Solar Neutrons and Related Phenomena (eBook)

Lev Dorman (Autor)

eBook Download: PDF

2010 | 2010
XLVI, 873 Seiten
Springer Netherland (Verlag)
978-90-481-3737-4 (ISBN)

Infos

Short Historical Overview In the 1940s, two phenomena in the ?eld of cosmic rays (CR) forced scientists to think that the Sun is a powerful source of high-energy particles. One of these was discovered because of the daily solar variation of CR, which the maximum number of CR observed near noon (referring to the existence of continuous ?ux of CR from the direction of the Sun); this became the experimental basis of the theory that CR's ´ originate from the Sun (or, for that matter, from within the solar system) (Alfven 1954). The second phenomenon was discovered when large ?uxes of high energy particles were detected from several solar ?ares, or solar CR. These are the - called ground level events (GLE), and were ?rst observed by ionization chambers shielded by 10 cm Pb (and detected mainly from the secondary muon-component CR that they caused) during the events of the 28th of February 1942, the 7th of March 1942, the 25th of July 1946, and the 19th of November 1949. The biggest such event was detected on the 23rd of February 1956 (see the detailed description in Chapters X and XI of Dorman, M1957). The ?rst phenomenon was investigated in detail in Dorman (M1957), by ?rst correcting experimental data on muon temperature effects and then by using coupling functions to determine the change in particle energy caused by the solar-diurnal CR variation.

