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XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 1 The Solar Orbiter Mission: an Energetic Particle Perspective R. Gómez-Herrero, J. Rodr´ıguez-Pacheco, S. Sánchez-Prieto, M. Prieto, F. Espinosa Lara, I. Cernuda, J.J. Blanco, A. Russu, and O. Rodr´ıguez Polo Universidad de Alcala´, E-28871, Alcala´ de Henares, Spain R. F. Wimmer-Schweingruber, C. Mart´ın, S.R. Kulkarni, C. Terasa, L. Panitzsch, S.I. Böttcher, S. Boden, B. Heber, J. Steinhagen, J. Tammen, J. Köhler, C. Drews, R. Elftmann, A. Ravanbakhsh, L. Seimetz, B. Schuster, and M. Yedla Christian-Albrechts-Universita¨t zu Kiel, D-24118, Kiel, Germany G.M. Mason and G.C. Ho 7 Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA 1 0 E. Valtonen and R. Vainio 2 Department of Physics and Astronomy, University of Turku, 20014, Turku, Finland n a Solar Orbiter is a joint ESA-NASA mission planed for launch in October 2018. The science J payload includes remote-sensing and in-situ instrumentation designed with the primary goal of 5 understanding how the Sun creates and controls the heliosphere. The spacecraft will follow an 1 elliptical orbit around the Sun, with perihelion as close as 0.28 AU. During the late orbit phase the orbital plane will reach inclinations above 30 degrees, allowing direct observations of the solar ] polar regions. The Energetic Particle Detector (EPD) is an instrument suite consisting of several M sensors measuring electrons, protons and ions over a broad energy interval (2 keV to 15 MeV for electrons,3keVto100MeVforprotonsandfewtensofkeV/nucto450MeV/nucforions),providing I . composition, spectra, timing and anisotropy information. We present an overview of Solar Orbiter h fromtheenergeticparticleperspective, summarizingthecapabilitiesofEPDandtheopportunities p that these new observations will provide for understanding how energetic particles are accelerated - o during solar eruptions and how they propagate through the Heliosphere. r t s a I. THE SOLAR ORBITER MISSION • How do solar eruptions produce energetic parti- [ cle radiation that fills the heliosphere? 1 During the last decades, several space-based obser- • Howdoesthesolardynamoworkanddrivecon- v vatories have decisively contributed to improve our 7 nections between the Sun and the heliosphere? knowledge of different aspects of the Physics of the 5 Sun and the heliosphere. However, there have been 0 The third goal above is directly focused on the ori- 4 no missions before Solar Orbiter [1] and Solar Probe gin of Solar Energetic Particles (SEP). SEP events 0 Plus (SPP, [2]) specifically conceived to explore the are of great interest not only from the Space Weather . link between the Sun and the Solar wind. Solar Or- 1 point of view but also because Solar Orbiter with its 0 biter is a joint science mission between the European comprehensivesetofinstrumentswillprovideaunique 7 Space Agency (ESA) and the National Aeronautics opportunity to understand the physics of the injec- 1 and Space Administration (NASA) designed with the tion, acceleration and escape processes of energetic : primary objective of understanding how the Sun cre- v particles,whichisanimportantandubiquitousastro- i ates and controls the heliosphere. Solar Orbiter is physical process which can only be studied in situ in X the first medium-class mission of ESA’s Cosmic Vi- the heliosphere. r sion program. It is currently planned for launch in a The three-axis stabilized Sun-pointing spacecraft October 2018, carrying onboard a scientific payload (s/c) will follow an elliptical orbit around the Sun, consisting of a comprehensive set of remote-sensing with perihelion as close as 0.28 AU, allowing IS mea- (RS)andin-situ(IS)instrumentsdesignedtomeasure surements of the plasma, fields, waves and energetic fromthephotosphereintothesolarwind, workingto- particlesinaregionwheremuchofthecrucialphysics gethertoanswerfourinterdependenttop-levelscience relatedwithsolaractivitytakesplaceandisrelatively questions: undisturbed by interplanetary propagation processes [1]. Atthesametime, high-resolutionimaginginstru- • What drives the solar wind and where does the ments will permit a direct link between the IS obser- coronal magnetic field originate from? vations and the corresponding solar sources. While former pioneering missions such as Helios [3], already • How do solar transients drive heliospheric vari- explored the innermost region of the heliosphere and ability? highlighted the importance of IS measurements close eConf C16-09-04.3 2 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 Nominal mission Extended mission TABLE I: Solar Orbiter s/c key facts. 