Space Physics and Aeronomy, Solar Physics and Solar Wind

1 Cover

2 Series Page

3 Title Page

4 Copyright Page

5 List of Contributors

6 Preface

7 1 The Solar Wind 1.1. INTRODUCTION 1.2. OBSERVATIONS OF THE NASCENT SOLAR WIND 1.3. MEASUREMENTS OF THE SOLAR WIND IN THE INNER HELIOSPHERE 1.4. WAVES AND TURBULENCE 1.5. KINETIC PROCESSES AND HEATING IN THE SOLAR WIND 1.6. THE EVOLUTION OF THE SOLAR WIND FROM THE INNER TO OUTER HELIOSPHERE 1.7. OUTSTANDING QUESTIONS AND FUTURE PROSPECTS ACKNOWLEDGMENTS REFERENCES

8 2 The Heating of the Solar Corona 2.1. HISTORICAL VIEWPOINT ON THE CORONAL HEATING PROBLEM 2.2. OBSERVATIONAL CONSTRAINTS ON CHROMOSPHERIC AND CORONAL HEATING 2.3. MODELING OF THE SOLAR ATMOSPHERE 2.4. FUTURE PROSPECTS FOR MODELING AND OBSERVATIONS ACKNOWLEDGMENTS REFERENCES

9 3 Solar Magnetism and Radiation 3.1. INTRODUCTION 3.2. THE SOLAR MAGNETIC FIELD 3.3. SOLAR MAGNETIC FEATURES WITH RADIATIVE SIGNATURES 3.4. THE SUN AS A STAR: SOLAR IRRADIANCE VARIABILITY 3.5. CALCIUM II K OBSERVATIONS ACKNOWLEDGMENTS REFERENCES

10 4 Solar Energetic Particles 4.1 INTRODUCTION 4.2 HISTORY 4.3 SOLAR ENERGETIC ION VARIABILITY IN SHOCK‐ACCELERATED SEP EVENTS 4.4 3HE‐RICH SEP EVENTS 4.5 SEP ELECTRONS 4.6 UNDERSTANDING SEPs VIA ENERGETIC NEUTRAL ATOMS (ENAs) 4.7. THEORY OF SEP ACCELERATION AND TRANSPORT 4.8. CONCLUDING REMARKSREFERENCES

11 Chapter 5: Solar Flares and Coronal Mass Ejections 5.1. INTRODUCTION 5.2. HISTORY 5.3. OBSERVATIONAL SIGNATURES AND DETECTION PROPERTIES 5.4. THEORETICAL INTERPRETATIONS AND KEY PROBLEMS 5.5. SPACE WEATHER AND BEYOND ACKNOWLEDGMENTS REFERENCES

12 6 Fine‐Scale Features of the Sun’s Atmosphere: Spicules and Jets 6.1. INTRODUCTION 6.2. SOLAR SPICULES 6.3. CORONAL JETS 6.4. JET‐LIKE PHENOMENA ON DIFFERING SIZE SCALES 6.5. CORONAL JETS AND OTHER PHENOMENA 6.6. THE FUTURE ACKNOWLEDGMENTS REFERENCES

13 Chapter 7: Solar Interior 7.1 SOLAR DYNAMO 7.2 HELIOSEISMOLOGY 7.3 FLUX EMERGENCE ACKNOWLEDGMENTS REFERENCES

14 Index

15 End User License Agreement

1 Chapter 2 Table 2.1 Coronal Temperature and Energy Requirements of the Solar Atmosphere

2 Chapter 3Table 3.1 Relevant Ca II K Digitized Image Archives. Shown are: name of the o...

3 Chapter 4Table 4.1 3He‐Rich SEP Event AbundancesTable 4.2 Association with Other Phenomena

4 Chapter 7Table 7.1 Hierarchy of Magnetic Field Structures and Evolutionary Patterns

1 Preface Figure I.1 Illustration of the complex solar environment and the recent obse...

2 Chapter 1 Figure 1.1 Radial evolution of solar wind temperatures from the corona to 1 ... Figure 1.2 Outflow velocity (km/s) of the solar wind for the considered four... Figure 1.3 2D map of radial outflow velocity in the plane of the sky derived... Figure 1.4 Propagating brightness fluctuations (green/black) derived from CO... Figure 1.5 (a–c) Polar plots of the solar wind speed, colored by IMF polarit... Figure 1.6 Configuration in the inner heliosphere of a “ballerina skirt” hel... Figure 1.7 Typical time profiles of solar wind parameters for a selected sol... Figure 1.8 Element abundances as a function of the first ionization potentia... Figure 1.9 Left: The abundance of helium (computed as 100 times the density ... Figure 1.10 Two schematics illustrating CIRs where the fast solar wind catch... Figure 1.11 Solar wind number density data for 15 January 1997. Bottom x ‐axi... Figure 1.12 Occurrence distribution of flux tube sizes mapped to the solar s... Figure 1.13 Highly idealized planar projection of a slightly asymmetric reco... Figure 1.14 Top: Typical spectrum of magnetic field fluctuations in the sola... Figure 1.15 Electron temperature anisotropy of the halo ( A h= T h⊥/ T h∥... Figure 1.16 Typical electron velocity distribution function (VDF) observed b... Figure 1.17 Kinetic shells formed in the electron VDF by resonant electron–w...