Inhalt

Preface 8
Short Historical Overview 8
Physical Motivation and Background 9
Plan and Structure of the Book 11
Acknowledgements 18
Contents 22
Abbreviations 46
Interactions of Charged, Accelerated Particles in the Solar Atmosphere, and the Generation of Secondary Energetic Particles and Radiation: Pioneer Results 48
1.1 Interactions of Charged Accelerated Particles in the Solar Atmosphere and Expected Energetic Secondary Radiation from the Sun: The First Model Calculations 1.1.1 The Matter and Short History of the Problem 48
1.2 Estimations of Expected Solar Neutron and/or Gamma- Ray Fluxes from Historical Powerful Flare- Generated Energetic Charged Particles 65
1.3 Search for Solar Neutrons Using Balloon and Space Probe Experiments 67
1.4 Search for Solar Neutrons Using Ground Measurements 70
1.5 The First Attempts at Solar Gamma-Ray Search 76
1.6 The First Attempts to Search for Solar Positrons 77
References for Preface and Chapter 1 79
The Events of August 1972 and the Discovery of Solar Gamma- Radiation 82
2.1 Main Peculiarities of the August 1972 Events 82
2.2 The Discovery of Solar Gamma-Radiation 83
References for Chapter 2 85
The Events of June 1980 and June 1982, and the Discovery of Solar Neutrons 87
3.1 Main Peculiarities of the June 1980 and June 1982 Solar Events 87
3.2 Observations of Gamma Radiation During the Events of June 1980 and June 1982 as Evidence of Neutron Generation 90
3.3 The Discovery of Solar Neutrons by the Gamma Ray Spectrometer on the Solar Maximum Mission 93
3.4 June 3, 1982: the First Solar Neutron Event Observed by Neutron Supermonitors 97
3.5 Some Constraints for Neutron Generation Processes on the Sun Follow from June 21, 1980 and June 3, 1982 Event Data 100
References for Chapter 3 102
Space Probe Observations of Solar Neutron and Gamma Ray Events 104
4.1 The First Solar Neutron and Gamma Ray Event Observed on SMM 104
4.2 Solar Neutron and Gamma Ray Events Observed on the Satellites SMM and Hinotori 104
4.3 Solar Neutron and Gamma Ray Events Observed By the COMPTEL Experiment at the Compton Gamma- Ray Observatory 105
4.4 The Solar Neutron and Gamma Ray Event of April 25, 1984 106
4.5 The Solar Neutron and Gamma Ray Event of March 6, 1989 107
4.6 The Solar Neutron and Gamma Ray Event of June 4, 1991 110
4.7 The Solar Neutron and Gamma Ray Event of June 9, 1991 110
4.8 The Solar Neutron and Gamma Ray Event of June 15, 1991 112
4.9 The Solar Neutron and Gamma Ray Event of November 6, 1997 113
References for Chapter 4 113
Solar Neutron Propagation in the Earth’s Atmosphere, and the Sensitivity of Neutron Monitors and Other Ground Based Detectors to Solar Neutrons 115
5.1 The Atmospheric Depth for Ground Solar Neutron Observations in the Direction of the Sun 115
5.2 Integral Multiplicity and the Sensitivity of Neutron Monitors, Muon and Electron- Photon Detectors to High Energy Solar Neutrons ( Obtained by Using Experimental Data of the Geomagnetic Effects of Charged Particles) 117
5.3 The Integral Multiplicity and Sensitivity of Neutron Monitors and Detectors of Charged Particles to High Energy Solar Neutrons, Obtained by Using Results of Theoretical Calculations of Meson- Nucleon Cascades of Galactic Cosmic Rays 136
5.4 Calculations of Integral Multiplicity and Sensitivity of the Neutron Monitor at Various Depths Depending on the Zenith Angle of Primary Particle Incidence 145
5.5 On the Small Energy Solar Neutron Propagation in the Earth’s Atmosphere and the Sensitivity of Neutron Monitors and Other Ground Based Detectors to Solar Neutrons 152
5.6 On the ‘Refraction’ Effect in Solar Neutron Propagation Through the Earth’s Atmosphere 163
5.7 Simulation and Analytical Description of the Refraction Effect 166
5.8 Analytical Description of Solar Neutron Propagation in the Earth’s Atmosphere by Considering Scattering, Attenuation and Energy Change 189
References for Chapter 5 199
Statistical Investigations of Solar Neutron Events on the Basis of Ground Observations 205
6.1 Statistical Investigations of Solar Neutron Events Using the Rome Neutron Supermonitor 5- min Data for 1978– 1982 205
6.2 Statistical Investigation of Solar Neutron Events Using the Chacaltaya Neutron Supermonitor 5- min Data for 1980– 1982 208
6.3 Statistical Investigations of Solar Neutron Events Using the Tyan Shan Neutron Supermonitor 5- min Data 211
6.4 Statistical Investigation of Solar Neutron Events Using the 5- min Data of the Neutron Supermonitors of the Sayan Spectrograph 218
6.5 Upper Limits on High-Energy Solar Neutron Fluxes from Gamma Ray Flares According to Yangbajing NM Observations 221
References for Chapter 6 227
Observations of Solar Neutron Events by Ground Based Detectors, and Their Interpretation 228
7.1 Investigations of Solar Neutron Events by the Tyan Shan High Altitude Neutron Supermonitor 228
7.2 Possible Solar Neutron Event on May 9, 1980 Detected by Tyan Shan High Altitude Neutron Supermonitor 233
7.3 The Event of June 7, 1980 233
7.4 The Event of June 21, 1980 237
7.5 The Event of November 6, 1980 237
7.6 Possible Solar Neutron Events on the 1st and 2nd of April 1981, as Detected by Tyan Shan High Altitude Neutron Supermonitor 240
7.7 The Solar Neutron Event on April 4, 1981 240
7.8 The Possible Event on April 27, 1981 244
7.9 Possible Solar Neutron Event on July 19, 1981 244
7.10 Possible Solar Neutron Event on August 10, 1981 244
7.11 Full Differential Flux of Solar Neutrons at the Top of the Earth’s Atmosphere During the Event of 3 June 1982 244
7.12 Possible Solar Neutron Events on June 5 and 12, 1982 245
7.13 Possible Solar Neutron Events on July 6 and August 14, 1982 245
7.14 The Solar Neutron Event on November 26, 1982 246
7.15 The Solar Neutron Event on 25 April, 1984, and the Possible Neutron Event on May 20, 1984 248
7.16 On the Possible Solar Neutron Event on December 16, 1988 252
7.17 The Largest Solar Neutron Event on May 24, 1990 252
7.18 Solar Neutron Event on February 22, 1991 and Possible New Special Class of Solar Flares, Very Deep in the Chromosphere ( Near Photosphere) 258
7.19 Solar Neutron Events on March 22 and May 3, 1991 258
7.20 Solar Neutron Event at 1st June 1991: Surprisingly Intense Neutron Emission from a Flare Behind the Limb of the Sun 264
7.21 Solar Neutron Event on June 4, 1991 276
7.22 Solar Neutron Event on June 6, 1991 287
7.23 Solar Neutron Events on November 6, 1997 290
7.24 Possible Solar Neutron Event on November 23, 1998 296
7.25 Solar Neutron Event on November 28, 1998 298
7.26 Search for Solar Neutrons in Association with Large Solar Flares in July 2000 and in March– April 2001: Three Categories of Solar Neutron Events 302
7.27 Solar Neutron Event on November 24, 2000 306
7.28 The Solar Neutron and GLE Event of April 15, 2001 316