30 eg) 20 Dimensions 2.5×3.0×2.5 m3 d e ( 10 (launch configuration) d 0 u atit -10 Overall mass 1750 kg L -20 Maximum power demand 1100 W -30 Launcher Atlas V 411 (NASA) 1.0 U) 0.8 Mission operations center ESOC, Darmstadt, Germany R (A 0.6 Science operations center ESAC, Villafranca, Spain Nominal ground station Malarguë, Argentina 0.4 30/09/2018 30/09/2020 30/09/2022 30/09/2024 30/09/2026 30/09/2028 Date special scientific interest. FIG. 1: Solar Orbiter heliographic latitude (top) and he- liocentric distance (bottom) versus time. to the Sun, the lack of RS instrumentation onboard II. THE ENERGETIC PARTICLE didnotallowadetailedexplorationoftheconnections DETECTOR (EPD) SUITE between solar structures and IS observations. Duringthelateorbitphasethes/corbitalplanewill A. Key science questions reach inclinations >30 degrees above the heliographic equator,allowingdirectobservationsofthesolarpolar The inner heliosphere is filled by various energetic regions. During limited time intervals the s/c orbital particle populations of diverse origin. These popula- periodwillbeclosetothesolarrotationperiod(quasi tions include contributions from impulsive and grad- co-rotation), being able to monitor the evolution of ual Solar Energetic Particle (SEP) events accelerated the same solar region during extended periods. during solar eruptive phenomena such as flares and Solar Orbiter has been optimized in order to reuse coronal mass ejections (CMEs), from Stream Inter- designs and technology from the BepiColombo mis- action Regions (SIRs) in the solar wind, from plane- sion [4] to Mercury. A sophisticated heat shield will tarymagnetospheresandfromgalacticandanomalous protecttheconventionals/candthepayloadfromthe cosmic rays. The lowest (suprathermal) energy part intense direct solar flux when approaching perihelion. of the spectrum shows high variability and probably The two solar arrays can be tilted in order to con- includes contributions from previous SEP events and trol overheating close to the Sun. Multiple planetary from some quasi-continuous ion acceleration process gravity assist maneuvers (GAM) at Earth and Venus operating in the solar atmosphere or in the interplan- will be used in order to reach the final elliptical orbit etary medium. The EPD instrument suite onboard and to gradually increase the orbit inclination. Af- SolarOrbiterisdesignedtomeasurealltheseenergetic ter a Near Earth Commissioning Phase (NECP) and particlepopulations,fromsuprathermalenergiesupto a cruise phase lasting more than 2 years, the s/c will the lowest energy part of the galactic and anomalous start its 4-year long nominal mission phase (NMP). cosmic ray spectrum (affected by solar modulation). Thefirstperihelion<0.3AUwillbereached3.5years Solar Orbiter has been designed to provide an ef- after launch (see Figure 1). During the NMP, the ficient combination of RS and IS observations. This orbit inclination relative to the solar equator will re- meansthatEPDwillcontributetoachieveallthemis- main below 25 degrees, which will increase up to a sion science goals, however its role will be especially maximumof∼33degreesduringtheextendedmission relevanttoaddressthethirdgoal: “Howdosolarerup- phase (EMP). With the current mission schedule, the tionsproduceenergeticparticleradiationthatfillsthe maximumofsolarcycle25willbecoveredbytheNMP heliosphere?”. Thisquestioncanbebrokendowninto and EMP. Some key-facts of the s/c are summarized several key topics: in Table I. The10instrumentsthatcomprisethescientificpay- • Whataretheseedpopulationsforenergeticpar- load are summarized in Table II. RS instruments will ticles? providedataonlyduringcertaintimeintervalsofpar- ticular scientific relevance (RS windows), around per- • How and where are energetic particles acceler- ihelia and high latitude periods. IS instruments will ated at the Sun? operatecontinuously,startingatcruisephase. Instru- ments can trigger themselves autonomously to higher • How are energetic particles released from their