Session - Neutron Monitor science as a fundamental tool for space weather

C. Plainaki, C. Steigies

This session welcomes papers on all aspects of space weather monitoring and prediction, performed either explicitly or partially through the use of the ground-level Neutron Monitor network.

Focus will be given in modeling efforts, tools and space weather applications developed for an operational setting, aiming to the characterization of the solar energetic particles and CMEs properties and to the prediction of their effects to the Earth's atmosphere.
Papers on neutron dosimetry applications, in the context of human exposure to cosmic radiation at high altitudes, in aircraft and spacecraft, are highly welcome.
Cross-disciplinary issues, including the science performed with instruments like PAMELA, AMS, muon telescopes, solar neutron detectors and other, which can provide significant complementary information to the one derived through the use of ground-level neutron monitor data, are of high relevance to this session.
Moreover, GLE prediction efforts performed through the use of ground-based neutron monitor data, potentially in combination with satellite information and theoretical models predictions, are very welcome.
Presentations on future projects related to space weather applications based on the use of neutron monitor data are encouraged.

Talks
Friday November 27, 11:00 - 13:00, Mercator

Poster Viewing
Friday November 27, 10:00 - 11:00, Poster area

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Talks : Time schedule

Friday November 27, 11:00 - 13:00, Mercator

11:00	Contribution of simulation techniques to the space weather research	Paschalis, P et al.	Invited Oral
	Pavlos Paschalis[1], Helen Mavromichalaki[1], Lev I. Dorman[2], Christina Plainaki[3]
	[1] Athens Cosmic Ray Group, Nuclear and Particle Physics Department, Faculty of Physics, National and Kapodistrian University of Athens, Greece; [2] Israel Cosmic Ray & Space Weather Centre and Emilio Ségre Observatory, Tel Aviv University, Israel; [3] INAF-IAPS, Via del Fosso del Cavaliere, 00133, Rome, Italy
	For several decades, the Neutron Monitor detectors located in different places around the World measure the nucleonic component of the particle cascades that are generated in the Earth's atmosphere, due to the galactic cosmic rays. The formation and evolution of the cascades is in direct relation with the space weather conditions outside the Earth's atmosphere. Therefore, Neutron Monitor measurements become fundamental for interpreting the most energetic space weather events. An effective way to study the coupling between energetic solar particles arriving at 1 AU and Neutron Monitor measurements is via simulation techniques. Numerous efforts in this direction have contributed to our better understanding of the space weather events propagation through the terrestrial atmosphere. In this paper, we will present a new model, namely DYASTIMA, based on Geant4, which aims to reveal the particle cascades properties during solar particle events. This tool allows extensive parameterization regarding the structure of the Earth's atmosphere and the spectrum of the cosmic ray particles. The outputs of the application are provided to the user in an efficient format, in order to be easily integrated in further applications. Moreover, simulations have been performed in order to determine the detection efficiency of the Neutron Monitors for the different products of the cascades. DYASTIMA has been successfully used, promising important contributions to space weather applications.
11:15	Application of newly computed neutron monitor yield function for GLE analysis	Mishev, A et al.	Invited Oral
	Alexander Mishev[1], Ilya Usoskin[1], Gennady Kovaltsov[2], Leon Kocharov[3]
	[1] ReSolve Oulu University Finland, [2] Ioffe Physical-Technical Institute of Russian Academy of Sciences, St. Petersburg, Russia,[3] Sodankyla Geophysical Observatory (Oulu unit), University of Oulu
	Here we present recent results of an application of the newly computed neutron monitor yield function for study of spectral and angular characteristics of high-energy solar particles. A method for precise analysis of SEP (solar energetic particle) spectral and angular characteristics on the basis of neutron monitor (NM) data requires realistic modeling of propagation of those particles in the Earth's magnetosphere and atmosphere. The method consists of detailed computation of the NM assymptotic cones of acceptance, application of a NM yield function and a convenient optimization procedure. In this study we use realistic magnetospheric models, namely IGRF as the internal field model and Tsyganenko 89 with the corresponding Kp index as the external field for the computation of the assymptotic directions. In this study, we analyse several major GLE of the solar cycle 23: the Bastille day event on 14 July 2000 (GLE 59), the GLE 69 on 20 January 2005, and the GLE 70 on 13 December 2006. In several cases we assume a complicated particle flux and angular distribution. The SEP spectra and pitch angle distributions were computed with the time step ranging from 5 to 30 minuttes, which allow us to follow the dynamical development of the derived distributions. The obtained results are briefly discussed.
11:30	Global method of data processing: what do neutron monitors see?	Eroshenko, E et al.	Invited Oral
	Eroshenko E., Belov A., Yanke V., Oleneva V., Abunin A., Abunina M.
	Pushkov Institute of Terrestrial Magnetism, Ioniocphere and Radio Wave Propagation (IZMIRAN)
	The worldwide network of neutron monitors was created in the 50th years of the last century and successfully works more than 60 years. Almost all information on long-term modulation of cosmic rays by solar activity is obtained from the neutron monitor network data. The most exact and valuable information turns out when data of all neutron monitors are processed altogether by global methods of the analysis. It allows obtaining more exact variations of the CR density and their spectrum, and also anisotropy of CR. In work examples of various type of variations of CR, first of all Forbush decreases, and also long-term changes of the CR anisotropy are presented. The extensive data accumulated for the long period since 1957 allow one to study a relation of characteristics of CR with conditions in the interplanetary environment, with features of solar sources and with geomagnetic activity. The ground level network registers as well solar cosmic rays called as Ground Level Enhancements (GLEs) – the most energetic of particles which are accelerated on the Sun.
11:45	Variations of the vertical cutoff rigidities for the world wide neutron monitor network over the period of continues monitoring of cosmic rays	Dorman, L et al.	Invited Oral
	B. Gvozdevsky[1], L. Dorman[2,3], A. Abunin[2], M. Preobrazhensky[2], R. Gushchina[2], A. Belov[2], E. Eroshenko[2], U. Dai[3], L. Pustil’nik[3], V. Yanke[2]
	[1] Polar Geophysical Institute, 184209, Firsmana str., 14, Apatity, Russia; [2] IZMIRAN, Kalushskoe ave., 4, Troitsk, Moscow, 142190, Russia; [3] Israel Cosmic Ray and Space Weather Center with Emilio Segre’ Observatory on Mt. Hermon, affiliated to Tel Aviv University, Golan Research Institute, and Israel Space Agency, Israel
	Vertical cutoff rigidities for the world wide neutron monitor network are obtained with one year resolution during the period of 1950-2015 by the method of trajectory calculations. The models of Definitive Geomagnetic Reference Field and International Geomagnetic Reference Field have been used for 1950-2010 and 2015 correspondingly. Besides, cutoff rigidities for the whole period were obtained using model by Tsyganenko Ts89 with involving yearly mean values of Kp index. In each case an estimation of penumbra contribution was made in approximation of flat and low spectra (0 and -1) of cosmic ray variations. The results testify total decrease of cut off rigidities practically in the all locations, which is apparently connected to the common decrease of magnetic field in a considered period.