7.29 Solar Neutron Event in Association with a Large Solar Flare on August 25, 2001 329
7.30 Detection of Solar Neutrons During the Event in Association with the 24 September, 2001 Flare, Using Tibet Solar Neutron Telescope 333
7.31 Solar Neutron Event of October 28, 2003 336
7.32 Solar Neutron Event on November 2, 2003 348
7.33 Solar Neutron Event on 4 November, 2003 353
7.34 Solar Neutron Event of the 7th of September 2005 364
7.35 The Search for Solar Neutrons from the 8 September, 2005 Flare 379
7.36 Search for Solar Neutrons from the 13th December, 2006 Flare 382
7.37 Comparison of Power Spectral Indexes for Solar Neutron Events Observed by Neutron Monitors During 1982– 2005 384
References for Chapter 7 384
The Solar Neutron Decay Phenomenon 394
8.1 Solar Neutron Decay Protons During June 21, 1980 394
8.2 Solar Neutron Decay Protons During June 3, 1982 396
8.3 Solar Neutron Decay Protons During the April 24, 1984 Event 404
8.4 Possible High Energy Solar Neutron Decay Protons During October 19, 1989 409
8.5 Possible High Energy Solar Neutron Decay Protons During the October 28, 2003 Event: Where Were Energetic Particles Accelerated and Where Were Solar Neutrons Decayed? 412
8.6 Prediction and Possible Observation of Solar Neutron Decay Electrons 417
8.7 Observation of Electrons from the Decay of Solar Flare Neutrons 418
References for Chapter 8 426
Gamma Rays from Solar Energetic Particle Interactions with the Sun’s Atmosphere 431
9.1 The Matter of Problem: Why g-Ray Observations Are Very Important for Understanding the Nature of Solar Neutron Events, What Information May Be Obtained from Solar g- Ray Spectroscopy 431
9.2 Absorption of 2.223 MeV Solar Flare Gamma-Rays and Determination of the Solar Plasma Density Altitude Profile 434
9.3 Long-Duration Solar Gamma-Ray Flares and Their Possible Origin 452
9.4 Photospheric 3He to H Abundance Ratio Derived from Gamma-Ray Line Observations 478
9.5 Low-FIP to High-FIP Elements Gamma-Ray Line Ratio 482
9.6 Gamma Ray Measurements of the 1991 November 15 Solar Flare 486
9.7 Gamma-Ray Spectroscopy of the Giant 1991 June 1 Behind- the- Limb Flare: Evidence for Gamma- Ray Production in the Corona and Accelerated Heavy Ion Abundance Enhancements 490
9.8 Gamma-Ray Spectroscopy of the 1991 June 4 Solar Flare: Accelerated Particle Composition, Energetics, and Ambient Abundances 501
9.9 Main Properties of Solar Gamma-Ray Flares in the 23rd Solar Maximum: Yohkoh Observations Between November 1997 and March 1999 536
9.10 Gamma-Ray Observations of the 2000 July 14 Flare 543
9.11 The Solar Gamma-Ray Event of 24 November 2000 555
9.12 Comparison of g-Ray Flares at 27 October 1991, 6 November 1997, 14 July and 24 November 2000: Energy Spectra and Total Energy in Nonthermal Electrons and Protons 559
9.13 Gamma and X-Ray Solar Flare Emissions: CORONAS-F Measurements 562
9.14 The Event of 2002 July 23: First Gamma-Ray Images of a Solar Flare 568
9.15 The Event of 2002 July 23: Physical Implications of RHESSI Neutron- Capture Line Measurements 572
9.16 The Event of 2002 July 23: RHESSI Discovery of a Coronal Non- thermal Hard X- Ray Source, as a Precursor of the Impulse Flare 579
9.17 The Event of 2002 July 23: Magnetic Field, Ha, and RHESSI Observations, Evolution of Magnetic Fields Associated with the Flare and Energy Release Models 584
9.18 The 2003 October 28 X17 Flare: Gamma Rays and the Evolving Compact Structures 597
9.19 The 2003 October 28 X17 Flare: Time Profile of the 2.223 MeV Gamma Ray Line and Evolving Acceleration Parameter and Density Altitude Profile 612
9.20 Solar Flares of 28 October and 2 November 2003: Gamma- Ray Line Analysis and Model of Particle Acceleration and Density Profile 614
9.21 Gamma-Ray Solar Flare Events in January 2005: Temporal Profiles in Various Energy Bands by Data from AVS- F Apparatus on Board the CORONAS- F Satellite 623
9.22 Gamma-Ray Emission During the 20 January 2005 Solar Flare: Possible Observation of Neutron Capture Radiaton on 3He 630
References for Chapter 9 636
Positron Generation in the Nuclear Interactions of Flare Energetic Particles in the Solar Atmosphere 657
10.1 Expected Fluxes of Positrons from Nuclear Interactions of Solar Energetic Particles with the Atmosphere of the Sun, and the First Observations 657
10.2 Positron Annihilation Radiation from the 1997 November 6 Flare, Comparison with High Energy g- Ray Emission, and Possible Acceleration Mechanisms 658
10.3 The RHESSI Observation of the Solar Annihilation Line from the 2002 July 23 Solar Flare 662
10.4 Positron-Emitter Production in Solar Flares from 3He Reactions 665
References for Chapter 10 682
The Development of Models and Simulations for Solar Neutron and Gamma Ray Events 686
11.1 Solar Flare Neutron Production and the Angular Dependence of the 2.223 MeV Capture Gamma- Ray Line Emission 686
11.2 Determination of the 3He/H ratio in the Solar Photosphere from Flare Gamma-Ray Line Observations 716
11.3 Intensity and Directionality of Flare-Accelerated a- Particles at the Sun: Simulation and Estimation from Gamma- Ray Observations 721
11.4 Estimation of the Spectral Evolution of Energetic Protons in Solar Flares by Gamma- Ray Observations and Simulation 738
11.5 Gamma-Ray Measurement of Energetic Heavy Ions at the Sun 746
11.6 Estimation of the Ratio of Interaction to Interplanetary Energetic Protons by Gamma- Rays: Diverging Magnetic Field Lines and Stochastic Acceleration 751
11.7 Estimation of the Ratio of Interaction to Interplanetary Energetic Protons by Gamma- Rays: Diverging Magnetic Field Lines and Parallel Shock Wave Acceleration 764
11.8 High Energy Gamma Ray Generation in the Corona and Solar Wind Through Interactions of Flare Energetic 783
11.8 High Energy Gamma Ray Generation in the Corona and Solar Wind Through Interactions of Flare Energetic Particles with Matter Through p0 Decay and Bremsstrahlung 783
11.9 Pion-Related Gamma Rays: Problem on Interacting and Interplanetary High Energy Particles in Solar Flare Events 795
11.10 Angular and Energy-Dependent Neutron Emission from Solar Flare Magnetic Loops: Model and Monte Carlo Simulation 807
11.11 Production of Energetic Light Isotopes Due to Nuclear Interaction and Acceleration in the Flare Region: Modeling and Simulation 834
11.12 Gamma Rays from Excited States of 12C and Various Neutron Capture Lines: Investigation of Powerful Solar Flare Characteristics 842
References for Chapter 11 849
Appendix 862
Numerical Simulations by Monte Carlo Method (for Section 11.6) 862
Kinetic Equation and Monte Carlo Simulations (for Section 11.7) 864
References for Appendix 868
Conclusions and Problems 869
General Conclusion 869
Main Conclusions for Different Chapters 870
Actual Problems for Solving in Near Future 874
References for Monographs and Books 876
Author Index 879
Subject Index 900

