POLAR-ECLIPTIC PATROL (PEP) FOR SOLAR STUDIES AND MONITORING OF SPACE WEATHER
|
|
- Luke Hawkins
- 6 years ago
- Views:
Transcription
1 Proc. 2 nd International conference-exibition. Small satellities. New technologies, miniaturization. Areas of effective applications in XXI century. Section 1: Remote sensing of the Earth and space. Korolev, May 29 June 2, V.I.10. POLAR-ECLIPTIC PATROL (PEP) FOR SOLAR STUDIES AND MONITORING OF SPACE WEATHER V.D.Kuznetsov, V.N.Oraevsky IZMIRAN , Troitsk, Moscow Region Fax: (095) Abstract Two small satellites in heliocentric orbits inclined to the ecliptic plane are to be used for exploration of the Sun and monitoring of space weather in the Earth environment. The satellites achieve the inclined orbits at a distance of about 0.5 a.u. from the Sun through gravity-assisted maneuvers at the inner planets (Earth and Venus) with the aid of electric-jet engines. The orbital planes are mutually perpendicular and the satellites in orbit are spaced by a quarter of a period (the period being equal to about 130 days). This ballistic scheme ensures continuous survey of the Sun-Earth line from one, and for a considerable lapse of time from both satellites. The scheme allows exploration of the polar regions of the Sun, which are poorly seen from the ecliptic orbits. Reaching the working orbits for a reasonable time will require large energy consumption, which determines the choice of small missions with a limited set of scientific instruments. The payload of a total weight no more than 50 kg will comprise instruments for remote observations of the Sun (a combined X-ray telescope/vector-magnetograph and a coronograph or an all-sky camera) and a heliospheric complex (analyzer of solar wind and plasma particles, magnetometer, and detector of high-energy particles). Introduction Up-to-date requirements to solar observations are determined by the need for new data and the task of monitoring of the heliospheric (space) weather, which affects various aspects of human life [1]. Among these requirements, there is a possibility to observe the Sun from advantageous positions with respect to the Earth and the Sun-Earth line [2, 3]. Until now, all studies of the 3D coronal structure and solar active regions have been restricted to observations from the Earth. We do not know what the Sun and the associated disturbances and ejections look like when viewed from the poles. Observations from these new positions can provide a deeper insight into the long-existing problems, such as the global structure and evolution of the corona; triggering mechanism of coronal mass ejections; coronal heating and solar-wind acceleration; coupling between the rotation, magnetic fields, and convection in the solar interior, and the principal mechanism of generation of magnetic fields; the mechanism of acceleration of high-energy particles in solar flares and their distribution pattern; the loss rate of the solar angular momentum; etc. One of the main tasks of the space weather program [4] is to determine the fact in itself and the instant when solar heliospheric disturbances (coronal mass ejections, shock waves, etc.) arrive at the Earth. Observations in the immediate Earth environment against the bright Sun are blind to such disturbances. They can only detect active phenomena in the Sun and fix the starting time of heliospheric disturbance. Its arrival at the Earth can only be predicted with more or less confidence. A number of such predictions of different reliability were made using the
2 SOHO data. The scheme of monitoring heliospheric disturbances onboard a spacecraft (SC) situated in the ecliptic plane on one side of the Sun-Earth line [4] has a disadvantage associated with a deficit of projection of disturbances propagating in different azimuthal directions onto the Sun-Earth line. With this scheme, one can not precisely determine the heliolongitude of disturbances that propagate in the ecliptic plane; and therefore can not reliably predict their arrival at the Earth. A better result can be achieved with two SC that carry out synchronous observations in the ecliptic plane on both sides of the Sun-Earth line ( STEREO missions) providing stereo-images of heliospheric disturbances [5, 6]. Out-of-ecliptic SC offer significant advantages in determining the heliolongitude of propagation of heliospheric disturbances and monitoring the conditions along the Sun-Earth line. If only one spacecraft is used, the dead zones that appear as it crosses the ecliptic plane disrupt the continuity of regular monitoring of the Sun-Earth line. The Polar Ecliptic Patrol mission (PEP) [7] comprises two small satellites at a distance of about 0.5 a.u. from the Sun in heliocentric orbits inclined to the ecliptic plane. The orbital planes are mutually perpendicular (see Fig.); and the satellites in orbit are spaced by a quarter of a period (the period being equal to about 130 days). This ballistic scheme (see Fig.) ensures continuous survey of the Sun-Earth line from one, and for a considerable lapse of time from both satellites. When one spacecraft (SC) is in the ecliptic plane, another is over a solar pole; as one moves away from the ecliptic plane, another approaches it. Thus, the monitoring is simultaneously performed in the ecliptic and polar regions, which enables a continuous study of low- and high-speed solar wind and 3D imaging of the solar corona and ejections. Observation of solar ejections on two spaced satellites will make it possible to establish their exact propagation direction relative to the Sun-Earth line, the extension in heliolatitude and heliolongitude, and the beginning of interaction with the Earth magnetosphere. Occasionally, one of the satellites will occupy a position along the Sun-Earth line on the opposite side of the Sun with respect to the Earth. Therefore, it will be able to observe the reverse side of the Sun invisible from the Earth. When the spacecraft is behind the Sun, the information can be stored onboard and transmitted after entering the Earth view zone. On-line information can also be transmitted to the Earth through the second SC, which will be staying within view. Thus, the PEP mission will ensure continuous monitoring of solar activity and solar wind, as well as solar ejections and heliospheric disturbances moving to the Earth. Besides, it will make possible observations of the polar regions and the reverse side of the Sun. The mission will serve a significant supplement to and extension of the STEREO mission (Solar TErrestrial Relations Observatory) [6], which is under development at several space agencies. Ballistic Scheme of the Polar Ecliptic Patrol (PEP) The ballistic scheme previously developed for the Interhelioprobe ( Interhelios ) [8] can be used to achieve the working orbits. The scheme comprises two gravity-assisted maneuvers at Venus that will enable a decrease of perihelion of the heliocentric orbit and inclination of the orbital plane to the ecliptic. As shown by calculations, the maximum inclination angles that can be achieved through gravity-assisted maneuvers at the inner planets of the solar system is about 38 [9]. The use of low-thrust electrojet engines will allow us to improve the proposed ballistic scheme and reduce the travel time to the working orbits. SC orbits will be matched in phase to the Earth rotation, so as to have the best view of the Sun- Earth line and obtain stereo images by joint near-earth observations. The possibility to attain greater inclination of SC orbit (up to 90 ) depends on the development and successful trial of a new engine based on the solar sail technology [10]. As shown by preliminary estimates, a sail with a size of ~200 m 2 and a density of ~0.6 g/m 2 is
3 sufficient for the mission under consideration [10]. The capabilities of the mission can be expanded significantly by designing lightweight subsystems and instruments. Thus, the ballistic scheme proposed for the PEP mission is an optimal alternative for creating a system of continuous observation of the Sun, monitoring of solar activity, and forecasting of space weather in the Earth environment in the course of a year. Scientific objectives Out-of-ecliptic observations of the Sun, in particular, of the polar zones and active events mainly clustered towards the ecliptic plane, will allow us to make essential progress in understanding the nature of solar activity and accomplishing the task of continuous monitoring and forecast of space weather. The main objectives of the project are as follows: To study the global structure and evolution of the corona and solar wind, and to provide a 3D space-time pattern of occurrence and propagation of coronal mass ejections. To examine the magnetic field structure and convection in the polar zones of the Sun. To study the interaction between the rotation, magnetic field, and convection in the solar interior. To determine the loss of angular momentum of the Sun. To provide a space-time pattern of propagation of high-energy particles accelerated by active phenomena in the Sun.
