NMDB Meeting 2025: Cosmic Ray studies with Neutron Detectors

19 Mar 2025, 09:00 → 21 Mar 2025, 19:10 Europe/Athens

Seminar Room (Physics Department )

 

                                                         Announcement

In light of the unusual cosmic ray events of 2024, and the milestone 25th anniversary of the Athens Neutron Monitor's operation, we are pleased to announce a new in-person NMDB meeting to be held in Athens. This event follows nearly three years since the last hybrid ‘NMDB@Athens’ meeting and will take place in the Seminar Room of the Department of Physics at the National and Kapodistrian University of Athens, located at the University Campus of Zografos.

We are looking forward to welcome you in Athens!

      On Behalf of the Organizing Committee
                   Em. Prof. Helen Mavromichalaki

Meeting poster

A.Ne.Mo.S Brochure

 

Pre-meeting Announcement

An interactive pre-meeting concerning software, data quality etc of Neutron Monitors with Christian Steigies will be held on Tuesday 18 March at 12:00 (LT) in the Physics Department (3rd floor), for those who will have already arrived in Athens!

Wednesday, 19 March

09:30 → 10:00 Registration

10:00 → 11:30 Welcome & Introductory Talks

10:00 Welcome to the University of Athens

Speaker: Prof. Ε. Nistazakis (Chairman of Physics Department, University of Athens)

10:10 Welcome to NMDB meeting 2025

Speaker: Helen Mavromichalaki (University of Athens)

Opening speech Mavromichalaki.pdf

10:15 The Significance of Neutron Monitor Measurements over Time

Neutron Monitors (NM) have been in continuous operation in a global network since the International Geophysical Year (IGY) 1957/58. Their main purpose is the ground-based observation of temporal fluctuations in the low GeV part of the energy spectrum of cosmic ray particles hitting the Earth's atmosphere. The focus in the use of NM data has however significantly changed over time, from fundamental astrophysical research in the past to applications in the space weather era, and more recently in the domains of environmental metrology as well as geotechnical and agricultural engineering. In this process, the establishment of the real-time database NMDB was essential, and its continued operation is of utmost importance.

Speaker: Erwin Flückiger (University of Bern, Switzerland)

11:00 The history and the current status of the Neutron Monitor DataBase

The Neutron Monitor DataBase (NMDB) has been created as an EU FP7 project in 2008. Since then, NMDB has grown from 12 participating institutes with 15 stations to more than 50 stations, about half of them currently provide data in real-time. While we created NMDB for the use of Cosmic Ray researchers, the data has been quickly found by and is nowadays being used in many different fields of research. Over the years not only has the database software changed, but also the setup of the database servers. I will describe our journey from a single MySQL server via a set of distributed mirrors to a single MariaDB Galera Cluster, the problems that have been solved, the problems that have been created, and the problems that we will face in the (near) future.

Speaker: Christian Steigies (CAU Kiel)

11:30 → 11:45 Coffee Break

11:45 → 13:00 Cosmic Rays in the Heliosphere: Session 1

Galactic cosmic rays are subjected to modulation when entering the heliosphere. An overview of these modulation processes along with computations with various modulation models provide useful information regarding the size and shape of the heliosphere, the local interstellar spectra at lower energies, the modulation in the heliosheath,

11:45 Observational evidence on the mechanism of relativistic particle acceleration in solar eruptions

Ground-level enhancements (GLE) designate eventS where relativistic protons and ions of solar origin trigger a cascade of secondary nucleons in the Earth’s atmosphere that can be detected on ground. GLEs require primary particles with energies of at least 430 MeV/nucleon, with a spectrum that may extend to several tens of GeV. They are extremes of solar particle acceleration, which pose challenging problems to candidate ac- celeration processes. The association with eruptive solar flares suggests processes related to magnetic reconnection in the flaring corona and shock waves driven by particularly fast coronal mass ejections. Pion-decay gamma-rays, which come from the interaction of nucleons with energies above 300 MeV/nucleon with the low solar atmosphere, have shown that relativistic proton acceleration is much more frequent than GLEs. In this talk I will review observational evidence on the acceleration process and discuss the pros and cons of the two categories invoked in the literature.

