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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 -
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. -
Level and Length of Cyclic Solar Activity During the Maunder Minimum As Deduced from the Active-Day Statistics
A&A 577, A71 (2015) Astronomy DOI: 10.1051/0004-6361/201525962 & c ESO 2015 Astrophysics Level and length of cyclic solar activity during the Maunder minimum as deduced from the active-day statistics J. M. Vaquero1,G.A.Kovaltsov2,I.G.Usoskin3, V. M. S. Carrasco4, and M. C. Gallego4 1 Departamento de Física, Universidad de Extremadura, 06800 Mérida, Spain 2 Ioffe Physical-Technical Institute, 194021 St. Petersburg, Russia 3 Sodankylä Geophysical Observatory and ReSoLVE Center of Excellence, University of Oulu, 90014 Oulu, Finland e-mail: [email protected] 4 Departamento de Física, Universidad de Extremadura, 06071 Badajoz, Spain Received 25 February 2015 / Accepted 25 March 2015 ABSTRACT Aims. The Maunder minimum (MM) of greatly reduced solar activity took place in 1645–1715, but the exact level of sunspot activity is uncertain because it is based, to a large extent, on historical generic statements of the absence of spots on the Sun. Using a conservative approach, we aim to assess the level and length of solar cycle during the MM on the basis of direct historical records by astronomers of that time. Methods. A database of the active and inactive days (days with and without recorded sunspots on the solar disc) is constructed for three models of different levels of conservatism (loose, optimum, and strict models) regarding generic no-spot records. We used the active day fraction to estimate the group sunspot number during the MM. Results. A clear cyclic variability is found throughout the MM with peaks at around 1655–1657, 1675, 1684, 1705, and possibly 1666, with the active-day fraction not exceeding 0.2, 0.3, or 0.4 during the core MM, for the three models. -
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. -
Coronal Mass Ejections and Solar Radio Emissions
CORONAL MASS EJECTIONS AND SOLAR RADIO EMISSIONS N. Gopalswamy∗ Abstract Three types of low-frequency nonthermal radio bursts are associated with coro- nal mass ejections (CMEs): Type III bursts due to accelerated electrons propagating along open magnetic field lines, type II bursts due to electrons accelerated in shocks, and type IV bursts due to electrons trapped in post-eruption arcades behind CMEs. This paper presents a summary of results obtained during solar cycle 23 primarily using the white-light coronagraphic observations from the Solar Heliospheric Ob- servatory (SOHO) and the WAVES experiment on board Wind. 1 Introduction Coronal mass ejections (CMEs) are associated with a whole host of radio bursts caused by nonthermal electrons accelerated during the eruption process. Radio bursts at low frequencies (< 15 MHz) are of particular interest because they are associated with ener- getic CMEs that travel far into the interplanetary (IP) medium and affect Earth’s space environment if Earth-directed. Low frequency radio emission needs to be observed from space because of the ionospheric cutoff (see Fig. 1), although some radio instruments permit observations down to a few MHz [Erickson 1997; Melnik et al., 2008]. Three types of radio bursts are prominent at low frequencies: type III, type II, and type IV bursts, all due to nonthermal electrons accelerated during solar eruptions. The radio emission is thought to be produced by the plasma emission mechanism [Ginzburg and Zheleznyakov, 1958], involving the generation of Langmuir waves by nonthermal electrons accelerated during the eruption and the conversion of Langmuir waves to electromagnetic radiation. Langmuir waves scattered off of ions or low-frequency turbulence result in radiation at the fundamental (or first harmonic) of the local plasma frequency. -
Minima, When the Type B Redauroras Are Predominant. SOLAR
