Session 12 - Enhanced Space Weather Monitoring System (LAGRANGE MISSIONS & D3S)

Stefan Kraft (ESA - ESOC); Steven W. Clarke (NASA)
Thursday 30/11, 9:45 - 13:00
Permeke


KEYWORDS - instruments, hosted payloads, satellite systems, distributed SWE sensor system, Lagrange missions

Observation of the Sun’s activity and its interaction with the Earth is of vital interest to mankind since it enables awareness of space weather conditions and permits assessment, forecasting and the mitigation of potential hazardous impacts on ground based, airborne and space borne sensitive infrastructure. ESA and its partners are working on the realisation of an enhanced and more comprehensive observational system that is expected to enable future improved services with longer warning times, better understanding and modelling of the environment. The foreseen measurement system is based on 3 elements namely (1) Ground Observations, (2) a Distributed Space Weather Sensor System (D3S), and (3) satellite systems positioned in the Lagrange points L1 and L5. In this session we call for submissions related to developments and studies underway for Space Weather Missions either positioned in L1 and/or L5 or in the Earth environment. Topics are therefore mission concepts, satellite systems, instrumentation and related precursors that are suitable to become part of a future operational enhanced space weather monitoring system. In order to stimulate and foster collaborations, we invite also contributions from our international partners.

Poster Viewing
From Thursday morning to Friday noon

Talks
Thursday November 30, 09:45 - 11:00, Permeke
Thursday November 30, 11:45 - 13:00, Permeke

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Talks : Time schedule

Thursday November 30, 09:45 - 11:00, Permeke

09:45	Enhanced Space Situational Awareness from L5	Glover, A et al.	Invited Oral
	Alexi Glover, Stefan Kraft, Juha-Pekka Luntama
	ESA Space Situational Awareness Programme Office, ESA/ESOC, Darmstadt, Germany
	The SSA Programme’s Space Weather Segment is developing a system capable of providing timely and reliable space weather services to a range of end users working in domains ranging from spacecraft operation through to power grid operation. In order to provide key data which will enable critical user-driven services, a range of measurement systems are being developed. The objective of the mission to L5 currently under study is to maintain and enhance observational capabilities necessary to monitor and predict space weather conditions. This will be done through a combination of remote sensing and in-situ measurements, with measurements selected based on their expected utilisation in a service capacity. As such, the resulting data are expected to enable substantial improvement in the operational space weather applications and services which can currently be provided to end users. This presentation will address the L5 mission requirements, and discuss these in the context of anticipated improvements to and opportunities for space weather service provision.
10:05	A remote-sensing package for ESA’s enhanced space-weather monitoring system	Davies, J et al.	Oral
	Jackie Davies[1], Paul Eccleston[1], Richard Harrison[1], Ian Tosh[1], David Berghmans[2], Matthew West[2], Jean-Herve Lecat[3], Peter Barthol[4], Achim Gandorfer[4], Sami Solanki[4]
	[1]STFC-RAL Space, UK; [2]ROB, Belgium; [3]CSL, Belgium; [4]MPS, Germany
	Continuous monitoring is crucial in providing awareness of conditions on the Sun and in the solar wind that could result in detrimental space-weather effects on ground-based, airborne and space-based infrastructure; such monitoring permits the potential mitigation of space weather effects. To this end, ESA and its partners are working on the realization of an enhanced space-weather monitoring system that would potentially include spacecraft at the L1 and/or L5 Lagrangian points. It is envisaged that these Lagrangian spacecraft would provide a complement of both remote-sensing observations and in-situ measurements for operational space-weather usage. In terms of the former, it is suggested that the highest-priority observations comprise visible-light imaging of the outer corona and heliosphere, extreme-ultraviolet (EUV) imaging of the chromosphere and/or low corona, and magnetic mapping of the solar photosphere. Such observations would be realized by an operational coronagraph, heliospheric imager, EUV imager and magnetograph, respectively. The raising of these instruments to technology readiness level (TRL) 6 is the subject of a phase A/B1 study recently initiated under the Lagrangian element of ESA’s Space Situational Awareness programme. Here, we present an assessment of the observational requirements for such instruments and, based on consideration of current operational and scientific instrumentation, either under development or in flight, present a roadmap to achieving the required TRL. The instruments under consideration include, amongst others, the Solar Coronagraph for Operations (SCOPE), the EUV Solar Imager for Operations (ESIO), the Extreme Ultraviolet Imager (EUI) and Polarimetric and Helioseismic Imager (PHI) instruments on ESA’s Solar Orbiter mission, due for launch in 2019, and the Heliospheric Imager (HI) instruments that have been operating successfully for the last decade on NASA’s STEREO mission.
