Session 3 - Ground-based Instruments for Advanced Space Weather Projects

Francesca Zuccarello (University of Catania); Francesco Berrilli (University of Roma Tor Vergata); Paola De Michelis (Istituto Nazionale di Geofisica e Vulcanologia); Stuart Jefferies (University of Hawaii).
Monday 27/11, 14:15 - 17:15
Ridderzaal


KEYWORDS - Eruptive events; ground-based instruments.

Eruptive events on the Sun can affect the near Earth environment and ground-based critical infrastructures. As such, the ability to monitor and forecast these sources of space weather, is of paramount importance. This session provides a forum for the presentation of state-of-the-art and novel instruments for the observation and prediction of solar eruptive events. Authors are invited to submit abstracts dealing with topics applied to observations of the solar photosphere and chromosphere, as well as of the solar magnetic field, which can be acquired by the new generation of ground-based instruments.

Poster Viewing
From Monday noon to Wednesday morning

Talks
Monday November 27, 14:15 - 15:30, Ridderzaal
Monday November 27, 16:00 - 17:15, Ridderzaal

Click here to toggle abstract display in the schedule

Talks : Time schedule

Monday November 27, 14:15 - 15:30, Ridderzaal

14:15	Welcome and presentation of the Session	Berrilli, F et al.	Oral
	Francesco Berrilli
14:20	Science with the European Solar Telescope	Martínez gonzález, M et al.	Invited Oral
	M. J. Martínez González
	The European Solar Telescope (EST) is a 4-m class telescope concept that is planned to see first light in 2026. EST will be optimised for multiwavelength, spectro-polarimetric studies at the highest spatial resolution (25 km). To achieve such large spatial resolution, the EST will be the first telescope to incorporate a multi-conjugate adaptive optics system that will enable diffraction-limited observations. These technical capabilities will foster frontier research in the magnetic coupling of the solar atmosphere. In this presentation, the telescope concept will be presented as well as the future science with the EST, highlighting its potential for the diagnostic of thermal and magnetic properties of the chromosphere and of chromospheric structures embedded in the corona.
14:40	Event based verification of the automatic flare detection system at Kanzelhöhe Observatory	Pötzi, W et al.	Oral
	Werner Pötzi[1], Astrid Veronig[1,2]
	[1]Kanzelhöhe Observatory for Solar and Environmental Research, University of Graz, Austria; [2]Institute of Physics/IGAM, University of Graz, Austria
	In the framework of ESAs Space Situational Awareness (ESA-SSA) program an automatic flare detection algorithm was developed at the Kanzelhöhe Observatory. The H-alpha images, which are taken at a cadence of 10 images per minute with a resolution of 1 arcsec/pixel, are processed almost in real time. The algorithm detects filaments and flares, for the latter ones alerts are issued in case they reach a certain importance class. The system is now running for almost 4 years and more than 140 flares of importance class 1 and higher have been detected. Based on this long time series a new improved algorithm was developed and all data has been recalculated with this algorithm. The automatically detected flares are evaluated against visual observations using verification measures like hitrates and skill scores. In order to improve the significance of the scores an event based approach was applied in the evaluation. With the new algorithm the hitrate of detecting flares importance class 1 and above improved from 79% to 96%, and the rate of false alarm went down from 23% to 4%.
14:50	Investigation of Heliospheric Faraday Rotation Due to a Coronal Mass Ejection (CME) Using the LOw Frequency ARray (LOFAR) and Space-Based Imaging Techniques	Bisi, M et al.	Oral
	Mario M. Bisi[1], Elizabeth A. Jensen[2], Richard A. Fallows[3], Charlotte Sobey[3,4,5], Brian Wood[6], Bernard V. Jackson[7], Alessandra Giunta[1], David Barnes[1], P. Paul L. Hick[8,7], Tarraneh Eftekhari[9], Hsiu-Shan Yu[7], Dusan Odstrcil[10,11], Munetoshi Tokumaru[12], Caterina Tiburzi[13], and Joris Verbiest[13].
	[1]STFC-RAL Space, UK; [2]Planetary Science Institute, AZ, USA; [3]ASTRON, NL; [4]Curtain Institute of Radio Astronomy, WA, Australia; [5]CSIRO Astronomy and Space Science, WA, Australia; [6]NRL, DC, USA; [7]CASS-UCSD, CA, USA; [8]SDSC-UCSD, CA, USA; [9]University of New Mexico, NM, USA; [10]GMU, VA, USA; [11]NASA GSFC, MD, USA; [12]ISEE, Nagoya University, Japan; [13]Universität Bielefeld, Germany.
	Observations of Faraday rotation (FR) can be used to attempt to determine average magnetic-field orientations in the inner heliosphere. Such a technique has already been well demonstrated through the corona, ionosphere, and also the interstellar medium. Measurements of the polarisation of astronomical (or spacecraft in superior conjunction) radio sources (beacons/radio frequency carriers) through the inner corona of the Sun to obtain the FR have been demonstrated but mostly at relatively-high radio frequencies. Geomagnetic storms of the highest intensity are generally driven by coronal mass ejections (CMEs) impacting the Earth’s space environment. Their intensity is driven by the speed, density, and, most-importantly, their magnetic-field orientation and magnitude of the incoming solar plasma. The most-significant magnetic-field factor is the North-South component (Bz in Geocentric Solar Magnetic - GSM - coordinates). At present, there are no reliable prediction methods available for this magnetic-field component ahead of the {\it in-situ} monitors around the Sun-Earth L1 point. Here we show some initial results of true heliospheric FR using the Low Frequency Array (LOFAR) below 200 MHz to investigate the passage of a CME across the line of sight. LOFAR is a next-generation low-frequency radio interferometer, and a pathfinder to the Square Kilometre Array (SKA) – LOW telescope. We demonstrate our latest heliospheric FR results through the analysis of observations of pulsar J1022+1001, which commenced on 13 August 2014 at 13:00UT and spanned over 150 minutes in duration. We also show detailed comparisons to the FR results via additional context information and various modelling techniques to understand/untangle the structure of the inner heliosphere being detected. This observation could indeed pave the way to an experiment which might be implemented for space-weather purposes that will eventually lead to a near-global method for determining the magnetic field throughout the inner heliosphere.