12:00	On the origin of relativistic solar particle events: neutron monitor observations, radio emission, and interplanetary transport modelling	Klein, K et al.	Oral
	K.-L. Klein[1], N. Agueda[2], R. Bütikofer[3]
	[1] Observatoire de Paris, LESIA, 92190 Meudon, France; [2] Departament d’Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, Spain; [3] University of Bern, Space Research & Planetary Sciences, 3012 Bern, Switzerland
	The highest energies of solar energetic nucleons detected in space or through gamma-ray emission in the solar atmosphere are in the GeV energy range. Where and how these particles are accelerated is still under debate. Possible processes are related to magnetic reconnection in a flare or in the aftermath of a coronal mass ejection (CME), and to the shock wave driven by a fast CME. The subject is of general astrophysical interest, because it is through energetic particles that many astrophysical objects become detectable. Energetic particles are also a major vector of solar-terrestrial relationships, and the fastest of them can be used in advance warning schemes. We search for observational evidence of the acceleration site, via comparative analyses of the timing of the relativistic solar proton intensity, observed by neutron monitors on the Earth, and electromagnetic emissions of the associated eruptive solar activity. The microwave emission, at frequencies above 10 GHz, emphasises the impulsive flare phase, while emissions at lower frequencies (hundreds of MHz to a few GHz) reveal both the impulsive flare and post-impulsive particle acceleration. We use different time profiles of the radio emission to describe the solar injection function and model the interplanetary particle transport taking into account the effects of focusing by an average Archimedean magnetic field, and scattering by its fluctuations. The predicted time profiles of the relativistic protons at 1 AU are compared with neutron monitor observations of events in solar cycle 23 (1997-2006). We use the results to discuss the nature of the prompt and delayed relativistic proton releases that have been identified in neutron monitor recordings of relativistic solar particle events.
12:15	About influence of the coronal holes lon the geomagnetic activity and cosmic ray variations	Abunina, M et al.	Oral
	Maria Abunina[1], Artem Abunin[1], Anatoly Belov[1], Evgenia Eroshenko[1], Sergey Gaidash[1], Victoria Oleneva[1], Victor Yanke[1], Olga Kryakunova[2]
	[1] Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Russia; [2] Institute of Ionosphere, Kazakhstan
	Variations of cosmic ray density and anisotropy in high-speed streams of a solar wind from various solar coronal holes are studied in relation with changes of indexes of geomagnetic activity. About 400 coronal holes observed in 1996-2013 were divided into groups accordingly to their polarity and heliolatitude. It is shown that northern holes with negative polarity and the southern holes with positive polarity are more effective in creation of geomagnetic activity than other holes. The behavior of the cosmic ray vector anisotropy (especially its North -southern component) significantly depends on polarity of a magnetic field in a high-speed stream. The obtained results have to be useful to the prognosis of geomagnetic activity and diagnostics of large-scale interplanetary disturbances.
12:30	Can We Observe Remote Coronal Mass Ejections using Neutron Monitor Data?	Thomas, S et al.	Oral
	Simon R Thomas[1], Mathew J Owens[2], Mike Lockwood[2], Chris Owen[1]
	[1] Mullard Space Science Laboratory, University College London, UK; [2] University of Reading, UK.
	Neutron monitor (NM) count rates are modulated by both particle drift patterns and solar wind structures on a range of time scales. Over solar cycles, they vary as a function of the total open solar magnetic flux and the latitudinal extent of the heliospheric current sheet. Over time-scales of hours, drops of a few percent in NM count rates (Forbush decreases, FDs) are well known to be associated with the near-Earth passage of solar wind structures resulting from corotating interaction regions (CIRs) and transient coronal mass ejections (CMEs). We present observations of FDs seen at ground-based NMs which cannot be immediately associated with significant structures in the local solar wind. Similarly, there are significant near-Earth structures which do not produce any variations in NM count rates. Three FDs are shown to be during the STEREO era, enabling in-situ and remote observations from three well-separated heliospheric locations. Extremely large CMEs passed the STEREO- A spacecraft, which was behind the West limb of the Sun, approximately 2-3 days before each near-Earth FD. Solar wind simulations suggest that the CMEs combined with pre-existing CIRs, enhancing the pre-existing barriers to GCR propagation. Our observations provide strong evidence for the modulation of GCR flux by remote solar wind structures and an investigation into changes in the diurnal variation of NM count rates displays a good potential to detect these remote structures using neutron monitor data.
12:45	Mini neutron monitor measurements at the Neumayer III station and on the German research vessel Polarstern	Heber, B et al.	Invited p-Poster
	B. Heber[1], D. Galsdorf[1], J. Gieseler[1], C. Herbst[1], J. Labrenz[1], C. Schwerdt[2], M. Walther[2], R. Fuchs[3], H. Krueger[3], and H. Moraal[3]
	[1] Christian-Albrechts-Universität zu Kiel; [2] Deutsches Elektronen-Synchrotron DESY, D-15738 Zeuthen; [3] Center for Space Research, North-West University, Potchefstroom 2520, South Africa
	Neutron monitors (NMs) are ground-based devices to measure the variation of cosmic ray intensities. They are reliable devices but difficult to install because of their size and weight. Therefore a portable mini NM (MNM) that can be installed as an autonomous station at any location that provides suitable conditions has been developed recently. The first continuous measuring MNMs are installed at Neumayer III and the German vessel Polarstern. They are providing scientific data since October 2012 and January 2014, respectively. NM measurements are influenced by the (variable) Earth magnetic field and the atmospheric conditions. Thus in order to interpret the data a detailed knowledge of the instrument sensitivity with geomagnetic latitude (rigidity) and atmospheric pressure is essential. The rigidity dependence is determined experimentally by utilizing several latitude scans. The Polarstern was specially designed for working in the polar seas and scans usually twice a year the rigidity range below 1 GV and above 10 GV. The results of different latitude scans from October 2012 to October 2015 will be presented and discussed in the framework of a yield function.
12:50	The ICME’s magnetic field and the role on the galactic cosmic ray modulation for the solar cycle 23	Paouris, E et al.	Invited p-Poster
	Evangelos Paouris, Helen Mavromichalaki
	Faculty of Physics, National and Kapodistrian University of Athens, Athens, Greece
	It is well known that the interplanetary coronal mass ejections (ICMEs) play the most important role on the interactions with the magnetosphere as they are the dominant drivers of intense geomagnetic storms. In this work the reproduction of galactic cosmic ray intensity using for the first time the magnetic field of ICMEs is presented. A number of 165 ICMEs associated with CMEs were spotted from SOHO-LASCO coronagraph and their characteristics were calculated by in situ observations from ACE data covering the years 1996–2009. The result of this study is a new ICME list which contains all the available information for the background geomagnetic conditions before the arrival of the shock, the sheath between the shock and the main part of the ICME and the ICME itself, such as velocities, magnetic fields (Bsheath, BICME and Bz) and plasma characteristics (plasma β, temperature and density) and the geomagnetic conditions, such as the Dst index minimum and the maximum Ap values. This new ICME list has been used for the reformation of the CME-index (Pi) taking into account for first time the magnetic field of these ICMEs and other characteristics as well, such as their angular width and their velocity. This CME-index is used in combination with other solar and heliospheric variables in order to study the cosmic ray modulation for the solar cycle 23, which was a very interesting solar cycle in the sense of solar activity.

