Revisiting the Sunspot Number a 400-Year Perspective on the Solar Cycle
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Centennial Variations in Sunspot Number, Open Solar Flux and Streamer Belt Width: 2
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Central Archive at the University of Reading Centennial variations in sunspot number, open solar flux and streamer belt width: 2. Comparison with the geomagnetic data Article Published Version Creative Commons: Attribution 3.0 (CC-BY) Open Access Lockwood, M., Owens, M. J. and Barnard, L. (2014) Centennial variations in sunspot number, open solar flux and streamer belt width: 2. Comparison with the geomagnetic data. Journal of Geophysical Research: Space Physics, 119 (7). pp. 5183-5192. ISSN 2169-9402 doi: https://doi.org/10.1002/2014JA019972 Available at http://centaur.reading.ac.uk/36855/ It is advisable to refer to the publisher's version if you intend to cite from the work. Published version at: http://onlinelibrary.wiley.com/doi/10.1002/2014JA019972/abstract To link to this article DOI: http://dx.doi.org/10.1002/2014JA019972 Publisher: American Geophysical Union All outputs in CentAUR are protected by Intellectual Property Rights law, including copyright law. Copyright and IPR is retained by the creators or other copyright holders. Terms and conditions for use of this material are defined in the End User Agreement . www.reading.ac.uk/centaur CentAUR Central Archive at the University of Reading Reading's research outputs online PUBLICATIONS Journal of Geophysical Research: Space Physics RESEARCH ARTICLE Centennial variations in sunspot number, open solar 10.1002/2014JA019972 flux, and streamer belt width: 2. Comparison This article is a companion to Lockwood with the geomagnetic data et al. [2014] doi:10.1002/2014JA019970 and Lockwood and Owens [2014] M. -
Connection Between Solar Activity Cycles and Grand Minima Generation A
A&A 599, A58 (2017) Astronomy DOI: 10.1051/0004-6361/201629758 & c ESO 2017 Astrophysics Connection between solar activity cycles and grand minima generation A. Vecchio1, F. Lepreti2, M. Laurenza3, T. Alberti2, and V. Carbone2 1 LESIA – Observatoire de Paris, 5 place Jules Janssen, 92190 Meudon, France e-mail: [email protected] 2 Dipartimento di Fisica, Università della Calabria, Ponte P. Bucci Cubo 31C, 87036 Rende (CS), Italy 3 INAF–IAPS, via Fosso del Cavaliere 100, 00133 Roma, Italy Received 20 September 2016 / Accepted 28 November 2016 ABSTRACT Aims. The revised dataset of sunspot and group numbers (released by WDC-SILSO) and the sunspot number reconstruction based on dendrochronologically dated radiocarbon concentrations have been analyzed to provide a deeper characterization of the solar activity main periodicities and to investigate the role of the Gleissberg and Suess cycles in the grand minima occurrence. Methods. Empirical mode decomposition (EMD) has been used to isolate the time behavior of the different solar activity periodicities. A general consistency among the results from all the analyzed datasets verifies the reliability of the EMD approach. Results. The analysis on the revised sunspot data indicates that the highest energy content is associated with the Schwabe cycle. In correspondence with the grand minima (Maunder and Dalton), the frequency of this cycle changes to longer timescales of ∼14 yr. The Gleissberg and Suess cycles, with timescales of 60−120 yr and ∼200−300 yr, respectively, represent the most energetic contribution to sunspot number reconstruction records and are both found to be characterized by multiple scales of oscillation. -
A Decadal Strategy for Solar and Space Physics
Space Weather and the Next Solar and Space Physics Decadal Survey Daniel N. Baker, CU-Boulder NRC Staff: Arthur Charo, Study Director Abigail Sheffer, Associate Program Officer Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities to retain US scientific leadership • Provides well-respected source for priorities & scientific motivations to agencies, OMB, OSTP, & Congress” “Most useful approach: • Frame discussion identifying key science questions – Focus on what to do, not what to build – Discuss science breadth & depth (e.g., impact on understanding fundamentals, related fields & interdisciplinary research) • Explain measurements & capabilities to answer questions • Discuss complementarity of initiatives, relative phasing, domestic & international context” *From “The Role of NRC Decadal Surveys in Prioritizing Federal Funding for Science & Technology,” Jon Morse, Office of Science & Technology Policy (OSTP), NRC Workshop on Decadal Surveys, November 14-16, 2006 2 Context The Sun to the Earth—and Beyond: A Decadal Research Strategy in Solar and Space Physics Summary Report (2002) Compendium of 5 Study Panel Reports (2003) First NRC Decadal Survey in Solar and Space Physics Community-led Integrated plan for the field Prioritized recommendations Sponsors: NASA, NSF, NOAA, DoD (AFOSR and ONR) 3 Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities -
Solar Activity Affecting Space Weather
