Table Of ContentCONTENTS
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