4 To predict and register at the Earth the arrival of coronal mass ejections, shock waves, and other heliospheric disturbances. To ensure the monitoring and forecast of heliospheric (space) weather along the Earth orbit. To study the true variability of the solar irradiance. (i) Global structure and evolution of the corona and solar wind. Simultaneous in-situ measurements on two satellites at different heliolatitudes will provide a true picture of the solar wind in the vicinity of the Sun, similar to that obtained on Ulysses at large distances (~2 a.u.). Combined with remote observations of solar wind sources, these data will allow a better understanding of the solar wind acceleration mechanism, global structure, and dynamics of the solar corona and solar wind. (ii) 3D space-time pattern of the occurrence and propagation of coronal mass ejections (CME). The CME source region in the Sun is mainly confined to the belt of streamers, i.e. to a heliolongitude zone near the ecliptic plane. CMEs are detected with coronographs by a weak Thompson scattering of photospheric emission in the corona. For that reason, they are only observed in the picture plane. When looking from the Earth, this plane is perpendicular to the Sun-Earth line; and therefore, we can only detect CMEs projected onto this line, i.e. those that do not move to the Earth. Simultaneous observations from one side of the Sun-Earth line and from out-of-ecliptic positions (above and below the Sun-Earth line with respect to the ecliptic plane) will ensure two additional viewpoints. It will allow us to obtain 3D images of CMEs, their heliolatitude and heliolongitude distribution patterns, and a global picture of propagation in the heliosphere and arrival at the Earth. Thus, the high-latitude parts of SC orbits and the sectors beyond the Sun- Earth direction will give a unique possibility of continuous survey of the Sun-Earth line, i.e. we shall be able to observe the occurrence and propagation of CMEs traveling to the Earth and, hence, to predict geomagnetic storms. The remote facilities (EUV spectroscopes, imaging telescopes, and coronographs) will record the occurrence times and parameters of CMEs moving from the Sun. Plasma measurements in the Earth environment with SOHO, Cluster, ACE, or Wind-type SC will be used to identify the CME properties that have the greatest effect on the Earth. SOHO observations infer the existence of global CMEs, i.e. the events covering a significant part of the streamer belt in heliolatitude, or multiple CMEs that occur as a result of permanently recurrent CME activity in a considerable heliolatitude zone of the streamer belt. High-latitude observations will allow a detailed study and global survey of the events under consideration. Of no small importance is also the possibility to observe the dynamics of local magnetic fields responsible for the occurrence of active events, flares, ejections, etc., from the position of out-of-ecliptic SC. The magnetic poles of active regions (footpoints of magnetic loops in the photosphere) have mainly East-West orientation, so that most loops are stretched in the same direction. Thus, the out-of-ecliptic mission provides a unique possibility to observe the whole loop without the projection and side view effects that complicate diagnostics and impede determination of the exact length and true shape of the loop and the type of motion of its footpoints in the photosphere. These observations can be used to establish the triggering mechanisms of flares and ejections. (iii) Polar regions of the Sun.
