Sun, Weather, and Climate
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→ Investigating Solar Cycles a Soho Archive & Ulysses Final Archive Tutorial
→ INVESTIGATING SOLAR CYCLES A SOHO ARCHIVE & ULYSSES FINAL ARCHIVE TUTORIAL SCIENCE ARCHIVES AND VO TEAM Tutorial Written By: Madeleine Finlay, as part of an ESAC Trainee Project 2013 (ESA Student Placement) Tutorial Design and Layout: Pedro Osuna & Madeleine Finlay Tutorial Science Support: Deborah Baines Acknowledgements would like to be given to the whole SAT Team for the implementation of the Ulysses and Soho archives http://archives.esac.esa.int We would also like to thank; Benjamín Montesinos, Department of Astrophysics, Centre for Astrobiology (CAB, CSIC-INTA), Madrid, Spain for having reviewed and ratified the scientific concepts in this tutorial. CONTACT [email protected] [email protected] ESAC Science Archives and Virtual Observatory Team European Space Agency European Space Astronomy Centre (ESAC) Tutorial → CONTENTS PART 1 ....................................................................................................3 BACKGROUND ..........................................................................................4-5 THE EXPERIMENT .......................................................................................6 PART 1 | SECTION 1 .................................................................................7-8 PART 1 | SECTION 2 ...............................................................................9-11 PART 2 ..................................................................................................12 BACKGROUND ........................................................................................13-14 -
Doc.10100.Space Weather Manual FINAL DRAFT Version
Doc 10100 Manual on Space Weather Information in Support of International Air Navigation Approved by the Secretary General and published under his authority First Edition – 2018 International Civil Aviation Organization TABLE OF CONTENTS Page Chapter 1. Introduction ..................................................................................................................................... 1-1 1.1 General ............................................................................................................................................... 1-1 1.2 Space weather indicators .................................................................................................................... 1-1 1.3 The hazards ........................................................................................................................................ 1-2 1.4 Space weather mitigation aspects ....................................................................................................... 1-3 1.5 Coordinating the response to a space weather event ......................................................................... 1-3 Chapter 2. Space Weather Phenomena and Aviation Operations ................................................................. 2-1 2.1 General ............................................................................................................................................... 2-1 2.2 Geomagnetic storms .......................................................................................................................... -
Effect of Solar Variability on the Earth's Climate Patterns
Advances in Space Research 40 (2007) 1146–1151 www.elsevier.com/locate/asr Effect of solar variability on the Earth’s climate patterns Alexander Ruzmaikin Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA Received 30 October 2006; received in revised form 8 January 2007; accepted 8 January 2007 Abstract We discuss effects of solar variability on the Earth’s large-scale climate patterns. These patterns are naturally excited as deviations (anomalies) from the mean state of the Earth’s atmosphere-ocean system. We consider in detail an example of such a pattern, the North Annular Mode (NAM), a climate anomaly with two states corresponding to higher pressure at high latitudes with a band of lower pres- sure at lower latitudes and the other way round. We discuss a mechanism by which solar variability can influence this pattern and for- mulate an updated general conjecture of how external influences on Earth’s dynamics can affect climate patterns. Ó 2007 COSPAR. Published by Elsevier Ltd. All rights reserved. Keywords: Solar irradiance; Climate and inter-annual variability; Solar variability impact; Climate dynamics 1. Introduction in solar irradiance. The solar cycle variations in total solar irradiance are small, 0.1%. However the magnitude of The center of attention of this paper is the response of irradiance variations strongly depends on the wavelength the Earth to solar variability on Space Climate time scales. and increases for the shorter wavelengths. Thus solar UV, In the context of Space Climate, the Earth can respond to which amounts to only a few percentage of the total irradi- solar variability on the 27-day solar rotation time scale, the ance, contributes 15% to the change in total irradiance 11-year solar cycle, the century scale Grand Minima, and (Lean et al., 2005). -