3 Chapter 2 Figure 2.1 A total solar eclipse viewed in white light from Earth. Figure 2.2 Plotted is a typical temperature as a function of height defining... Figure 2.3 Left shows an X‐ray image taken on 7 March 1970 from an Aerobee r... Figure 2.4 Shown is a composite image from the SDO. Three images of the Sun ... Figure 2.5 This cartoon shows the atmospheric layers of the Sun. Large‐scale... Figure 2.6 Similar to Figure 2.5, with additional complexity of the observat... Figure 2.7 Alfvén waves observed in the chromosphere. (A) Spicules in Hinode... Figure 2.8 A cartoon representation of a magnetic reconnection event generat... Figure 2.9 Active region (AR) differential emission measure curve. The emiss... Figure 2.10 Emission measure as a function of temperature for nanoflare trai... Figure 2.11 Magnetic reconnection observed after braiding in Hi‐C for a C1.7... Figure 2.12 Results from the DEM inversion for different areas (indicated by... Figure 2.13 Map of temperature in an active region (AR). The Green scale ref...Figure 2.14 High‐resolution radiative MHD simulation spanning the convection...Figure 2.15 Diagnostics from a thermodynamic MHD model of the global corona ...

4 Chapter 3Figure 3.1 Full‐disk image of the photospheric longitudinal (line‐of‐sight) ...Figure 3.2 Quiet Sun at the disk center as observed by the Hinode SOT‐SP on ...Figure 3.3 Schematic diagram of the major global photospheric flux‐transport...Figure 3.4 Butterfly diagram (latitude–time plot) based on Kitt Peak magneto...Figure 3.5 The latitudinal centroids of the active‐region fields as function...Figure 3.6 Ten‐day averages of the north (red solid lines) and south (blue d...Figure 3.7 Potential‐field source‐surface models representing the beginnings...Figure 3.8 South polar view of the magnetic field strength taken at 12:02:19...Figure 3.9 A TiO band (706 nm) photospheric image of a sunspot observed on 2...Figure 3.10 Schematic representation of a magnetic flux tube (green lines in...Figure 3.11 High‐resolution H α image of a filament on the disk. A main ...Figure 3.12 Two contrasting examples of solar prominences observed above the...Figure 3.13 Three‐dimensional representation of the photospheric vector magn...Figure 3.14 A diagram representing a model for filament formation due to she...Figure 3.15 A TRACE 171 Ǻ image of the coronal loop structure above an activ...Figure 3.16 An SDO/AIA 193 Ǻ image of the full solar disk showing a prominen...Figure 3.17 (a–c) Polar plots of the solar wind speed for Ulysses ’s three po...Figure 3.18 Top: Soft X‐ray (red), hard X‐ray (blue), and gamma‐ray (purple)...Figure 3.19 Top: Schematic drawing of the standard CSHKP (Carmichael Sturroc...Figure 3.20 Scatter plot of free magnetic energy against relative magnetic h...Figure 3.21 Solar spectral irradiance received at the top of Earth’s atmosph...Figure 3.22 Comparison of five different TSI composites.Figure 3.23 Comparison of SSI measurements obtained by various instruments w...Figure 3.24 Variation of measured total solar irradiance (TSI) compared to t...Figure 3.25 Solar spectral irradiance variability.Figure 3.26 Top: Solar images acquired with AIA at 211 nm. Middle: Total sol...Figure 3.27 Schematic representation of the main steps involved in a semi‐em...Figure 3.28 TSI variability obtained from two cosmogenic isotopes records us...Figure 3.29 Reconstructions of irradiance variability from the Maunder minim...Figure 3.30 (Panel a) Synoptic maps of Carrington Rotation 1708 of pseudo‐ma...Figure 3.31 An early observation of the solar chromosphere in the Ca II K li...Figure 3.32 Number of available Mount Wilson solar Ca II K spectroheliograms...Figure 3.33 These solar images illustrate typical data for three consecutive...Figure 3.34 Number of calibrated solar Ca II K spectroheliograms per year....Figure 3.35 Left: Relationship between the annual mean values of the plage i...Figure 3.36 Typical Ca II K Sun‐as‐a‐star spectrum obtained by the ISS instr...