cadencemodes(burstmode)duringlimitedperiodsof sources and distributed in space and time? eConf C16-09-04.3 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 3 TABLE II: Solar Orbiter scientific payload. Instrument Acronym Type Principal Investigator Energetic Particle Detector suite EPD IS J. Rodr´ıguez-Pacheco (Spain) Magnetometer experiment MAG IS T.S. Horbury (UK) Radio and Plasma Waves experiment RPW IS M. Maksimovic (France) Solar Wind Analyser instrument suite SWA IS C.J. Owen (UK) Extreme Ultraviolet Imager EUI RS P. Rochus (Belgium) Multi Element Telescope for Imaging METIS RS E. Antonucci (Italy) and Spectroscopy (Coronagraph) Polarimetric and Helioseismic Imager (Magnetograph) PHI RS S.K. Solanki (Germany) Solar Orbiter Heliospheric Imager SoloHI RS R.A. Howard (USA) Spectral Imaging of the Coronal Environment SPICE RS European-led (Extreme ultraviolet imaging spectrograph) facility instrument Spectrometer/Telescope for Imaging X-rays STIX RS S. Krucker (Switzerland) Suprathermalparticleswithenergiesabovetheam- bient plasma in the outer corona and the solar wind are known to play an important role as seed population for acceleration during SEP events. The variability of this seed population may be a key factor to explain the wide range of intensities and composition observed in SEP events. EPD will have the opportunity to perform IS measurements of the composition and temporal variations of the suprathermal seed population close to the Sun, contributing also to understand the origins of the suprathermal ion pool itself. Energetic particles escaping from the acceleration sites continue their propagation through the turbu- lent interplanetary magnetic field. As shown by He- FIG.2: EnergywindowscoveredbytheEPDinstruments lios observations [5], SEP events close to the Sun are for different species. much less disturbed by interplanetary transport effects compared to 1 AU observations. As the observ- ing s/c goes farther from the Sun, the interplanetary Theenergyintervalscoveredbythedifferentinstru- scattering effects become more important and often ments for various particle species are summarized in multiple injections closely spaced in time cannot be Figure 2. The four EPD sensors share a common In- resolved. For this reason, Solar Orbiter observations strument Control Unit (ICU). EPD instruments and closetotheperihelionwillbecrucialtounveilSEPin- the ICU have significant heritage from previous mis- jection, acceleration, trapping, release and transport sions, improved and optimized for the close approach processes. These observations will contribute to solve to the Sun. Figure 3 shows a picture of the whole the controversy about the SEP acceleration sites, dis- EPDinstrumentsuiteduringtheintegrationtestsper- entangling the contribution of acceleration at CME- formed in July 2016. driven shocks and at reconnection sites in solar flares or behind CMEs. The EPD sensors will measure the composition, EPD consists of four instruments measuring ener- spectra and anisotropies of energetic particles with getic electrons, protons and ions, operating at partly sufficient temporal, spectral, angular and mass res- overlapping energy ranges covering from few keV to olution to achieve the mission science goals. The ge- 450 MeV/nuc: ometric factors are scaled to avoid saturation by high particle fluxes close to the perihelia. Since Solar Or- • SupraThermal Electrons and Protons (STEP) biter is a three-axis stabilized s/c, EPD uses multiple apertures and sectoring to cover different pointing di- • Suprathermal Ion Spectrograph (SIS) rections, providing information about the directional distribution of energetic particles reaching the s/c. • Electron Proton Telescope (EPT) This information combined with the magnetic field • High Energy Telescope (HET) data will be used to obtain energetic particle pitch eConf C16-09-04.3 4 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 FIG. 5: STEP pixelated SSD. The top pixel dedicated to FIG.3: EPDinstrumentsuiteduringtheintegrationtests monitor the background produced by galactic cosmic ray performed in July 2016. andthebottom3×5pixelarrayusedtoobtaindirectional information. mented into 16 2×2 mm2 pixels (see Figure 5). One ofthesepixelsisusedtomonitorthebackgroundcon- tributionfromgalacticcosmicrays,whiletheother15 