10:25	In-situ environment monitoring by space weather missions to the Sun-Earth Lagrange points	Kataria, D et al.	Oral
	Dhiren Kataria
	Mullard Space Science Laboratory, Department of Space and Climate Physics, University College London, Holmbury St. Mary, Dorking Surrey RH5 6NT
	In-situ monitoring of the magnetic, plasma and radiation environment of interplanetary space is essential for any advanced space-weather early warning system. Near real-time measurements from well-chosen locations are extremely valuable in alerting satellite operators and utility providers on Earth when there is an increased risk of hazards from geomagnetic storms and other space weather effects. Interplanetary phenomena of interest include, but are not limited to, high speed solar wind streams, stream interaction regions, solar energetic particle events and interplanetary coronal mass ejections. Towards this goal, the European Space Agency initiated assessment studies for space weather monitoring missions to the L1 and L5 Solar Lagrangian points within its Space Situational Awareness (SSA) Programme. Pre-Phase A mission studies have already been completed and Phase A/B1 studies are now in preparation, probably with a growing emphasis towards space weather monitoring from an L5 mission. In order to provide effective forecasts and warnings, such missions are expected to carry an in-situ instrument suite to measure the energetic particle environment, bulk solar wind conditions, solar X-ray emissions and the interplanetary magnetic field. We discuss science and measurement requirements for space weather monitoring missions at L1 and L5, including operational needs and key challenges for reliable in-situ environment monitoring. We also highlight the value of joint measurements at both L5 and L1 for improving existing models of the inner heliosphere that will, in turn, improve space weather prediction capabilities. Finally, we will present a brief overview of the types of instruments and techniques available for such a mission.
10:45	A Wide-Field Coronal EUV Imager-Spectrometer for Improved Space Weather Forecasting	Golub, L et al.	Oral
	Leon Golub
	Harvard-Smithsonian Center for Astrophysics
	We have designed a novel wide field, dual-use EUV imager to observe the dynamics of solar coronal streamers and other large-scale structures from the solar surface out to at least ~3 R_sol. The COSIE instrument is proposed with the objectives of: 1.) understanding the dynamics of the Transition Corona, the region of the upper corona in which the plasma beta changes from low to high and the atmosphere transitions from being dominated by magnetically confined closed structures to high beta with generally open radially-directed regions with outflowing solar wind streams, and 2.) providing new tools for space weather forecasting via early detection of coronal mass ejections (CMEs), tracking of CMEs during their main acceleration phase and early path changes, and modeling of the CME magnetic configuration at event initiation. The imaging channel has ~1,000X greater sensitivity than existing EUV imagers and is capable of detecting streamers out to at least 2.5 R_sol and CMEs to substantially greater distances. A novel feature of COSIE is that the observing mode is switchable between ultra-high sensitivity direct EUV imaging and a global spectroscopic imaging mode. The overlapped spectra can be unfolded to provide spectral resolution of 20,000 over the 185-206Å passband covering a wide coronal temperature range, as well as providing full-Sun density images every 10 seconds. This presentation will introduce the COSIE concept and address uses of global EUV spectra in the study of coronal heating and dynamics. The sensitivity and field of view of the design are flexible and many observing locations are feasible, including L1, L4 and L5.

