POLAR-ECLIPTIC PATROL (PEP) FOR SOLAR STUDIES AND MONITORING OF SPACE WEATHER

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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.

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