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Planetary Challenges & Spiritual Evolution
Planetary Challenges & Spiritual Evolution – Citizen Summary Planetary Challenges & Spiritual Evolution Summary For Citizens of Planet Earth Written by Susan Joy Rennison, B. Sc Hons (Physics & Geophysics), June 2011 (Editorial Revision), Olten, Switzerland Copyright © 2011 Susan Joy Rennison Planetary Challenges & Spiritual Evolution – Citizen Summary Planetary Challenges & Spiritual Evolution Citizen Summary Table of Contents Table of Contents i Illustrations ii Foreword iv Introduction vii Our Sun, A Variable Star 1 The Extraordinary Quiet Solar Minimum of Solar Cycle 23 2 Space Weather & The Delivery of Evolutionary Energies 4 The Precession of the Equinoxes 5 Extreme Space Weather 6 The Gamma & Cosmic Ray Blitz From Across the Galaxy 8 The Global Warming Controversy 9 Atmospheric Change: New Electrical Manifestations 10 Extreme Physics right here on Earth 12 Asteroids, Comets & Meteors? “We’re living in a bowling alley” 13 Heavenly Phenomena: Strange Fireballs 16 The Geological Response 17 Strange Atmospheric Cloud Emissions 19 The ‘Orb’ Phenomena & ‘Diamond’ Rain 20 Earth’s Shadow Biosphere 21 The Planetary ‘Refresh’ 27 i Copyright Susan Joy Rennison Sunday, June 05, 2011 Planetary Challenges & Spiritual Evolution – Citizen Summary The ‘Upgrade’ of the Planetary Grid 31 Space Weather Drives Biological Changes 32 The Choice: Spiritual Evolution or Devolution? 33 Rapid Evolutionary Change 34 Conclusion 38 References 39 Illustrations The White House i Medieval Engraving of Gioacchino da Fiore (Joachim of Fiore) vi Space Weather Turns Into an International Problem vii The Sun −Earth Connection viii Aurora over Southern New Jersey (1989) ix Exploration of Near Earth Objects Workshop Poster x The Eventful Universe Workshop Poster xi Massive Coronal Mass Ejection Proceeding X45 Solar Flare. -
Ionospheric Radars Development
UNT Ionospheric radars development Enrico Zuccheretti, Umberto Sciacca [email protected] - [email protected] Istituto Nazionale di Geofisica e Vulcanologia - Rome, Italy The following slides were presented during the lectures of the course “Desarrollo de radares ionosféricos” held within the post graduate course on “Geofísica espacial” organised by the Universidad Nacional de Tucumán - Facultad de Ciencias Exactas y Tecnología - Departamento de Posgrado in Tucumán on 4 – 7 October 2010. UNT Module 1 Basics of radar theory and design elements Introduction UNT •Amongst the big variety of techniques used to study the geophysical environment, methods using electromagnetic waves occupy a very prominent position. •These techniques exploit radio waves modifications when they interact with the medium they pass through. •The ionosphere is no exception: the most common way to study its behaviour is to emit radio wave pulses into the ionosphere and to study the backscattered echo. •The echo signal contains information about the layers in which it may be refracted, reflected or absorbed. •Also signals coming from satellites (NNSS, GPS) or from terrestrial emitting station (VLF emitters) can be used. They do not exploit the radar technique but their properties are affected by the medium they pass through. Radio Frequencies Bands UNT ELF SLF ULF VLF LF MF HF VHF UHF SHF EHF 3 Hz 30 Hz 300 Hz 3 kHz 30 kHz 300 kHz 3 MHz 30 MHz 300 MHz 3 GHz 30 GHz 30 Hz 300 Hz 3 kHz 30 kHz 300 kHz 3 MHz 30 MHz 300 MHz 3 GHz 30 GHz 300 GHz The vertical sounding technique UNT •The measure technique is based on sending pulses of energy at different frequencies towards the ionosphere and in measuring the backscattered echo delay to properly evaluate the position of ionospheric layers. -
Chapter 10 IONOSPHERICRADIO WAVE PROPAGATION Section 10.1 S