Posters

Friday November 27, 10:00 - 11:00, Poster area

1	Mini neutron monitor measurements at the Neumayer III station and on the German research vessel Polarstern	Heber, B et al.	Invited p-Poster
	B. Heber[1], D. Galsdorf[1], J. Gieseler[1], C. Herbst[1], J. Labrenz[1], C. Schwerdt[2], M. Walther[2], R. Fuchs[3], H. Krueger[3], and H. Moraal[3]
	[1] Christian-Albrechts-Universität zu Kiel; [2] Deutsches Elektronen-Synchrotron DESY, D-15738 Zeuthen; [3] Center for Space Research, North-West University, Potchefstroom 2520, South Africa
	Neutron monitors (NMs) are ground-based devices to measure the variation of cosmic ray intensities. They are reliable devices but difficult to install because of their size and weight. Therefore a portable mini NM (MNM) that can be installed as an autonomous station at any location that provides suitable conditions has been developed recently. The first continuous measuring MNMs are installed at Neumayer III and the German vessel Polarstern. They are providing scientific data since October 2012 and January 2014, respectively. NM measurements are influenced by the (variable) Earth magnetic field and the atmospheric conditions. Thus in order to interpret the data a detailed knowledge of the instrument sensitivity with geomagnetic latitude (rigidity) and atmospheric pressure is essential. The rigidity dependence is determined experimentally by utilizing several latitude scans. The Polarstern was specially designed for working in the polar seas and scans usually twice a year the rigidity range below 1 GV and above 10 GV. The results of different latitude scans from October 2012 to October 2015 will be presented and discussed in the framework of a yield function.
2	The ICME’s magnetic field and the role on the galactic cosmic ray modulation for the solar cycle 23	Paouris, E et al.	Invited p-Poster
	Evangelos Paouris, Helen Mavromichalaki
	Faculty of Physics, National and Kapodistrian University of Athens, Athens, Greece
	It is well known that the interplanetary coronal mass ejections (ICMEs) play the most important role on the interactions with the magnetosphere as they are the dominant drivers of intense geomagnetic storms. In this work the reproduction of galactic cosmic ray intensity using for the first time the magnetic field of ICMEs is presented. A number of 165 ICMEs associated with CMEs were spotted from SOHO-LASCO coronagraph and their characteristics were calculated by in situ observations from ACE data covering the years 1996–2009. The result of this study is a new ICME list which contains all the available information for the background geomagnetic conditions before the arrival of the shock, the sheath between the shock and the main part of the ICME and the ICME itself, such as velocities, magnetic fields (Bsheath, BICME and Bz) and plasma characteristics (plasma β, temperature and density) and the geomagnetic conditions, such as the Dst index minimum and the maximum Ap values. This new ICME list has been used for the reformation of the CME-index (Pi) taking into account for first time the magnetic field of these ICMEs and other characteristics as well, such as their angular width and their velocity. This CME-index is used in combination with other solar and heliospheric variables in order to study the cosmic ray modulation for the solar cycle 23, which was a very interesting solar cycle in the sense of solar activity.
3	Computation of Ion Production Rate and Ionization Effect During Bastille Day GLE 59 and GLE 70 Events	Mishev, A et al.	e-Poster
	Alexander Mishev[1], Peter Velinov[2]
	[1] ReSolve University of Oulu; [2] Institute for Space Research and Technology, Bulgarian Academy of Sciences
	Cosmic ray particles play an important role in various processes related to atmospheric physics and chemistry via the ionization. The galactic cosmic rays (GCR) are the main source of ionization in the Earth stratosphere and troposphere. In addition, solar energetic particles enhance the ion production, specifically over polar caps during major solar eruptive processes. A special case of such events, namely ground level enhancements (GLE) deserve special interest. During the solar cycle 23, sixteen GLE events were observed with intensities ranging ∼ 3 – 277%. The first event occurred on 6 November 1997 (GLE 55) and the last event occurred on 13 December 2006 (GLE 70). In the paper presented here we focus on GLE 59, which is the first major event positioned exactly at the maximum of solar cycle 23. The previous four events (GLE 55 – 58) in the rise phase of solar cycle 23 were observed with intensities ranging ∼ 3 − 11% of enhancement of the neutron monitor count above the background. The largest neutron monitor (NM) count rate increase on GLE 59 was observed at the South Pole and SANAE with increase of 58.3% and 54.5%, respectively. During the GLE 70 the cosmic rays reached an increase of 92% at Oulu NM. Therefore, the Bastille day event on 14 July 2000 as well as the event observed on 13 December 2006 are among the strongest and the most interesting events at a recent time. Here we presented the computation of ion production rate and corresponding ionization effect during the Bastille day and GLE 70 events. We apply a full Monte Carlo 3-D model for cosmic ray induced ionization in order to compute the ion production. The ion production rate during the events is considered as a superposition of realistically considered galactic cosmic ray flux taking into account the accompanying Forbush decrease and solar energetic particles. The ion production rate and ionization effect are computed as a function of the altitude above the sea level at several rigidity cut-offs, namely 1 GV, 2 GV and 3 GV. In the work are given some applications of GCR ionization effects to explaining the processes and mechanisms of the space weather.
4	Understanding SEP properties through Neutron Monitor data modeling	Plainaki, C et al.	e-Poster
	C. Plainaki[1,2], H. Mavromichalaki[2], M. Laurenza[1], M. Andriopoulou[3], M. Gerontidou[2], A. Belov[4], E. Eroshenko[4], V. Yanke[4]
	[1] INAF-IAPS, Via del Fosso del Cavaliere, 00133, Rome, Italy; [2] Nuclear and Particle Physics Section, Physics Dpt., National and Kapodistrian University of Athens, Greece; [3] Space Research Institute, Austrian Academy of Sciences, Graz, Austria; [4] Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation by Pushkov (IZMIRAN), Moscow, Russia
	It is now widely known that the GLE data recorded by the worldwide Neutron Monitor network are a useful resource for space weather modeling during solar extreme events. Among the numerous space weather models available to the community, the NMBANGLE PPOLA [1] is a modified version of the original NMBANGLE model [2], based on Dorman's coupling coefficient method [3], aiming at the calculation of the SEP properties during GLEs through the exclusive use of ground-based Neutron Monitor data from the worldwide network. Technically, the model treats this network as an integrated omnidirectional spectrometer and solves the inverse problem of the SEP-GLE coupling. In particular, the NMBANGLE PPOLA model dynamically calculates the SEP spectrum and flux spatial distribution at some altitude in the atmosphere, assuming a power-law in rigidity primary spectrum with two free parameters (spectral index and amplitude) and a narrow-beam angular distribution for the SEP flux direction [1]. In this paper, we present a short overview of the application of the NMBANGLE PPOLA model to different GLEs, discussing the derived characteristics of the relativistic SEP fluxes. We also discuss some improvements of the current model in the context of Space Weather efficient monitoring. [1] Plainaki C, et al. 2010 Sol. Physics 264 239 [2] Plainaki C, et al. 2007 J. Geophys. Res. A 112 4102 [3] Dorman LI 2004 Astrophys. Space Sci. Libr. 303
5	Spectra and anisotropy of GLEs on the basis of NM data	Mishev, A et al.	e-Poster
	Alexander Mishev, Ilya Usoskin
	ReSolve Oulu University Finland
	Here we present recent results of an application of the newly computed neutron monitor yield function for study of spectral and angular characteristics of high-energy solar particles. A method for precise analysis of SEP (solar energetic particle) spectral and angular characteristics on the basis of neutron monitor (NM) data requires realistic modeling of propagation of those particles in the Earth's magnetosphere and atmosphere. The method consists of detailed computation of the NM assymptotic cones of acceptance, application of a NM yield function and a convenient optimization procedure. In this study we use realistic magnetospheric models, namely IGRF as the internal field model and Tsyganenko 89 with the corresponding Kp index as the external field for the computation of the assymptotic directions. In this study, we analyse several major GLE of the solar cycle 23: the Bastille day event on 14 July 2000 (GLE 59), the GLE 69 on 20 January 2005, and the GLE 70 on 13 December 2006. In several cases we assume a complicated particle flux and angular distribution. The SEP spectra and pitch angle distributions were computed with the time step ranging from 5 to 30 minuttes, which allow us to follow the dynamical development of the derived distributions. The obtained results are briefly discussed.