15:00	The SAMM project	Piazzesi, R et al.	Oral
	Roberto Piazzesi, Marco Stangalini, Roberto Speziali
	INAF (Istituto Nazionale di Astrofisica) - OAR Osservatorio Astronomico di Roma
	Over the last years the MOF (magneto-optical filter) technology has provided important results, paving the way for its use for the tomographic monitoring of the solar atmosphere for space weather applications. A number of successful test campaigns have demonstrated it’s capabilities in terms of magnetic field and doppler sensitivity and temporal resolution. Based on this, SAMM, the Solar Activity MOF Monitor project, was conceived to further advance this technological solution. SAMM has been designed to offer a complete robotic telescope specifically engineered to ensure its reliability, scalability and high performance. SAMM has been designed and built, through funding from the Italian Ministry for Economic Development (MiSE), by a partnership of the Italian Institute for Astrophysics (INAF-OAR) and the Dal Sasso srl firm through their brand Avalon Instruments. The SAMM project, therefore, represents a succesful example of synergy between research institutions and industry. The first light is expected in mid 2017. In this contribution we present the project, its main technical aspects and its first results.
15:10	SPRING - Proposed Instrument Concept	Roth, M et al.	Invited Oral
	Roth Markus[1], Gosain Sanjay[1,2], Hill Frank[2], Thompson Michael[3]
	[1]Kiepenheuer-Institut für Sonnenphysik, Freiburg, Germany; [2]National Solar Observatory, Boulder, USA; [3]High Altitude Observatory, Boulder, USA
	Real-time observations showing the large-scale dynamics and magnetism at different layers of the solar atmosphere are crucial to understand the global behaviour of solar phenomena. However, despite the amount of information coming from space and ground-based full-Sun telescopes, real-time information about the variation of important parameters such as velocities, magnetic field and intensity at different solar layers is still lacking. The solar physics and space weather communities worldwide have a high demand of a network of telescopes with a small aperture but a large field-of-view to obtain images of the Sun with better than 1 arcsec spatial resolution and in multiple spectral lines. Such a configuration as SPRING (Solar Physics Research Integrated Network Group, Hill et al. 2013) aims at observing with a cadence of less than 10 sec for at least 25 years to collect as much information as possible on, e.g., active regions, over a long time in detail, in order to study the configuration of the magnetic field. These contiguous observations shall include 2D spectroscopy and polarimetry measurements, and must allow obtaining vector magnetograms. The definition of an adequate network of small telescopes, as well as the most suited instrumentation for SPRING took place within the FP7 Integrated Activity “Solarnet”. In this talk I will describe the technical concept developed for the setup of this new ground-based network for continuous solar observations serving a large research community.

Monday November 27, 16:00 - 17:15, Ridderzaal

16:00	Comprehensive analysis of the Geoeffective Solar Event of June 21, 2015: Effects on the Magnetosphere, Plasmasphere and Ionosphere Systems - part 1	Piersanti, M et al.	Oral
	Mirko Piersanti[1,2], Tommaso Alberti[3], Alessandro Bemporad[4], Francesco Berrilli[5], Roberto Bruno[6], Vincenzo Capparelli[7], Vincenzo Carbone[3], Claudio Cesaroni[8], Giuseppe Consolini[6], Alice Cristaldi[9], Alfredo Del Corpo[1], Dario Del Moro[5], Simone Di Matteo[1,2], Ilaria Ermolli[9], Silvano Fineschi[4], Fabio Giannattasio[6], Fabrizio Giorgi[9], Luca Giovannelli[5], Salvatore Luigi Guglielmino[7], Monica Laurenza[6], Fabio Lepreti[3], Maria Federica Marcucci[6], Matteo Martucci[5,10], Matteo Mergè[5], Michael Pezzopane[8], Ermanno Pietropaolo[1], Paolo Romano[11], Roberta Sparvoli[5], Luca Spogli[8,12], Marco Stangalini[9], Antonio Vecchio[13], Massimo Vellante[1], Umberto Villante[1,2], Francesca Zuccarello[7].
	[1]Department of Physical and Chemical Sciences, University of L’Aquila, L’Aquila, Italy; [2]Consorzio Area di Ricerca in Astrogeofisica, L’Aquila, Italy; [3]Department of Physics, University of Calabria, Cosenza, Italy; [4]INAF-Osservatorio Astrofisico di Torino, Turin, Italy; [5]Physics Department, University of Rome Torvergata, Rome, Italy; [6]INAF-Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy; [7]Department of Physics and Astronomy, University of Catania, Catania, Italy; [8]Istituto di Geofisica e Vulcanologia, Roma, Italy; [9]INAF-Osservatorio Astronomico di Roma, Roma, Italy; [10]INFN, Laboratori Nazionali di Frascati, Frascati, Italy; [11]INAF-Osservatorio Astrofisico di Catania, Catania, Italy; [12]SpacEarth Technology, Roma, Italy; [13]LESIA-Observatoire de Paris, 5 place Jules Janssen, 92190 Meudon, France.
