The Many Faces of the Sun: A Summary of the Results from NASA's Solar Maximum MissionKeith T. Strong 1. The Solar Maximum Mission.- 1.1 The Origins of the Mission.- 1.2 Scientific Objectives of the Mission.- 1.3 The SMM Instrument Package.- 1.3.1 The ?-Ray Spectrometer (GRS).- 1.3.2 The Hard X-Ray Burst Spectrometer (HXRBS).- 1.3.3 The Hard X-Ray Imaging Spectrometer (HXIS).- 1.3.4 The Bent Crystal Spectrometer (BCS).- 1.3.5 The Flat Crystal Spectrometer (FCS).- 1.3.6 The Ultraviolet Spectrometer/Polarimeter (UVSP).- 1.3.7 The Coronagraph/Polarimeter (C/P).- 1.3.8 The Active Cavity Radiometer Irradiance Monitor (ACRIM).- 1.4 Scientific Discoveries.- 1.5 Concluding Remarks.- 2. Solar Irradiance Variations.- 2.1 Development of Solar Irradiance Monitors.- 2.1.1 Early Space-Based Solar Observations.- 2.1.2 Sounding-Rocket Experiments.- 2.1.3 Nimbus-7 ERB Experiment.- 2.1.4 The SMM ACRIM Experiment.- 2.1.5 ACRIM I Results During Solar Cycles 21 and 22.- 2.1.5.1 Variability on Solar Cycle Timescales.- 2.1.6 Level of Significance of the Long-Term Data Base.- 2.1.7 Variability on Solar Active-Region Timescales.- 2.1.7.1 The "Sunspot Deficit" Effect.- 2.1.7.2 Facular "Excess" Effect.- 2.1.7.3 Energy Balance in Active Regions.- 2.1.8 Short-Term Variability: Global Oscillations.- 2.2 Models of the Solar-Cycle TSI Variation.- 2.2.1 Active-Region Timescales.- 2.2.2 Solar-Cycle Timescales.- 2.2.3 Shortcomings of Linear Regression Models.- 2.2.4 Multivariate Spectral Analysis.- 2.3 ACRIM I and Succeeding Observations.- 2.3.1 Solar Monitoring by ERBE Experiments.- 2.3.2 ACRIM II on UARS.- 2.3.3 Measurement Strategy for the Climate TSI Data Base.- 2.4 The Long-Term Climate TSI Data Base.- 2.4.1 ACRIM II Relationship to ACRIM I, ERB and ERBS.- 2.4.2 Sustaining the TSI Database.- 2.4.3 Future Total Solar Irradiance Monitoring.- 3. Active Regions.- 3.1 Magnetic Field Strength and Structure.- 3.1.1 Results Prior to SMM.- 3.1.2 First Results with SMM.- 3.1.3 Subsequent Results: 1983-1987.- 3.1.4 The Coronal Magnetic Structures Observing Campaign.- 3.1.5 Coronal Magnetic Field Studies after SMM.- 3.2 Dynamics and Heating of the Solar Corona.- 3.2.1 FCS Line-Broadening Measurements.- 3.2.1.1 Large Nonthermal Velocities.- 3.2.1.2 Spatial Variations.- 3.2.1.3 Correlation Studies.- 3.2.2 FCS Line-Broadening Data.- 3.2.3 Interpreting the FCS Line Broadening.- 3.2.3.1 Constraints on Mass Motions.- 3.2.3.2 Link to Heating.- 3.2.3.3 Discussion.- 3.2.4 Coronal Heating, Magnetic Fields, and Flares.- 3.2.4.1 UVSP Observations of Active Regions.- 3.3 Transition Region Brightenings: UV Microflares.- 3.4 Sunspots.- 3.4.1 Magnetic Field and Height of the Transition Region.- 3.4.2 Sunspot Plumes.- 3.4.3 Sunspot Flows.- 3.4.3.1 Horizontal Flows.- 3.4.3.2 Vertical Flows.- 3.4.3.3 Nonthermal Line Broadening.- 3.4.3.4 Umbral Oscillations.- 3.4.3.5 A Look Backward, a Look Forward.- 3.5 Prominences and Filaments.- 3.5.1 Prominence Environment and Structure.- 3.5.2 Steady Flows in Prominence Material.- 3.5.3 Activity in Prominences.- 3.5.4 Postflare Loops and Surges.- 3.5.5 Conclusion.- 4. Coronal Abundances.- 4.1 Flare X-Ray Measurements from BCS.- 4.1.1 Calcium Abundance.- 4.1.2 Fe/H and Fe/Ca Abundance.- 4.1.3 Relative Abundances of Ar, Ca, and Fe in Flares.- 4.1.4 Factors Affecting Abundance Determinations from X-Ray Spectra.- 4.2 FCS Abundances.- 4.2.1 FCS Active-Region Abundances.