6	Forbush decreases associated to Stealth Coronal Mass Ejections	Heber, B et al.	e-Poster
	B.Heber[1],  D. Galsdorf[1], C. Herbst[1], P. Kuehl[1] ,  M. Dumbovic[2],   B. Vršnak[2],   A. Veronig[3],   M. Temmer[3],   C. Moestl[3]
	[1] Christian-Albrechts-Universität zu Kiel; [2] Hvar Observatory, Faculty of Geodesy, University of Zagreb; [3] Institute of Physics/Kanzelhöhe Observatory, University of Graz, Austria
	Interplanetary coronal mass ejections (ICMEs) are structures in the solar wind that are the counterparts of coronal mass ejections (CMEs) at the Sun. It is commonly believed that enhanced magnetic fields in interplanetary shocks and solar ejecta as well as the increased turbulence in the solar wind sheath region are the cause of Forbush decreases (FDs) representing decreases of galactic cosmic ray (GCR) intensities. Recently, stealth CMEs i.e.~CMEs with no apparent solar surface association have become a subject in recent studies of solar activity. Whether all of such stealth CMEs can drive a FD is difficult to investigate on the basis of neutron monitor NM measurements because these measurements not only reflect the GCR intensity variation in interplanetary space but also the variation of the geomagnetic field as well as the conditions in the Earth atmosphere. However, together with single detector counters from spacecraft instrumentation with a counting statistic simillar to the one of NMs allows allows the investigation of such small FDs. This work has been supported in part by Croatian Science Foundation under the project 6212 „Solar and Stellar Variability“ and by MZOS/DAAD bilateral project CORAMOD.
7	Rapid determination of cutoff rigidities and asymptotic directions for near real-time space weather applications based on neutron monitor measurements	Bütikofer, R et al.	e-Poster
	Rolf Bütikofer[1], Erwin Flückiger[1], Dennis Galsdorf[2], Bernd Heber[2], Konstantin Herbst[2], Christian Steigies[2]
	[1] Physikalisches Institut, University of Bern / HFSJG, Bern, Switzerland; [2] Institut für Experimentelle und Angewandte Physik / Extraterrestrial Physics, Christian-Albrechts-Universität, Kiel, Germany
	The investigation of solar cosmic ray events based on neutron monitor measurements requires detailed knowledge about the trajectories of charged particles in the Earth’s magnetic field. This information is needed with a high time resolution and for the current level of disturbance of the geomagnetic field. The determination by the standard technique of trajectory computation is a time-consuming process. Furthermore, the magnetic field controlling the transport of charged particles near Earth is dynamic and exhibits variations on different time scales ranging from minutes to millenia. Today’s space weather applications request computations in near real-time. Therefore it is reasonable to compute trajectories of cosmic ray particles in the magnetic field of the Earth in advance and to stack parameters to describe cutoff rigidities and asymptotic directions at the locations of the neutron monitors of the worldwide network into a database for quick computation. In this work we investigate the possibility to rapidly describe the cutoff rigidity and the asymptotic directions of neutron monitor locations for specific times and geomagnetic activity by a quick procedure based on a limited number of parameters archived in a database.
8	Upgrading the Dourbes cosmic ray observatory for research and development of improved space weather monitoring services	Sapundjiev, D et al.	e-Poster
	D. Sapundjiev[1], C. Steigies[2], T. Verhulst[1], J. C. Jodogne[1], S. Stankov[1]
	[1] Royal Meteorological Institute (RMI), Ringlaan 3, B-1180 Brussels, Belgium; [2] Christian-Albrechts-Universität, Olshausenstrasse 40, D-24098 Kiel, Germany
	This presentation will outline the recent and future activities at the Royal Meteorological Institute (RMI) regarding space weather research, monitoring, and developing of related services, with focus on the modernisation and use of the cosmic ray observatory. At the RMI Geophysical Centre in Dourbes (50.1°N, 4.6°E), various space weather observations -- cosmic ray, ionospheric, geomagnetic -- have been carried out for a long time. During the years, a large database has been accumulated and used for space weather research and development of services. Currently, the Dourbes cosmic ray observatory consists of a standard NM64 neutron monitor (with 9 counters) which is in operation since 1965 (http://www.nmdb.eu/?q=node/469). Considering that the ground-based neutron monitors are still state-of-the-art and most popular instrumentation for monitoring the cosmic rays, we have invested in 9 new counter tubes which will allow us to build an extended 18-counter neutron monitor. A larger neutron monitor will provide a much better time resolution and lower uncertainty thanks to the greater counting rate. The statistical fluctuations of the measurements will be decreased and allow detection of smaller variations in the cosmic ray intensity and therefore smaller events in the solar activity. The improved geometry and volume with the additional sections of the monitor will increase three to four times the counting rate and allow investigation of a lower intensity solar events. The Dourbes neutron monitor is a member of the international family of neutron monitors, providing data to the International Neutron Monitor Database (NMDB). Earlier this year, new computer hardware and software was installed at the site, allowing for the real-time data provision to NMDB. It is well understood that advanced space weather services are possible only when high time resolution and real time data from multiple sources are readily available and our institute is doing its best to provide such data to the international community of scientists and other users. Investment plans are put in place to complement the neutron monitor observations with measurements of the muon component of the atmospheric cascade. Muon detectors use the good penetration capability of muons in matter to easily distinguish muons from other cosmic ray components (except for neutrinos). Thus, the installation of an underground muon detector in Dourbes will allow the monitoring of the high-energy part of the muon component.
9	Meteorological effects of muon component at the mountain muon detectors	Dorman, L et al.	e-Poster
	L. Dorman[2], A. Asipenka[1], A. Abunin[1], V. Yanke[1], U. Dai[2], L. Pustil’nik[2], M. Zazayan[3], M. Ganeva[4], Zhang Ji Long[5], Jean-Luc Autran[6], I. Angelov[7], A. Sternlieb[2]
	[1] IZMIRAN, Kalushskoe ave., 4, Troitsk, Moscow, Russia, 142190; [2] Israel Cosmic Ray and Space Weather Center with Emilio Segre’ Observatory on Mt. Hermon, affiliated to Tel Aviv University, Golan Research Institute, and Israel Space Agency; [3] Yerevan Physics Institute, Alikhanian Brothers Str. 2, 0036, Yerevan, Armenia; [4] Jülich Centre for Neutron Science (JCNS), Outstation at MLZ, Lichtenbergstr. 1, 85747 Garching, Germany; [5] Institute of High Energy Physics, Beijing, China; [6] Aix-Marseille University, BP 146, F-13384 Marseille Cedex 13, France; [7] South West University “N. Rilski” Institute For Nuclear Reasearch and Nuclear Energy, BAS
	Temperature effect of mountain muon detectors which exceeds a little that expected theoretically, was studied in this work. Meteorological effects of such detectors have their own peculiarities and practically were not investigated before. Data from multidirectional detectors YangBaJing, Moussala, Bure, Mt. Hermon, Yerevan (2000 м) were used for calculations from the created in IZMIRAN database of muon detectors “mddb”. To exclude model dependence the meteorological effects were studied by different methods.