Speaker: Karl-Ludwig Klein (Observatoire de Paris)

12:35 Shape and extend of the solar wind transition surfaces: Solar Alfven and Sonic surfaces, the heliosphere and CR modulation

We investigate the shape and extend of the solar wind transition surfaces, namely the slow (sonic), the fast magnetosonic and the Alven surface, as a function of heliospheric latitude using actual experimental data from Ulysses, Parker Solar Probe and Solar Orbiter pole to pole journey. We also derive the temporal variation of the radius of these surfaces using measurements from spacecraft at 1 au. Moreover, a semi-analytical calculation of the shape and extend of the heliosphere, the heliospheric termination shock and CR modulation is made based on spacecraft data input for the initial conditions. We estimate directly the consequences of the solar wind latitudinal variation on the shape of the termination shock. The model that we use is an approximate gas-dynamic model based on Fahr et al. 1993; Nerney & Suess 1995. We develop a semi-analytical model that can use any spacecraft measurements as data input to give the distance and shape of the termination shock from the Sun in a simple computational way that gives realistic results. A comparison is made of the Voyager crossing of the termination shock and NM CR data.

Speaker: Xenophon Moussas (Department of Astrophysics, Astronomy and Mechanics, National and Kapodistrian University of Athens)

X MOUSSAS_G EXARCHOS 2025 Solar Alfven sonic surface.pdf

X MOUSSAS_G EXARCHOS 2025 Solar Alfven sonic surface.pptx

13:00 → 14:30 Lunch

14:30 → 15:40 Intense Events of 2024: Session 2

Solar cycle 25, which is already progressing and is currently moving towards the solar maxima, is characterized by increased solar activity and highly disturbed interplanetary conditions. As a result extreme space weather events are recorded. For example the unusual Forbush Decrease on March 2024, the strongest geomagnetic storm G5 in over two decades on May 2024, and finally the new Ground Level Enhancement events, GLE74, GLE75 and GLE 76 on May, June and November 2024 respectively were recorded.

14:30 Neutron Monitors and Cosmic Ray Science

Neutron monitors (NMs) have been continuously measuring the secondary nucleonic component of the galactic cosmic ray (CR) intensity for more than 70 years. NMs have played a fundamental role in our understanding of: solar modulation, namely significant global and temporal variations in the galactic CR intensity and energy spectra as a function of position inside the heliosphere on long time scales (11-year solar activity cycle, 22-year magnetic polarity cycle); short-term variations such as Forbush decreases, i.e. depressions in the GCR intensity due to effect of interplanetary perturbations; ground level enhancements produced by the arrival of relativistic solar particles (the so-called solar cosmic rays) in the Earth atmosphere. This tutorial provides an overview of neutron monitors measurements and cosmic ray science, focusing on the physical processes in the interplanetary space responsible for CR short-term variations and those favoring the high energy particle acceleration at the Sun.

Speaker: Dr Monica Laurenza (INAF- Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy)

15:00 GOES Solar Energetic Particle Observations During the Ground Level Enhancements 74-76 of 2024

During 2024, three ground level enhancements (GLEs) were observed, with onsets on 11 May, 8 June, and 21 November. GOES-16 and -18 made observations during all three GLEs, and additionally GOES-19 (launched 7 July 2024) made observations during GLE 76. Each satellite carries three solar energetic particle (SEP) instruments: two Solar and Galactic Proton Sensors (SGPS), looking eastward and westward in the orbit, and the Energetic Heavy Ion Sensor (EHIS), looking toward zenith. SGPS is the primary instrument for observing solar proton (1-500 MeV, >500 MeV) and alpha particle (1-224 MeV/n) fluxes. EHIS reports heavy ion fluxes by atomic number (Z) in five energy channels whose energies vary with Z (18-334 MeV/n for carbon, 38-826 MeV/n for iron). We use the 2024 GLEs as a framework for describing the status of the GOES SEP observations, including recent cross-calibrations, and we summarize current and planned availability of retrospective and real-time data.

