Table Of Content

CONTENTS Cover Geophysical Monograph Series Title page Copyright page Contributors Preface Section I: Introduction 1 Magnetotail: Unsolved Fundamental Problem of Magnetospheric Physics 1.1. Introduction 1.2. Essential Properties 1.3. Global Stress Balance Problem 1.4. What Maintains a Magnetotail? 1.5. Conclusion Appendix: Some Questions about Internal Pressure Acknowledgments References Section II: Tutorials 2 Mercury’s Magnetotail 2.1. Introduction 2.2. Planetary Magnetic Field 2.3. Magnetosphere 2.4. External Driving 2.5. Tail Dynamics 2.6. Summary References 3 Magnetotails of Mars and Venus 3.1. Introduction 3.2. General Features of Magnetotails on Mars and Venus 3.3. Ion Acceleration 3.4. Bursty Flows 3.5. Reconnection in Induced Tails 3.6. Pressure Balance and Asymmetry of Plasma Sheet 3.7. Ion Escape through Tails 3.8. Induced Magnetic Tails for Flow Aligned IMF 3.9. Effect of Crustal Fields on Near-Mars Tail 3.10. Conclusions Acknowledgments References 4 Earth’s Magnetotail 4.1. Introduction 4.2. Dynamic Magnetotail 4.3. Magnetospheric Substorm 4.4. Steady Magnetospheric Convection 4.5. Sawtooth Injection Events 4.6. Pseudo Breakups 4.7. Poleward Boundary Intensifications 4.8. Questions Related to Dynamics of Magnetotail Acknowledgments References 5 Jupiter’s Magnetotail 5.1. Introduction 5.2. Particle Parameters of Jupiter’s Magnetotail 5.3. Energetic Events and Magnetic Reconnection 5.4. Summary 5.5. Future Exploration Acknowledgments References 6 Saturn’s Magnetotail 6.1. Introduction 6.2. Large-Scale Tail Structure 6.3. Magnetospheric Dynamics 6.4. Remote Sensing of Tail Dynamics 6.5. Discussion Acknowledgments References 7 Magnetotails of Uranus and Neptune 7.1. Introduction 7.2. Magnetospheres of Uranus and Neptune 7.3. Magnetotail Configuration at Uranus and Neptune 7.4. Magnetotail Dynamics 7.5. Discussion Acknowledgments References 8 Satellite Magnetotails 8.1. Introduction 8.2. Inert Moons 8.3. Conducting/Mass-Loading Moons 8.4. A Strongly Magnetized Moon: Ganymede 8.5. Summary Acknowledgments References 9 Moon’s Plasma Wake 9.1. Introduction 9.2. Structure and Dynamics of Lunar Wake 9.3. Simulations of Lunar Wake 9.4. Frontiers in Study of Lunar Wake Acknowledgments References 10 Physics of Cometary Magnetospheres 10.1. Introduction 10.2. The Coma 10.3. Mass Loading 10.4. Mathematical Description 10.5. Bow Shock and Cometosheath 10.6. Cometary Magnetotails 10.7. Model-Data Comparison 10.8. Rosetta Acknowledgments References 11 Heliotail 11.1. Introduction 11.2. Observations of the Heliotail 11.3. Discussion Acknowledgments References Section III: Specialized Topics 12 Formation of Magnetotails: Fast and Slow Rotators Compared 12.1. Introduction 12.2. Terrestrial Tail Formation: Solar Wind Reconnection Dominant 12.3. Tail Formation and Structure in Fast Rotating Magnetosphere 12.4. Saturn’s Polar Cap and Solar Wind: Dungey Cycle 12.5. Cassini Magnetometer Observations at High Invariant Latitude 12.6. Modulation of Saturn Tail 12.7. Magnetic Field in Polar Cap 12.8. Theories for Modulation at Saturn 12.9. Differences Between Jupiter and Saturn 12.10. Concluding Remarks Acknowledgments References 13 Solar Wind Interaction with Giant Magnetospheres and Earth's Magnetosphere 13.1. Introduction 13.2. Momentum Transfer From Solar Wind 13.3. Magnetic Reconnection and Ionospheric Convection 13.4. Viscous Interaction 13.5. Internal Drivers and Plasma Transport 13.6. Auroral Signatures 13.7. Magnetospheric Scale 13.8. Solar Wind Interaction and Magnetotail Structure 13.9. Conclusions References 14 Solar Wind Entry Into and Transport Within Planetary Magnetotails 14.1. Introduction 14.2. Plasma Transport Across Magnetopause (Solar Wind Entry) 14.3. Plasma Transport Within Plasma Sheet 14.4. Summary and Conclusion Acknowledgments References 15 Magnetic Reconnection in Different Environments: Similarities and Differences 15.1. Introduction 15.2. Energy Transport 15.3. Time-Dependent Reconnection 15.4. Reconnection Line Orientation for Asymmetric Reconnection 