5 a) Magnetic fields and convection in the polar regions of the Sun. Near the minimum of solar activity, the magnetic field poloidal component is best pronounced in the polar caps. This component is in many respects responsible for interplanetary field and constitutes an important element in understanding the solar magnetic cycle and the interaction between the rotation, magnetic field, and convection as a possible mechanism of generation of magnetic fields in the solar convection zone. SOHO helioseismologic observations show that the rotation near the poles may be slower than expected. When viewed from the Earth or from a spacecraft in the ecliptic plane, the polar regions are seen at a large angle, which severely constrains remote observations and mapping of magnetic fields. Spectroscopic and magnetographic observations on out-of-ecliptic SC will allow a better understanding of the magnetic solar cycle, structure, and dynamics of polar regions and particular phenomena, such as polar plumes, solar tornado, polar coronal holes, mass ejections, solar wind acceleration, etc. b) Polar coronal holes (CH) and high-speed streams of solar wind Crossing repeatedly the boundaries of coronal holes, the PEP mission will carry out remote and in-situ measurements in these important regions that can provide a key to understanding the CH formation, stability, and evolution. The boundaries of coronal holes separate the magnetic fields with open and closed field lines in the Sun, and the activity at these boundaries determines the evolution of coronal holes and reconstruction of the global solar magnetic field. Polar coronal holes originate high-speed solar wind that flows out to interplanetary space and controls the dynamics of the heliosphere outside the ecliptic plane. Out-of-ecliptic spectroscopy of polar coronal holes will provide a deeper insight into the occurrence of solar wind streams; and multiple crossing of CH boundaries, i.e. the high- and low-speed solar wind streams, will make it possible to study the transition region between these streams, determine their parameters, and understand the acceleration mechanisms. (iv) Propagation of high-energy particles accelerated in active events on the Sun; radiation conditions in the Earth environment. Multipositional in-situ measurements on the PEP-mission satellites at different heliolatitudes and heliolongitudes combined with remote observations of solar active events will provide a space-time propagation pattern for particles accelerated in solar flares. It will allow us to better understand the formation of radiation conditions in the Earth environment and improve their forecasting techniques. (v) Solar irradiance Observations from the Earth orbit show that solar irradiance varies by about 0.1% over a solar cycle. These variations are attributed to intensity variations of the magnetic field and their manifestations on the solar disk, sunspots, plages, etc., whose location is known to be restricted in heliolatitude. Since all available measurements of the solar constant have been made in the ecliptic plane, the true variation of the total solar irradiance (i.e. the total radiation energy emitted in all directions) over a solar cycle is still not clear. Irradiance variations of the solartype stars is by a factor of 2-3 greater than observed in the Sun. This means that either the conditions in the Sun are unbelievably stable, or the solar irradiance variations are small,
6 because observed from a specific position in the equatorial plane. A response to this question may be provided by out-of-ecliptic observations. Scientific payload To achieve these objectives, the PEP strategy must combine remote observations of the Sun, corona, and interplanetary medium with in-situ measurements of the solar wind, highenergy particles, and heliospheric magnetic field. Remote observations will provide images of the solar disk and its particular elements, solar corona, and ejections moving away from the Sun. In situ measurements will provide parameters of the solar wind (density, velocity, and composition), heliospheric magnetic field, and high-energy particles. Simultaneously, in situ diagnostics of heliospheric disturbances (shock waves, ejections, plasma streams, and highenergy particles fluxes) passing through the spacecraft will be carried out. The strategy of designing lightweight instruments for the missions of the type of Interhelios [8], NASA Polar Solar Orbiter [10], Solar Probe [11], ESA Solar Orbiter [12] and small missions for monitoring space weather [4] can be used as a basis for the PEP scientific complex. Technological requirements to the scientific equipment of small solar-heliospheric missions are set forth in [2]. They comprise: Advanced, radiation-tolerant sensors (Visible, UV, X-ray), Large format, small pixel, large dynamic range; Lightweight, ultra-low-scatter optics; Compact, high-resolution filters; Advanced grid fabrication technologies; Miniature spectral imagers; Interferometric imagers; UV and optical polarimeters. Potential instruments and their tentative parameters are listed below.
7 A 1 Instrument Imaging facilities Hard UV and X-ray telescope/ Spectrometer 2 Magnetograph 3 Coronograph or allsky camera B Heliospheric instruments LIST OF INSTRUMENTS Task, Specifications Full image of the Sun with a resolution of 1 arc.sec. per pixel or less. Mapping of magnetic fields. Field of vision 30x30 arc. min.; size of a pixel 0.5 arc. sec. Tracing mass ejections and heliospheric disturbances from the Sun up to 1 AU. A single white-light coronograph with field of vision of 360 deg. The minimum field of vision in the range of 1.5 to 20 Ro; the size of the pixel 5 arc. sec. or less. Mass Telemetry, kbit/s Consumed energy, W kev ion and 0-10 kev 4 Solar wind analyzer electron measurements, velocity distributions, mass and charge analysis. 5 Plasma wave analyzer Plasma wave measurements Magnetometer 0.1 nt 1 T magnetic field measurements Ions and electrons from 10 7 Detector of highenergy kev to 100 MeV, angle and particles energy distributions. 8 Radiospectrograph 9 Dust detector Multichannel scanning spectrometer in the range of 0.1 MHz -1 GHz Measurements of interplanetary dust particles in the range of mass of 10E-16 up to 10E-6 g TOTAL
8 Spacecraft concept The main requirements imposed on SC by the scientific complex are: stabilization in 3 axes, orientation to the Sun, short-term stabilization of 0.1 arc.sec./30 min, absolute stabilization within several arc. min. The operational parameters are close to the Helios [13] and Interhelios [8] missions. References. 1. L.J.Lanzerotti, D.J.Thomson, C.G.Maclennan. Engineering issues in space weather. Modern Radio Science, p.25, Space Physics Strategy - Implementation Study. Vol.1: Goals, Objectives, Strategy. Report of Workshop 1 January 22-26, 1990, Baltimore, Maryland. NASA, April A Crossroads For European Solar and Heliospheric Physics. Recent Achievements and Future Mission Possibilities. ESA, SP-417, June Coronal Transients and Space Weather Prediction Mission. H.D.Harris (ed.)., JPL D-12611, 15 April The Sun and Heliosphere In Three Dimensions. Report of the NASA Science Definition Team for the STEREO Mission. Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, 1 December V.M.Grigoryev, G.A.Zherebtsov, V.E.Kosenko, S.V.Kavanosyan, V.S,Konovalov, P.G.Papushev, A.V.Tsepin, V.E.Chebotarev. Development of a long-term solar stereoscopic observatory at the triangle libration points of the Sun-Earth system V1. Proc. of the 1st International Exhibition Conference "Small satellites, novel technologies, achievements, problems, and prospects for international collaboration in the new millennium", November, 16-20, 1998, Korolev, Moscow Region, v.1, issue 1, 1 p. 7. V.N.Oraevsky, V.D.Kuznetsov. International program for investigation of the Sun. Novosti cosmovavtiki, 11(178), pp.37-38, E.Marsch, A.Kogan, W.I.Axford, T.Breus, V.D.Kuznetsov, V.N.Oraevsky. Interhelios - Sun and Heliosphere Observer. Proc. of Workshop A Cross-Road for European Solar and Heliospheric Space Physics. Puerto De La Cruz, March 23-27, 1998, Tenerife, Spain, 1998, SP-417, ESA, p V.N.Oraevsky, V.D.Kuznetsov, V.I.Axford, E.Marsh, T.K.Breau, L.V.Ksanfomaliti, S.D.Kulikov, K.M.Pichkhadze, A.V.Zaitsev, G.R.Uspensky, A.V.Tselin. "Interhelios" mission for heliophysical studies. Proc. of the 1st International Exhibition Conference "Small satellites, novel technologies, achievements, problems, and prospects for international collaboration in the new millennium", November, 16-20, 1998, Korolev, Moscow Region, v.1, issue 2, 12 p. 9. R.Marsden. Solar Orbiter: A Pre-Assessment Study. Solar system News. ESA, N 24, p.6, September Sun-Earth Connection Roadmap. Strategic Planning for the Years NASA Close Encounter with the Sun. Report of the Minimum Solar Mission Science Definition Team. Scientific Rationale and Mission Concept. JPL D R.Harrisson. ESA Solar Orbiter. harrison/orbiter.html years HELIOS. Publ.Celebr. 10 th Anniversary of the Launch of HELIOS on December 10, Ed. H.Porsche. Munchen, 1984.