	A full-halo coronal mass ejection left the sun on June 21, 2015 from the active region NOAA 12371 encountering Earth on June 22, 2015, generating a strong geomagnetic storm whose manimum Dst value was -204 nT . The CME was associated with an M2 class flare observed at 01:42 UT, located near the center disk (N12E16). Using satellite data from solar, heliospheric, magnetospheric missions and ground-based instruments, we performed a comprehensive Sun-to-Earth analysis. In particular, in this paper we present the "Solar part" analuysis. Namely, we analyzed the active region evolution using ground-based and satellite instruments (BBSO, IRIS, HINODE, SDO/AIA, RHESSI -- Halpha, EUV, UV, X), the AR magnetograms, using data from SDO HMI, the relative particle data, using PAMELA instruments and the effects of interplanetary perturbation on cosmic ray intensity. We also evaluated the 1-8 $\AA$ soft X-ray and low-frequency ($\sim$ 1 MHz) Type III radio burst time-integrated intensity (or fluence) of the flare in order to make a prediction of the associated Solar Energetic Particle (SEP) event by using the model developed by Laurenza [2009].
16:10	Comprehensive analysis of the Geoeffective Solar Event of June 21, 2015: Effects on the Magnetosphere, Plasmasphere and Ionosphere Systems - part 2	Piersanti, M et al.	Oral
	Mirko Piersanti[1,2], Tommaso Alberti[3], Alessandro Bemporad[4], Francesco Berrilli[5], Roberto Bruno[6], Vincenzo Capparelli[7], Vincenzo Carbone[3], Claudio Cesaroni[8], Giuseppe Consolini[6], Alice Cristaldi[9], Alfredo Del Corpo[1], Dario Del Moro[5], Simone Di Matteo[1,2], Ilaria Ermolli[9], Silvano Fineschi[4], Fabio Giannattasio[6], Fabrizio Giorgi[9], Luca Giovannelli[5], Salvatore Luigi Guglielmino[7], Monica Laurenza[6], Fabio Lepreti[3], Maria Federica Marcucci[6], Matteo Martucci[5,10], Matteo Mergè[5], Michael Pezzopane[8], Ermanno Pietropaolo[1], Paolo Romano[11], Roberta Sparvoli[5], Luca Spogli[8,12], Marco Stangalini[9], Antonio Vecchio[13], Massimo Vellante[1], Umberto Villante[1,2], Francesca Zuccarello[7]
	[1]Department of Physical and Chemical Sciences, University of L’Aquila, L’Aquila, Italy; [2]Consorzio Area di Ricerca in Astrogeofisica, L’Aquila, Italy; [3]Department of Physics, University of Calabria, Cosenza, Italy; [4]INAF-Osservatorio Astrofisico di Torino, Turin, Italy; [5]Physics Department, University of Rome Torvergata, Rome, Italy; [6]INAF-Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy; [7]Department of Physics and Astronomy, University of Catania, Catania, Italy; [8]Istituto di Geofisica e Vulcanologia, Roma, Italy; [9]INAF-Osservatorio Astronomico di Roma, Roma, Italy; [10]INFN, Laboratori Nazionali di Frascati, Frascati, Italy; [11]INAF-Osservatorio Astrofisico di Catania, Catania, Italy; [12]SpacEarth Technology, Roma, Italy; [13]LESIA-Observatoire de Paris, 5 place Jules Janssen, 92190 Meudon, France
	A full-halo coronal mass ejection left the sun on June 21, 2015 from the active region NOAA 12371 encountering Earth on June 22, 2015, generating a strong geomagnetic storm whose manimum Dst value was -204 nT . The CME was associated with an M2 class flare observed at 01:42 UT, located near the center disk (N12E16). Using satellite data from solar, heliospheric, magnetospheric missions and ground-based instruments, we performed a comprehensive Sun-to-Earth analysis. In particular, in this paper we show the "Geomagnetic part" analysis. Namely, using ground based observations from lower to higher latitudes (INTERMAGNET and EMMA), we reconstructed the ionospheric current system associated to the geomagnetic sudden impulse. Furthermore, SuperDARN measurements are used to image the global ionospheric polar convection during the SI and during the principal phases of the geomagnetic storm. In addition, to investigate the influence of the disturbed electric field on the low latitude ionosphere induced by geomagnetic storms, we focused on the morphology of the crests of the equatorial ionospheric anomaly, by the simultaneous use of GNSS receivers, ionosondes and Langmuir probes on board the SWARM constellation. Moreover, we investigated the dynamics of the plasmasphere during the different phases of the geomagnetic storm by examining the time evolution of the radial profiles of the equatorial plasma mass density derived from field line resonances detected at the EMMA network (1.5 $<$ L $<$ 6.5). Finally, we presented the general features of the geomagnetic response to the CME, by applying innovative data analysis tools that allow to investigate the time variation of ground-based observations of the Earth's magnetic field during the associated geomagnetic storm.