A Spectral Solar/Climatic Model H
A Spectral Solar/Climatic Model H. PRESCOTT SLEEPER, JR. Northrop Services, Inc. The problem of solar/climatic relationships has prove our understanding of solar activity varia- been the subject of speculation and research by a tions have been based upon planetary tidal forces few scientists for many years. Understanding the on the Sun (Bigg, 1967; Wood and Wood, 1965.) behavior of natural fluctuations in the climate is or the effect of planetary dynamics on the motion especially important currently, because of the pos- of the Sun (Jose, 1965; Sleeper, 1972). Figure 1 sibility of man-induced climate changes ("Study presents the sunspot number time series from of Critical Environmental Problems," 1970; "Study 1700 to 1970. The mean 11.1-yr sunspot cycle is of Man's Impact on Climate," 1971). This paper well known, and the 22-yr Hale magnetic cycle is consists of a summary of pertinent research on specified by the positive and negative designation. solar activity variations and climate variations, The magnetic polarity of the sunspots has been together with the presentation of an empirical observed since 1908. The cycle polarities assigned solar/climatic model that attempts to clarify the prior to that date are inferred from the planetary nature of the relationships. dynamic effects studied by Jose (1965). The sun- The study of solar/climatic relationships has spot time series has certain important characteris- been difficult to develop because of an inadequate tics that will be summarized. understanding of the detailed mechanisms respon- sible for the interaction. The possible variation of Secular Cycles stratospheric ozone with solar activity has been The sunspot cycle magnitude appears to in- discussed by Willett (1965) and Angell and Kor- crease slowly and fall rapidly with an. -
Trajectory Coordinate System Information We Have Calculated the New Horizons Trajectory and Full State Vector Information in 11 Different Coordinate Systems
Trajectory Coordinate System Information We have calculated the New Horizons trajectory and full state vector information in 11 different coordinate systems. Below we describe the coordinate systems, and in the next section we describe the trajectory file format. Heliographic Inertial (HGI) This system is Sun centered with the X-axis along the intersection line of the ecliptic (zero longitude occurs at the +X-axis) and solar equatorial planes. The Z-axis is perpendicular to the solar equator, and the Y-axis completes the right-handed system. This coordinate system is also referred to as the Heliocentric Inertial (HCI) system. Heliocentric Aries Ecliptic Date (HAE-DATE) This coordinate system is heliocentric system with the Z-axis normal to the ecliptic plane and the X-axis pointes toward the first point of Aries on the Vernal Equinox, and the Y- axis completes the right-handed system. This coordinate system is also referred to as the Solar Ecliptic (SE) coordinate system. The word “Date” refers to the time at which one defines the Vernal Equinox. In this case the date observation is used. Heliocentric Aries Ecliptic J2000 (HAE-J2000) This coordinate system is heliocentric system with the Z-axis normal to the ecliptic plane and the X-axis pointes toward the first point of Aries on the Vernal Equinox, and the Y- axis completes the right-handed system. This coordinate system is also referred to as the Solar Ecliptic (SE) coordinate system. The label “J2000” refers to the time at which one defines the Vernal Equinox. In this case it is defined at the J2000 date, which is January 1, 2000 at noon. -
National Space Weather Program Implementation Plan, 2Nd Edition, July 2000
National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ The National Space Weather Program The Implementation Plan 2nd Edition July 2000 National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ NATIONAL SPACE WEATHER PROGRAM COUNCIL Mr. Samuel P. Williamson, Chairman Federal Coordinator Dr. David L. Evans Department of Commerce Colonel Michael A. Neyland, USAF Department of Defense Mr. Robert E. Waldron Department of Energy Mr. James F. Devine Department of the Interior Mr. David Whatley Department of Transportation Dr. Edward J. Weiler National Aeronautics and Space Administration Dr. Margaret S. Leinen National Science Foundation Lt Col Michael R. Babcock, USAF, Executive Secretary Office of the Federal Coordinator for Meteorological Services and Supporting Research National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ NATIONAL SPACE WEATHER PROGRAM Implementation Plan 2nd Edition Prepared by the Committee for Space Weather for the National Space Weather Program Council Office of the Federal Coordinator for Meteorology FCM-P31-2000 Washington, DC July 2000 National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ National Space Weather Program Implementation Plan, 2nd Edition, July 2000 http://www.ofcm.gov/ FOREWORD We are pleased to present this Second Edition of the National Space Weather Program Implementation Plan. We published the program's Strategic Plan in 1995 and the first Implementation Plan in 1997. In the intervening period, we have made tremendous progress toward our goals but much work remains to be accomplished to achieve our ultimate goal of providing the space weather observations, forecasts, and warnings needed by our Nation. -