pixelscombinedwiththepinholeapertureprovidedi- rectionalinformation. TheuseofSSDswithultra-thin ohmic contacts provides high sensitivity compared to traditional electrostatic analyzers used for solar wind electron instruments. STEP is able to measure electron and ion fluxes with up to 1 s cadence. One of the unit’s sensors is equipped with a magnetic deflection system which rejects electrons, while leaving ion FIG. 4: EPD sensors fields of view. trajectories almost unaffected (see Figure 6). This unit will provide ion fluxes while the second unit will measure both, electrons and ions. The difference be- angledistributions,offundamentalimportancetoun- tween both measurements will be used to obtain the derstandtheinterplanetarypropagationofSEPs. Fig- electron flux. The nominal geometric factor of each ure 4 shows the fields of view of the different EPD STEP unit is 7.5·10−3 cm2sr. During periods with sensors in the s/c reference frame. The background very high fluxes the geometric factor can be reduced is color-coded as a function of the the interplanetary to 1.7·10−4 cm2sr by reducing the active area of the magneticfieldvectordistributionobservedbytheHe- pixels to 0.3×0.3 mm2. Monte Carlo simulations re- liosmission. ThedifferentunitswhichconstituteEPD sultsshowingtheangularresolutioncapabilitiesofthe are described in the following sections. STEP proton telescope are shown in Figure 7. B. Suprathermal Electrons and Protons (STEP) C. Suprathermal Ion Spectrograph (SIS) STEP will measure electrons and ions in the suprathermal energy range, covering 2-100 keV for SIS is a time-of-flight mass spectrometer that will electrons and 3-100 keV for protons. It has heritage measure all elements from He to Fe, sampling also from the Suprathermal Electron Instrument (STE, trans-iron elements. The energy window is species- [6]) onboard the Solar Terrestrial Relations Observa- dependent, covering between 50 keV/nuc and 14 tory (STEREO), and consists of two identical units MeV/n for CNO. The instrument design has her- sharingcommonelectronics. Bothunitshaveidentical itage from the Ultra-Low-Energy Isotope Spectrom- rectangular 54◦×26◦ fields of view, pointing sunward eter(ULEIS,[7])onboardtheAdvancedComposition alongthenominaldirectionoftheParkerspiral. Both Explorer (ACE) and the Suprathermal Ion Telescope apertures consists of a pinhole in combination with (SIT, [8]) onboard STEREO. SIS consists of two par- bafflesattheentrance. Thisconfigurationreducesthe ticle telescopes, one looking sunward along the nom- amountofstray-lightonthedetector. Eachunithasa inal Parker spiral direction and the other looking ap- singlelayerofsiliconsolid-statedetectors(SSDs)seg- proximately in the anti-sunward direction, 130◦ away eConf C16-09-04.3 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 5 particle trajectories in B=0.1T, protons at 4000eV in red, at 100keV in green, electrons at 100keV in blue 0.02 0.015 0.01 0.005 y / [m] 0 -0.005 -0.01 -0.015 -0.02 -0.01 -0.005 0 0.005 0.01 0.015 0.02 0.025 0.03 0.035 x / [m] FIG. 6: Simulation of STEP magnetic deflection system. Twopermanentmagnets(greenrectangles)effectivelyde- flectelectrons(bluetrajectories)whileprotonswithinthe instrument energy range (green and red trajectories) re- main almost unaffected. The black vertical solid lines symbolize the entrance system of STEP (aperture and pinhole). Since the deflected electrons do not cross the FIG. 8: Cross-section view of the SIS sensor. pinhole, they would stop at the entrance system. FIG.7: MonteCarlosimulationresultsoftheangularres- olution achieved by the STEP 3×5 pixelated proton detector (equipped with magnet). FIG. 9: SIS mass and energy resolution obtained using a 241Am radioactive source. from the sunward-pointing telescope. Each telescope has a conical field of view with a full aperture of 22◦ measure 3He/4He ratios with uncertainty <1%. Fig- and a nominal geometric factor of 0.2 cm2sr. Both ure 9 shows the mass and energy resolution achieved telescopes share a single electronics box. A sketch of by one of the SIS telescopes (proto flight model) ob- one of the SIS telescopes is shown in Figure 8. Time tainedduringthecalibrationtestsperformedusingan of flight information is collected when the ion passes 241Am alpha particle source. These calibration tests through the Start-1, Start-2, and Stop detector foils