16:20	The MOTH Doppler-magnetographs and data calibration pipeline	Berrilli, F et al.	Oral
	Roberta Forte[1], Ermanno Pietropaolo[2], Stuart Jefferies[3], Dario Del Moro[1], Luca Giovannelli[1], Maurizio Oliviero[4], Francesco Berrilli[1,5,6]
	[1]Dipartimento di Fisica, Università di Roma Tor Vergata, Rome, Italy; [2]Dipartimento di Scienze Fisiche e Chimiche, Università di L'Aquila, Italy; [3]Department of Physics and Astronomy, Georgia State University, USA; [4]INAF-OACN, Naple, Italy; [5]INFN (National Institute of Nuclear Physics) – Sezione Tor Vergata, Rome, Italy; [6]INAF(National Institute for Astrophysics) associate, Rome, Ital5
	The calibration pipeline of the zero level images obtained from the solar telescope Magneto-Optical filters at Two Heights (MOTH II) is presented. MOTH II consists in a dual channel telescope, each mounting a tandem of Magneto-Optical Filters (MOFs), at 589 nm (Na D2-line) and 770 nm (K I-line) respectively. MOTH II provides full disk line-of-sight Doppler velocity and magnetic field at two levels of the solar atmosphere, between 400 km and 700 km. MOTH II is usually operated at the Mees Observatory (Maui, USA) and periodically deployed to South Pole for observing campaigns. The developed MOTH II pipeline is mainly focused on the correction for the signal leakage, due to the non-ideal polarizers behavior, and on the geometrical registration between images acquired by 4 CMOS cameras for two channels and two circular polarization states. MOTH II data are used to investigate atmospheric dynamics (e.g., gravity waves and portals) and Space Weather phenomena. Particularly, flare forecasting algorithms, based on the detection of magnetic active regions and associated flare probability estimation, are currently under development. The possible matching of MOTH II data with HMI and AIA images into a flux rope model developed in collaboration between Harvard-Smithsonian CfA and MIT Laboratory for Nuclear Science.
16:30	Worldwide network of particle detectors SEVAN: 10 years of operation	Karapetyan, T et al.	Invited Oral
	V.Babayan[1], A.Chilingarian[1], T.Karapetyan[1], B.Mailyan[2] and M.Zazyan[1]
	[1]Alikhanyan National Lab (Yerevan Physics Institute), 2 Alikhanyan Brothers, Yerevan 0036, Armenia; [2]Geospace Physics Laboratory, Florida Institute of Technology, Fl, USA
	“Space Environment Viewing and Analysis Network” (SEVAN) aim to improve the fundamental research on particle acceleration in the vicinity of sun and - space environment conditions. The new type of particle detectors simultaneously measures changing fluxes of most species of secondary cosmic rays, thus turning into a powerful integrated device for exploration of solar modulation effects. The SEVAN modules are operating at the Aragats Space Environmental Center (ASEC) in Armenia, in Croatia, Bulgaria, Slovakia and India. The network of hybrid particle detectors, measuring neutral and charged fluxes provide the following advantages over existing detector networks measuring single species of secondary cosmic rays (Neutron Monitors and Muon detectors): • Measure count rates of the 3 species of the Secondary cosmic rays (SCR): charged particles with energy threshold 7 MeV, neutral particles (gamma rays and neutrons) and high-energy muons (above 250 MeV); • Significantly enlarge statistical accuracy of measurements; • Probe different populations of primary cosmic rays with rigidities from 7 GV up to 20 GV; • Reconstruct SCR spectra and determine position of the spectral “knees”; • Classify GLEs in “neutron” or “proton” initiated events; • Estimate and analyze correlation matrices among different fluxes; • Significantly enlarge the reliability of Space Weather alerts due to detection of 3 particle fluxes instead of only one in existing neutron monitor and muon telescope worldwide networks; • Perform research on runaway electron acceleration during thunderstorms; research the enigma of lightning. In the paper we present the most interesting results of SEVAN network operation last decade devoted to 10-th anniversary of the IHY-2007.
16:50	Neutron Monitors for Space Weather	Eroshenko, E et al.	Oral
	Anatoly Belov[1],Eugenia Eroshenko[1],Victor Yanke[1], Artem Abunin[1],Maria Abunina[1],Raisa Gushchina[1],Victoria Oleneva[1],Dimitra Lingri[2],Helen Mavromichalaki[2]
	[1]Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation RAS,Moscow, Russia; [2]Nuclear and Particle Physics Department, Faculty of Physics, National and Kapodistrian University of Athens, Athens, Greece.
	During the last 10 years we have continued our work with the NMDB which in this year marks its continue 10-year operating. Since our main work is related to study of the solar-heliospheric phenomena and unforeseen impact on Earth, we need cosmic ray parameters beyond the atmosphere and magnetosphere, and we apply special global survey method (GSM) to the NM data from as many as possible stations. It takes only hourly (or daily mean) data from the nmdb, thus a big work was done on the unification these data. Some of the Applications which were elaborated during last eyars can fully use all data coming to NMDB. It concerns the rigidity spectra of galactic cosmic rays (GCR) which are necessary for fundamental science and for a set of applications as well. For example, these spectra allow us the estimation of dangerous for satellite electronic and cosmonauts CR fluxes. Algorithm for calculation the rigidity spectrum of GCR based on the mean daily data of the neutron monitor network is realized now in operating as Internet version. Neutron monitor network data allows obtaining specific angle distribution of the CR variations which is used for defining predictors of Forbush effects and geomagnetic storms. The results after GSM processing – isotropic and anisotropic parts of the galactic cosmic rays with one hour resolution, are combined together with relevant data on the solar wind, interplanetary magnetic field, geomagnetic activity etc. into database on the Forbush effects and interplanetary disturbances over the period since 1957 up to now. This database now is in an open access in the internet and gives a chance to study various events of ~ 7000 presented there.
17:00	ORCA: A new instrument for Space Weather	Blanco, J et al.	Oral
	J.J. Blanco[1], O. García-Población[1], J. Medina[1], I. García-Tejedor[1], M. Prieto[1], G. Díaz-Romeral[1], S. Ayuso[1], R. Gómez-Herrero[1], J. A. Garzón[2], A. Gomis[3], V. Villasante-Marcos[3], M. Seco[2], A. Morozova[4], G. Kornakov[5], T. Kurtukian[6], A. Blanco[7], D. González-Diaz[2], B. Heber[8], C. Steigies[8] and H. Kruger[9].