- 4.2.1.1 Abundance Variability in Active Regions.- 4.2.1.2 Impact of Resonance Scattering.- 4.2.1.3 Assessment of FCS Active-Region Abundance Results.- 4.2.2 FCS Flare Abundance Studies.- 4.2.2.1 Coronal Cl/S and Ar/S Measurements.- 4.2.2.2 DEM Studies of Flare Abundances.- 4.3 Determination of Solar Abundances by Solar Flare ?-Ray Spectrometry.- 4.3.1 ?-Ray Spectral Analysis.- 4.3.2 ?-Ray Results.- 4.4 Solar Energetic Particles.- 4.4.1 Major Proton Events.- 4.4.2 CIR Events from Coronal Holes.- 4.4.3 Impulsive Flare Events.- 4.5 Theory of Abundance Fractionation.- 4.5.1 Gravitational Settling.- 4.5.2 Pressure Gradient and Stationary Diffusion.- 4.5.3 Ion-Neutral Separation Due to Curr... |
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Page 293
... Kundu , White and Schmahl 1989 ) was often found above the photospheric magnetic neutral line ( Marsh et al . 1981 ; Kundu et al . 1982 ; Hoyng et al . 1983 ; Shevgaonkar and Kundu 1985 ; Kundu 1985 ) and was supposedly located near the ...
... Kundu , White and Schmahl 1989 ) was often found above the photospheric magnetic neutral line ( Marsh et al . 1981 ; Kundu et al . 1982 ; Hoyng et al . 1983 ; Shevgaonkar and Kundu 1985 ; Kundu 1985 ) and was supposedly located near the ...
Page 559
... Kundu and B. Woodgate ) , NASA CP - 2439 , p.7-1 Kopp , R.A. and Pneuman , G.W. 1976 , Solar Phys . , 50 , 85 Kopp ... Kundu , M.R. 1961 , JGR 66 , 4308 Kundu , M.R. 1965 , Solar Radio Astronomy , Interscience , New York Kundu , M.R. ...
... Kundu and B. Woodgate ) , NASA CP - 2439 , p.7-1 Kopp , R.A. and Pneuman , G.W. 1976 , Solar Phys . , 50 , 85 Kopp ... Kundu , M.R. 1961 , JGR 66 , 4308 Kundu , M.R. 1965 , Solar Radio Astronomy , Interscience , New York Kundu , M.R. ...
Page 560
... Kundu , M.R. , Schmahl , E.J. and Rao , A.P. 1981 , Astron . Astrophys . , 94 , 72 Kundu , M.R. , Schmahl , E.J. and Velusamy , T. 1982 , Ap.J. , 253 , 963 Kundu , M.R. and Vlahos , L. 1982 , Spa . Sci . Rev. , 32 , 405 Kundu , M.R. ...
... Kundu , M.R. , Schmahl , E.J. and Rao , A.P. 1981 , Astron . Astrophys . , 94 , 72 Kundu , M.R. , Schmahl , E.J. and Velusamy , T. 1982 , Ap.J. , 253 , 963 Kundu , M.R. and Vlahos , L. 1982 , Spa . Sci . Rev. , 32 , 405 Kundu , M.R. ...
Contents
The Solar Maximum Mission | 1 |
Chapter | 13 |
Solar Irradiance Variations | 19 |
Copyright | |
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abundances acceleration active regions analysis Antonucci Ap.J appears arch associated Astron atmosphere blueshifted broadening bursts changes chromospheric comparable component consistent coronal correlation Cosmic Ray decay Dennis density dependence derived detected direct discussed distribution effects electron elements energetic energy et al evaporation evidence example Figure flux footpoints hard X-ray heating images impulsive increase indicated intensity interacting ions limited line profiles loop lower magnetic field mass ejections material maximum measurements mechanism motions nonthermal observed obtained occur particles peak period phase photospheric physical plasma possible produced prominence radiation radio Ramaty range ratio relative resolution satellite shock showed shown significant soft X-ray solar flares Solar Phys Space spatial spectra Spectrometer spectrum stars strong structure suggested temperature thermal transition values variation velocities wavelength waves X-ray emission y-ray