VOL. 43, 1957 GEOPHYSICS: J. BARTELS 75 are being slowed down much higher in the atmosphere than occurs at sunspot minima, when the Type B red auroras are predominant. From the general physical interpretation of the observations of unusual heights of aurora, it seems probable that a consideration of the degree of ionization of the upper atmosphere may account for the wide range found in auroral heights. For this reason the degree of ionization may become one of the problems of auroral morphol- ogy. The auroral program for the International Geophysical Year, 1957-1958, was de- signed with many of the above-mentioned problems in auroral morphology in mind. Hence we may expect to have answers for some of the problems in the next two or three years. 1 J. A. Van Allen, Phys. Rev., 99, 609, 1955. 2 S. Chapman and C. G. Little, J. Atm. and Terrest. Phys. (in press). 3 J. P. Heppner, J. Geophys. Research, 59, 329, 1954. 4 C. W. Gartlein, Nat. Geographic Mag., 92, 683, 1947. 5 F. T. Davies, Transactions of the Oslo Meeting, August 19-928, 1948 (Washington: Interna- tional Union of Geodesy and Geophysics, 1950). 6 A. B. Meinel, Astrophys. J., 113, 50, 1951; 114, 431, 1951. 7 A. B. Meinel and C. Y. Fan, Astrophys. J., 115, 330, 1952. 8 H. Leinbach, Sky and Telescope, 15, 329, 1956. 9 C. T. Elvey, Seventh Alaska Science Conference, Alaska Division, AAAS, Juneau, September 26-29, 1956. 10 C. St0rmer, The Polar Aurora (Oxford: Clarendon Press, 1955). 1 M. Sugiura, Proceedings of the Third Alaska Science Conference, September 22-97, 1962, p. -
Galactic Cosmic Ray Radiation Hazard in the Unusual Extended Solar Minimum Between Solar Cycle 23 and 24
1 Galactic Cosmic Ray Radiation Hazard in the Unusual Extended Solar 2 Minimum between Solar Cycle 23 and 24 3 4 N. A. Schwadron, A. J. Boyd, K. Kozarev 5 Boston University, Boston, Mass, USA 6 M. Golightly, H. Spence 7 University of New Hampshire, Durham New Hampshire, USA 8 L. W. Townsend 9 University of Tennessee, Knoxville, TN, USA 10 M. Owens 11 Space Environment Physics Group, Department of Meteorology, University of Reading, 12 UK 13 14 Abstract. Galactic Cosmic Rays (GCRs) are extremely difficult to shield against and 15 pose one of most severe long-term hazards for human exploration of space. The recent 16 solar minimum between solar cycle 23 and 24 shows a prolonged period of reduced solar 17 activity and low interplanetary magnetic field strengths. As a result, the modulation of 18 GCRs is very weak, and the fluxes of GCRs are near their highest levels in the last 25 19 years in the Fall of 2009. Here, we explore the dose-rates of GCRs in the current 20 prolonged solar minimum and make predictions for the Lunar Reconnaissance Orbiter 21 (LRO) Cosmic Ray Telescope for the Effects of Radiation (CRaTER), which is now 22 measuring GCRs in the lunar environment. Our results confirm the weak modulation of 23 GCRs leading to the largest dose rates seen in the last 25 years over a prolonged period of 24 little solar activity. 25 26 Background – Galactic Cosmic Rays and Human Health 27 28 In balloon flights in 1912-1913, Hess first measured a form of radiation that intensified 29 with altitude [Hess, 1912; 1913]. -
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. -
Determining the Rotation Period of the Sun
SOLAR PHYSICS AND TERRESTRIAL EFFECTS 2+ Activity 8 4= Activity 8 Determining the Rotation Period of the Sun Relevant Reading Chapter 2, section 3 Purpose Determine the rotation period of the Sun. Although numerous methods for accurate measurement are used in solar research, the method described here, using photographs taken over several days, will allow determination to within an Earth-day. Materials Photo set that shows at least one solar feature that can be followed over a several-day period. For real challenge, take the photos yourself, or make a simple projection sketch of sunspots over several days. 1 sheet of clear plastic used for overhead transparencies or viewgraphs, or something similar such as a clear plastic report folder a mm ruler, compass and protractor a fine-tipped marking pen suitable for plastic graph paper with 1-mm squares Procedures 1. Measure, to the nearest millimeter, the diameter of the Sun on the photo taken near the middle of the data period. 2. Use a compass and draw a circle with the same diameter on the transpar- ent sheet. 3. With the circle aligned over the photo on the date used for the diameter, trace the axis orientation marks onto the transparency. 4. Pick a solar feature that traverses the solar disk for as many days as pos- sible. Align the circle on the transparency over each successive photo and carefully mark the position of the chosen solar feature along with its date. 5. Carefully draw the best fitting straight line through the marked positions and measure its length across the circle as accurately as possible. -
On the Determination and Constancy of the Solar Oblateness