March 7, 2006, STP11, Rio de Janeiro, Brazil Solar Activity Affecting Space Weather Kazunari Shibata Kwasan and Hida Observatories Kyoto University, Japan contents • Introduction • Flares • Coronal Mass Ejections(CME) • Solar Wind • Future Projects Japanese newspaper reporting the big flare of Oct 28, 2003 and its impact on the Earth big flare (third largest flare in record) on Oct 28, 2003 X17 X-ray Intensity time A big flare on Oct 28, 2003 (third largest X-ray intensity in record) EUV Visible light SOHO/EIT SOHO/LASCO • Flare occurred at UT11:00 on Oct 28 Magnetic Storm on the Earth Around UT 6:00- Aurora observed in Japan on Oct 29, 2003 at around UT 14:00 on Oct 29, 2003 During CAWSES campaign observations (Shinohara) Xray X17 X6.2 Proton 10MeV 100MeV Vsw 44h 30h Bt Bz Dst Flares What is a flare ? Hα chromosphere 10,000 K Discovered in Mid 19C Near sunspots=> energy source is magnetic energy size~(1-10)x 104 km Total energy 1029 -1032erg (~ 105ー108 hydrogen bombs ) (Hida Observatory) Prominence eruption (biggest: June 4, 1946) Electro- magnetic Radio waves emitted from a flare (Svestka Visible 1976) UV 1hour time Solar corona observed in soft X-rays (Yohkoh) Soft X-ray telescope (1keV) Coronal plasma 2MK-10MK X-ray view of a flare Magnetic reconneciton Hα X-ray MHD simulation of a solar flare based on reconnection model including heat conduction and chromospheric evaporation (Yokoyama-Shibata 1998, 2001) A solar flare Observed with Yohkoh soft X-ray telescope (Tsuneta) Relation between filament (prominence) eruption and flare A flare -
Optical and Radio Solar Observation for Space Weather
2 Solar and Solar wind 2-1 Optical and Radio Solar Observation for Space Weather AKIOKA Maki, KONDO Tetsuro, SAGAWA Eiichi, KUBO Yuuki, and IWAI Hironori Researches on solar observation technique and data utilization are important issues of space weather forecasting program. Hiraiso Solar Observatory is a facility for R & D for solar observation and routine solar observation for CRL's space environment information service. High definition H alpha solar telescope is an optical telescope with very narrow pass-band filter for high resolution full-disk imaging and doppler mapping of upper atmos- phere dynamics. Hiraiso RAdio-Spectrograph (HiRAS) provides information on coronal shock wave and particle acceleration in the soar atmosphere. These information are impor- tant for daily space weather forecasting and alert. In this article, high definition H alpha solar telescope and radio spectrograph system are briefly introduced. Keywords Space weather forecast, Solar observation, Solar activity 1 Introduction X-ray and ultraviolet radiation resulting from solar activities and solar flares cause distur- 1.1 The Sun as the Origin of Space bances in the ionosphere and the upper atmos- Environment Disturbances phere, which in turn cause communication dis- The space environment disturbance phe- ruptions and affect the density structure of the nomena studied in space weather forecasting Earth's atmosphere. CME induce geomagnet- at CRL include a wide range of phenomena ic storms and ionospheric disturbances upon such as solar energetic particle (SEP) events, reaching the Earth's magnetosphere, and are geomagnetic storms, ionospheric disturbances, believed to be responsible for particle acceler- and radiation belt activity. All of these space environment disturbance events are believed to have solar origins. -
Coordinate Systems for Solar Image Data
A&A 449, 791–803 (2006) Astronomy DOI: 10.1051/0004-6361:20054262 & c ESO 2006 Astrophysics Coordinate systems for solar image data W. T. Thompson L-3 Communications GSI, NASA Goddard Space Flight Center, Code 612.1, Greenbelt, MD 20771, USA e-mail: [email protected] Received 27 September 2005 / Accepted 11 December 2005 ABSTRACT A set of formal systems for describing the coordinates of solar image data is proposed. These systems build on current practice in applying coordinates to solar image data. Both heliographic and heliocentric coordinates are discussed. A distinction is also drawn between heliocentric and helioprojective coordinates, where the latter takes the observer’s exact geometry into account. The extension of these coordinate systems to observations made from non-terrestial viewpoints is discussed, such as from the upcoming STEREO mission. A formal system for incorporation of these coordinates into FITS files, based on the FITS World Coordinate System, is described, together with examples. Key words. standards – Sun: general – techniques: image processing – astronomical data bases: miscellaneous – methods: data analysis 1. Introduction longitude and latitude – only need to worry about two spatial dimensions. The same can be said for normal cartography of Solar research is becoming increasingly more sophisticated. a planet such as Earth. However, to properly treat the complete Advances in solar instrumentation have led to increases in spa- range of solar phenomena, from the interior out into the corona, tial resolution, and will continue to do so. Future space mis- a complete three-dimensional coordinate system is required. sions will view the Sun from different perspectives than the Unfortunately, not all the information necessary to determine current view from ground-based observatories, or satellites in the full three-dimensional position of a solar feature is usually Earth orbit. -
CESRA Workshop 2019: the Sun and the Inner Heliosphere Programme
