Solar and Stellar Magnetic Activity.

By: Schrijver, C. JContributor(s): Zwaan, CMaterial type: TextTextSeries: Cambridge AstrophysicsPublisher: Cambridge : Cambridge University Press, 2000Copyright date: ©2000Description: 1 online resource (402 pages)Content type: text Media type: computer Carrier type: online resourceISBN: 9780511151293Subject(s): Solar magnetic fields | Stars -- Magnetic fieldsGenre/Form: Electronic books.Additional physical formats: Print version:: Solar and Stellar Magnetic ActivityDDC classification: 523.7/2 LOC classification: QB539.M23 -- S37 2000ebOnline resources: Click to View
Contents:
Cover -- Half-title -- Series-title -- Title -- Copyright -- Contents -- Preface -- 1 Introduction: solar features and terminology -- 2 Stellar structure -- 2.1 Global stellar structure -- 2.1.1 Stellar time scales -- 2.1.2 Shell model for Sunlike stars -- 2.1.3 Stellar interiors: basic equations and models -- 2.2 Convective envelopes: classical concepts -- 2.2.1 Schwarzschild's criterion for convective instability -- 2.2.2 The mixing-length approximation -- 2.3 Radiative transfer and diagnostics -- 2.3.1 Radiative transfer and atmospheric structure -- 2.3.2 Magnetic field measurements: possibilities and limitations -- 2.3.3 Stellar brightness, color, and size -- 2.3.4 Radiative diagnostics of outer atmospheres -- 2.4 Stellar classification and evolution -- 2.4.1 Hertzsprung-Russell diagram and other diagrams -- 2.4.2 Stellar evolution -- 2.4.2.1 Protostars, pre-main-sequence contraction, and ZAMS -- 2.4.2.2 Main-sequence phase and beyond -- 2.4.3 Stars with convective envelopes -- 2.5 Convection in stellar envelopes -- 2.5.1 Observed properties of the granulation -- 2.5.2 Properties of supergranulation and mesogranulation -- 2.5.3 Numerical models of convection in stellar envelopes -- 2.5.4 Mimicking the photospheric flow patterns -- 2.6 Acoustic waves in stars -- 2.6.1 The generation of sound -- 2.6.2 Acoustic waves, resonance, and asteroseismology -- 2.7 Basal radiative losses -- 2.8 Atmospheric structure not affected by magnetic fields -- 3 Solar differential rotation and meridional flow -- 3.1 Surface rotation and torsional patterns -- 3.2 Meridional and other large-scale flows -- 3.3 Rotation with depth -- 4 Solar magnetic structure -- 4.1 Magnetohydrodynamics in convective envelopes -- 4.1.1 Basic concepts of magnetohydrodynamics -- 4.1.2 Interaction between flows and magnetic field -- 4.1.3 Magnetic reconnection.
4.2 Concentrations of strong magnetic field -- 4.2.1 Sunspots -- 4.2.2 Pores -- 4.2.3 Faculae and network patches -- 4.2.4 Hierarchic pattern -- 4.3 Magnetohydrostatic models -- 4.3.1 Flux-tube models -- 4.3.2 Sunspot models -- 4.3.3 Discussion of magnetostatic models -- 4.4 Emergence of magnetic field and convective collapse -- 4.5 Omega loops and toroidal flux bundles -- 4.6 Weak field and the magnetic dichotomy -- 5 Solar magnetic configurations -- 5.1 Active regions -- 5.1.1 Evolution of a bipolar active region -- 5.1.1.1 Emergence and growth -- 5.1.1.2 Storage and emergence of flux tubes -- 5.1.1.3 Around maximum development -- 5.1.1.4 Decay phase -- 5.1.2 Evolution of ephemeral active regions -- 5.2 The sequence of magnetoconvective configurations -- 5.3 Flux positioning and dynamics on small scales -- 5.4 The plage state -- 5.5 Heat transfer and magnetic concentrations -- 6 Global properties of the solar magnetic field -- 6.1 The solar activity cycle -- 6.1.1 Activity indices and synoptic magnetic maps -- 6.1.2 Characteristics of the solar activity cycle -- 6.2 Large-scale patterns in flux emergence -- 6.2.1 Activity nests and complexes -- 6.2.2 Properties of bipolar active regions -- 6.2.3 Subphotospheric structure of the strong magnetic field -- 6.2.4 Unipolar and mixed-polarity network -- 6.3 Distribution of surface magnetic field -- 6.3.1 Distribution of photospheric flux densities -- 6.3.1.1 Large-scale patterns -- 6.3.1.2 Global time-dependent distribution of the magnetic field -- 6.3.2 Dispersion by random walk and large-scale flows -- 6.3.2.1 An analytical model -- 6.3.2.2 The large-scale dispersal of flux -- 6.3.2.3 Random walk and the width of the network -- 6.3.2.4 The photospheric flux budget -- 6.4 Removal of magnetic flux from the photosphere -- 6.4.1 Flux cancellation and the retraction of flux loops -- 6.4.2 Flux elimination.