Thursday November 30, 11:45 - 13:00, Permeke

11:45	ASHI: An All Sky Heliospheric Imager for Viewing Thomson-Scattered Light	Jackson, B et al.	Oral
	Bernard V. Jackson[1], Andrew Buffington[1], Hsiu-Shan Yu[1], P. Paul Hick[1], and Mario M. Bisi[2]
	[1]University of California, San Diego, United States; [2]Science and Technology Facilities Council - Rutherford Appleton Laboratory, United Kingdom
	We have developed, and are now funded by NASA to ready for flight an All-Sky Heliospheric Imager (ASHI) for future missions. ASHI’s principal objective is a precision photometric map of the inner heliosphere from deep space. The zodiacal-light photometers on the twin Helios spacecraft, the Solar Mass Ejection Imager (SMEI) on the Coriolis satellite, and the Heliospheric Imagers (HIs) on the Solar-TErrestrial RElations Observatory (STEREO) twin spacecraft, all point the way towards an optimum instrument for visible light Thomson-scattering observations. The system we have designed includes viewing the whole sky starting beyond a few degrees of the Sun, and covering a hemisphere or more of sky. A key photometric specification for ASHI is 0.1% differential photometry which enables the 3-D reconstruction of density starting from near the Sun and extending outward. SMEI analyses have demonstrated the success of this technique: when employed by ASHI, this will provide an order of magnitude better resolution in three dimensions over time. As a new item we include velocity in this concept, and for a heliospheric imager in deep space, the ability to provide both high-resolution comparisons of in-situ plasma density and velocity measurements obtained at the spacecraft to solar wind structures observed remotely. In practice we find that 3-D velocity determinations allow a better-timing depiction of heliospheric structures, especially those that are not Earth directed, and we discuss the simple concept behind this as well as the instrument development progress, characteristics, and specifications to date.
12:05	Small Satellite Constellation for ESA's Distributed Space Weather3S	Gardosi, F et al.	Oral
	Federico Gardosi, Nicolas Faber, Hubert Moser, Pierre Morin, Marino Poppé
	LuxSpace SARL
	Within ESA's SSA programme, there is a preliminary architecture for an Enhanced Space Weather Monitoring System (ESWMS). ESWMS is a system of systems made up of deep space probes, most likely at L1 and/or L5, and a Distributed Space Weather Sensor System (D3S) located in Earth proximity. D3S in turn consists of a distributed network of monitoring nodes either located on ground, or flying onboard large spacecraft as hosted payloads, or flying as part of a dedicated small satellite system. This contribution presents a mission design for the dedicated small satellite system of D3S. The goal is to place half a dozen of microsatellites in two low Earth elliptic orbits with apogees placed in a way to constantly monitor the Sun interaction with the Earth geomagnetic poles. Thanks to the properties of the elliptic orbits, the altitude of the apogee and the perigee allow to implement two different approaches for remote sensing the aurorae both in UV and in the visible range of the electromagnetic spectrum. Simultaneous monitoring of North and South pole aurorae also allows the study of possible correlations between opposite pole aurorae. On top of the aurorae monitoring, the implemented mini-constellation will also perform a wide range of in-situ measurements in Earth’s vicinity: measuring the Magnetic Field and Micro Particle environment, for higher altitudes, and Atomic Oxygen for the lower ones. The orbit will be maintained once per day to allow the constellation to provide constant service for three years of mission lifetime. To have a timely SWE forecasting service, one of the mission requirements is to guarantee a data timeliness of a few minutes only. This calls for an innovative solution for the ground segment and the communications architecture of the mission, possibly including GEO or MEO data relay systems.
12:25	SMILE: A Novel and Global Way to Explore Solar-Terrestrial Relationships	Branduardi-raymont, G et al.	Oral
	Graziella Branduardi-Raymont[1], Chi Wang[2], Steve Sembay[3], Lei Dai[2], Lei Li[2], Eric Donovan[4], Tianran Sun[2], Dhiren Kataria[1], Rumi Nakamura[5], Huigen Yang[6], Andrew Read[3], Emma Spanswick[4], David Sibeck[7], Kip Kuntz[8], Philippe Escoubet[9], David Agnolon[9], Walfried Raab[9], Jianhua Zheng[2]
	[1]Mullard Space Science Laboratory – UCL, Holmbury St Mary, United Kingdom; [2]National Space Science Center – CAS, Beijing, China; [3]University of Leicester, Leicester, United Kingdom; [4]University of Calgary, Calgary, AB, Canada; [5]IWF, Austrian Academy of Sciences, Graz, Austria; [6]Polar Research Institute of China, Shangai, China; [7]NASA Goddard Space Flight Center, Greenbelt, MD, USA; [8]Johns Hopkins University, Baltimore, MD, USA; [9]European Space Technology Centre, Noordwijk, The Netherlands
	SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) aims to investigate the dynamic coupling of the solar wind with the Earth’s magnetosphere in a novel and global manner. From a highly elliptical Earth polar orbit, SMILE will combine charge exchange soft X-ray imaging of the Earth’s magnetic boundaries and polar cusps with simultaneous UV imaging of the northern aurora, while measuring solar wind/magnetosheath plasma and magnetic field conditions in situ. SMILE is a scientific precursor of space weather operational satellites which are expected to forecast the arrival and impact of solar storms on the terrestrial environment. SMILE does not provide forecasting capabilities, rather its measurements will inform the science underpinning our still limited understanding of space weather and its fundamental drivers. For the first time we will be able to trace and link the processes of solar wind injection in the magnetosphere with those acting on the charged particles precipitating into the cusps and eventually creating the aurora. SMILE is a joint mission between the European Space Agency and the Chinese Academy of Sciences, due for launch at the end of 2021. This presentation will cover the science that SMILE will deliver and its impact on our understanding of the way the solar wind interacts with the Earth’s environment; it will provide an overview of SMILE’s payload and mission and demonstrate the scientific potential of SMILE through simulations of the data that it will return.