	[1]University of Alcal\'a; [2]University of Santiago de Compostela; [3]Instituto Geogr\'afico Nacional; [4]CGUC-Univ. de Coimbra; [5]TU-Darmstadt; [6]CEN-Bordeaux; [7]LIP-Coimbra; [8]IEAP, Christian-Albrechts-Universität zu Kiel; [9]Faculty of Natural Sciences, North-West University
	A new cosmic ray instrument, the Antarctic Cosmic Ray Observatory (ORCA), has been designed to perform a North to South latitudinal survey, onboard the research vessel Hesperide, in the end of 2018 and to be finally settled at Juan Carlos I Antarctic Station. ORCA will feature a 3NM64 neutron monitor, a set of three bare BP28 counters, a muon telescope (MITO) and a RPC based detector (TRISTAN). The combination of these detectors will allow us to measure neutrons, muons, protons, electrons and gamma rays arriving to the ORCA’s location. Both MITO and TRISTAN will provide direct directional information about incoming particles. ORCA will be built into a 5.8x2.3x2.3 m maritime container, equipped with environmental control, data transmission capabilities and solar and/or battery-backed power supply. Together with ORCA, a mini-neutron monitor will also operate along this initial stage of the project. The set up of ORCA is scheduled in a three year period, commissioning (2017), shipping (end of 2018) and initial operation (2019). Two main milestones will be tackled by ORCA in this period, a latitudinal survey on board the Spanish research vessel Hesperides, and its installation in the Antarctic Spanish Base Juan Carlos I.
17:10	Conclusions and Recap	Zuccarello, F et al.	Oral
	Francesca Zuccarello

Posters

1	LOFAR4SpaceWeather: Towards Space Weather Monitoring with Europe’s Largest Radio Telescope	Fallows, R et al.	e-Poster
	Richard Fallows[1], Rene Vermeulen[1], and Gert Kruithof[1], on behalf of the LOFAR4SW consortium[2]
	[1]ASTRON - the Netherlands Institute for Radio Astronomy; [2]Various institutes
	The Low Frequency Array (LOFAR) is a radio astronomy array consisting of a dense core of 24 stations within an area of diameter ~4km, 14 stations spread further afield across the north-east of the Netherlands, and a further thirteen stations internationally (six across Germany, three in northern Poland, and one each in France, Ireland, Sweden and the UK). Each station is capable of observing over a wide bandwidth across the frequency range 10-250 MHz, at high time and frequency resolutions, and forming multiple beams to point in any direction on the sky. Any number of the stations can be combined as an interferometer for radio imaging, and/or the core stations combined to form up to ~200 narrow pencil beams (“tied-array beams”). The latter enables raster imaging techniques to be used or multiple radio sources to be observed simultaneously. These capabilities make LOFAR one of the world’s most flexible radio instruments and enable studies of several aspects of space weather to be advanced beyond the current state-of-the-art. This includes high time and frequency resolution dynamic spectra and imaging of the Sun, using interplanetary scintillation to observe the solar wind and the passage of Coronal Mass Ejections, attempting measurement of the interplanetary magnetic field in the inner heliosphere, and expanding the view of ionospheric scintillation beyond single-frequency time series’. LOFAR4SW is a design study, recently awarded a grant under the latest Horizon2020 INFRADEV call, to commence investigations into upgrading LOFAR to enable regular space weather monitoring observations in parallel with radio astronomy operations. In this poster, we summarise the aims of the LOFAR4SW study and the longer-term goals envisaged for LOFAR to become a major instrument for space weather monitoring observations.
2	Difference of Multiplicities in neutron monitor	Balabin, Y et al.	p-Poster
	Yury Balabin, Boris Gvozdevsky, Aleksey Germanenko
	Polar Geophysical Institute
	There are two ways to describe multiplicity generation in a neutron monitor (NM). The first one could be called “single particle origin”. It is based on the suggestion that a single very high energetic particle (nucleon) produces a great many (up to thousands) secondary neutrons in the lead shield of NM. It is conventional viewpoint on multiplicity. The second one could be called “shower origin”. It based on the assumption that a shower of energetic particles covers NM. Due to out fast recording system developed in Polar Geophysical Institute fine temporal and spatial structures of multiplicity can be study. These structures modify fluently along multiplicity number M growth, but differences between M < 10 and M > 30 become already significant. And fine structures of large multiplicity (M > 30) conform to the shower origin. This result is carried out from four NMs. Multiplicity structures on Barentsburg NM with having original design give clear and unambiguously answer: multiplicity M > 40 can be only generated by the shower.
3	Service Platform SAFE(Safety during Aviation Flight Environment from radiation) System	Kim, D et al.	p-Poster
	SeungBum Yang[1], TaeYoung Kim[1], JangSeok Choi[2], DoHyun Kim[1], SoYeon Kang[1], MyungJin Choi[1]
	[1]InSpace.co.,ltd; [2]Korea Space Weather Center (KSWC) Radio Research Agency
	In this paper, we describe the development of SAFE (Safety during Aviation Flight Environment from radiation) system which can retrieve and manage information on aerospace radiation dose as a nationwide service. If existing SAFE is centered on aerospace radiation dose management and service using Web browser, the current SAFE system has completed the aerospace radiation data service, Interlocking data of aerospace radiation actual measurement data, Establish an environment to compare/analyze actual values ​​and model values, Establish an environment to compare/analyze between aerospace radiation prediction models, development of Open API, Build an environment to apply and manage standard codes, Build distribution environment of program for development to international service. As a result, not only domestic airlines but also researchers and general users who research aerospace radiation can receive equivalent data services. In this paper, we introduce SAFE development process and service for expansion to platform.