15.5. Summary Acknowledgments References 16 Origin and Evolution of Plasmoids and Flux Ropes in the Magnetotails of Earth and Mars 16.1. Introduction 16.2. Observations at Earth 16.3. Observations at Mars 16.4. Conclusions Acknowledgments References 17 Current Sheets Formation in Planetary Magnetotail 17.1. Introduction 17.2. Current Sheet Thinning Physics 17.3. Midnight MFD and CS Thinning 17.4. Entropy Changes and CS Formation 17.5. Summary and Discussion Acknowledgments References 18 Substorms: Plasma and Magnetic Flux Transport from Magnetic Tail into Magnetosphere 18.1. Introduction 18.2. Thinning of Plasma Sheet and Recession of Outer Boundary of Dipolar Magnetosphere 18.3. Magnetic Flux and Plasma Transport Along Tail After Onset of Reconnection 18.4. Penetration of Plasma and Magnetic Flux into Dipolar Magnetosphere 18.5. Further Progression Into Dipolar Magnetosphere 18.6. Observations Related to Plasma Entry into Magnetosphere of Jupiter and Saturn References 19 Injection, Interchange, and Reconnection: Energetic Particle Observations in Saturn's Magnetosphere 19.1. Introduction 19.2. Observations 19.3. Current Sheet Events; Charged Particles 19.4. Interchange Injection Events: Charged Particles 19.5. Discussion 19.6. Energetic Neutral Atom Injections 19.7. Relationship With Saturn Kilometric Radiation 19.8. Summary and Conclusions Acknowledgments References 20 Radiation Belt Electron Acceleration and Role of Magnetotail 20.1. Introduction 20.2. Early Observations 20.3. Radiation Belt Revolution 20.4. Phase Space Density Gradients 20.5. Phase Space Density Observations 20.6. Van Allen Probes 20.7. Discussion Acknowledgments References 21 Substorm Current Wedge at Earth and Mercury 21.1. Introduction 21.2. Background 21.3. Discussion 21.4. Conclusions Acknowledgments References 22 Review of Global Simulation Studies of Effect of Ionospheric Outflow on Magnetosphere-Ionosphere System Dynamics 22.1. Introduction 22.2. Magnetospheric Methods 22.3. Outflow methods 22.4. Impacts 22.5. Summary and Future Directions Acknowledgments References Index End User License Agreement List of Tables Chapter 02 Table 2.1 Interplanetary conditions at Mercury orbit. Chapter 06 Table 6.1 List of key planetary and magnetospheric parameters for Saturn. Chapter 07 Table 7.1 Basic scales and parameters for the magnetospheres of Uranus and Neptune Table 7.2 Solar wind statistics near Uranus and Neptune based on Voyager 2 magnetic field and plasma data showing median and 10th and 90th percentile values (in parentheses) of various solar wind parameters Chapter 08 Table 8.1 General properties of the major satellites of Jupiter and Saturn. Chapter 13 Table 13.1 Characteristics of solar wind interaction with Earth, Jupiter, and Saturn Chapter 16 Table 16.1 Observations of plasmoids Chapter 21 Table 21.1 Comparisons of scale lengths and locations of magnetospheric boundaries and substorm phenomena at Mercury and Earth. Table 21.2 Reflection coefficients and the impact on an impinging Alfvén wave. List of Illustrations Chapter 01 Figure 1.1 Schematic view of a magnetosphere, cut in the noon-midnight meridian plane. Open arrows: solar wind bulk flow. Solid lines within magnetosphere: magnetic field lines. The figure continues to the right out to distances in general much larger than the width of the figure. (In all figures of this chapter: sunward direction to the left; unless otherwise stated, magnetic field line directions appropriate for Earth or Mercury, reversed for Jupiter or Saturn.) Figure 1.2 Same as Figure 1.1, with dotted lines added to show integration surfaces for discussion of stress balance. Figure 1.3 “Box model” representation of Figure 1.2 (see text for description). Figure 1.4 Schematic topological view of a magnetically open magnetosphere. (a) Noon-midnight meridian plane (solid lines: magnetic field lines, open arrows: plasma bulk flow directions). (b) Equatorial plane (lines: plasma flow streamlines, line of x’s: magnetic X line = closed/interplanetary field line