12:45	Ground Level Event Monitor – an energetic particle instrument in interplanetary medium	Heber, B et al.	Oral
	Heber, B.[1], Casolino, M.[2], Blanco Avalos, J.[3], Wimmer-Schweingruber, R.[1]
	[1]Christian-Albrechts-Universität Kiel, Leibnizstr. 11, 24118 Kiel, Germany; [2]Department of Physics University of Rome Tor Vergata Scientifica 1, Via della Ricerca 00133 Rome,Italy; [3]Department of Physics and Mathematics, Universidad de Alcalá, DP28871 Alcalá de Henares,Madrid, SPAIN
	Deploying a mission at Sun-Earth L5 and/or L4 has several key benefits for heliophysics, especially on magnetic structures inside and outside the solar surface. Among others energetic particle detection at multiple locations (L5 in combination with L1 and/or L4) is essential in gaining insight into the widespread nature of Solar Energetic Particle (SEP) events, especially in the energy range from 300 MeV to 2 ~GeV that was not measured by STEREO. Recently it has been shown by Kühl et al. (2015, 2016, 2017) that a simple solid state detector telescope like the Electron Proton Helium INstrument (EPHIN) consisting out of a set of silicon detectors is capable to measure the proton spectra to above 800 MeV. However, a discrimination against SEP electrons is impossible leading to too hard proton spectra above 600 MeV. Among others like the missing pitch angle coverage this hinders a reasonable modeling of SEP events through the Earth magneto- and atmosphere in order to understand Neutron Monitor measurements. One way to avoid such contamination is to implement an aerogel Cherenkov detector as realized by the Ulysses COSPIN Kiel Electron Telescope. Further improvements would rely on the dE/dx-Cherenkov method as has been realized by the Helios E6 instrument. In this contribution the three above mentioned instruments and their measurement capabilities as well as the consequence for an energetic particle instrument for future missions are discussed.

Posters

1	Development of a miniaturised energetic particle detector for Space Weather applications	Bogdanova, Y et al.	p-Poster
	Yulia Bogdanova[1], Nicola Guerrini[2], Simon Woodland[1], Henrique Araujo[3], Rain Irshad[1], Doug Griffin[4], Eamonn Daly[5]
	[1]STFC Rutherford Appleton Laboratory, RAL Space, Harwell, Oxford, OX11 0QX, UK; [2]STFC Rutherford Appleton Laboratory, Technology Department, Harwell, Oxford, OX11 0QX, UK; [3]Imperial College London, High Energy Physics, Blackett Laboratory, London SW7 2BZ, UK; [4]UNSW Canberra, School of Engineering and IT, Campbell, ACT 2612, Australia; [5]European Space Agency, Space Environments and Effects Section, ESTEC, 2200 AG, Noordwijk, The Netherlands
	Energetic particles in the near-Earth space, i.e. within Solar Energetic Particle events (SEP) and inside radiation belts, are of crucial importance for Space Weather research and operations. These measurements are required in order to monitor the health of the spacecraft itself and to mitigate technological effects of Space Weather, which are damaging to the satellite electronics and human health. It is important to monitor the energetic particle population over extended energy range, as different populations are causing different effects, i.e., keV electrons causing surface charging, keV-MeV electrons causing internal charging and MeV-GeV ions causing single event effects. Provision of energetic particle data is required by many customers and such measurements are necessary on L1/L5 SWE missions, on the GEO telecommunication satellites and EP orbit raising and on the D3S systems. Here we report on the status of a miniaturised energetic particle detector, the Highly Miniaturised Radiation Monitor (HMRM), which is under development at the STFC. The instrument is based on the use of bespoke application-specific CMOS Active Pixel Sensors. This technology was selected in order to reduce the noise of the signal, as well to simplify data processing and minimize mass and volume of the instrument. The instrument concept comprises a telescopic configuration of active pixel sensors enclosed in a titanium shield, with an estimated total mass of 100-200g. The detector is designed as a real-time radiation monitor which provides additional scientific data sets, such as reconstructed spectra of high-energy particle population, with energy coverage of 35 keV – 6 MeV for electrons and 600 keV – 500 MeV for protons. A descoped version of the HMRM instrument is flying on the UK TechDemoSat-1. In this paper, we present the initial concept of the instrument, discuss development progress, present the results of the instrument calibrations and tests, including tests with radiation sources, and discuss potential ways forward in the development of miniaturised energetic particle sensors.