CESRA Workshop 2019: The Sun and the Inner Heliosphere July 8-12, 2019, Albert Einstein Science Park, Telegrafenberg Potsdam, Germany Programme and abstracts Last update: 2019 Jul 04 CESRA, the Community of European Solar Radio Astronomers, organizes triennial workshops on investigations of the solar atmosphere using radio and other observations. Although special emphasis is given to radio diagnostics, the workshop topics are of interest to a large community of solar physicists. The format of the workshop will combine plenary sessions and working group sessions, with invited review talks, oral contributions, and posters. The CESRA 2019 workshop will place an emphasis on linking the Sun with the heliosphere, motivated by the launch of Parker Solar Probe in 2018 and the upcoming launch of Solar Orbiter in 2020. It will provide the community with a forum for discussing the first relevant science results and future science opportunities, as well as on opportunity for evaluating how to maximize science return by combining space-borne observations with the wealth of data provided by new and future ground-based radio instruments, such as ALMA, E-OVSA, EVLA, LOFAR, MUSER, MWA, and SKA, and by the large number of well-established radio observatories. Scientific Organising Committee: Eduard Kontar, Miroslav Barta, Richard Fallows, Jasmina Magdalenic, Alexander Nindos, Alexander Warmuth Local Organising Committee: Gottfried Mann, Alexander Warmuth, Doris Lehmann, Jürgen Rendtel, Christian Vocks Acknowledgements The CESRA workshop has received generous support from the Leibniz Institute for Astrophysics Potsdam (AIP), which provides the conference venue at Telegrafenberg. Financial support for travel and organisation has been provided by the Deutsche Forschungsgemeinschaft (DFG) (GZ: MA 1376/22-1). -
A Method for the Prediction of Relative Sunspot Number for the Remainder of a Progressing Cycle with Application to Cycle 23
A&A 392, 301–307 (2002) Astronomy DOI: 10.1051/0004-6361:20020616 & c ESO 2002 Astrophysics A method for the prediction of relative sunspot number for the remainder of a progressing cycle with application to cycle 23 K. J. Li1;2,L.S.Zhan1;2;3;4,J.X.Wang2,X.H.Liu5,H.S.Yun6,S.Y.Xiong7,H.F.Liang1;2, and H. Z. Zhao1;2 1 Yunnan Observatory, YN650011, China 2 National Astronomical Observatories, CAS, China 3 Academy of Graduates, CAS, Beijing, China 4 Department of Physics, Jingdezhen Comprehensive College, Jiangxi, China 5 Department of Physics, Jiaozuo Educational College, Henan, China 6 Astronomy Program, SEES, Seoul National University, Seoul, Korea 7 Library, Yunnan Observatory, Yunnan, China Received 28 May 2001 / Accepted 18 April 2002 Abstract. In this paper, we investigate the prospect of using previously occurring sunspot cycle signatures to determine future behavior in an ongoing cycle, with specific application to cycle 23, the current sunspot cycle. We find that the gross level of solar activity (i.e., the sum of the total number of sunspots over the course of a sunspot cycle) associated with cycle 23, based on a comparison of its first several years of activity against similar periods of preceding cycles, is such that cycle 23 best compares to cycle 2. Compared to cycles 2 and 22, respectively, cycle 23 appears 1.08 times larger and 0.75 times as large. Because cycle 2 was of shorter period, we infer that cycle 23 also might be of shorter length (period less than 11 years), ending sometime in late 2006 or early 2007. -
Sunspot Number Calculation Methods
This article was published in an Elsevier journal. The attached copy is furnished to the author for non-commercial research and education use, including for instruction at the author’s institution, sharing with colleagues and providing to institution administration. Other uses, including reproduction and distribution, or selling or licensing copies, or posting to personal, institutional or third party websites are prohibited. In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier’s archiving and manuscript policies are encouraged to visit: http://www.elsevier.com/copyright Author's personal copy Advances in Space Research 40 (2007) 919–928 www.elsevier.com/locate/asr From the Wolf number to the International Sunspot Index: 25 years of SIDC Fre´de´ric Clette *, David Berghmans, Petra Vanlommel, Ronald A.M. Van der Linden, Andre´ Koeckelenbergh, Laurence Wauters Solar Influences Data Analysis Center, Royal Observatory of Belgium, 3, Avenue Circulaire, B-1180 Bruxelles, Belgium Received 10 October 2006; received in revised form 15 December 2006; accepted 19 December 2006 Abstract By encompassing four centuries of solar evolution, the sunspot number provides the longest available record of solar activity. Now- adays, it is widely used as the main reference solar index on which hundreds of published studies are based, in various fields of science. In this review, we will retrace the history of this crucial solar index, from its roots at the Zu¨rich Observatory up to the current multiple indices established and distributed by the Solar Influences Data Analysis Center (SIDC), World Data Center for the International Sun- spot Index, which was founded in 1981, exactly 25 years ago. -
Mission Operations and Communication Services