Speaker: Juan Rodriguez (University of Colorado CIRES)

NMDB_2025_Rodriguez_etal_v3.pdf

15:25 Discussion on GOES satellites

15:40 → 16:00 Coffee Break

16:00 → 17:00 Intense Events of 2024: Session 2

Solar cycle 25, which is already progressing and is currently moving towards the solar maxima, is characterized by increased solar activity and highly disturbed interplanetary conditions. As a result extreme space weather events are recorded. For example the unusual Forbush Decrease on March 2024, the strongest geomagnetic storm G5 in over two decades on May 2024, and finally the new Ground Level Enhancement events, GLE74, GLE75 and GLE 76 on May, June and November 2024 respectively were recorded.

16:30 Solar events of the 25th activity cycle

The surprising increase in solar activity in 2024, following a relatively tranquil 24th cycle, suggests that we are approaching the solar maximum of the 25th cycle. The complex interplay between disturbed interplanetary and geomagnetic fields affects the cosmic rays reaching the Earth’s surface in various ways.
Positioning the particle spectrometers at elevated altitudes, which analyze the energy spectra of muons and neutrons, is a strategic decision aimed at comprehending the intricate interactions between colliding interplanetary and geomagnetic fields and the solar proton accelerators. Direct comparison between the measured energy spectra of secondary neutrons and muons (MeV) via appropriate simulations is related to energy spectra of solar energetic protons (GeV).
The report highlights advanced instrumentation and data analysis methods to investigate solar-induced phenomena in cosmic rays by analyzing the solar events of the 25th cycle.

Speaker: Prof. Ashot Chilingarian (Yerevan Physics Institute)

NMDB2025_Chilingarian.pptx

Thursday, 20 March

10:00 → 11:45 Intense Events of 2024: Session 2

Solar cycle 25, which is already progressing and is currently moving towards the solar maxima, is characterized by increased solar activity and highly disturbed interplanetary conditions. As a result extreme space weather events are recorded. For example the unusual Forbush Decrease on March 2024, the strongest geomagnetic storm G5 in over two decades on May 2024, and finally the new Ground Level Enhancement events, GLE74, GLE75 and GLE 76 on May, June and November 2024 respectively were recorded.

10:00 High energy proton recordings during GLE74 on 11 May 2024

Ground-level enhancements (GLEs) represent the highest-energy end of solar energetic particle (SEP) events, forming a distinct class where ions are accelerated to relativistic speeds. This leads to a sudden, significant increase in cosmic rays detected by ground-based instruments, primarily neutron monitors (NMs). This work focuses on GLE74, which occurred on May 11, 2024. Proton observations up to ~ 2.4 GV, gathered from neutron monitors, SOHO, GOES, and STEREO-A, are combined with soft X-ray flare data, CME detections, and radio bursts to determine the solar origin of the event. A time-shift analysis was also performed to correlate detected particles with their solar sources. Finally, GLE74 is compared to past events to provide further insight into its characteristics.

Speaker: Athanasios Papaioannou (National Observatory of Athens)

PAPAIOANNOU_GLE74.pdf

10:30 GLE #75 caused by a solar energetic particle event on 8 June 2024

Some solar energetic particle (SEP) events can be registered by ground-based neutron monitors (NMs) measuring the variability of cosmic rays. Those events are called Ground-Level Enhancements (GLEs) and are seen as rapid increases in NM count rates over the background of galactic cosmic rays. GLEs are rare, but the year 2024 was rich for three of them. We report the second GLE of the year that happened on 8 June 2024, initially overlooked but discovered retrospectively after a review of NM data. That GLE #75 is associated with an SEP event induced by the same active region 13697/13664 that caused the previous GLE #74. During GLE#75, there were statistically significant responses at NMs DOMC, PWNK, and SOPO/SOPB, and an enhancement of the proton flux measured by satellite GOES-16. We present the GLE, reconstructed SEP spectra and angular distributions, and describe the procedure of assessment of the statistical significance of increases.