2	The Worldwide Interplanetary Scintillation (IPS) Stations (WIPSS) Network as a Future Worldwide Space-Weather Instrument	Bisi, M et al.	p-Poster
	Mario M. Bisi[1], J. Americo Gonzalez-Esparza[2,3,4], Bernard V. Jackson[5], Hsiu-Shan Yu[5], Munetoshi Tokumaru[6], Igor Chashei[7], Sergey Tyul’bashev[7], Richard A. Fallows[8], Periasamy K. Manoharan[9], Ernesto Aguilar-Rodriguez[2,3,4], Oyuki Chang[4], Dusan Odstrcil[10,11], David F. Webb[12], Vladimir Shishov[7], and David Barnes[1].
	[1]STFC-RAL Space, UK; [2]SCiESMEX, MX; [3]MEXART, MX; [4]UNAM, MX; [5]CASS-UCSD, CA, USA; [6]ISEE, Nagoya University, Japan; [7]Pushchino Radio Observatory, Russia; [8]ASTRON, NL; [9]TIFR, Ooty, India; [10]GMU, VA, USA; [11]NASA GSFC, MD, USA; [12]Boston College, MA, USA.
	Interplanetary Scintillation (IPS) allows for the determination of velocity and a proxy for plasma density to be made throughout the corona and inner heliosphere. It also provides signs of field rotation somewhere along the line of sight. IPS has been in use for over half a century and is a technique that can be implemented for space-weather purposes as a standalone technique and also as a complementary technique to space-based assets and in various forms of space-weather modelling. IPS occurs due to density variations and turbulence throughout the inner heliosphere which exhibits itself as a variation (twinkling) in amplitude (and phase) of the radio signal received from a distant, point-like radio source traversing through the interplanetary medium. Where sufficient observations are undertaken, the results can be used as input to the University of California, San Diego (UCSD) three-dimensional (3-D) time-dependent tomography suite to allow for the full 3-D reconstruction of both velocity and density throughout the inner heliosphere. In addition, source-surface magnetic fields can also be propagated out to the Earth (and elsewhere in the inner heliosphere) as well as the incorporation of {\it in-situ} data into the 3-D reconstructions. By combining IPS results from multiple observing locations around the globe, we can increase both the temporal and spatial coverage across the whole of the inner heliosphere. These 3-D reconstructions can be used for both scientific investigations as well as for forecasting purposes ({\it e.g.} http://ips.ucsd.edu/) and also for driving space weather MHD models such as ENLIL ({\it e.g.} http://helioweather.net/models/ipsbd/vel1e4/). IPS also provides an excellent opportunity to enhance collaborations between developed and developing countries thanks to the locations of many of the IPS-capable systems used. The WIPSS Network aims to bring together the worldwide real-time-capable IPS observatories, as well as those used on a campaign-only basis, with well-developed and tested analyses techniques being unified across the majority of the IPS-capable systems. We also undertake an initial demonstration analysis of some of these WIPSS data incorporated into the UCSD tomography, and highlight the prospects of the WIPSS Network going forward as a future potential worldwide space-weather Instrument.