showedthatSISmeetsorexceedsthemissionrequire- and secondary electrons are emitted, accelerated to ments. ∼1 kV, and directed via isochronous mirrors onto mi- crochannel plate stacks. Finally, they deposit their energyintheSSDatthebackoftheinstrument. The combination of the total energy and time of fight in- D. Electron-Proton Telescope (EPT) formation permits particle identification. SIS will ac- quire data with a nominal cadence of 30 s, being able EPTwillmeasure20-400keVelectronsand20keV- to achieve 3 s during burst mode periods. The very 7 MeV protons. It has direct heritage from the So- high mass resolution of m/σ ∼ 50 will allow SIS to lar Electron and Proton Telescope (SEPT, [9]) in- m eConf C16-09-04.3 6 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 Bi-207 spectrum seen through EPT- Foil and Magnet sides 1e+07 Foil Magnet 1e+06 100000 10000 Counts/Ch 1000 481.6 keV553.8 keV 100 975.6 keV 10 1047.7 keV 1 0.1 0 200 400 600 800 1000 1200 Energy seen in Silicon detectors [channel number] FIG.10: Cross-sectionviewofanEPTdouble-endedtele- scope. FIG.11: 207Biradioactivesourcespectraobtainedbythe EPTengineeringmodel. Theelectronpeaksdisappearfor the EPT aperture equipped with a magnet, meaning that the deflection system effectively rejects electrons. strumentonboardSTEREO,usingamagnet-foiltech- niqueforparticleseparation. Eachdouble-endedEPT telescope has two closely spaced SSDs operating in the Mars Science Laboratory (MSL). HET consists anti-coincidence. As shown in Figure 10, one SSD of two double-ended sensor heads, one pointing sun- looks through a polyimide foil while the second SSD ward and anti-sunward along the nominal Parker spi- looks through a magnetic deflection system. The ral, the other pointing above and below the orbital foil stops low-energy protons while leaving electrons plane. Thus, HET has a total of four viewing direc- mostly unaffected. The magnet system effectively tions (analogous to EPT, see section IID and Figure deflects electrons leaving protons unaffected. Since 4). Both HET sensors are identical and consist of a the magnets corresponding to each pair of double- double-ended set of SSDs and a a high-density Bis- ended telescopes are closely placed together and form muthGermanate(BGO)calorimeterscintillator(Fig- a compensating pair of dipoles, the long-range field ure12). EachdoubleHETsensorunitsharestheelec- is strongly attenuated, minimizing the disturbance of tronic box with an EPT unit. HET allows separation the measurements by the magnetometer onboard So- of the helium isotopes down to a 3He/4He isotope ra- lar Orbiter. Figure 11 shows EPT engineering model tio of about 1% in a limited energy range. Figure 13 calibration results with a 207Bi radioactive source showMonteCarlosimulationresultsillustratingHET demonstrating the effective rejection of electrons by response to heavy ions, light ions and electrons. HET the magnet system. There are two EPT units, each has a conical field of view with a full aperture of 43◦ one consisting of two double-ended telescopes. This and a nominal geometric factor of 0.27 cm2sr. The setupprovidesatotaloffourviewdirections. Thefirst front detectors of HET (both sides) are protected by EPT unit apertures point along the nominal Parker laminated Kapton+Al foil (Kapton is 50 µm and Al spiral in sunward and anti-sunward direction. The is 25 µm thick) to reduce low energy particle flux. second unit apertures point 56◦ above and below the In addition, the front detector is divided into concen- orbital plane. The electronics box of each EPT unit tricsegmentsthatallowthereductionofprotoncount is shared with a HET unit. Each EPT aperture has rates during high intensity events. In such situations, a conical field of view with a full aperture of 30◦ and the thresholds on the larger segment are increased to a nominal geometric factor of 0.01 cm2sr. The maxi- beyond the energy deposit of protons. This scheme mum time cadence is 1 s. retains the detection power for the much rarer heavy ionswhilereducingthecountingratefortheabundant protons. The maximum instrument cadence is 1 s. E. High Energy Telescope (HET) HET covers the energy range, which is of specific F. Instrument Control Unit (ICU) interest for space weather, and will perform the measurements needed to understand the origin of high- The ICU provides a single point of