Produkt-Details

• Erscheint lt. Verlag: 15.7.2010
• Reihe/Serie: Astrophysics and Space Science Library
• Reihe/Serie: Astrophysics and Space Science Library
• Zusatzinfo: XLVI, 873 p. 586 illus.
• Verlagsort: Dordrecht
• Sprache: englisch
• Themenwelt: Naturwissenschaften ► Geowissenschaften ► Geologie
• Themenwelt: Naturwissenschaften ► Geowissenschaften ► Geophysik
• Themenwelt: Naturwissenschaften ► Physik / Astronomie ► Angewandte Physik
• Themenwelt: Naturwissenschaften ► Physik / Astronomie ► Astronomie / Astrophysik
• Themenwelt: Naturwissenschaften ► Physik / Astronomie ► Atom- / Kern- / Molekularphysik
• Themenwelt: Technik ► Luft- / Raumfahrttechnik
• Schlagworte: chromosphere • Corona • cosmic rays • hydrogen atom • Meson-nucleon cascades • Neutron • Neutron monitors • particles • Photosphere • Planet • Solar • solar flares • Solar Gamma Rays • Solar Neutron Decay • Solar Neutrons • Solar Neutron Telescopes • Space Science • space weather • Sun
• ISBN-10: 90-481-3737-3 / 9048137373
• ISBN-13: 978-90-481-3737-4 / 9789048137374