3	Space weather data from high resolution space radiation monitoring with the miniaturized spacecraft payload SATRAM/Timepix on board Proba-V satellite	Granja, C et al.	p-Poster
	Carlos Granja
	Czech Space Research Center (CSRC), Brno, Czech Republic ; Nucl. Phys. Inst. Czech Acad. of Sciences Prague
	High-resolution wide-dynamic range monitoring of the near Earth space radiation environment on board satellites is valuable not only for spacecraft operation and assessment of radiation effects on aerospace components and electronic devices but it can be also exploited for space radiation and cosmic ray research and space weather studies. For example, time- and spatially-correlated measurements in Earth’s orbit serve for a range of studies ranging from models of geomagnetic and solar activity, via interaction of solar particle events and coronal mass ejections, the interplay of solar radiation and galactic cosmic rays with Earth’s magnetosphere and distribution and dynamics of the Earth radiation belts as well as systematic studies and forecasting models of space weather phenomena. The Space Application of Timepix based Radiation Monitor (SATRAM) is a spacecraft platform radiation monitor payload (300 g, 10 cm size) on board the Proba-V satellite operating in an 820 km altitude low Earth orbit since launch in 2013. The technology demonstration miniaturized payload carries the highly integrated ASIC chip Timepix equipped with a 300 um silicon sensor. The device in the harsh environment provides a signal threshold of 8 keV/pixel sensitive to low-energy X-rays and all charged particles including minimum ionizing particles. For X-rays the energy operating range is 10–30 keV. Event count rates can be up to 10^6 cnt/cm2/s for detailed event-by-event analysis or over 10^11 cnt/cm2/s for particle-counting only measurements. The single quantum sensitivity (zero-dark current noiseless operation) combined with per-pixel (deposited energy) spectrometry and micro-scale pattern recognition analysis of single particle tracks enables to determine the composition (particle type) and spectral characterization (energy loss of energetic charged particles) of mixed radiation fields. Timepix's pixel granularity and particle tracking capability also provides limited directional sensitivity for energetic charged particles. Following successful commissioning the SATRAM payload has been sampling the space radiation field in the satellite environment along its orbit at a rate of several frames per minute. The preliminary evaluation of data of interest and value for space weather studies is presented. Potential value for extended or distributed spacecraft including inner solar system missions is discussed.
4	Energetic Neutrals for Space Environment Monitoring	Futaana, Y et al.	p-Poster
	Yoshifumi Futaana[1], Xiao-Dong Wang[1], Martin Wieser[1], Georgios Nicolaou[1], Stas Barabash[1], Berndt Klecker[2], Peter Wurz[3], Phillipe Escoubet[4], Alain Hilgers[4], Fabrice Cipriani[4]
	[1]Swedish Institute of Space Physics, Kiruna, Sweden; [2]Max-Planck-Institut für extraterrestrische Physik, Garching, Germany; [3]University of Bern, Bern, Switzerland; [4]European Space Research and Technology Centre, European Space Agency, Noordwijk, the Netherlands
	We investigate a potential use of energetic neutral atoms (ENAs) for future space weather monitoring. ENAs are produced everywhere in the solar system due to the interaction between space plasma and ambient particles (neutrals and other plasma populations). Due to their neutrality, ENAs are freed from the electromagnetic forces, and fly along ballistic trajectories, keeping the information of the source plasma. Thus, ENAs have been used widely to visualise plasma populations in a remote sensing manner in the space plasma physics community. Such characteristics of ENAs provide potential applications to the space weather monitoring, complimentarily to the other measurement techniques such as in situ plasma measurements and telescopic measurements at various wavelengths. Particular interests of using the ENAs for this purpose are that they conserve information of the velocity distribution function of the plasma disturbed by space weather events, and that they can be detected earlier than the plasma. From thorough literature survey, we identified five space-weather related ENA populations potentially produced near the Sun and around planets. 1. High energy (MeV range) ENAs produced during solar flares in the solar corona, typically within 20 solar radii. 2. Low to medium energy (1-10 keV) ENAs produced in front of the interplanetary coronal mass ejection. 3. Neutralized solar wind (0.5-3 keV) produced in front of the Earth by extended geocorona beyond the bow shock. 4. High energy (MeV range) inner magnetospheric ENAs. 5. Low energy ENAs (0.5-3 keV) of the solar wind origin produced inside the terrestrial magnetosheath We further characterised each component, and assessed whether or not they can be used for the space weather monitoring. We conclude that the populations 1 through 3 can be used for predicting the geoeffective solar events, and the populations 4 and 5 can be used for evaluating the effects of the space weather event at Earth. We evaluated if the existing ENA sensors can feasibly measure these components and concluded that monitoring of populations 2 through 5 is possible by optimising the existing instruments, while a large technology gap exists to measure the population 1. In this presentation, we will overview each space-weather ENA components, and discuss the feasibility of the measurements. We also propose a possible deployment system for space weather monitoring using ENAs.