4	Ground based cosmic radiation monitoring with passive monitoring stations based on thermoluminescent detectors	Van hoey, O et al.	p-Poster
	Olivier Van Hoey, Filip Vanhavere
	The Belgian Nuclear Research Center SCK-CEN
	The Belgian Nuclear Research Center SCK•CEN has been monitoring radiation dose around nuclear sites for more than 20 years to check for possible increases due to human activities. This is done by poles equipped with cheap, compact and passive thermoluminescent LiF:Mg,Cu,P detectors. These detectors are collected every three months and read out with the Harshaw 5500 reader. From these readings and with the proper calibration the radiation doses cumulated over three months are then calculated. Analysis of the calculated doses since 1995 has demonstrated that the LiF:Mg,Cu,P detectors can also be used for cosmic radiation monitoring. The time evolution of the measured dose rate shows a clear correlation with the signal of the Belgian neutron monitor in Dourbes. This is because the LiF:Mg,Cu,P detectors measure mostly the relatively constant terrestrial gamma radiation from the soil and building materials, but also the muons and thermal neutrons from the secondary cosmic radiation varying with the solar cycle. Therefore, we propose a new type of cheap, compact and passive cosmic radiation monitoring station. By using lead shielding (for eliminating terrestrial gamma radiation and creating spallation neutrons from high energy neutrons), pairs of LiF:Mg,Cu,P detectors enriched in Li-6 and Li-7 (for separation of thermal neutrons and muons) and polyethylene moderation (for slowing down fast neutrons to allow detection) one can measure muons, thermal neutrons and fast neutrons. By proper calibration based on calibration irradiations and radiation transport simulations the measured signals can be converted into muon and neutron fluence rates. By using LiF:Mg,Cu,P detectors at different depths in the polyethylene moderator it should even be possible to obtain a rough neutron energy spectrum. Such a passive monitoring station could be complementary to active neutron monitoring stations. Of course they will never provide the same time resolution, because integration over at least one month is necessary to get a significant signal. But the number of neutron monitoring stations is limited due to their complexity and cost. The passive monitoring stations could easily be placed at many locations without requiring large investments or manpower. In this way the monthly muon fluence and the neutron fluence spectrum could be provided for many locations, leading to a better understanding of the interaction between the cosmic radiation and our atmosphere.
5	Atmospheric temperature profiles at the Antarctic node of LAGO: Quiet and perturbed conditions	Dasso, S et al.	p-Poster
	V.E. López[1,5], A.M. Gulisano[2,3,4] and S. Dasso[3,4,5], for the LAGO Collaboration[6 ]
	[1]Servicio Meteorológico Nacional de Argentina; [2]Instituto Antártico Argentino, Dirección Nacional del Antártico; [3]Instituto de Astronomía y Física del Espacio, UBA-CONICET; [4]Departamento de Física, FCEN, UBA; [5]Departamento de Ciencias de la Atmósfera y los Océanos, FCEN, UBA;[6]The Latin American Giant Observatory Collaboration: www.lagoproject.org
	The Latin American Giant Observatory (LAGO) is a collaborative network formed by eleven countries (Argentina, Bolivia, Brazil, Chile, Colombia, Ecuador, Guatemala, Mexico, Perú, Spain, and Venezuela). LAGO has a Space Weather program and one of its main goals is to study the modulation of variability of Cosmic Rays (CRs) using its net of Water Cherenkov Detector (WCDs) and making numerical simulations of the transport of CRs in different physical scenarios. LAGO plans to deploy WCDs at the Antarctic peninsula, in the Argentinean Marambio base. Observations at this node will help to make scientific studies and also to make a monitoring of space weather conditions. Due to the low rigidity cut-off of this high latitude site, observations of Ground Level Enhancements(GLEs) will be possible. In order to carry out numerical simulations to better understand the ground observations of the CRs fluxes, it is necessary to characterize the atmosphere, where the secondary particles are created during the extended CRs shower. In this work, we present a characterization of the atmospheric conditions at the Argentinean Marambio base, where the Antarctic LAGO node will be deployed. In particular, we analyze the temperature altitude profile in a range covering the upper troposphere, and the low-mid stratosphere, for quiet conditions and during two major geomagnetic storms. We analyze the seasonal climatology of temperatures and investigated possible variations during five intense geomagnetic storms, analyzing the possibility of physical and chemical effects during these events. In order to make a detailed description of the mentioned atmospheric levels, we analyze data obtained from balloon surveys measured at Marambio by the National Meteorological Service of Argentina from 1998 to 2016. We present the seasonal behavior of the temperature variable environment from 8 to 40 km throughout the period and analyze the median and quartile statistics during two geomagnetic storms: one in summer and one in winter, extending the analysis period to seven days prior to the occurrence of the storms and to the fourteen subsequent days. In addition, given the different values of the Dst index, we calculated the temperature anomalies, for each geomagnetic storm and the subsequent days, and also obtained the levels of cooling and heating, relative to the days prior to the five events. The results of this study will be useful to better understand the possible events of Space Weather and to make corrections to the flow of cosmic rays,which will be observed in the near future with the particle detector of LAGO to study the solar modulation of the cosmic ray flux and GLE events, in the site with the lower rigidity cut off of this observatory.