connection be- energy SEP events at the Sun. HET will measure tweenthes/candallthe EPD sensors, actingas data electronsbetween300keVand15MeV,protonsfrom and power interface. It is composed of the Common 10 to 100 MeV and ions from 20 MeV/nuc to 450 Data Processing Unit (CDPU) and the Low Voltage MeV/nuc(theexactintervalisZ-dependent,see[10]). Power Supply (LVPS). The ICU shares information Incident particles will be identified using the dE/dx with other EPD instruments to allow synchronized vs. total energy technique. It has heritage from the burst-mode operations following on-board identifica- Radiation Assessment Detector (RAD, [11]) onboard tion of predefined triggering events in the EPD data. eConf C16-09-04.3 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 7 mented in a RTAX2000 FPGA from Actel, it contains external RAM, EEPROM and PROM memo- ries, two hot redundant SpaceWire interfaces, and fouridenticalseriallinks(UART-LVDS)withthesen- sors. The CDPU PROM contains the boot code and itcanbeusedtoloadflightcodefromeithertheEEP- ROM,thatcontainstwocopiesoftheapplicationsoft- ware, orfromthes/cinterfaceviatelecommand. The LVPS board is responsible for filtering, monitoring andswitchingthes/cprimarypower. Italsoprovides the power supply to both CDPUs. FIG. 12: Cross-section view of a HET double-ended telescope. NotethelargeBGOscintillatorlocatedinthecen- G. EPD data products ter and the two SSDs located at both sides. EPD has a total telemetry budget of 3600 bit/s (housekeeping + science data). Solar Orbiter telemetry rate is highly variable during the orbit. This implies that data will be downliked to ground with strongly varying latencies of up to several months. A minimal set of science data from all the instruments willbedownlinkeddaily(lowlatencydataset),mainly for planning/monitoring purposes, but also with scientific value. In order to optimize the science return fulfillingtelemetrylimitations, EPDsciencedatasent togroundwillvarydependingonradialdistance,hav- ing higher cadences close to the perihelia. Following in-orbit commissioning, the Principal In- vestigators of the different instruments onboard Solar Orbiterretainexclusivedatarightsforthepurposeof calibrationandverificationforaperiodof3monthsaf- terthereceiptoftheoriginalsciencetelemetry. Upon delivery of data to the ESA Science Operations Cen- ter, they will be made available to the scientific com- munitythroughtheESAsciencedataarchive. Thein- strumentteamswillproviderecordsofprocesseddata with all relevant information on calibration and instrument properties to the ESA science data archive, which will be the repository of all mission products [14]. Solar Orbiter’s IS instruments will provide pro- cessed data using the Common Data Format (CDF) FIG.13: MonteCarlosimulationresultsofHETresponse tolightionsandelectrons(top)andheavyions(bottom). standard. EachplotshowstheproductoftheenergylossintheSSD and the total energy versus their ratio. III. MULTIPOINT OBSERVATION OPPORTUNITIES The ICU has strong architecture heritage from the CommonDataProcessingUnit(CDPU)fortheCom- Solar Orbiter will offer excellent opportunities for prehensive Suprathermal and Energetic Particle An- multi-point observation campaigns combining mea- alyzer (COSTEP, [12]) and the Energetic and Rel- surements by multiple s/c. Synergies with the SPP ativistic Nuclei and Electron (ERNE, [13]) instru- mission are of particular relevance, since both mis- ments onboard the Solar and Heliospheric Observa- sions have overlapping timelines and the SPP perihe- tory (SOHO). The ICU is designed to manage sen- lion,reachingupto<10solarradii,willpermitISob- sor’s control and monitoring, timing clock, and data servations at the SEP acceleration region close to the collection, compression, and packetization for teleme- Sun simultaneous to ISmeasurementsat larger radial try. ICU is also responsible for the s/c telecommand distances and with continuous RS coverage provided receptionanddeliverytothesensorsifnecessary. The by Solar Orbiter and near-Earth s/c. Certain geo- CDPU in based on a LEON2 soft-processor imple- metric configurations will be particularly appropriate eConf C16-09-04.3 8 XXV European Cosmic Ray Symposium, Turin, Sept. 4-9 2016 formulti-pointmeasurementsinordertooptimizethe IV. SUMMARY AND CONCLUSIONS science return: Solar Orbiter is