6.4.3 Convective blowup of flux tubes -- 6.4.4 Discussion of removal, transfer, and dissipation of field -- 7 The solar dynamo -- 7.1 Mean-field dynamo theory -- 7.2 Conceptual models of the solar cycle -- 7.3 Small-scale magnetic fields -- 7.4 Dynamos in deep convective envelopes -- 8 The solar outer atmosphere -- 8.1 Topology of the solar outer atmosphere -- 8.2 The filament-prominence configuration -- 8.3 Transients -- 8.3.1 Ejecta -- 8.3.2 Small-scale, transient brightenings -- 8.3.3 Flares -- 8.3.4 Radio bursts -- 8.3.5 The role of outer-atmospheric transients in the development of magnetic activity -- 8.4 Radiative and magnetic flux densities -- 8.4.1 Around the temperature minimum -- 8.4.2 The Ca II resonance lines as a magnetometer -- 8.4.3 The C IV doublet -- 8.4.4 Other chromospheric and transition-region activity measures -- 8.4.5 Coronal radiative losses -- 8.5 Chromospheric modeling -- 8.6 Solar coronal structure -- 8.7 Coronal holes -- 8.8 The chromosphere-corona transition region -- 8.9 The solar wind and the magnetic brake -- 8.9.1 Solar wind and mass loss -- 8.9.2 Angular-momentum loss by the solar wind -- 9 Stellar outer atmospheres -- 9.1 Historical sketch of the study of stellar activity -- 9.2 Stellar magnetic fields -- 9.2.1 Measurements of stellar magnetic fields -- 9.2.2 Scaled flux-tube models and structural hierarchy of stellar fields -- 9.3 The Mt. Wilson Ca II HK project -- 9.3.1 The Wilson-Bappu effect -- 9.3.2 Spectrophotometry: Ca II H and K variability -- 9.3.3 The solar-neighborhood program -- 9.4 Relationships between stellar activity diagnostics -- 9.5 The power-law nature of stellar flux-flux relationships -- 9.5.1 Solar data with angular resolution -- 9.5.2 Hemisphere-averaged stellar data -- 9.6 Stellar coronal structure -- 9.6.1 Coronal spectroscopy -- 9.6.2 Observed temperature structure -- 9.6.3 Loop geometry.
9.6.4 Loop lengths and area coverage -- 9.6.5 Coronal densities -- 9.6.6 Abundances and radiative transport -- 10 Mechanisms of atmospheric heating -- 11 Activity and stellar properties -- 11.1 Activity throughout the H-R diagram -- 11.2 Measures of atmospheric activity -- 11.3 Dynamo, rotation rate, and stellar parameters -- 11.4 Activity in stars with shallow convective envelopes -- 11.5 Activity in very cool main-sequence stars -- 11.6 Magnetic activity in T Tauri objects -- 11.7 Long-term variability of stellar activity -- 12 Stellar magnetic phenomena -- 12.1 Outer-atmospheric imaging -- 12.2 Stellar plages, starspots, and prominences -- 12.3 The extent of stellar coronae -- 12.4 Stellar flares -- 12.5 Direct evidence for stellar winds -- 12.6 Large-scale patterns in surface activity -- 12.7 Stellar differential rotation -- 13 Activity and rotation on evolutionary time scales -- 13.1 The evolution of the stellar moment of inertia -- 13.2 Observed rotational evolution of stars -- 13.3 Magnetic braking and stellar evolution -- 13.3.1 Magnetic braking for mature main-sequence stars -- 13.3.2 Magnetic braking while the moment of inertia changes -- 13.3.3 Post-main-sequence evolution -- 13.3.4 Rotational evolution of very young stars -- 14 Activity in binary stars -- 14.1 Tidal interaction and magnetic braking -- 14.2 Properties of active binaries -- 14.3 Types of particularly active stars and binary systems -- 15 Propositions on stellar dynamos -- Appendix I: Unit conversions -- Bibliography -- Index.
Summary: The first comprehensive review and synthesis of current understanding of magnetic fields in the Sun and similar stars.
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Cover -- Half-title -- Series-title -- Title -- Copyright -- Contents -- Preface -- 1 Introduction: solar features and terminology -- 2 Stellar structure -- 2.1 Global stellar structure -- 2.1.1 Stellar time scales -- 2.1.2 Shell model for Sunlike stars -- 2.1.3 Stellar interiors: basic equations and models -- 2.2 Convective envelopes: classical concepts -- 2.2.1 Schwarzschild's criterion for convective instability -- 2.2.2 The mixing-length approximation -- 2.3 Radiative transfer and diagnostics -- 2.3.1 Radiative transfer and atmospheric structure -- 2.3.2 Magnetic field measurements: possibilities and limitations -- 2.3.3 Stellar brightness, color, and size -- 2.3.4 Radiative diagnostics of outer atmospheres -- 2.4 Stellar classification and evolution -- 2.4.1 Hertzsprung-Russell diagram and other diagrams -- 2.4.2 Stellar evolution -- 2.4.2.1 Protostars, pre-main-sequence contraction, and ZAMS -- 2.4.2.2 Main-sequence phase and beyond -- 2.4.3 Stars with convective envelopes -- 2.5 Convection in stellar envelopes -- 2.5.1 Observed properties of the granulation -- 2.5.2 Properties of supergranulation and mesogranulation -- 2.5.3 Numerical models of convection in stellar envelopes -- 2.5.4 Mimicking the photospheric flow patterns -- 2.6 Acoustic waves in stars -- 2.6.1 The generation of sound -- 2.6.2 Acoustic waves, resonance, and asteroseismology -- 2.7 Basal radiative losses -- 2.8 Atmospheric structure not affected by magnetic fields -- 3 Solar differential rotation and meridional flow -- 3.1 Surface rotation and torsional patterns -- 3.2 Meridional and other large-scale flows -- 3.3 Rotation with depth -- 4 Solar magnetic structure -- 4.1 Magnetohydrodynamics in convective envelopes -- 4.1.1 Basic concepts of magnetohydrodynamics -- 4.1.2 Interaction between flows and magnetic field -- 4.1.3 Magnetic reconnection.