10	Inversion of Source and Transport Parameters of Relativistic SEPs from Neutron Monitor Data	Bütikofer, R et al.	e-Poster
	Rolf Bütikofer[1], Neus Agueda[2], Rami Vainio[3], Bernd Heber[4], Alexander Afanasiev[3], Olga E. Malandraki[5]
	[1] University of Bern (Switzerland); [2] University of Barcelona, ICCUB (Spain); [3] University of Turku (Finland); [4] Christian-Albrechts-Universität zu Kiel (Germany); [5] National Observatory of Athens (Greece)
	We present a new methodology to study the release processes of relativistic solar energetic particles (SEPs) based on the direct inversion of Ground Level Enhancements (GLEs) observed by the worldwide network of neutron monitors (NMs). The new approach makes use of several models, including: i) the propagation of relativistic SEPs from the Sun to the Earth, ii) their transport in the geomagnetosphere, and iii) in the Earth's atmosphere, as well as iv) the detection of the nucleon component of the secondary cosmic rays in the atmosphere by ground based NMs. The combination of these models allows us to compute the expected ground-level NM counting rates for a series of instantaneous releases from the Sun. The amplitudes of the source components are then inferred by fitting the NM observations with the modeled NM counting rate increases. Within the HESPERIA project, we will develop the first software package for the direct inversion of GLEs and we will make it freely available for the solar and heliospheric communities. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 637324.
11	Improvements on the Neutron Monitor Data Acquisition System	Garcia, O et al.	p-Poster
	Oscar Garcia-Poblacion[1,2], Ignacio Garcia-Tejedor[1,2], Juan Jose Blanco[1,2], Raul Gomez-Herrero[1,2], Jose Medina[1,2]
	[1] Space Research Group, University of Alcala. Spain; [2] The CaLMa Neutron Monitor, Science and Technology Park of Guadalajara, Spain
	The data acquisition system developed as a result of the Neutron Monitor Database European project has been evolved with new features that will ease the adoption by new or existing stations. A new modular design, support for different types of barometers and high voltage power supply monitoring features have been introduced. This work also describes the efforts in providing new IP cores for pulse counting, pulse height analysis and multiplicity detection, along with the software needed to obtain usable data for further study. This data acquisition system can be easily adapted to the existing neutron monitors, providing a common electronics foundation to all the stations that would allow more coherent data comparison among them.
12	Account of dynamic effect of the atmospheric wind in the neutron monitor data at the Antarctic station Mirny.	Eroshenko, E et al.	p-Poster
	Kobelev P., Yanke V., Belov A., Eroshenko E., Gushchina R., Smirnov D.
	Pushkov Institute of Terrestrial Magnetism, Ionosphere and Rdio Wave Propagation, [IZMIRAN]
	Estimation of barometric coefficient for neutron component of cosmic rays was performed for Antarctic station Mirny taking into account effect of dynamic pressure caused by wind in the atmosphere. Hourly data of continue monitoring of neutron component and data of the local meteo station have been used for the period 2007-2014. Wind velocity at the observatory Mirny reaches 45 m/s in winter that corresponds to dynamic pressure of 5-6 mb and leads to the error of 5% in variations of neutron component because of dynamic effect in the atmosphere. The results are interesting for high latitude and high mountain detectors, where dynamic effect may be significant.
13	Method of global survey (GSM) and corresponding tools for data preparation.	Eroshenko, E et al.	p-Poster
	E. Eroshenko, A. Abunin, M. Abunina, A.Belov, V. Oleneva, V. Yanke
	Pushkov Institute of Terrestrial Magnetism, Ioniocphere and Radio Wave Propagation (IZMIRAN)
	Need to have the global parameters of cosmic rays independent of the location of a point of observation on Earth, led to creation of special methods ("Methods of global survey") which use data from as big as possible number of the stations distributed on the globe. In effect, in all options is a method of the spherical analysis where decomposition of a variation of cosmic rays on spherical harmonics is used. If the network of observing stations was located not on Earth surface, and outside the atmosphere and a magnetosphere, the task would be reduced simply to the spherical analysis. But before using this method, it is necessary to prepare data of neutron monitors as appropriate. In this work instruments of preliminary preparation of data, and also one of options of a method of global survey developed in IZMIRAN are considered.
14	A study of the polar and middle latitude neutron monitors during the extended geomagnetic storm of March 17, 2015	Mavromichalaki, H et al.	p-Poster
	H. Mavromichalaki[1], M. Gerontidou[1], E. Paouris[1], A. Belov[1], E. Eroshenko[2], V. Yanke[2], D. Lingri[1], A. Laoutaris[1], A. Kanellakopoulos[1], A. Abunin[2], M. Abunina[2]
	[1] Nuclear and Particle Physics Department, Faculty of Physics, National and Kapodistrian University of Athens; [2] Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation by Pushkov (IZMIRAN), Moscow, Russia
	Although the current solar cycle 24 is characterized by low solar activity, on March 2015 the most intense geomagnetic storm (G4) of the current solar cycle was recorded. It started on March 17th and it was the result of the interaction between the complex solar activity which spotted at the active region AR2297 S22W29 and a high speed solar wind stream from a huge south polar coronal hole with Earth’s magnetosphere. Especially a magnetic filament accompanied by a C9.1 solar flare with peak time at 02:13 U.T. hurled an Earth directed CME into the interplanetary space. This ICME arrived at Earth in the first hours of March 17th and a minimum of Dst index of -223 nT (preliminary data) was noticed at 22:00-23:00 U.T. The daily value of Ap was 108, that is the highest daily Ap from October 2004. Analyzing cosmic ray intensity data among polar and middle latitude neutron monitor stations the existence of a geomagnetic storm was observed, resulting to the variation of the energy threshold and magnetic rigidity of the middle latitude stations. Moreover an extended study of the asymptotic cones of the neutron monitor stations during this event according to Tsyganeko T96 model showed that the disturbances of Kp were recorded before those of Dst index. Interesting results on the geomagnetic indices are discussed.