a unique mission conceived to un- • Close approaches of Solar Orbiter to SPP or veil the Sun-heliosphere connection. The orbital con- other s/c providing the opportunity for cross- figuration includes a close perihelion, high inclination calibration of the particle instruments onboard. intervals allowing the observation of the solar polar • Radial alignments enabling the observation of regions and quasi-co-rotation periods. These orbital plasma“packets”fromthesamesolarsourcere- characteristics are combined with a comprehensive gion at progressive radial distances as well the combination of IS and RS instruments and excellent study of energetic particle radial gradients. opportunities for multi-s/c studies. The EPD suite will provide high-quality energetic particle observa- • Alignments along the same interplanetary mag- tions over a wide energy range and multiple species, netic field line allowing the observation of SEPs key to understand the seed populations, injection, ac- originating at the same acceleration site by two celeration and transport processes of SEPs. ormores/clocatedatdifferentradialdistances. • Combination of RS observations of near-limb source regions and IS plasma observations by s/c with angular separations close to 90◦. Acknowledgments • Observations of SEP events by multiple s/c covering wide angular regions (both, in longi- The authors acknowledge the financial support of tude and latitude) in order to investigate the theSpanishMINECOunderprojectsESP2013-48346- spatial distribution of SEPs and the physical C2-1-R and ESP2015-68266-R (MINECO/FEDER). mechanismsproducingwide-spreadSEPsevents SIS was funded by ESA as a European-led facility in- (see e.g. [15, 16]). These observations will strument. CAU acknowledges the financial support help to understand the possible role played by from the German space Agency (DLR) under grants interplanetary cross-field diffusion, acceleration 50OT1002 and 50OT1202 and by the University of at wide shocks and distorted coronal magnetic Kiel. fields with large latitudinal/longitudinal devia- tions from the radial direction. [1] D. Mu¨ller, R. G. Marsden, O. C. St. Cyr, and H. R. L.Duvet,T.Sanderson,B.Butler,B.Johlander,and Gilbert, Solar Physics 285, 25 (2013), 1207.4579. H. Smit, Space Science Reviews 136, 363 (2008). [2] N.J.Fox,M.C.Velli,S.D.Bale,R.Decker,A.Dries- [10] J. Tammen, R. Elftmann, S. R. Kulkarni, S. I. man, R. A. Howard, J. C. Kasper, J. Kinnison, Bo¨ttcher,andR.F.Wimmer-Schweingruber,Nuclear M. Kusterer, D. Lario, et al., Space Science Reviews InstrumentsandMethodsinPhysicsResearchB360, 204, 7 (2016). 129 (2015). [3] H. Porsche, Journal of Geophysics Zeitschrift Geo- [11] D. M. Hassler, C. Zeitlin, R. F. Wimmer- physik 42, 551 (1977). Schweingruber, S. Bo¨ttcher, C. Martin, J. Andrews, [4] J. Benkhoff, J. van Casteren, H. Hayakawa, M. Fuji- E.Bo¨hm,D.E.Brinza,M.A.Bullock,S.Burmeister, moto, H. Laakso, M. Novara, P. Ferri, H. R. Middle- et al., Space Science Reviews 170, 503 (2012). ton, and R. Ziethe, Planetary and Space Science 58, [12] R. Mu¨ller-Mellin, H. Kunow, V. Fleißner, E. Pehlke, 2 (2010). E. Rode, N. Ro¨schmann, C. Scharmberg, H. Sierks, [5] G. Wibberenz and H. V. Cane, Astrophys. J. 650, P. Rusznyak, S. McKenna-Lawlor, et al., Solar 1199 (2006). Physics 162, 483 (1995). [6] R.P.Lin,D.W.Curtis,D.E.Larson,J.G.Luhmann, [13] J. Torsti, E. Valtonen, M. Lumme, P. Peltonen, S.E.McBride,M.R.Maier,T.Moreau,C.S.Tindall, T. Eronen, M. Louhola, E. Riihonen, G. Schultz, P. Turin, and L. Wang, Space Science Reviews 136, M.Teittinen,K.Ahola,etal.,SolarPhysics162,505 241 (2008). (1995). [7] G.M.Mason,R.E.Gold,S.M.Krimigis,J.E.Mazur, [14] R. Marsden, Tech. Rep., European Space Agency G. B. Andrews, K. A. Daley, J. R. Dwyer, K. F. (SOL-EST-PL-00880) (2012). Heuerman,T.L.James,M.J.Kennedy,etal.,Space [15] D. Lario, A. Aran, R. Go´mez-Herrero, N. Dresing, Science Reviews 86, 409 (1998). B. Heber, G. C. Ho, R. B. Decker, and E. C. Roelof, [8] G. M. Mason, A. Korth, P. H. Walpole, M. I. De- Astrophysical Journal 767, 41 (2013). sai, T. T. von Rosenvinge, and S. A. Shuman, Space [16] N.Dresing,R.Go´mez-Herrero,B.Heber,A.Klassen, Science Reviews 136, 257 (2008). O.Malandraki,W.Dröge,andY.Kartavykh,Astron- [9] R. Mu¨ller-Mellin, S. Bo¨ttcher, J. Falenski, E. Rode, omy & Astrophysics 567, A27 (2014). eConf C16-09-04.3