Sun Earth Connection Missions
Sun Earth Connection Missions ACE Advanced Composition Explorer The Earth is constantly bombarded with a stream of accelerated particles arriving not only from the Sun, but also from interstellar and galactic
More informationSOLAR ORBITER Linking the Sun and Inner Heliosphere. Daniel Müller
SOLAR ORBITER Linking the Sun and Inner Heliosphere Outline Science goals of Solar Orbiter Focus of HELEX joint mission Mission requirements Science payload Status update Top level scientific goals of
More informationSpace Physics: Recent Advances and Near-term Challenge. Chi Wang. National Space Science Center, CAS
Space Physics: Recent Advances and Near-term Challenge Chi Wang National Space Science Center, CAS Feb.25, 2014 Contents Significant advances from the past decade Key scientific challenges Future missions
More informationSolar Orbiter. T.Appourchaux, L.Gizon and the SO / PHI team derived from M.Velli's and P.Kletzkine's presentations
Solar Orbiter T.Appourchaux, L.Gizon and the SO / PHI team derived from M.Velli's and P.Kletzkine's presentations 2 nd Solar-C definition meeting, Tokyo, Japan Content Science Objectives of Solar Orbiter
More informationPossible stereoscopic Hard X-ray observations with STIX and SORENTO instruments
Possible stereoscopic Hard X-ray observations with STIX and SORENTO instruments Tomasz Mrozek 1,2 1 Space Research Centre, Polish Academy of Sciences, Solar Physics Division 2 Astronomical Institute, University
More information1 A= one Angstrom = 1 10 cm
Our Star : The Sun )Chapter 10) The sun is hot fireball of gas. We observe its outer surface called the photosphere: We determine the temperature of the photosphere by measuring its spectrum: The peak
More informationThe importance of solar wind magnetic. the upcoming Sunjammer solar sail. field observations & mission
The importance of solar wind magnetic field observations & the upcoming Sunjammer solar sail mission J. P. Eastwood The Blackett Laboratory, Imperial College London, London SW7 2AZ, UK 13 November 2013
More informationThe Solar Wind Space physics 7,5hp
The Solar Wind Space physics 7,5hp Teknisk fysik '07 1 Contents History... 3 Introduction... 3 Two types of solar winds... 4 Effects of the solar wind... 5 Magnetospheres... 5 Atmospheres... 6 Solar storms...
More informationThe 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
More informationThe Structure of the Sun. CESAR s Booklet
How stars work In order to have a stable star, the energy it emits must be the same as it can produce. There must be an equilibrium. The main source of energy of a star it is nuclear fusion, especially
More informationASPIICS: a Giant Solar Coronagraph onboard the PROBA-3 Mission
SOLI INVICTO ASPIICS: a Giant Solar Coronagraph onboard the PROBA-3 Mission Andrei Zhukov Principal Investigator of PROBA-3/ASPIICS Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium
More informationChapter 8 Geospace 1
Chapter 8 Geospace 1 Previously Sources of the Earth's magnetic field. 2 Content Basic concepts The Sun and solar wind Near-Earth space About other planets 3 Basic concepts 4 Plasma The molecules of an
More informationNASA s STEREO Mission
NASA s STEREO Mission J.B. Gurman STEREO Project Scientist W.T. Thompson STEREO Chief Observer Solar Physics Laboratory, Helophysics Division NASA Goddard Space Flight Center 1 The STEREO Mission Science
More informationOperational Aspects of Space Weather-Related Missions
Operational Aspects of Space Weather-Related Missions Richard G. Marsden, ESA/SCI-SH Outline SOHO: Example of Near-Earth Observatory-class Mission Ulysses: Example of Deep Space Monitor-class Mission Solar
More informationILWS Related Activities in Germany (Update) Prague, June 11-12, 2008
ILWS Related Activities in Germany (Update) Prague, June 11-12, 2008 ILWS, DLR, Dr. Frings Overview Update is based on previous ILWS Presentations Focus on recent developments and achievements SOL-ACES
More informationA Concept for Real-Time Solar Wind Monitor at Multiple Locations
A Concept for Real-Time Solar Wind Monitor at Multiple Locations L5 in Tandem with L1: Future Space-Weather Missions Workshop March 8 th, 2017 George C. Ho Sector Science and Space Instrumentation Branch
More informationLecture 5 The Formation and Evolution of CIRS
Lecture 5 The Formation and Evolution of CIRS Fast and Slow Solar Wind Fast solar wind (>600 km/s) is known to come from large coronal holes which have open magnetic field structure. The origin of slow
More informationINTERPLANETARY ASPECTS OF SPACE WEATHER
INTERPLANETARY ASPECTS OF SPACE WEATHER Richard G. Marsden Research & Scientific Support Dept. of ESA, ESTEC, P.O. Box 299, 2200 AG Noordwijk, NL, Email: Richard.Marsden@esa.int ABSTRACT/RESUME Interplanetary
More informationSolar-B. Report from Kyoto 8-11 Nov Meeting organized by K. Shibata Kwasan and Hida Observatories of Kyoto University
Solar-B Report from Kyoto 8-11 Nov Meeting organized by K. Shibata Kwasan and Hida Observatories of Kyoto University The mission overview Japanese mission as a follow-on to Yohkoh. Collaboration with USA
More informationSolar-terrestrial relation and space weather. Mateja Dumbović Hvar Observatory, University of Zagreb Croatia
Solar-terrestrial relation and space weather Mateja Dumbović Hvar Observatory, University of Zagreb Croatia Planets Comets Solar wind Interplanetary magnetic field Cosmic rays Satellites Astronauts HELIOSPHERE
More informationGeomagnetic Disturbance Report Reeve Observatory