15	Pressure correction of the Neutron Monitor data during the last solar cycle	Gerontidou, M et al.	p-Poster
	M. Gerontidou, I. Platanos, P. Paschalis, H. Mavromichalaki
	Nuclear and Particle Physics Department, Faculty of Physics, National and Kapodistrian University of Athens, 15784 Athens Greece
	The barometric effect induces variations to the measured data of the Neutron Monitors which are related to the variations of local atmospheric pressure of each station. For this reason the calculation of barometric coefficient constitutes a prerequisite for the quality of data. In this work the long-term variation of the barometric coefficient using for the pressure correction of the Neutron Monitor data over the last solar cycle, is studied. For the estimation of the barometric coefficient the online barometric coefficient tool provided as a web application through the Athens Cosmic Ray Station (http://cosray.phys.uoa.gr/index.php/data/nm-barometric-coefficient) and the European High Resolution Neutron Monitor Database (NMDB; http://www.nmdb.eu), are used. This application has an advantage to use data of a reference station that leads to satisfactory results even in the active cosmic ray periods (Paschalis et al., 2013). The accurate calculation of the barometric coefficient from datasets of different Neutron Monitor stations indicates that it seems to follow the 11-years behavior of the solar cycle. (Paschalis et al., New Astronomy, 19, 10-18, 2013)
16	Proton enhancements of solar cosmic rays in January and March 2012	Kryakunova, O et al.	p-Poster
	A.Belov[1], E.Eroshenko[1], O.Kryakunova[2], N.Nikolayevskiy[2], A.Malimbayev[2], I.Thepakina[2], V.Yanke[1]
	[1] Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation (IZMIRAN), Moscow, Russia; [2] Institute of Ionosphere, Almaty, Kazakhstan
	The behavior of the cosmic ray intensity at the worldwide neutron monitor network in the events of 2012, when there was a significant increase of the integral proton flux with energies > 100 MeV, namely in the events of January 27 , March 7 and March 13, 2012 was analyzed together with the parameters of the interplanetary space. On January 27, 2012 an increase of the neutron monitors (NMs) counting rate of ~2%, coincides in time with a proton increase at the integral intensity recorded onboard the GOES satellite (E>100 MeV) and also with increases at the differential intensities of HEPAD at several high energy channels (>500 MeV). On March 13, 2012 an increase at the counting rate similar in size to the event on January 27 is observed on several high-latitude NMs at the same time that an increase in GOES high energy protons. The most difficult and most interesting situation that deserves a detailed analysis, modeling and further investigation, took place on March 7. In this event, the arrival of solar cosmic rays to Earth coincided in time with large modulation effects in galactic cosmic rays and with significant magnetospheric disturbance. All three events at the beginning of 2012 may be considered as candidate ground level enhancements of solar cosmic rays (GLEs).
17	Effective and ambient dose calculation at flight altitudes with the newly computed yield functions	Mishev, A et al.	p-Poster
	Alexander Mishev, Ilya Usoskin
	ReSolve CoE University of Oulu Finland
	An important topic in the field of space weather research is estimation of the expected exposure of aircrew at flight altitudes due to cosmic rays, specifically during major solar energetic particle events. The primary cosmic ray particles induce a complicated nuclear-electromagnetic-muon cascade in the Earth’s atmosphere. The secondary particles form the main source of increased exposure at flight latitudes compared to the sea level. In this work we propose a numerical model for computation of the effective/ambient dose equivalent at flight altitude. It represents a full chain analysis, namely estimation of the solar particle spectral and angular characteristics from neutron monitor data and application of the newly computed yield function for the effective/ambient dose. The new computed yield functions for conversion of secondary particle flux to dose were obtained on the basis of extensive Monte Carlo simulation of the atmospheric cascade induced by primary protons and alpha particles and subsequent application of recently computed conversion coefficients. A comparison with the reference data is performed. A good agreement is achieved. Several example calculations are demonstrated.
18	A Comparative study of the Longitudinal and Latitudinal Cosmic Ray Diurnal Anisotropy for the time period 2001-2014	Tezari, A et al.	p-Poster
	A. Tezari[1], S. Kolovi[1], A. Kanellakopoulos[1], H. Mavromichalaki[1], C. Plainaki[2], M. Andriopoulou[3]
	[1] Nuclear and Particle Physics Department, Faculty of Physics, National and Kapodistrian University of Athens,  Zografos,  15784 Athens, Greece; [2] INAF-IAPS, Via del Fosso del Cavaliere, 00133, Rome, Italy; [3] Space Research Institute, Austrian Academy of Sciences, Graz, Austria
	The diurnal anisotropy of cosmic ray intensity for the time period 2001 to 2014 is studied, covering the maximum and the descending phase of the solar cycle 23, the minimum of the solar cycles 23/24 and the ascending phase of the solar cycle 24. Cosmic ray intensity data from the neutron monitor stations of Athens (Rc = 8.53 GV), Oulu (Rc = 0.81 GV) and Lomnický štít (Rc = 3.84 GV) located at the same geographic longitudes and different geographic longitudes, are used. Moreover data from Moscow (Rc = 2.43 GV), Kiel (Rc = 2.36 GV) and Newark (Rc = 2.40 GV) stations characterized by the same cut-off rigidities, are also examined. Τhe amplitude and the phase of the diurnal anisotropy vectors have been calculated on annual and monthly basis using Fourier analysis. The geomagnetic bending for each station is determined from the asymptotic cones of each station via the Tsyganenko96 magnetospheric model. From our analysis, it is resulted that there is a different behavior of the diurnal anisotropy vector during the different phases of the solar cycles depending on the solar magnetic field polarity. Results will be useful for long- term space weather monitoring, to be integrated in the existing ones based on ground based data or/and modeling.
19	The Behaviour of Galactic Cosmic Rays near the Heliospheric Current Sheet	Thomas, S et al.	p-Poster
	Simon R Thomas[1], Mathew J Owens[2], Mike Lockwood[2], Chris Scott[2], Chris Owen[1]
	[1] Mullard Space Science Laboratory, University College London, UK; [2] University of Reading, UK.
	Neutron monitor (NM) count rates (used here as a proxy for the galactic cosmic ray (GCR) flux arriving at Earth) are modulated by transient features such as coronal mass ejections or the heliospheric current sheet (HCS). The HCS separates the outward and inward polarities of magnetic field from the Sun and hence is a large-scale feature which extends out through the heliosphere. Due to the close association between the HCS, the streamer belt, and the band of slow solar wind, HCS crossings are often associated with corotating interaction regions (CIRs) where fast solar wind catches up and compresses slow solar wind ahead of it. However, not all HCS crossings are associated with strong compressions. Therefore, by observing only HCS crossings without an intense CIR, we observe only the effect of the change in magnetic field polarity across the HCS. We find that NM count rates have a tendency to peak in the away magnetic field sector. The data is further split by the dominant polarity at each solar polar region which reveals information on differences in large-scale GCR drifts. Spacecraft data of energetic particles is used to establish whether the enhancement in GCR flux is due to connectivity with the heliosphere, or whether it is present within the solar wind.