On the determination and constancy of the solar oblateness Mustapha Meftah, Abdanour Irbah, Alain Hauchecorne, Thierry Corbard, Sylvaine Turck-Chièze, Jean-François Hochedez, Patrick Boumier, A. Chevalier, S. Dewitte, S. Mekaoui, et al. To cite this version: Mustapha Meftah, Abdanour Irbah, Alain Hauchecorne, Thierry Corbard, Sylvaine Turck-Chièze, et al.. On the determination and constancy of the solar oblateness. Solar Physics, Springer Verlag, 2015, 290 (3), pp.673-687. 10.1007/s11207-015-0655-6. hal-01110569 HAL Id: hal-01110569 https://hal.archives-ouvertes.fr/hal-01110569 Submitted on 16 Nov 2016 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Solar Phys (2015) 290:673–687 DOI 10.1007/s11207-015-0655-6 On the Determination and Constancy of the Solar Oblateness M. Meftah1 · A. Irbah1 · A. Hauchecorne1 · T. Corbard2 · S. Turck-Chièze3 · J.-F. Hochedez1,4 · P. Boumier 5 · A. Chevalier6 · S. Dewitte6 · S. Mekaoui6 · D. Salabert3 Received: 19 November 2013 / Accepted: 21 January 2015 / Published online: 11 February 2015 © The Author(s) 2015. This article is published with open access at Springerlink.com Abstract The equator-to-pole radius difference (r = Req −Rpol) is a fundamental property of our star, and understanding it will enrich future solar and stellar dynamical models. -
Pecularities of Cosmic Ray Modulation in the Solar Minimum 23/24
PECULARITIES OF COSMIC RAY MODULATION IN THE SOLAR MINIMUM 23/24. M. V. Alania 1,2, R. Modzelewska 1 and A. Wawrzynczak 3 1 Institute Math. & Physics, Siedlce University, 3 Maja 54, 08-110 Siedlce, Poland. 2 Institute of Geophysics, Tbilisi State University, Tbilisi, Georgia. 3Institute of Computer Science, Siedlce University, 3 Maja 54, 08-110 Siedlce, Poland. [email protected], [email protected], [email protected], Abstract We study changes of the galactic cosmic ray (GCR) intensity for the ending period of the solar cycle 23 and the beginning of the solar cycle 24 using neutron monitors experimental data. We show that an increase of the GCR intensity in 2009 is generally related with decrease of the solar wind velocity U, the strength B of the interplanetary magnetic field (IMF), and the drift in negative (A<0) polarity epoch. We present that temporal changes of rigidity dependence of the GCR intensity variation before reaching maximum level in 2009 and after it, do not noticeably differ from each other. The rigidity spectrum of the GCR intensity variations calculated based on neutron monitors data (for rigidities > 10 GV) is hard in the minimum and near minimum epoch. We do not recognize any non-ordinary changes in the physical mechanism of modulation of the GCR intensity in the rigidity range of GCR particles to which neutron monitors respond. We compose 2-D non stationary model of transport equation to describe variations of the GCR intensity for 1996-2012 including the A>0 (1996-2001) and the A<0 (2002-2012) periods; diffusion coefficient of cosmic rays for rigidity 10-15 GV is increased by ~ 30% in 2009 (A<0) comparing with 1996 (A>0). -
Reconstruction of Solar EUV Flux 1840-2014
Reconstruction of Solar Extreme Ultraviolet Flux 1740–2015 Leif Svalgaard1 ([email protected]) 1 Stanford University, Cypress Hall C13, W.W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA Abstract: Solar Extreme Ultraviolet (EUV) radiation creates the conducting E–layer of the ionosphere, mainly by photo ionization of molecular Oxygen. Solar heating of the ionosphere creates thermal winds which by dynamo action induce an electric field driving an electric current having a magnetic effect observable on the ground, as was discovered by G. Graham in 1722. The current rises and sets with the Sun and thus causes a readily observable diurnal variation of the geomagnetic field, allowing us the deduce the conductivity and thus the EUV flux as far back as reliable magnetic data reach. High– quality data go back to the ‘Magnetic Crusade’ of the 1830s and less reliable, but still usable, data are available for portions of the hundred years before that. J.R. Wolf and, independently, J.–A. Gautier discovered the dependence of the diurnal variation on solar activity, and today we understand and can invert that relationship to construct a reliable record of the EUV flux from the geomagnetic record. We compare that to the F10.7 flux and the sunspot number, and find that the reconstructed EUV flux reproduces the F10.7 flux with great accuracy. On the other hand, it appears that the Relative Sunspot Number as currently defined is beginning to no longer be a faithful representation of solar magnetic activity, at least as measured by the EUV and related indices.