Event type: Various geomagnetic disturbances including coronal hole high-speed stream, coronal mass ejection, sudden impulse and reverse shock effects Background: This background section defines the various
More informationGeomagnetic storms. Measurement and forecasting
Geomagnetic storms. Measurement and forecasting Anna Gustavsson 17 October 2006 Project of the Space Physics Course 2006 Umeå University 1 Introduction Effects of magnetic storms on technology Geomagnetic
More informationSOLAR-C Mission Option-A (Plan-A)
SOLAR-C Mission Option-A (Plan-A) H. Hara(NAOJ) JAXA SOLAR-C WG 2010 Oct 10 3 rd SOLAR-C Science Definition Meeting Interim Report SOLAR-C Concept Two options are under study: Option-A (so-called Plan-A):
More informationToward Interplanetary Space Weather: Strategies for Manned Missions to Mars
centre for fusion, space and astrophysics Toward Interplanetary Space Weather: Strategies for Manned Missions to Mars Presented by: On behalf of: Jennifer Harris Claire Foullon, E. Verwichte, V. Nakariakov
More informationOoty Radio Telescope Space Weather
Ooty Radio Telescope Space Weather P.K. Manoharan Radio Astronomy Centre National Centre for Radio Astrophysics Tata Institute of Fundamental Research Ooty 643001, India mano@ncra.tifr.res.in Panel Meeting
More informationLecture 3: The Earth, Magnetosphere and Ionosphere.
Lecture 3: The Earth, Magnetosphere and Ionosphere. Sun Earth system Magnetospheric Physics Heliophysics Ionospheric Physics Spacecraft Heating of Solar Corona Convection cells Charged particles are moving
More informationSolar Energetic Particles measured by AMS-02
Solar Energetic Particles measured by AMS-02 Physics and Astronomy Department, University of Hawaii at Manoa, 96822, HI, US E-mail: bindi@hawaii.edu AMS-02 collaboration The Alpha Magnetic Spectrometer
More informationSpace weather studies in the Russian Academy of Sciences S.A. Bogachev, V.D. Kuznetsov, L.M Zelenyi. Russian Academy of Sciences, Russian Federation
Space weather studies in the Russian Academy of Sciences S.A. Bogachev, V.D. Kuznetsov, L.M Zelenyi Russian Academy of Sciences, Russian Federation Introduction Russian Academy of Sciences (RAS) is the
More informationEFFECT OF SOLAR AND INTERPLANETARY DISTURBANCES ON SPACE WEATHER
Indian J.Sci.Res.3(2) : 121-125, 2012 EFFECT OF SOLAR AND INTERPLANETARY DISTURBANCES ON SPACE WEATHER a1 b c SHAM SINGH, DIVYA SHRIVASTAVA AND A.P. MISHRA Department of Physics, A.P.S.University, Rewa,M.P.,
More informationThe Sun. Never look directly at the Sun, especially NOT through an unfiltered telescope!!
The Sun Introduction We will meet in class for a brief discussion and review of background material. We will then go outside for approximately 1 hour of telescope observing. The telescopes will already
More informationOn 1 September 1859, a small white light flare erupted on the Solar surface
The Sun Our Star On 1 September 1859, a small white light flare erupted on the Solar surface 17 hours later Magnetometers recorded a large disturbance Aurorae were seen in the Carribean, Telegraphs went
More informationInterplanetary Field During the Current Solar Minimum
Interplanetary Field During the Current Solar Minimum C.T. Russell 1, L.K. Jian 1, J. G. Luhmann 2, T.L. Zhang 3 1 UCLA, 2 UCB, 3 SRI, OEAW SOHO 23 Understanding a Peculiar Solar Minimum Asticou Inn, Northeast
More informationRadio Observations and Space Weather Research
Radio Observations and Space Weather Research Jasmina Magdalenić Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium What is space weather and why is it important? Eruptive processes:
More informationThe Sun as Our Star. Properties of the Sun. Solar Composition. Last class we talked about how the Sun compares to other stars in the sky
The Sun as Our Star Last class we talked about how the Sun compares to other stars in the sky Today's lecture will concentrate on the different layers of the Sun's interior and its atmosphere We will also
More informationExploring the Solar Wind with Ultraviolet Light
Timbuktu Academy Seminar, Southern University and A&M College, November 19, 2003 Exploring the Solar Wind with Ultraviolet Light Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics, Cambridge,
More informationSpace Weather Activities in Switzerland
Space Weather Activities in Switzerland Margit Haberreiter PMOD/WRC, Davos, Switzerland 1 Reports Space Research in Switzerland 2012-2014 In preparation: Space Research in Switzerland 2015-2017 2 Reports
More informationAn L5 Mission Concept for Compelling New Space Weather Science
An L5 Mission Concept for Compelling New Space Weather Science RESCO (China) REal-time Sun-earth Connections Observatory INSTANT (Europe) INvestigation of Solar-Terrestrial Associated Natural Threats Ying
More informationILWS Italian SpaceAgency (ASI) Contribution
ILWS Italian SpaceAgency (ASI) Contribution Ester Antonucci Nice April 14-15 2003 ILWS Italian SpaceAgency (ASI) Contribution LWS NASA ESA SPECTRE SolarDynamicsObservatory HERSCHEL Solar Orbiter Bepi Colombo
More informationThe Interior Structure of the Sun
The Interior Structure of the Sun Data for one of many model calculations of the Sun center Temperature 1.57 10 7 K Pressure 2.34 10 16 N m -2 Density 1.53 10 5 kg m -3 Hydrogen 0.3397 Helium 0.6405 The
More informationSpace Weather and Satellite System Interaction
Space Engineering International Course, Kyutech, 4 th Quarter Semester 2017 Space Weather and Satellite System Interaction Lecture 2: Space Weather Concept, Reporting and Forecasting Assoc. Prof. Ir. Dr.