Space Communications and Navigation (SCaN) Overview Astrophysics Explorers SMEX Preproposal Conference Jerry Mason May 2, 2019 Agenda • Space Communications and Navigation (SCaN) overview • AO Considerations and Requirements • Spectrum Access & Licensing • SCaN’s Mission Commitment Offices • Points of contact •2 SCaN is Responsible for all NASA Space Communications • Responsible for Agency-wide operations, management, and development of all NASA space communications capabilities and enabling technology. • Expand SCaN capabilities to enable and enhance robotic and human exploration. • Manage spectrum and represent NASA on national and international spectrum management programs. • Develop space communication standards as well as Positioning, Navigation, and Timing (PNT) policy. • Represent and negotiate on behalf of NASA on all matters related to space telecommunications in coordination with the appropriate offices and flight mission directorates. •3 Supporting Over 100 Missions • SCaN supports over 100 space missions with the three networks. – Which includes every US government launch and early orbit flight • Earth Science – Earth observation missions – Global observation of climate, Land, Sea state and Atmospheric conditions. – Aura, Aqua, Landsat, Ice Cloud and Land Elevation Satellite (ICESAT-2), Orbiting Carbon Observatory (OCO- 2) • Heliophysics – Solar observation-Understanding the Sun and its effect on Space and Earth. – Parker Solar Probe, Solar Dynamics Observer (SDO), Solar Terrestrial Relations Observatory (STEREO) • Astrophysics – Studying the Universe and its origins. – Hubble Space Telescope, Chandra X-ray Observatory, James E. Webb Space Telescope (JWST), WFIRST • Planetary – Exploring our solar system’s content and composition – Voyagers-1/2, Mars Atmosphere and Volatile Evolution (MAVEN), InSight, Lunar Reconnaissance Orbiter (LRO) • Human Space Flight – Human tended Exploration missions, Commercial Space transportation and Space Communications. -
The Magnetic Sun CESAR’S Booklet
The Magnetic Sun CESAR’s Booklet 1 Introduction to planetary magnetospheres and the interplanetary medium Most of the planets in our Solar system are enclosed by huge magnetic structures, named magnetospheres that are generated by the planets’ interior magnetic field. These magnetospheres form the biggest structures in our Solar System with their size being 10-100 times bigger than the planet itself. This if the heliosphere is not included. The solar wind moves around these magnetic “bubbles” and interacts with them. A planet’s magnetosphere can either be induced by the interaction of the solar wind with the ionosphere (comets, Venus) of the body or via a dynamo process (Mercury, Earth or giant planets). Now we know that there are magnetic structures. The second question is: what they are and how do we know about their shapes? The shape of it is determined by the strength of its magnetic field. Furthermore, as the flow of the solar wind passes the field, the motion of a solar charge particle goes in the direction of the magnetosphere’s lines. Charged particles are present in all magnetospheres, though the composition of the particles and density varies from one planet to another. The particles in the magnetosphere may originate from the ionosphere of the planet, the solar wind or on satellites or ring particles whose orbits are entirely or partly within the magnetic field of the planet. The motion of these charged particles increases to great scale electric fields and currents, which affect the magnetic field and the motion of the particles through the field. -
Proposed Changes to Sacramento Peak Observatory Operations: Historic Properties Assessment of Effects
TECHNICAL REPORT Proposed Changes to Sacramento Peak Observatory Operations: Historic Properties Assessment of Effects Prepared for National Science Foundation October 2017 CH2M HILL, Inc. 6600 Peachtree Dunwoody Rd 400 Embassy Row, Suite 600 Atlanta, Georgia 30328 Contents Section Page Acronyms and Abbreviations ............................................................................................................... v 1 Introduction ......................................................................................................................... 1-1 1.1 Definition of Proposed Undertaking ................................................................................ 1-1 1.2 Proposed Alternatives Background ................................................................................. 1-1 1.3 Proposed Alternatives Description .................................................................................. 1-1 1.4 Area of Potential Effects .................................................................................................. 1-3 1.5 Methodology .................................................................................................................... 1-3 1.5.1 Determinations of Eligibility ............................................................................... 1-3 1.5.2 Finding of Effect .................................................................................................. 1-9 2 Identified Historic Properties ...............................................................................................