Solar Wind Variation with the Cycle I. S. Veselovsky,* A. V. Dmitriev
J. Astrophys. Astr. (2000) 21, 423–429 Solar Wind Variation with the Cycle I. S. Veselovsky,* A. V. Dmitriev, A. V. Suvorova & M. V. Tarsina, Institute of Nuclear Physics, Moscow State University, 119899 Moscow, Russia. *e-mail: [email protected] Abstract. The cyclic evolution of the heliospheric plasma parameters is related to the time-dependent boundary conditions in the solar corona. “Minimal” coronal configurations correspond to the regular appearance of the tenuous, but hot and fast plasma streams from the large polar coronal holes. The denser, but cooler and slower solar wind is adjacent to coronal streamers. Irregular dynamic manifestations are present in the corona and the solar wind everywhere and always. They follow the solar activity cycle rather well. Because of this, the direct and indirect solar wind measurements demonstrate clear variations in space and time according to the minimal, intermediate and maximal conditions of the cycles. The average solar wind density, velocity and temperature measured at the Earth's orbit show specific decadal variations and trends, which are of the order of the first tens per cent during the last three solar cycles. Statistical, spectral and correlation characteristics of the solar wind are reviewed with the emphasis on the cycles. Key words. Solar wind—solar activity cycle. 1. Introduction The knowledge of the solar cycle variations in the heliospheric plasma and magnetic fields was initially based on the indirect indications gained from the observations of the Sun, comets, cosmic rays, geomagnetic perturbations, interplanetary scintillations and some other ground-based methods. Numerous direct and remote-sensing space- craft measurements in situ have continuously broadened this knowledge during the past 40 years, which can be seen from the original and review papers. -
Craniord High to Graduate Largest Class Next Tuesday
A.,. rue six CRANTOBD <N. J.) CITIZEN AND . JtOT*; !*•> been installed as the dominant in terior motif. ^- , - '.- •. City Savings Founded in 1887. City" Federal, Savings has grown from a single Opens New office in downtown Elizabeth to four' offices/including the new air- domebranch in,Elmora, with total Air-Dome assets in excess of $55,000,000. The ^ssociatlon'is'.'tlieTlarigEStrfederaUjr Association, with; offices in Eliza chartered savings association in the beth, Kenilworth and Linden; state and the largest sayings and opened the world's first air-dome loan association in Union County financial building in, the Elmora Entered as second class mall matter al section of Elizabeth on Saturday Vol. LXVH. No.2J. 3 SecUbn^, 24 Pages . NEW JERSEY, THURSDAY; JUNE 16,1960 The Post Office at Cranford. tt. J. TEN CENTS Erected as an interim measur while a new' permanent Elmora Office is. being built, the u'niqui savings center,has walls of trans Record Year J as estion parent vinyl.material supported by 's School Craniord High to Graduate an air pressure differential of onl; HOME PURCHASED—air. and Mre. Louis MoncelM of Bayonne Report Given four-hundredths of a point per have purchased the above home at 2 Amherst road* Mr. and Mrs. At Elizabeth, North Avenues square inch. A. special revolving George Miller, the former owners, have moved to Scotch Plains. diplomas to71 In an effort to help alleviate traffic congestion during the morn- door'" permits;.', only a minimal On Cranteen ing rush hour at Elizabeth and North avenues, a traffic patrolman •J..L-! This home was sold through the offices of G. -
The Enigmatic WR46: a Binary Or a Pulsator in Disguise
A&A 385, 619–631 (2002) Astronomy DOI: 10.1051/0004-6361:20020076 & c ESO 2002 Astrophysics The enigmatic WR46: A binary or a pulsator in disguise III. Interpretation P. M. Veen1,A.M.vanGenderen1, and K. A. van der Hucht2 1 Leiden Observatory, Postbus 9513, 2300 RA Leiden, The Netherlands 2 Space Research Organization Netherlands, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands Received 1 September 2000 / Accepted 5 November 2001 Abstract. Photometric and spectroscopic monitoring campaigns of WR 46 (WN3p), as presented in Veen et al. (2002a,b; hereafter Papers I and II, respectively), yield the following results. The light- and colour variations 89 91 reveal a dominant single-wave period of Psw =0.1412 d in 1989, and Psw =0.1363 d in 1991. Because of a small difference in the minima, this periodicity may be a double-wave phenomenon (Pdw). The line fluxes vary in concert with the magnitudes. The significant difference of the periods can be either due to the occurence of two distinct periods, or due to a gradual change of the periodicity. A gradual brightening of the system of 0m. 12 appeared to accompany the period change. In addition, the light variations in 1989 show strong evidence for an additional period Px =0.2304 d. Generally, the radial velocities show a cyclic variability on a time scale of the photometric double-wave. However, often they do not vary at all. The observed variability confirms the Population I WR nature of the light source, as noted independently by Marchenko et al. (2000). In the present paper, we first show how the photometric double-wave variability can be interpreted as a rotating ellipsoidal density distribution in the stellar wind. -