Speaker: Dr Stepan Poluianov (University of Oulu, Finland)

10:50 Modeling the solar event responsible for GLE74 in May 2024

A Ground-Level Enhancement (GLE) was detected on May 11, 2024, following a significant Forbush decrease. Simultaneously, a powerful Solar Energetic Particle (SEP) event was measured at the Lagrange L1 point and by the Solar-Terrestrial Relations Observatory Ahead (STEREO-A). This event was triggered by an X5.8 flare and a fast Coronal Mass Ejection (CME) with a speed >1500 km/s which generated a shock wave in the solar corona.
We modelled this coronal shock wave using a 3D reconstruction technique and a magneto-hydrodynamic model. The results of this reconstruction are presented with an observational analysis of the SEP event and electromagnetic signatures. This work was coordinated under the Horizon Europe SPEARHEAD project.

Speaker: Manon Jarry (IAASARS - NOA)

11:10 High latitude muon and neutron observation of the Forbush decrease during the May 2024 solar storms

A series of intense solar flares occurred in May 2024. Among other effects, a remarkable Forbush decrease in the cosmic ray flux was observed on the Earth. This event was observed by neutron and muon detectors installed at the Svalbard, in a high latitude site, characterized by a weak geomagnetic shielding. For this analysis we employed at Ny-Alesund three scintillator-based muon telescopes of the Extreme Energy Events (EEE) project, 14 channels of a Bonner Sphere neutron Spectrometer (BSS), thermal and epithermal neutron sensors used for hydrological monitoring, and data from NM Barentsburg.

Most sensors showed significant responses and correlation during the event. The observed relative magnitude of the Forbush decrease was estimated to be ≈ 9% for thermal neutrons, ≈ 8% for high-energy neutrons, and ≈ 3% for muons. A correlation analysis of the time series provided by all these detectors will be discussed in this contribution.

Speaker: Martin Schrön (Helmholtz Centre for Environmental Research GmbH - UFZ, Leipzig, Germany)

11:30 Research of cosmic rays at the Lomnicky stit observatory

In our lecture we will look at the history and present of cosmic ray research by the staff of the Institute of Experimental Physics SAS at the Lomnickom Peak site. We will summarize the history of the site and measurements, the results of our work and future perspectives. You will learn, for example, about how the cosmic ray observations with different instruments since 1957 and what instruments we use to observe cosmic rays today. We are also looking forward to a discussion focusing on new opportunities for research and collaboration in the future.

Speaker: Ján Kubančák (Institute of Experimental Physics SAS)

nmdb_Kubancak.pdf

11:45 → 12:00 Coffee Break

12:00 → 13:10 Cosmic Rays and Space Weather effects: Session 3

Cosmic rays are modulatated by solar and geomagnetic activity, which are key aspects of Space Weather. Space Weather events, like solar storms, can enhance or interact with cosmic ray effects, particulary in terms of radiations hazards and atmospheric ionization. Radiation dose models allow the calculation of the ionization and radiation levels during a flight due to the enhanced radiation environment created by solar energetic particle events.

12:00 Neutron Monitor Data as input to European projects: SWESNET and PECASUS

Various European projects that provide space weather services, such as spacecraft operations and aviation, rely on neutron monitor data. In this presentation, two major European projects will be discussed, respectively ESA Space Safety Program (S2P) Space WEather Service NETwork (SWESNET, https://swe.ssa.esa.int/) and Pan-European Consortium for Aviation Space weather User Services (PECASUS, https://pecasus.eu/). Neutron monitor data is used by several products in the SWESNET Space Radiation Expert Service Centre (R-ESC) product portfolio (e.g., ANeMoS, AVIDOS, COMESEP, and UTU-SEP products). PECASUS relies on neutron monitor data to estimate the radiation exposure at flight level, a key input for compiling ICAO radiation advisories. To maintain these products continued operation of neutron monitor stations must be ensured. Further extensions and support of the current network with new or updated stations and services in terms of reliable real-time data is thus encouraged.