Chapter 10 IONOSPHERICRADIO WAVE PROPAGATION Section 10.1 S. Basu, J. Buchau, F.J. Rich and E.J. Weber Section 10.2 E.C. Field, J.L. Heckscher, P.A. Kossey, and E.A. Lewis Section 10.3 B.S. Dandekar Section 10.4 L.F. McNamara Section 10.5 E.W. Cliver Section 10.6 G.H. Millman Section 10.7 J. Aarons and S. Basu Section 10.8 J.A. Klobuchar Section 10.9 J.A. Klobuchar Section 10.10 S. Basu, M.F. Mendillo The series of reviews presented is an attempt to introduce in HF communications is leading to a rejuvenation of the ionospheric radio wave propagation of interest to system global ionosonde network. users. Although the attempt is made to summarize the field, the individuals writing each section have oriented the work 10.1.1.1 Ionogram. Ionospheric sounders or ionosondes in the direction judged to be most important. are, in principle, HF radars that record the time of flight or We cover areas such as HF and VLF propagation where travel of a transmitted HF signal as a measure of its ionos- the ionosphere is essentially a "black box", that is, a vital pheric reflection height. By sweeping in frequency, typically part of the system. We also cover areas where the ionosphere from 0.5 to 20 MHz, an ionosonde obtains a meas- is essentially a nuisance, such as the scintillations of trans- urement of the ionospheric reflection height as a function ionospheric radio signals. of frequency. A recording of this reflection height meas- Finally, we have included a summary of the main fea- urement as a function of frequency is called an ionogram. -
Statistical Properties of Superactive Regions During Solar Cycles 19–23⋆
A&A 534, A47 (2011) Astronomy DOI: 10.1051/0004-6361/201116790 & c ESO 2011 Astrophysics Statistical properties of superactive regions during solar cycles 19–23 A. Q. Chen1,2,J.X.Wang1,J.W.Li2,J.Feynman3, and J. Zhang1 1 Key Laboratory of Solar Activity of Chinese Academy of Sciences, National Astronomical Observatories, Chinese Academy of Sciences, PR China e-mail: [email protected]; [email protected] 2 National Center for Space Weather, China Meteorological Administration, PR China 3 Helio research, 5212 Maryland Avenue, La Crescenta, USA Received 26 February 2011 / Accepted 20 August 2011 ABSTRACT Context. Each solar activity cycle is characterized by a small number of superactive regions (SARs) that produce the most violent of space weather events with the greatest disastrous influence on our living environment. Aims. We aim to re-parameterize the SARs and study the latitudinal and longitudinal distributions of SARs. Methods. We select 45 SARs in solar cycles 21–23, according to the following four parameters: 1) the maximum area of sunspot group, 2) the soft X-ray flare index, 3) the 10.7 cm radio peak flux, and 4) the variation in the total solar irradiance. Another 120 SARs given by previous studies of solar cycles 19–23 are also included. The latitudinal and longitudinal distributions of the 165 SARs in both the Carrington frame and the dynamic reference frame during solar cycles 19–23 are studied statistically. Results. Our results indicate that these 45 SARs produced 44% of all the X class X-ray flares during solar cycles 21–23, and that all the SARs are likely to produce a very fast CME. -
Introductionto the Ionoshpereand Geomagnetism
N6517513 INTRODUCTION TO THE IONOSHPERE AND GEOMAGNETISM OCT 1964 SEL-64-111 INTRODUCTION TO THE IONOSPHERE AND GEOMAGNETISM by H. Rishbeth and O. K. Garriott October 1964 Reproduction in whole or in part is permitted for any purpose of the United States Government. Technical Report No. 8 Prepared under National Aeronautics and Space Administration Grant NsG 30-60 Radioscience Laboratory Stanford Electronics Laboratories Stanford University Stanford, California CONTENTS -=_:_!-_¸ Paze I. THE NEUTRAL ATMOSPHERE .................. 1 I. Atmospheric Nomenclature ............... 1 2. Evolution of the Earth's Atmosphere ......... 5 3. Structure of the Atmosphere ............. 7 4. Dissociation and Diffusive Separation ........ 12 5. Thermal Balance ................... 16 6. The Exosphere .................... 2O __J, 7. Experimental Techniques ............... 21 II. MEASUREMENT OF IONOSPHERIC PARAMETERS .......... 