More informationAn Introduction to Space Weather. J. Burkepile High Altitude Observatory / NCAR
An Introduction to Space Weather J. Burkepile High Altitude Observatory / NCAR What is Space Weather? Space Weather refers to conditions in interplanetary space, produced by the Sun, that can disrupt
More informationThe Moon as a Platform for High Resolution Solar Imaging
The Moon as a Platform for High Resolution Solar Imaging F. Berrilli, Dept of Physics, Univ. Of Rome Tor Vergata A. Bigazzi, CE Consulting-Altran and INAF A.Ruzmaikin, N. Murphy, NASA JPL F.Manni, SRS
More informationLecture 17 The Sun October 31, 2018
Lecture 17 The Sun October 31, 2018 1 2 Exam 2 Information Bring a #2 pencil! Bring a calculator. No cell phones or tablets allowed! Contents: Free response problems (2 questions, 10 points) True/False
More informationSun-Earth Connection Missions
ACE (1997 ) Cosmic and Heliospheric Study of the physics and chemistry Advanced Composition Explorer Learning Center of the solar corona, the solar wind, http://helios.gsfc.nasa.gov/ace/ http://helios.gsfc.nasa.gov
More informationNASA s Contribution to International Living With a Star
NASA s Contribution to International Living With a Star Madhulika Guhathakurta Office of Space Science, CodeSS NASA Headquarters October 17,2002 Sun-Earth Connection (Sec) Program Planet Varying Radiation
More informationGeomagnetic Disturbance Report Reeve Observatory
Event type: Geomagnetic disturbances due to recurrent coronal hole high-speed stream Background: This background section defines the events covered. A coronal hole is a large dark region of less dense
More information1-4-1A. Sun Structure
Sun Structure A cross section of the Sun reveals its various layers. The Core is the hottest part of the internal sun and is the location of nuclear fusion. The heat and energy produced in the core is
More informationExtended Missions. Dr. Art Poland Heliophysics Senior Review Chair George Mason University
Extended Missions Dr. Art Poland Heliophysics Senior Review Chair George Mason University My Experience Experiment scientist on Skylab 1973- Experiment scientist on SMM 1980- US project Scientist for the
More informationSpace Weather. S. Abe and A. Ikeda [1] ICSWSE [2] KNCT
Space Weather S. Abe and A. Ikeda [1] ICSWSE [2] KNCT Outline Overview of Space Weather I. Space disasters II. Space weather III. Sun IV. Solar wind (interplanetary space) V. Magnetosphere VI. Recent Space
More informationLong term data for Heliospheric science Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt, MD 20771, USA
Long term data for Heliospheric science Nat Gopalswamy NASA Goddard Space Flight Center Greenbelt, MD 20771, USA IAU340 1-day School, Saturday 24th February 2018 Jaipur India CMEs & their Consequences
More informationmichele piana dipartimento di matematica, universita di genova cnr spin, genova
michele piana dipartimento di matematica, universita di genova cnr spin, genova first question why so many space instruments since we may have telescopes on earth? atmospheric blurring if you want to
More informationWhy Go To Space? Leon Golub, SAO BACC, 27 March 2006
Why Go To Space? Leon Golub, SAO BACC, 27 March 2006 Solar Observation Observation of the Sun has a long and distinguished history Especially important as calendar where e.g. seasonal monsoons produced
More informationLEARNING ABOUT THE OUTER PLANETS. NASA's Cassini spacecraft. Io Above Jupiter s Clouds on New Year's Day, Credit: NASA/JPL/University of Arizona
LEARNING ABOUT THE OUTER PLANETS Can see basic features through Earth-based telescopes. Hubble Space Telescope especially useful because of sharp imaging. Distances from Kepler s 3 rd law, diameters from
More informationThere are two more types of solar wind! The ballerina Sun right before activity minimum. The ballerina dancing through the solar cycle
There are two more types of solar wind! 3. Low speed wind of "maximum" type Similar characteristics as (2), except for Lectures at the International Max-Planck-Research School Oktober 2002 by Rainer Schwenn,
More information1.3j describe how astronomers observe the Sun at different wavelengths
1.3j describe how astronomers observe the Sun at different wavelengths 1.3k demonstrate an understanding of the appearance of the Sun at different wavelengths of the electromagnetic spectrum, including
More informationGeomagnetic Disturbances (GMDs) History and Prediction
Geomagnetic Disturbances (GMDs) History and Prediction J. Patrick Donohoe, Ph.D., P.E. Dept. of Electrical and Computer Engineering Mississippi State University Box 9571 Miss. State, MS 39762 donohoe@ece.msstate.edu
More informationSolar Wind Ion Composition Measurements: Direct Measurements of Properties of the Corona
Solar Wind Ion Composition Measurements: Direct Measurements of Properties of the Corona White Paper Submitted to the Decadal Survey Panel on Solar and Heliospheric Physics November 12, 2010 Stefano A.
More informationGuidepost. Chapter 08 The Sun 10/12/2015. General Properties. The Photosphere. Granulation. Energy Transport in the Photosphere.
Guidepost The Sun is the source of light an warmth in our solar system, so it is a natural object to human curiosity. It is also the star most easily visible from Earth, and therefore the most studied.
