameters in different locations – Contains turbulence, waves, energetic particles • Measurements – In situ spacecraft data – Magnetic and electric fields – Bulk plasma: density, velocity, temperature, … – Full distribution functions – Energetic particles 45 Solar wind as a plasma experiment 46 47 48 Three months of solar wind data Ulysses: 4.5 AU • Field and particle measurements • MHD on these scales • Variable speed, density, magnetic field, … • Not random: presence of large scale structures • 30‐day repeats 49 Typical conditions at 0.3 AU • Closest measurements to date • Before stream‐stream interactions are important • Highest density in slow wind Density and temperature anticorrelated Magnetic field ~0º from radial 50 Typical conditions at 1.0 AU • Stream‐stream interactions more important • Shocks beginning to form Density and temperature correlated: compression at velocity increase Magnetic field ~45º from radial: Parker spiral 51 Stream dependence: cross helicity • Wavelets: measure time and frequency dependence of waves Fast wind Positive cross helicity: anti‐sunward Alfvén waves Sharp transition To mixed sense waves Slow wind Mixed sense, but very variable 52 53 54 55 56 57 Dominance of outward‐propagating waves Speed • Solar wind accelerates as it Solar wind speed leaves the corona • Alfvén speed decreases as field magnitude drops Critical point • Alfvén critical point: equal speed (~10‐20 solar radii) Alfvén speed • Above critical point, all waves carried outward Therefore, • Outward‐propagating low Distance from Sun frequency waves generated in corona! 58 59 60 61 Problem turbulence anisotropy 62 63 64 The turbulent solar wind f ‐1 turbulence waves f ‐5/3 Power spectrum • Broadband • Fluctuations on all • Low frequencies: f ‐1 measured scales • High frequencies: f ‐5/3 65 Large scale variations in power levels • Power in high speed wind, low and high latitudes • Ulysses agrees well with Helios • Data taken 25+ years apart • Increasing scatter in Helios reflects stream‐stream interactions 66 Results: Fundamental observations of waves and turbulence Alfvén waves • Waves of solar origin Active turbulent cascade • Not just remnant
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