Speaker: Norma Bock Crosby (Royal Belgian Institute for Space Aeronomy)

NormaCrosby_NMDB2025_FinalVersion.pdf

12:30 The response of ANeMoS GLE Alert system to the recent Ground Level Enhancements of 2024

Three years after GLE 73 (October 28, 2021), three distinct GLEs took place before the end of 2024.The first event, GLE 74 registered on May 11, 2024, followed by GLE75 on June, 8 and GLE 76 on November 21. Each event exhibited unique characteristics in terms of intensity, temporal evolution, and spectral properties. Notably,GLE 74 occurred during an irregular Forbush Decrease with sharp amplitude reduction and rapid recovery. Specifically, a 15% decrease was recorded, followed by an exceptionally fast 10% recovery within 1.5 hours, as observed by the Oulu neutron monitor station.This event triggered the strongest geomagnetic storm in two decades (May 10–11, 2024), causing auroras at unprecedented latitudes worldwide.
In this study, we analyze and present the response of the GLE Alert system to these Ground Level Enhancements, offering insights into their implications for space weather forecasting and radiation hazard.

Speaker: Maria Gerontidou (National an Kapodistrian University of Athens)

Gerontidou .pptx

12:50 GLE alert and afterwards

The availability of high time resolution NM data in near real-time through NMDB makes it possible to generate GLE alerts. Potential stakeholders are researchers in the field of space weather as well as e.g. airlines who have to assess the radiation dose exposure of crew members and passengers along the flight routes. Currently, at least two institutions operate such alert applications. These routines continuously monitor the NM data provided by NMDB. A GLE alarm is triggered as soon as predefined criteria are met, and the registered interested parties get an immediate notification by e-mail. While this approach is certainly adequate for many of the service subscribers, more interested parties lack further information. We, therefore, discuss whether forecasts can be made of the development of a GLE based on NM data in the course of an event and how this information could be made available e.g. through a continuously updated webpage.

Speaker: Rolf Bütikofer (University of Bern, Switzerland)

GLE_AlertAndAfterwards.pdf

13:10 → 14:30 Lunch

14:30 → 16:20 Cosmic Rays and Space Weather effects: Session 3

Cosmic rays are modulatated by solar and geomagnetic activity, which are key aspects of Space Weather. Space Weather events, like solar storms, can enhance or interact with cosmic ray effects, particulary in terms of radiations hazards and atmospheric ionization. Radiation dose models allow the calculation of the ionization and radiation levels during a flight due to the enhanced radiation environment created by solar energetic particle events.

14:30 Energy Sensitivity of a Neutron Monitor: A Monte Carlo Study

Neutron monitors (NMs) play a crucial role in studying cosmic-ray interactions and atmospheric neutron cascades. However, their response to high-energy neutrons (above 20 MeV) remains uncertain due to the limited availability of neutron cross-section data in simulation frameworks such as GEANT4. This study aims to evaluate the energy sensitivity of a neutron monitor using Monte Carlo techniques, focusing on its differential energy and directional response. By analyzing the contributions of thermal, epithermal, and fast neutrons, produced within atmospheric cascades, we assess the limitations of current response models. Understanding these factors is essential for improving the applicability of neutron monitor data and the neutron monitor response function.

Speaker: Danislav Sapundjiev (Royal Meteorological Institute of Belgium)

15:00 Selection of the Solar-Diurnal Anisotropy of Cosmic Rays by Local and Global Methods

According to the data of Moscow and Climax neutron monitors, using harmonic analysis, the characteristics of the solar-diurnal anisotropy of cosmic rays on quiet days have been obtained for a long period from 1957 to 2023. A comparison with the average daily characteristics of the equatorial component of cosmic rays vector anisotropy, obtained from the data of the worldwide neutron monitor network using the global survey method showed a good agreement between the results of the two methods. From a comparison of local and global results, estimates were obtained for the coupling coefficients of the first harmonic of the cosmic ray anisotropy for Moscow and Climax neutron monitors, and a new experimental method for calculating the coupling coefficients of individual detectors was proposed. The limitations of the local method, as well as the possibility of continuing and expanding this study, have been discussed and justified.