boundary). (c) Projection on ionosphere (lines: plasma flow streamlines, line of x’s: open/closed field line boundary = projection of magnetic X line = polar cap boundary) Figure 1.5 Sketch of the open magnetosphere and magnetotail in the noon-midnight meridian, showing magnetic field lines (solid lines), magnetopause (dashed line), and plasma sheet (dashed area) Figure 1.6 Possible flow patterns that provide stress to maintain magnetotail, described in text. Figure 1.7 Possible changes of the magnetic field topology in the magnetotail of an open magnetosphere [Vasyliūnas, 1976]. Each panel has the format of Figure 1.4. Figure 1.8 Qualitative sketch of planetary wind flow and magnetic topology [Vasyliūnas, 1983]. Magnetic field directions are appropriate for Jupiter. Chapter 02 Figure 2.1 Overview of MESSENGER’s orbit during the primary mission: (a) short tail orbit, (b) dusk side orbit, (c) long tail orbit, and (d) dawn side orbit. Lines mark the approximate location of the magnetopause and the bow shock for each viewing geometry. Figure 2.2 Mercury’s offset dipole. The schematic shows how the zero-inclination offset can be used to determine the dipole position, given that the magnetic field and rotational axes are aligned. Figure 2.3 Trace of the dipole offset vs local time and planetary longitude. Figure 2.4 Schematic overview of Mercury’s magnetosphere, including features observed during the M1 and M2 flybys. Figure 2.5 Ion gyro-radii and gyro periods within Mercury’s magnetosphere. The black, red and blue lines mark the expected properties of H+, O+, and Na+, respectively, with the solid lines representing 1 keV ions and the dashed lines 5 keV. Approximate magnetic fields in different significant areas of the magnetosphere are indicated at the top. Figure 2.6 MESSENGER observations from the dayside low-latitude boundary layer observed during the M1 flyby. The two dashed lines mark the inner current sheet (CS) and the magnetopause proper (MP). Figure 2.7 Equatorial plasma sheet pressures inferred from the magnetic pressure deficit: (a) distribution normalized to a heliocentric distance of 0.39 AU: (b) each bin has also been normalized by the ratio of contributing orbits, in order to reduce the influence of outliers in the data. Figure 2.8 MESSENGER observation of an FTE shower. During a period of ~25 min, MESSENGER observed 163 FTEs and TCRs in the southern magnetotail and magnetosheath, each marked by an arrow in the bottom panel. Figure 2.9 MESSENGER observations of a KH wave train. The top two panels show the FIPS energy over charge spectrogram and Na+ count rate, and the bottom four panels show the X, Y, Z, and absolute components of the magnetic field. Figure 2.10 Magnetotail magnetic field measurements for the first Mariner 10 and the three MESSENGER flybys. The top and bottom panels show events with northward and southward IMF, respectively. For each measurement set, the fit to equation (2.3) is overlain on the data. Figure 2.11 Series of dipolarization events observed inside the plasma sheet. Each dipolarization front is marked by a rapid increase in the Z component of the magnetic field. Figure 2.12 Distribution of energetic electron events in Mercury’s magnetosphere: (a) location of the most intense bursts of electrons; (b) both moderate- and high-intensity events. Chapter 03 Figure 3.1 (a) Magnetic field polarity (the B component) of the Venus tail in the Y*Z* x plane (magnetic coordinates) based on analysis of 160 VEX orbits crossing the tail current sheet from August 2006 to January 2011. (b) Magnetic field vectors in the X*Y* plane. Figure 3.2 Energy-time spectrograms of electron and ion (O+) fluxes measured by ASPERA-3 on MEX crossing the tail. The main plasma domains, plasma sheet (PS), polar wind, boundary layer, and the characteristic boundaries bow shock (PS), magnetospheric boundary (MB) are marked. Left panel shows a sketch of the Martian magnetotail with the main plasma domains. Figure 3.3 Suprathermal solar electrons can be used to monitor the position of the