5	Solar Observations from Off the Sun-Earth Line: Sun-Earth Lagrangian Explorer (SELEX)	Gopalswamy, N et al.	p-Poster
	Nat Gopalswamy, Barbara J. Thompson, Terry Kucera, Joseph M. Davila, O. Christopher St. Cyr, Charles N. Arge, Douglas Rabin, Qian Gong[1]; Sarbani Basu[2]; Leon Golub, Ed DeLuca[3]; Craig DeForest[4]; Valentin Martinez-Pillet, Frank Hill[5], Mark Miesch[6]; Jesper Schou, Sami K. Solanki[7]; Jackie Davies, Richard A. Harrison[8]; David Berghmans[9]; S. Paul Rajaguru[10]
	[1]NASA Goddard Space Flight Center; [2]Yale University; [3]Smithsonian Astrophysical Observatory; [4]South West Research Institute; [5]National Solar Observatory; [6]High Altitude Observatory; [7]Max Planck Institute for Solar System Research; [8]Rutherford Appleton Laboratory; [9]Royal Observatory of Belgium; [10]Indian Institute of Astrophysics
	Solar magnetism defines the heliosphere and is responsible for a vast number of Heliophysical processes. Helioseismic studies have led to the conclusion that the site of the solar dynamo is at the base of the convection zone. All the knowledge we have gained so far on the magnetic field in the solar interior is from observations along the Sun-Earth line. In order to make rapid progress in a more detailed understanding of the magnetic coupling between the solar interior and atmosphere/heliosphere, we need to make observations from off the Sun-Earth line such as L5 and/or L4. By combining Doppler measurements from L5/L4 and Sun-Earth line (e.g., GONG, HMI) one can use helioseismology techniques to track subsurface signatures of active regions and derive physical properties of the convection zone. Detailed information on the life cycle of active regions is important for tracking polar field build up, a key feature of the solar dynamo. Measurements of meridional flow and its spatial structure using the larger range of ray paths, depths and lat/lon extents available from the multiview (L5/L4 and Sun-Earth line combination) are critical in discriminating Dynamo models. Once the active regions are on the surface, how they erupt and disturb the heliosphere can be best tracked using multiview observations, as demonstrated by the STEREO mission. In particular, we can determine the acceleration profile of coronal mass ejections (CMEs) by combining wide-field EUV images and coronagraph images to identify the forces acting on CMEs. We can identify and track the evolution of CME flux ropes fully characterized using flare reconnection flux derived from EUV post-eruption arcades and compare them with in-situ flux ropes. This paper describes a mission concept known as Sun-Earth Lagrangian Explorer (SELEX) that will observe signatures of magnetic coupling from the solar interior to the inner heliosphere.
6	Occurrence of anomalies on operating ESA satellites	Clavie, C et al.	p-Poster
	C. Clavie, S. Kraft, J.P. Luntama
	European Space Agency, ESA-ESOC, SSA Programme Office
	Space weather is a major cause of satellite anomalies or unexpected events and material or electronics degradation. The present study examined the occurrence of these effects on currently operating ESA satellites: Cluster, XMM-Newton, Integral, Lisa Pathfinder, Mars- Express, Proba-1, Proba-2, Proba-V, Cryosat-2, Swarm and GAIA. Space weather induced effects were examined with relation to long term solar weather phenomena (e.g. solar cycle) as well as short term solar events. Special attention was also given to the role of the satellite orbits in space weather induced effects. It was observed that every critical event (proton flux >10 pfu for energies >10 Mev) caused anomalies on multiple spacecraft in the last 7 years. During several of these events a critical degradation of the solar array output power was found under the influence of displacement damage doses. In HEO, the study of long-term variation of space weather showed a correlation between the GCR flux and disturbed satellite operations due to SEUs. In LEO orbits, the SAA is the main cause of SEUs, with the polar regions as the second most important influence. Thebiggest solar storm of this solar cycle, thestorm of September 2017, showed the importance of the further development of space weather services. In total, 18 critical anomalies or unexpected events occurred on 11 different spacecraft distributed over LEO, HEO and interplanetary orbits. This study showed that solar energetic particles are clearly a source of satellite anomalies. It also showed that a better understanding of this correlation is essential for stable operation of satellites, especially considering large solar events like the September 2017 storms or even Carrington sized events.