4.2 Concentrations of strong magnetic field -- 4.2.1 Sunspots -- 4.2.2 Pores -- 4.2.3 Faculae and network patches -- 4.2.4 Hierarchic pattern -- 4.3 Magnetohydrostatic models -- 4.3.1 Flux-tube models -- 4.3.2 Sunspot models -- 4.3.3 Discussion of magnetostatic models -- 4.4 Emergence of magnetic field and convective collapse -- 4.5 Omega loops and toroidal flux bundles -- 4.6 Weak field and the magnetic dichotomy -- 5 Solar magnetic configurations -- 5.1 Active regions -- 5.1.1 Evolution of a bipolar active region -- 5.1.1.1 Emergence and growth -- 5.1.1.2 Storage and emergence of flux tubes -- 5.1.1.3 Around maximum development -- 5.1.1.4 Decay phase -- 5.1.2 Evolution of ephemeral active regions -- 5.2 The sequence of magnetoconvective configurations -- 5.3 Flux positioning and dynamics on small scales -- 5.4 The plage state -- 5.5 Heat transfer and magnetic concentrations -- 6 Global properties of the solar magnetic field -- 6.1 The solar activity cycle -- 6.1.1 Activity indices and synoptic magnetic maps -- 6.1.2 Characteristics of the solar activity cycle -- 6.2 Large-scale patterns in flux emergence -- 6.2.1 Activity nests and complexes -- 6.2.2 Properties of bipolar active regions -- 6.2.3 Subphotospheric structure of the strong magnetic field -- 6.2.4 Unipolar and mixed-polarity network -- 6.3 Distribution of surface magnetic field -- 6.3.1 Distribution of photospheric flux densities -- 6.3.1.1 Large-scale patterns -- 6.3.1.2 Global time-dependent distribution of the magnetic field -- 6.3.2 Dispersion by random walk and large-scale flows -- 6.3.2.1 An analytical model -- 6.3.2.2 The large-scale dispersal of flux -- 6.3.2.3 Random walk and the width of the network -- 6.3.2.4 The photospheric flux budget -- 6.4 Removal of magnetic flux from the photosphere -- 6.4.1 Flux cancellation and the retraction of flux loops -- 6.4.2 Flux elimination.