More informationSpace Weather Effects of Coronal Mass Ejection
J. Astrophys. Astr. (2006) 27, 219 226 Space Weather Effects of Coronal Mass Ejection K. N. Iyer 1,, R. M. Jadav 1, A. K. Jadeja 1, P. K. Manoharan 2, Som Sharma 3 and Hari Om Vats 3 1 Department of Physics,
More informationSolar eruptive phenomena
Solar eruptive phenomena Andrei Zhukov Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium 26/01/2018 1 Eruptive solar activity Solar activity exerts continous influence on the solar
More informationPayload & Data Rate for Option-A. H. Hara(NAOJ) JAXA SOLAR-C WG 2010 Mar 9
Payload & Data Rate for Option-A H. Hara(NAOJ) JAXA SOLAR-C WG 2010 Mar 9 Requirements for S/C System Design Sojourn time >40 days (TBD) for a solar latitude of >30 deg (TBD) Target of max. latitude :
More informationTHE SOLAR WIND & SOLAR VARIABILITY
The Sun-Earth System: CONTENTS AN OVERVIEW The Stars Around Us 1 Our Dependence on the Sun 3 The Sun s Inconstancy 3 Intruders from Afar 5 What Gets By 5 Voyages of Discovery in an Age of Exploration 6
More information! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun. The Sun & Solar Activity
! The Sun as a star! Structure of the Sun! The Solar Cycle! Solar Activity! Solar Wind! Observing the Sun The Sun & Solar Activity The Sun in Perspective Planck s Law for Black Body Radiation ν = c / λ
More informationThe point in an orbit around the Sun at which an object is at its greatest distance from the Sun (Opposite of perihelion).
ASTRONOMY TERMS Albedo Aphelion Apogee A measure of the reflectivity of an object and is expressed as the ratio of the amount of light reflected by an object to that of the amount of light incident upon
More informationCESAR BOOKLET General Understanding of the Sun: Magnetic field, Structure and Sunspot cycle
CESAR BOOKLET General Understanding of the Sun: Magnetic field, Structure and Sunspot cycle 1 Table of contents Introduction to planetary magnetospheres and the interplanetary medium... 3 A short introduction
More informationAIA DATA ANALYSIS OVERVIEW OF THE AIA INSTRUMENT
AIA DATA ANALYSIS OVERVIEW OF THE AIA INSTRUMENT SDO SUMMER SCHOOL ~ August 2010 ~ Yunnan, China Marc DeRosa (LMSAL) ~ derosa@lmsal.com WHAT IS SDO? The goal of Solar Dynamics Observatory (SDO) is to understand:
More informationRemote Imaging of Electron Acceleration at the Sun with a Lunar Radio Array
Remote Imaging of Electron Acceleration at the Sun with a Lunar Radio Array J. Kasper Harvard-Smithsonian Center for Astrophysics 6 October 2010 Robotic Science From the Moon: Gravitational Physics, Heliophysics
More informationSpace weather. Introduction to lectures by Dr John S. Reid. Image courtesy:
Space weather Introduction to lectures by Dr John S. Reid Image courtesy: http://www.astro-photography.com/ss9393.htm Sunspot 9393 First pass from late March to early April, 2001 See: Storms from the Sun
More informationWhat do we see on the face of the Sun? Lecture 3: The solar atmosphere
What do we see on the face of the Sun? Lecture 3: The solar atmosphere The Sun s atmosphere Solar atmosphere is generally subdivided into multiple layers. From bottom to top: photosphere, chromosphere,
More informationThe importance of ground-based observations of the solar corona
The importance of ground-based observations of the solar corona J. Burkepile 1, S. Tomczyk 1, P. Nelson 1, A.G. dewijn 1, S. Sewell 1, D. Elmore 2, L. Sutherland 1, R. Summers 1, D. Kolinski 1, L. Sitongia
More informationOutline. Astronomy: The Big Picture. Earth Sun comparison. Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned.
Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned. Next homework due Oct 24 th. I will not be here on Wednesday, but Paul Ricker will present the lecture! My Tuesday
More informationpre Proposal in response to the 2010 call for a medium-size mission opportunity in ESA s science programme for a launch in 2022.
Solar magnetism explorer (SolmeX) Exploring the magnetic field in the upper atmosphere of our closest star preprint at arxiv 1108.5304 (Exp.Astron.) or search for solmex in ADS Hardi Peter & SolmeX team
More informationSpace environment (natural and artificial) Realtime solar activity and space environment information for spacecraft operation
ISO 2008 All rights reserved ISO TC 20/SC 14 N873 Date: 2012-07-31 ISO/CDV 16709 ISO TC 20/SC 14/WG 4 Secretariat: Space environment (natural and artificial) Realtime solar activity and space environment
More informationHow is Earth s Radiation Belt Variability Controlled by Solar Wind Changes
How is Earth s Radiation Belt Variability Controlled by Solar Wind Changes Richard M. Thorne Department of Atmospheric and Oceanic Sciences, UCLA Electron (left) and Proton (right) Radiation Belt Models
More informationThe Frequency Agile Solar Radiotelescope
The Frequency Agile Solar Radiotelescope Associated Universities, Inc. National Radio Astronomy Observatory University of California, Berkeley California Institute of Technology New Jersey Institute of
More informationSolar Magnetic Fields Jun 07 UA/NSO Summer School 1
Solar Magnetic Fields 1 11 Jun 07 UA/NSO Summer School 1 If the sun didn't have a magnetic field, then it would be as boring a star as most astronomers think it is. -- Robert Leighton 11 Jun 07 UA/NSO
More informationNext quiz: Monday, October 24 Chp. 6 (nothing on telescopes) Chp. 7 a few problems from previous material cough, cough, gravity, cough, cough...
Next quiz: Monday, October 24 Chp. 6 (nothing on telescopes) Chp. 7 a few problems from previous material cough, cough, gravity, cough, cough... 1 Chapter 7 Atoms and Starlight Kirchhoff s Laws of Radiation
More information19 The Sun Introduction. Name: Date:
Name: Date: 19 The Sun 19.1 Introduction The Sun is a very important object for all life on Earth. The nuclear reactions that occur in its core produce the energy required by plants and animals for survival.