Solar Data Handling
United Nations Educational. Scientific The Abdus Salam International Centre for Theoretical Physics Intem3tion.1l Atomic Energy Agency 310/1749-25 ICTP-COST-USNSWP-CAWSES-INAF-INFN International Advanced School on Space Weather 2-19 May 2006 Solar Data Handling Robert BENTLEY UCL Department of Space and Climate Physics Mullard Space Science Laboratory Hombury St. Mary Dorking Surrey RH5 6NT U.K. These lecture notes are intended only for distribution to participants Strada Costiera 11, 34014 Trieste, Italy - Tel. +39 040 2240 11 I; Fax +39 040 224 163 - [email protected], www.ictp.it i f Solar data Handling 1 Rob Bentley University College London (UCL) C Mullard Space Science Laboratory Trieste, 3 May 2006 International Advanced School on Space Weather Nature of Observations Data management issues • Types of data | • Storage of data I • Access to data (current) : • Standards • Temporal and spatial coordinates • File Formats • Types of Metadata I • Data Models egso Nature of solar observations The appearance of the Sun changes dramatically with wavelength • Emissions originate from different layers in the atmosphere and different physical phenomena K • For a complete picture we need to use as 2x106K wide a range of observations as possible 1 • Mixture of types of observations • Different wavelengths and time intervals • Mixture of observations from space- and ground-based platforms 8x104K • Increasing desire to study problems that span communities • Desire relevant to Space Weather, climate I physics, planetary physics, astrophysics 3 • Identifying observations across community 6x10 K boundaries and then retrieving them are major problems r Sun at different wavelengths egso o J K I egso TVPes of Data • Types of data/observation: • single values • spectra (includes and dispersed quantity) • images | • compound - e.g. -
19710023003.Pdf
General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) X-625-71-308 PkEFRlil NASA T1:1 X- ELECTRON AND POSITIVE ION DENSITY ALTITUDE DISTRIBUTIONS IN THE EQUATORIAL Q REGION A. C. AIKIN R. A. GOLDBERG Y. V. SOMAYAJULU Aq ^F q "9,>/ #44#i4 a^F/j/F C-r; AI!riICT 1471 Jp ,32479 Ole °o (ACCESSi JN N MBCR) (THR 0 'i (NASA CR R TMX OR AD NUMBER) (CATEGORY) --- GODDARD SPACE FLIGHT CENTER GREENBELT, MARYLAND - it %0 ELECTRON AND POSITIVE ION DENSITY ALTITUDE DISTRIBUTIONS IN THE EQUATORIAL D REGION by A. C. Aikin R. A. Goldberg • Laboratory for .Planetary Atmospheres NASA/Goddard !7nace Flight Center Greenb?.. , Maryland and Y. V. Somayajulu National Physical Laboratory New Delhi, India ABSTRACT Three simultaneous rocket measurements of P region ionization sources and electron and ion densities have been made in one day. -
The Multiple Spectroscopic and Photometric Periods of DI Cru
The multiple spectroscopic and photometric periods of DI Cru ≡ WR 46 1 Alexandre S. Oliveira2, J. E. Steiner2 and M. P. Diaz2 [email protected],[email protected],[email protected] ABSTRACT In an effort to determine the orbital period of the enigmatic star DI Cru ≡ WR 46 ≡ HD 104994, we made photometric and spectroscopic observations of this object between 1996 and 2002. Both photometric and spectroscopic characteristics are quite complex. The star is highly variable on short (few hours) as well as on long (few months) time-scales. The optical spectrum is rich in strong emission lines of high ionization species such as He II, N IV, N V and O VI. Weak emission of C III and Hβ is also present. Emission lines have been compiled and identified from the ultraviolet to the infrared. In the UV, emission of O V and N IV is also observed, together with very weak emission of C IV. The N V 4603+19A/He˚ II 4686A˚ line ratios vary by a significant amount from night to night. Temporal Variance Spectrum – TVS – analysis shows that the He II 4686A˚ line has P Cyg-like variable absorption, while N V 4603/19A˚ lines have a strong and broad variable component due to the continuum fluorescence from a source (stellar atmosphere/optically thick wind) of variable temperature. We also show that the object has variable degree of ionization, probably caused by wind density variation. The star presents multiple periods in radial velocity and photometry. We derived, from our data, a main radial velocity period of 0.3319 d with an amplitude of K =58kms−1.