20	Multi-instrument radiation monitoring at the Testa Grigia high altitude Observatory	Laurenza, M et al.	p-Poster
	Monica Laurenza[1], Marisa Storini[1], Fabrizio Signoretti[1], Alba Zanini[2], Piero Diego[1,3], Stefano Massetti[1], Juan Carlos Terrazas[4], Alessandro Liberatore[2], Adolfo Esposito[5]
	[1] IAPS/INAF, via del Fosso del Cavaliere 100, 00133 Roma, Italy; [2] INFN Sez. Torino, Via Pietro Giuria 1, 10125 Torino, Italy; [3] Dipartimento di Fisica Università di Trento, Via Sommarive 14, 38123 Povo (TN), Italy; [4] INAF-OATo Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy; [5] LNF-INFN Via E. Fermi 40, 00044 Frascati, (RM), Italy
	Cosmic rays (CRs) are important components of the ionizing radiation that affects the Earth's environment. In particular, their interaction with the atmosphere produces secondary neutrons which are the main cause for the total dose of radiation absorbed by biological systems, especially at high altitudes and latitudes. A measurement campaign has been carried out in the high mountain Observatory of Testa Grigia (Italy, 45°56’ N, 7°42’ E, 3480 asl) during the period November 2014 – December 2014, in order to evaluate the neutron ambient dose equivalent H* and its correlation with variations in the CR intensity. The instrumental set up consists of several instruments: a modular neutron monitor (realized at SVIRCO Observatory and TPL in Rome) to register the CR intensity; 2) the Atomtex Rem Counter (INFN Torino), to measure the Ambient Dose Equivalent for neutrons in the range 0.025 eV - 14 MeV; 3) the Thermo Rad Eye Rem Counter (LNF, Frascati) to measure the Ambient Dose Equivalent for neutrons in the range 0.025 eV - 1 GeV. First, the performance of the modular detector was tested against the CR observations at the Jungfraujoch Station (Switzerland, 46.55° N, 7.98° E, 3475 m asl), because of its comparable geographic position. It was found that the modular detector provides a high counting rate together with a good reliability. Then, the CR data were carefully checked and used to investigate the detector response to the interplanetary perturbations propagating in the near Earth space to evaluate the induced variations in the galactic CR flux. In addition, the relative contribution of low and high energy neutrons to the ambient dose equivalent was estimated. Finally, a preliminary study was performed by combining the different type of data, indicating that variations of few percent in the galactic CR intensity can be associated with appreciable variations in the neutron ambient dose equivalent, with important consequences for the human radiation exposure in the framework of Space Weather.
21	CaLMa, toward an integrated neutron/muon system	Blanco, J et al.	p-Poster
	Juan José Blanco[1,2], José Medina[1,2], Óscar G. Población[1,2], Raúl Gómez-Herrero[1,2], Ignadio G. Tejedor[1,2], Sindulfo Ayuso[1,2]
	[1] Space Research Group, University of Alcala. Spain; [2] he CaLMa Neutron Monitor, Science and Technology Park of Castilla-La Mancha, Spain
	Castilla-La Mancha neutron monitor (CaLMa) is currently measuring secondary neutrons produced by the interaction between cosmic ray and atmospheric nuclei. Because of its vertical cut-off rigidity (6.95 GV) and its height (708 m above see level), CaLMa can follow the effect of solar activity on the cosmic ray flux arriving to the Earth. A planed improvement, and currently under development, is to incorporate to CaLMa's measurements the capability of measuring the muonic component by adding a muon telescope to the system. Both detectors will have a common acquisition system. Muon count rate and some directional information will enhance CaLMa's count rate.
22	Estimated Response of the Calgary Neutron Monitor to the Absolute Cosmic Ray Proton and Helium Spectra by a Simulation of Cascade Showers and Subsequent Thermal Neutron Transport	Kouznetsov, A et al.	p-Poster
	Alexei Kouznetsov[1], David Knudsen[2]
	[1] University of Calgary, [2] University of Calgary
	Nuclear spallation accompanying Galactic Cosmic Ray (GCR) propagation through the atmosphere forms a so-called "cascade shower" by means of production of secondary protons, neutrons, muons, pions, photons and other energetic particles. The World-wide Neutron Monitor (NM) network has been deployed for ground-based monitoring of energetic proton and neutron precipitation. Recent advances in numerical simulations of the atmospheric propagation of GCRs and induced neutron spectra calculated with contemporary three-dimensional Monte Carlo transport codes for high altitudes (up to 200 g/cm^3) [Clem, 2004] and on the ground [Palomares, 2013] give us an opportunity to calculate thermal neutron absorption rates for the NM-64 cosmic ray monitors. Each NM has its own detection efficiency, which depends on its location, design, operational and atmospheric parameters. As a result, NM counting rates should be normalized to the absolute cosmic ray proton and helium spectra. Using measured spectra of primary GCRs, NM location, its internal design, and atmospheric parameters as inputs, we have implemented a numerical technique for the direct estimation of NM count rates. We trace GCRs to the top of the atmosphere by means of our in-house computational tool [Kouznetsov and Knudsen, 2013] and a new MCNP-6 "CR" option [Palomares, 2013]. The absolute background thermal neutron spectra are computed at the Calgary NM location based on MCNP-6 simulations and an MSIS Atmosphere Model [http://omniweb.gsfc.nasa.gov/vitmo/msis_vitmo.html]. Results obtained for the Calgary NM are used to improve the regular atmospheric pressure correction procedure, and can be used to normalize counting rates for the entire world-wide NM network. References: Clem, J. M., G. De Angelis, P. Goldhagen5 and J. W. Wilson, " New Calculations of the Atmospheric Cosmic Radiation Field - Results For Neutron Spectra", Radiation Protection Dosimetry (2004), Vol. 110, Nos 1-4, pp. 423-428 doi:10.1093/rpd/nch175 Palomares, J., McKinney, G. W., “MCNP Simulations of Background Particle Fluxes from Galactic Cosmic Rays”, ANS Annual Meeting, 2013-06-16/2013-06-20 (Atlanta, Georgia, United States), LA-UR-13-20254 Kouznetsov, A., and D. J. Knudsen (2013), Forward mapping of solar energetic proton distributions through the geomagnetic field, J. Geophys. Res. Space Physics, 118, 4724–4738, doi:10.1002/jgra.50400.
23	Mexico City Neutron Monitor for Space Weather Studies.	González, X et al.	p-Poster
	X. González[1,2], J.F. Valdes-Galicia[1], A. Gonzalez[2], J. Mejia-Ambriz[2], V. M. De la Luz[2], P. Corona[2], A. Hurtado[1], O. Musalem[1].
	[1] Instituto de Geofisica, UNAM, D.F. Mexico; [2] SCiESMEX, Instituto de Geofisica, Unidad Michoacan, UNAM, Morelia, Mexico.
	We present the incorporation of the Mexico City Neutron Monitor into the new Mexican Space Weather Service (SCiESMEX), and the registered solar events for studies of Space Weather.
24	Barometric effect of the neutron component of cosmic rays with consideration for wind effect at the Antarctic station Mirny and station Mt. Hermon in Israel	Dorman, L et al.	p-Poster
	P. Kobelev[1], L. Dorman[1,2], A. Belov[1], E. Eroshenko[1], R. Gushchina[1], U. Dai[2], L. Pustil’nik[2], V. Yanke[1], I. Zukerman[2]
	[1] IZMIRAN, Kalushskoe ave., 4, Troitsk, Moscow, Russia, 142190; [2] Israel Cosmic Ray and Space Weather Center with Emilio Segre’ Observatory on Mt. Hermon, affiliated to Tel Aviv University, Golan Research Institute, and Israel Space Agency
	Estimation of barometric coefficient for neutron component of cosmic rays was performed for Antarctic station Mirny and Mt. Hermon in Israel taking into account effect of dynamic pressure caused by wind in the atmosphere. Hourly data of continue monitoring of neutron component and data of the local meteo station have been used for the period 2007-2014. Wind velocity at the observatory Mirny reaches 20-40 m/s in winter that corresponds to dynamic pressure of 5-6 mb and leads to the error of 5% in variations of neutron component because of dynamic effect in the atmosphere. The results are interesting for high latitude and high mountain detectors, where effect Bernulli may be significant.