6	Cosmic rays using water Cherenkov detectors in Antarctic: First Campaign toward the Antarctic node of the LAGO Collaboration	Dasso, S et al.	p-Poster
	Sergio Dasso[1,2,3], Adriana María Gulisano[1,3,4], Omar Areso[1], Maximiliano Ramelli[1], Matías Pereira[1], Ubaldo Ereñú[1], Viviana López[5], Héctor Ochoa[4], for the LAGO collaboration[6]
	[1]CONICET, Universidad de Buenos Aires, Instituto de Astronomia y Fisica del Espacio; [2]Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Departamento de Ciencias de la Atmosfera y los Oceanos; [3]Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Departamento de Fisica; [4]Instituto Antártico Argentino, DNA, Buenos Aires; [5]Servicio Meteorológico Nacional, Buenos Aires, Argentina; [6]lagoproject.org, see the full list of members and institutions at lagoproject.org/collab.html
	Ground observations of galactic Cosmic Rays (CRs) are systematically done from several decades using Neutron Monitors (NMs) at different locations. These observations allowed to quantify several effects of the interplanetary magnetic conditions on the transport of CRs in the heliosphere, both on large time scales (e.g., the solar cycle) as well as on shorter time scales (e.g. Forbush decreases). From NMs located at high latitudes it is also possible to observe solar cosmic rays (e.g., Ground Level Enhancements, GLEs). While observations using NMs are very useful to quantify CRs fluxes and have an indisputable importance in the present to determine the conditions of Space Weather, they are just proportional counters of neutrons that cannot discriminate energy bands for the observed particles. Water Cherenkov detectors (WCDs) have shown to be able to reproduce time structures observed with NMs (e.g., observations from surface detectors of the Pierre Auger collaboration). The major advantage of WCDs compared with NMs is that the former ones can discriminate energy channels for the observed secondary charged particles (as for instance muons, electrons, gamma rays producing creations of electron-positron pairs). From numerical simulations, this energy discrimination can be used for a better understanding of the flux of primary CRs arriving to the terrestrial environment. In this work, we present the project LAGO-Antarctic node (LAGO: Latin American Giant Observatory). The LAGO project is a collaborative network formed by eleven countries (Argentina, Bolivia, Brazil, Chile, Colombia, Ecuador, Guatemala, Mexico, Peru, Spain, and Venezuela). Many of these countries have LAGO-WCDs working in an operative way. The network of WCDs has nodes at sites with different rigidity cut-offs and different altitudes. One of the goals of LAGO is to study the flux of the secondary particles at ground level, and to link them with the associated primary fluxes to better understand the modulation of CRs in the heliosphere. Another main objective is to monitor this flux to provide operative Space Weather information. In particular, we present here an update of the state of the art of the LAGO Antarctic node, to be deployed in the Argentine Marambio base, in the Antarctic peninsula. This node will have the minimum rigidity cut-off ($R_c /sim$ 2 GV) of the collaboration, and will be the only LAGO node that will be able to observe GLEs. We will present the present LAGO Antarctic campaign of 2017-2018 in Marambio, where a meteorological station will be installed, a thermal control system will be tested, and several tests of telemetry from Antarctic to Buenos Aires will be done.
7	Atmospheric temperature profiles at the Antarctic node of LAGO: Quiet and perturbed conditions	Gulisano, A et al.	p-Poster
	V. E. López[1,5], A. M. Gulisano[2,3,4] and S. Dasso[3,4,5] for the LAGO Collaboration[6 ]
	[1]Servicio Meteorológico Nacional de Argentina; [2]Instituto Antártico Argentino, Dirección Nacional del Antártico; [3]Instituto de Astronomía y Física del Espacio, UBA-CONICET; [4]Departamento de Física, FCEN, UBA; [5]Departamento de Ciencias de la Atmósfera y los Océanos, FCEN, UBA; [6]The Latin American Giant Observatory Collaboration: www.lagoproject.org
	The Latin American Giant Observatory (LAGO) is a collaborative network formed by ten countries (Argentina, Bolivia, Colombia, Chile, Ecuador, Guatemala, Mexico, Perú, Venezuela, and Brazil). LAGO has a Space Weather program and one of its main aims is to study the modulation of variability of Cosmic Rays (CRs) using its net of Water Cherenkov Detector (WCDs) and making numerical simulations of the transport of CRs in different physical scenarios. LAGO plans to deploy WCDs at the Antarctic peninsula, in the Argentinean Marambio base. Observations at this node will help to make scientific studies and also to make a monitoring of space weather conditions. Due to the low rigidity cut-off of this high latitude site, observations of Ground Level Enhancements (GLEs) will be possible. In order to carry out numerical simulations to better understand the ground observations of the CRs fluxes, is necessary to characterize the atmosphere, where the secondary particles are created during the extended CRs shower. In this work, we present a characterization of the atmospheric conditions at the Argentinean Marambio base, where the Antarctic LAGO node will be deployed. In particular, we analyze the temperature altitude profile in a range covering the upper troposphere, and the low-mid stratosphere, for quiet conditions and during two major geomagnetic storms, the seasonal climatology of temperatures and investigated possible variations during five intense geomagnetic storms and the possibility of physical and chemical effects during these events. We analyze data obtained from balloon surveys measured at Marambio by the National Meteorological Service of Argentina from 1998 to 2016. We present the seasonal behavior, of the temperature variable environment from 8 to 40 km throughout the period, and analyze the median and quartile statistics during two geomagnetic storms: one in summer and one in winter, extending the analysis period to seven days prior to the occurrence of the storms and to the fourteen subsequent days. In addition, given the different values of the Dst index, we calculated the temperature anomalies, for each geomagnetic storm and the subsequent days, and we also obtained the degrees of cooling and heating, relative to the days prior to the five events.The results of this study will be useful to better understand the possible events of Space Weather and, on the other hand, will also be very useful to make corrections to the flow of cosmic rays, which will be observed in the near future with the particle detector of LAGO to study the solar modulation of the cosmic ray flux and GLE events, in the site with the lower rigidity cut off of this observatory.