More informationSpace Weather Awareness in the Arctic. Torsten Neubert Head of Section for Solar System Physics
Space Weather Awareness in the Arctic Torsten Neubert Head of Section for Solar System Physics Technology in the Arctic There is significant potential Resources Tourism helped by receding ocean ice There
More informationSTCE Newsletter. 7 Dec Dec 2015
Published by the STCE - this issue : 18 Dec 2015. Available online at http://www.stce.be/newsletter/. The Solar-Terrestrial Centre of Excellence (STCE) is a collaborative network of the Belgian Institute
More informationIntroductory Lecture II: An Overview of Space Storms
Introductory Lecture II: An Overview of Space Storms Jan J. Sojka Center for Atmospheric and Space Science Utah State University Logan, Utah 28 July 2010 Overview Space weather and its storms. Super storms
More informationOur Dynamic Star. Dr. Katherine Auld Bentonville Public Library March 14, 2017
Our Dynamic Star Dr. Katherine Auld Bentonville Public Library March 14, 2017 Overview Basics Energy Source History Changes in the Sun Sunspots CME How do We Know? Changes on Earth Aurora Ice Ages Ocean
More informationThe Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:
The Sun Basic Properties Radius: Mass: 5 R Sun = 6.96 km 9 R M Sun 5 30 = 1.99 kg 3.33 M ρ Sun = 1.41g cm 3 Luminosity: L Sun = 3.86 26 W Effective Temperature: L Sun 2 4 = 4πRSunσTe Te 5770 K The Sun
More informationIn-Situ vs. Remote Sensing
In-Situ vs. Remote Sensing J. L. Burch Southwest Research Institute San Antonio, TX USA Forum on the Future of Magnetospheric Research International Space Science Institute Bern, Switzerland March 24-25,
More informationSolar Energetic Particles in the Inner Heliosphere
Author: Mariona Adillón Corbera Advisor: Neus Agueda Costafreda Facultat de Física, Universitat de Barcelona, Diagonal 645, 08028 Barcelona, Spain. Abstract: The upcoming missions Solar Orbiter (SolO)
More informationThe first telescopes at the lunar outpost will be observing the Sun. Ed DeLuca CfA Heliophysics Subcommittee
The first telescopes at the lunar outpost will be observing the Sun Ed DeLuca CfA Heliophysics Subcommittee Overview The need for an operational solar telescope In situ space weather forecasting / nowcasting
More informationChapter 14 Lecture. The Cosmic Perspective Seventh Edition. Our Star Pearson Education, Inc.
Chapter 14 Lecture The Cosmic Perspective Seventh Edition Our Star 14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is
More informationThe Sun sends the Earth:
The Sun sends the Earth: Solar Radiation - peak wavelength.visible light - Travels at the speed of light..takes 8 minutes to reach Earth Solar Wind, Solar flares, and Coronal Mass Ejections of Plasma (ionized
More informationThe Dancing Lights Program
The Sun Teacher Background: The Dancing Lights Program Margaux Krahe Many people think the Sun is just a fiery yellow ball. The Sun is not actually burning because fire requires oxygen. Really, the Sun
More informationSolar System Exploration in Germany
Solar System Exploration in Germany German Space Program (Key points) Formation and development of the Solar System Formation of stars and planets Comparison of terrestrial planets with Earth The Sun and
More informationInstrumentation for Interstellar Exploration
Instrumentation for Interstellar Exploration Mike Gruntman Department of Aerospace Engineering University of Southern California Los Angeles, California Houston, October 2002 World Space Congress II 1/31
More informationA NEW MODEL FOR REALISTIC 3-D SIMULATIONS OF SOLAR ENERGETIC PARTICLE EVENTS
A NEW MODEL FOR REALISTIC 3-D SIMULATIONS OF SOLAR ENERGETIC PARTICLE EVENTS Nicolas Wijsen KU Leuven In collaboration with: A. Aran (University of Barcelona) S. Poedts (KU Leuven) J. Pomoell (University
More informationHigh energy particles from the Sun. Arto Sandroos Sun-Earth connections
High energy particles from the Sun Arto Sandroos Sun-Earth connections 25.1.2006 Background In addition to the solar wind, there are also particles with higher energies emerging from the Sun. First observations
More informationMulti-wavelength VLA and Spacecraft Observations of Evolving Coronal Structures Outside Flares
Multi-Wavelength Investigations of Solar Activity Proceedings of IAU Symposium No. 223, 2004 A.V. Stepanov, E.E. Benevolenskaya & A.G. Kosovichev, eds. Multi-wavelength VLA and Spacecraft Observations
More informationRussian Federation experiments in IHY frame
Russian Federation experiments in IHY frame L.M.Zelenyi, S.I.Klimov Space Research Institute, RAS V.D.Kuznetsov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation, RAS HISTORY AND
More informationTRACE DOWNFLOWS AND ENERGY RELEASE
TRACE DOWNFLOWS AND ENERGY RELEASE Ayumi Asai (1), T. Yokoyama (2), M. Shimojo (3), R. TanDokoro (4), M. Fujimoto (4), and K. Shibata (1) (1 ) Kwasan and Hida Observatories, Kyoto University, Kyoto, 607-8471
More informationTeacher Background: The Dancing Lights Program
Teacher Background: The Dancing Lights Program The Sun Many people think the Sun is just a fiery yellow ball. The Sun isn t actually burning because fire requires oxygen. Really, the Sun a giant ball of
More informationSummer School Lab Activities
Summer School Lab Activities Lab #5: Predicting and Modeling the Arrival of the May 12 th 1997 CME In this lab we will use remote observations of the May 12, 1997 solar flare and halo CME made at and near
More informationSolar cycle variations of the energetic H/He intensity ratio at high heliolatitudes and in the ecliptic plane
Annales Geophysicae (2003) 21: 1229 1243 c European Geosciences Union 2003 Annales Geophysicae Solar cycle variations of the energetic H/He intensity ratio at high heliolatitudes and in the ecliptic plane
More informationInterplanetary coronal mass ejections that are undetected by solar coronagraphs
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2007ja012920, 2008 Interplanetary coronal mass ejections that are undetected by solar coronagraphs T. A. Howard 1 and
More information