25	Using one-minute CR data for forecasting on-line great fluxes of energetic particles from the Sun, dangerous for satellites operation and airplanes at regular about 10 km altitude airlines	Dorman, L et al.	p-Poster
	L. Dorman[1,2],  U. Dai[1], V. Kazanzev[1], L. Kozliner[1],  L. Pustil’nik[1], A. Sternlieb[1], I. Zukerman[1]
	[1] Israel Cosmic Ray and Space Weather Center with Emilio Segre’ Observatory on Mt. Hermon, affiliated to Tel Aviv University, Golan Research Institute, and Israel Space Agency, Israel; [2] IZMIRAN, Kalushskoe ave., 4, Troitsk, Moscow, 142190, Russia.
	Many years ago we developed method of using one-minute CR data for forecasting on-line great fluxes of energetic particles from the Sun, dangerous for satellites operation and airplanes at regular about 10 km altitude airlines. At those times there are no on-line CR one-minute data from many neutron monitors (NM) and we applied this method for the single NM, characterized with several coupling functions for different multiplicities. We approved this method on the basis of data for 29 September 1989, when our NM was on the Mt. Gran Sasso in Italian Alpes. Now, when became possible to have on-line one minute data simultaneously from several NM, we developed a new method for determining energy spectrum and and its changing with time. On the basis of obtaining data and solution of inverse problem we determine on-line source function and diffusion coefficient in interplanetary space, and then - expected radiation hazard for satellites at different orbits and airplanes et different altitudes and cutoff rigidities.
26	Radiation dosimetry at Argentine Antarctic Marambio base and its correlation with cosmic ray variability	Laurenza, M et al.	p-Poster
	Alba Zanini[1], Adolfo Esposito[2],Monica Laurenza[3], Marisa Storini[3], Fabrizio Signoretti[3], Juan Carlos Terrazas[4], Marco Caresana[5],Vicente Ciancio[6], Gustavo Di Giovan[6], Adriana Gulisano[7], Paolo Morfino[8], Marta DeBiaggi[8]
	[1] INFN Sez. Torino, Via Pietro Giuria 1, 10125 Torino, Italy; [2] LNF-INFN, Via E. Fermi 40, 00044 Frascati, Italy; [3] IAPS/INAF, via del Fosso del Cavaliere 100, 00133 Roma, Italy; [4] INAF-OATo,  Strada Osservatorio 20, 10025 Pino Torinese, Italy; [5] Politecnico di Milano, Piazza Leonardo da Vinci, 32, 20133 Milano, Italy; [6] Università National de La Plata, Avenida 7 776, 1900 La Plata, Buenos Aires, Argentina; [7] Istituto Antartico Argentino, Cerrito 1248 C1010AAZ, Buenos Aires, Argentina; [8] Efesto S.a.r.l, 55 Avenue Marceau – 75116 Paris 16
	The radiation environment around the Earth arises as a result of the interaction of primary galactic cosmic rays (GCR) with nuclei constituting the atmosphere. Primary particles, entering into the upper layers of the atmosphere, mainly interact with Oxigen (21%) and Nitrogen(78 %) nuclei and produce a secondary shower, consisting of different particles as protons, neutrons and mesons which can penetrate deeper into the atmosphere, undergoing further collisions, that leads to a cascade of particles. This radiation environment and consequently the human being exposure, varies with altitude , with latitude and with solar activity. A campaign is in progress since March 2015, to measure various components of the secondary radiation environment at the Marambio Antarctic base (Argentine, 64° 13’S – 56° 43’W). Because at present few dosimetric data are available in the Antarctic region, an accurate measurement of the different components of environment radiation dose is performed. Moreover, the correlation of the radiation dose with the cosmic ray variability registered at the Neutron Monitor Stations in the Antarctic region is investigated. A set of various active and passive detectors, previously inter-calibrated at the high mountain Research Station Testa Grigia (Italy, 45°56’ N, 7°42’ E, 3480 asl) is employed. Special attention is dedicated to measure the neutron Ambient Dose Equivalent in different energy ranges, by using two active detectors , the Atomtex Rem Counter, for neutron energy between 0.025 eV - 14 MeV and the Thermo Rad Eye Rem Counter for neutrons energy in the range 0.025 eV - 5 GeV. In addition, a set of passive neutron dosimeters, consisting of bubble detectors, Cr39 foils, Bi209 stack and a dual-detector spherical rem-counter hosting a CR39 foil are used. Charged particles and gamma rays are measured by LIULIN LET spectrometer and BDKG-94 Atomtex scintillation plastic detector respectively. The preliminary results of the first dosimetric campaign in the Antarctic region of secondary atmospheric radiation are presented.
27	Variations of the galactic cosmic ray spectrum on the Forbush decreases of March 2012	Mavromichalaki, H et al.	p-Poster
	D. Lingri[1], M. Livada[1], H. Mavromichalaki[1]. A. Belov[2]. E. Eroshenko[2]
	[1] University of Athens, Greece; [2] IZMIRAN Russia
	The solar cycle 24 is a low activity solar cycle. In this cycle March 2012, was a really active period, with a lot of intense solar events produced three great Forbush decreases starting from the March 7, 2012 and considered as the biggest storm of the solar cycle 24. It was affected from X- and M-class flares and Halo CMEs with velocity up to 2684 km/s. In the present work daily values of the cosmic ray intensity derived from the data of the neutron monitor network (www.nmdb.eu) were analysed. Moreover, all mathematical arguments for the derivation of the galactic cosmic ray spectrum during this intense series of Forbush decreases, using the coupling coefficient method that combines the secondary cosmic rays recorded at Earth to the primary cosmic ray flux at the edge of the magnetosphere, i.e. in free space, are presented analytically. Our calculations provide a spectrum of the galactic cosmic rays free of the detectors’ local characteristics. The values of the spectral index γ were fluctuated from 2 at the beginning of the Forbush decreases to 0.5 at its minimum.
28	Relation of the vector cosmic ray anisotropy to the parameters of solar wind	Abunina, M et al.	p-Poster
	Maria Abunina[1], Artem Abunin[1], Anatoly Belov[1], Evgenia Eroshenko[1], Victoria Oleneva[1], Victor Yanke[1], Olga Kryakunova[2]
	[1] Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Russia; [2] Institute of Ionosphere, Kazakhstan
	Variations of the cosmic ray vector anisotropy observed on Earth are closely related on the condition of near Earth interplanetary medium. The hourly characteristics of vector anisotropy obtained by the global survey method from the data of world wide neutron monitor network during 1957-2013 allow us to investigate connection of the cosmic ray anisotropy with the solar wind parameters. In the present work relation of the equatorial component Axy of the cosmic ray anisotropy (rigidity 10 GV) to the solar wind velocity and density, to intensity of the interplanetary magnetic field and to the changes of cosmic ray density in which the spatial gradient of CR is revealed in interplanetary space, is studied. Characteristics of the CR anisotropy for various combinations of interplanetary parameters corresponding to various conditions of the interplanetary medium are compared. Opportunity to judge on condition of a solar wind by cosmic ray anisotropy data is discussed.