8	A set of secondary cosmic rays monitoring	Balabin, Y et al.	p-Poster
	Yury Balabin, Boris Gvozdevsky, Aleksey Germanenko
	Polar Geophysical Institute
	In the Polar Geophysical Institute a complex installation created for secondary cosmic rays monitoring integrates detectors of neutron, charged (electron-muon) and electromagnetic components of secondary cosmic rays. The fluxes of these components are recorded continuously with the resolution of 1 minute. An integral spectrum is recorded by the scintillation detector on a Ø60×20 mm NaI(Tl) crystal within the range of 20-400 keV with two output channels: >20 and >100 keV. The neutron component is measured by two instruments: a conventional neutron monitor 18-NM-64 (NM) and a leadless section (bare NM, bNM). The conventional NM is sensitive to neutrons with energy exceeding ~50 MeV, while bNM is sensitive to neutrons with energy up to 100 keV only. The detector of a charged component consists of two layers of the Geiger-Muller counters. The output of the upper layer and the coincidence of the two layers are used. The upper layer records both the charged particles and gamma-quanta, the scheme of coincidence between the upper and lower layers selects the signal corresponding to a charged particle. The energy threshold for charged particles is estimated ~7 MeV. The installations operate some years and a great database has been accumulated and analyzed. Every year 50-70 increase events of 5 to 65 % in amplitude were registered in the gamma-ray background. The increase events are connected with precipitation. Simultaneously a small effects are in other components are present. An annual variation of the gamma-ray background with amplitude ~30 % were found too. The same installation is set in Barentsburg station (Spitsbergen). The same increase events and annual variation are present.
9	Barentsburg, Apatity, Baksan are neutron monitors with advanced equipment	Balabin, Y et al.	p-Poster
	Yury Balabin[1], Dakhir Dzhappuev[2], Boris Gvozdevsky[1], Aleksey Germanenko[1]
	[1]Polar Geophysical Institute; [2]Baksan Neutrino Observatory
	Neutron monitors (NM) at the stations Barentsburg (arch. Spitzbergen), Apatity (Murmansk reg.) and Baksan (Northern Caucasus) have new rapid recording system. New amplifier-discriminators developed in Polar Geophysical Institute were set. Also detecting tubes of NM were tested and calibrated with help of a weight magnitude analyzer. NMs have been equipped with a rapid registration system. The system records time of each pulse coming with 1 microsecond accuracy. With help of special processing of the data it is possible to detect, separate and investigate different fast phenomena or transform the data to various forms. For example, the "large dead time" mode now realized via soft processing against hardware earlier. It is possible to get "a posteriori" NM data with any time resolution too. It is used universal time and one can look at the NM count data with the same accuracy – 1 mcs.
10	Atmospheric temperature profiles at the Antarctic node of LAGO: Quiet and perturbed conditions	Gulisano, A et al.	p-Poster
	V. E. López[1,5], A. M. Gulisano[2,3,4] and S. Dasso[3,4,5] for the LAGO Collaboration[6 ]
	[1]Servicio Meteorológico Nacional de Argentina; [2]Instituto Antártico Argentino, Dirección Nacional del Antártico; [3]Instituto de Astronomía y Física del Espacio, UBA-CONICET; [4]Departamento de Física, FCEN, UBA; [5]Departamento de Ciencias de la Atmósfera y los Océanos, FCEN, UBA; [6]The Latin American Giant Observatory Collaboration: www.lagoproject.org
	The Latin American Giant Observatory (LAGO) is a collaborative network formed by ten countries (Argentina, Bolivia, Colombia, Chile, Ecuador,Guatemala, Mexico, Perú, Venezuela, and Brazil). LAGO has a Space Weather program and one of its main goals is to study the modulation of variability of Cosmic Rays (CRs) using its net of Water Cherenkov Detector (WCDs) and making numerical simulations of the transport of CRs in different physical scenarios. LAGO plans to deploy WCDs at the Antarctic peninsula, in the Argentinean Marambio base. Observations at this node will help to make scientific studies and also to make a monitoring of space weather conditions. Due to the low rigidity cut-off of this high latitude site, observations of Ground Level Enhancements(GLEs) will be possible. In order to carry out numerical simulations to better understand the ground observations of the CRs fluxes, it is necessary to characterize the atmosphere, where the secondary particles are created during the extended CRs shower. In this work, we present a characterization of the atmospheric conditions at the Argentinean Marambio base, where the Antarctic LAGO node will be deployed. In particular, we analyze the temperature altitude profile in a range covering the upper troposphere, and the low-mid stratosphere, for quiet conditions and during two major geomagnetic storms. We analyze the seasonal climatology of temperatures and investigated possible variations during five intense geomagnetic storms, analyzing the possibility of physical and chemical effects during these events. In order to make a detailed description of the mentioned atmospheric levels, we analyze data obtained from balloon surveys measured at Marambio by the National Meteorological Service of Argentina from 1998 to 2016. We present the seasonal behavior of the temperature variable environment from 8 to 40 km throughout the period and analyze the median and quartile statistics during two geomagnetic storms: one in summer and one in winter, extending the analysis period to seven days prior to the occurrence of the storms and to the fourteen subsequent days. In addition, given the different values of the Dst index, we calculated the temperature anomalies, for each geomagnetic storm and the subsequent days, and also obtained the levels of cooling and heating, relative to the days prior to the five events. The results of this study will be useful to better understand the possible events of Space Weather and to make corrections to the flow of cosmic rays,which will be observed in the near future with the particle detector of LAGO to study the solar modulation of the cosmic ray flux and GLE events, in the site with the lower rigidity cut off of this observatory.