6.4.3 Convective blowup of flux tubes -- 6.4.4 Discussion of removal, transfer, and dissipation of field -- 7 The solar dynamo -- 7.1 Mean-field dynamo theory -- 7.2 Conceptual models of the solar cycle -- 7.3 Small-scale magnetic fields -- 7.4 Dynamos in deep convective envelopes -- 8 The solar outer atmosphere -- 8.1 Topology of the solar outer atmosphere -- 8.2 The filament-prominence configuration -- 8.3 Transients -- 8.3.1 Ejecta -- 8.3.2 Small-scale, transient brightenings -- 8.3.3 Flares -- 8.3.4 Radio bursts -- 8.3.5 The role of outer-atmospheric transients in the development of magnetic activity -- 8.4 Radiative and magnetic flux densities -- 8.4.1 Around the temperature minimum -- 8.4.2 The Ca II resonance lines as a magnetometer -- 8.4.3 The C IV doublet -- 8.4.4 Other chromospheric and transition-region activity measures -- 8.4.5 Coronal radiative losses -- 8.5 Chromospheric modeling -- 8.6 Solar coronal structure -- 8.7 Coronal holes -- 8.8 The chromosphere-corona transition region -- 8.9 The solar wind and the magnetic brake -- 8.9.1 Solar wind and mass loss -- 8.9.2 Angular-momentum loss by the solar wind -- 9 Stellar outer atmospheres -- 9.1 Historical sketch of the study of stellar activity -- 9.2 Stellar magnetic fields -- 9.2.1 Measurements of stellar magnetic fields -- 9.2.2 Scaled flux-tube models and structural hierarchy of stellar fields -- 9.3 The Mt. Wilson Ca II HK project -- 9.3.1 The Wilson-Bappu effect -- 9.3.2 Spectrophotometry: Ca II H and K variability -- 9.3.3 The solar-neighborhood program -- 9.4 Relationships between stellar activity diagnostics -- 9.5 The power-law nature of stellar flux-flux relationships -- 9.5.1 Solar data with angular resolution -- 9.5.2 Hemisphere-averaged stellar data -- 9.6 Stellar coronal structure -- 9.6.1 Coronal spectroscopy -- 9.6.2 Observed temperature structure -- 9.6.3 Loop geometry.

9.6.4 Loop lengths and area coverage -- 9.6.5 Coronal densities -- 9.6.6 Abundances and radiative transport -- 10 Mechanisms of atmospheric heating -- 11 Activity and stellar properties -- 11.1 Activity throughout the H-R diagram -- 11.2 Measures of atmospheric activity -- 11.3 Dynamo, rotation rate, and stellar parameters -- 11.4 Activity in stars with shallow convective envelopes -- 11.5 Activity in very cool main-sequence stars -- 11.6 Magnetic activity in T Tauri objects -- 11.7 Long-term variability of stellar activity -- 12 Stellar magnetic phenomena -- 12.1 Outer-atmospheric imaging -- 12.2 Stellar plages, starspots, and prominences -- 12.3 The extent of stellar coronae -- 12.4 Stellar flares -- 12.5 Direct evidence for stellar winds -- 12.6 Large-scale patterns in surface activity -- 12.7 Stellar differential rotation -- 13 Activity and rotation on evolutionary time scales -- 13.1 The evolution of the stellar moment of inertia -- 13.2 Observed rotational evolution of stars -- 13.3 Magnetic braking and stellar evolution -- 13.3.1 Magnetic braking for mature main-sequence stars -- 13.3.2 Magnetic braking while the moment of inertia changes -- 13.3.3 Post-main-sequence evolution -- 13.3.4 Rotational evolution of very young stars -- 14 Activity in binary stars -- 14.1 Tidal interaction and magnetic braking -- 14.2 Properties of active binaries -- 14.3 Types of particularly active stars and binary systems -- 15 Propositions on stellar dynamos -- Appendix I: Unit conversions -- Bibliography -- Index.

The first comprehensive review and synthesis of current understanding of magnetic fields in the Sun and similar stars.

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Electronic reproduction. Ann Arbor, Michigan : ProQuest Ebook Central, 2018. Available via World Wide Web. Access may be limited to ProQuest Ebook Central affiliated libraries.

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