27 I. Introduction ..................... 27 2. Determination of Electron Density by Sounding .... 27 3, Propagation Methods ................. 36 4. Direct Measurements ................. 44 z, 5. Incoherent Scatter .................. 46 III. PROCESSES IN THE IONOSPHERE ............... 50 I. The Balance of Ionization .............. 50 2. Chapman's Theory ................... 53 3. Production and Loss ................. 63 4. The D, E and F1 Photochemical Regime ....... 69 5. Plasma Diffusion ................... 81 6. Solving the Continuity Equation ........... 88 IV. MORPHOLOGY OF THE IONOSPHERE 94 1. D Region .................... 94 2. -
Our Sun Has Spots.Pdf
THE A T M O S P H E R I C R E S E R V O I R Examining the Atmosphere and Atmospheric Resource Management Our Sun Has Spots By Mark D. Schneider Aurora Borealis light shows. If you minima and decreased activity haven’t seen the northern lights for called The Maunder Minimum. Is there actually weather above a while, you’re not alone. The end This period coincides with the our earth’s troposphere that con- of Solar Cycle 23 and a minimum “Little Ice Age” and may be an cerns us? Yes. In fact, the US of sunspot activity likely took place indication that it’s possible to fore- Department of Commerce late last year. Now that a new 11- cast long-term temperature trends National Oceanic and over several decades or Atmospheric Administra- centuries by looking at the tion (NOAA) has a separate sun’s irradiance patterns. division called the Space Weather Prediction Center You may have heard (SWPC) that monitors the about 22-year climate weather in space. Space cycles (two 11-year sun- weather focuses on our sun spot cycles) in which wet and its’ cycles of solar activ- periods and droughts were ity. Back in April of 2007, experienced in the Mid- the SWPC made a predic- western U.S. The years tion that the next active 1918, 1936, and 1955 were sunspot or solar cycle would periods of maximum solar begin in March of this year. forcing, but minimum Their prediction was on the precipitation over parts of mark, Solar Cycle 24 began NASA TRACE PROJECT, OF COURTESY PHOTO the U.S. -
Prediction of Solar Activity on the Basis of Spectral Characteristics of Sunspot Number
Annales Geophysicae (2004) 22: 2239–2243 SRef-ID: 1432-0576/ag/2004-22-2239 Annales © European Geosciences Union 2004 Geophysicae Prediction of solar activity on the basis of spectral characteristics of sunspot number E. Echer1, N. R. Rigozo1,2, D. J. R. Nordemann1, and L. E. A. Vieira1 1Instituto Nacional de Pesquisas Espaciais (INPE), Av. Astronautas, 1758 ZIP 12201-970, Sao˜ Jose´ dos Campos, SP, Brazil 2Faculdade de Tecnologia Thereza Porto Marques (FAETEC) ZIP 12308-320, Jacare´ı, Brazil Received: 9 July 2003 – Revised: 6 February 2004 – Accepted: 18 February 2004 – Published: 14 June 2004 Abstract. Prediction of solar activity strength for solar cy- when daily averages are more frequently available (Hoyt and cles 23 and 24 is performed on the basis of extrapolation of Schatten, 1998a, b). sunspot number spectral components. Sunspot number data When the solar cycle is in its maximum phase, there are during 1933–1996 periods (solar cycles 17–22) are searched important terrestrial consequences, such as the higher solar for periodicities by iterative regression. The periods signifi- emission of extreme-ultraviolet and ultraviolet flux, which cant at the 95% confidence level were used in a sum of sine can modulate the middle and upper terrestrial atmosphere, series to reconstruct sunspot series, to predict the strength and total solar irradiance, which could have effects on terres- of solar cycles 23 and 24. The maximum peak of solar cy- trial climate (Hoyt and Schatten, 1997), as well as the coronal cles is adequately predicted (cycle 21: 158±13.2 against an mass ejection and interplanetary shock rates, responsible by observed peak of 155.4; cycle 22: 178±13.2 against 157.6 geomagnetic activity storms and auroras (Webb and Howard, observed). -