Speaker: Nataly Shlyk (IZMIRAN)

Shlyk et al CR anisotropy.pptx

15:20 Ground-based observations of temporal variation of cosmic ray spectrum during Forbush decreases

Temporary decreases in the GCR flux due to the passage of an ICME can be observed in ground-based neutron monitors (NMs) and muon detectors. The details of these Forbush decreases are useful for space weather studies and alerts. We derive hourly variations in the GCR rigidity spectrum during several Forbush decreases using a global fit to count rates from the NM and muon-detector networks, and by calculating a "leader fraction" from the timing distributions of pulses in each NM counter at South Pole station. Results are consistent with daily variations in the spectral index as measured by AMS-02 onboard the ISS. Thus ground-based observations can be used to monitor GCR spectral variations during space weather events in real time. Partially supported by Thailand's NSTDA and NRCT: High-Potential Research Team Grant Program (N42A650868), and the NSRF via the Program Management Unit for Human Resources & Institutional Development, Research and Innovation (B39G670013).

Speaker: Alejandro Sáiz (Mahidol University)

15:40 Measurement of Cosmic-ray Neutrons with a High Efficiency Spectrometer

The High Efficiency Neutron Spectrometry Array (HENSA) project develops advanced neutron spectrometers for underground laboratories and cosmic-ray studies. Utilizing a modified Bonner Spheres System (BSS), HENSA achieves ten times higher efficiency than BSS, detecting neutrons from thermal energies to 10 GeV. This enables real-time spectral analysis of solar events such as Ground Level Enhancements and Forbush Decreases.
In 2020, a HENSA detector mapped cosmic-ray neutrons at altitudes up to 3000 m and magnetic rigidities from 5.5 to 8.5 GV. Building on these results, a new spectrometer, HENSA++, was developed with improved energy resolution and began commissioning in 2024, first in Valencia and later at the Observatorio Astrofisico de Javalambre, in Spain.
This talk presents HENSA’s latest results, including the evolution of the neutron spectrum and analyses of selected solar events. Finally, we outline future plans for continuous cosmic-ray neutron monitoring through the second half of Solar Cycle 25.

Speaker: Ariel Tarifeno-Saldivia (Instituto de Fisica Corpuscular (CSIC-UV))

ATarifeno_NMDB2025.pdf

16:00 Solar Energetic Particle transport during the GLE73 event on 28 October 2021

We investigate the transport of solar energetic particles (SEPs) during the 28 October 2021 (GLE73) event, focusing on their longitudinal spread. Multi-spacecraft observations revealed a remarkably wide longitudinal diffusion, enabling particles to reach very high energies. In this work, we incorporate SEP measurements from STEREO A, SolO/HET & SEPT, and SOHO/EPHIN, as well as newly available penetrating proton data from SolO/HET and SOHO/EPHIN. To interpret the observed time profiles, we carry out 1D and 2D numerical simulations of SEP transport, tuning free model parameters for optimal agreement with the measurements. From this inverse modelling procedure, we derive key physical parameters—such as the parallel and perpendicular mean free paths, acceleration and escape times, and the injection region size. We specifically explore the rigidity dependence of the physical parameters and discuss the broader physical implications of our findings.

Speaker: Eleni Lavasa (NKUA, NOA and ATHENA RC)

17:00 → 20:30 Social Event: Visit to the Stavros Niarchos Foundation Cultural Center

Friday, 21 March

10:00 → 11:50 Cosmic Ray Detection Instrumentation: Session 4

Methods and instruments in the service of cosmic ray detection. Innovations, renovations, alterations, repairs and upgrades of the existing neutron monitor detectors that improve their operation and functionality.

10:00 CaLMa’s way, from the space to ground

Cosmic rays below a few hundred GeV and solar energetic particles are key to understanding how the Sun is interacting with its own solar system, as they respond to the magnetic field that fills the entire Heliosphere, not only during quiet times, but also during episodes of solar activity, as they change the propagation conditions of cosmic rays and solar energetic particles through the Heliosphere. Direct observations of these two types of energetic particles can be made in space using detectors aboard spacecraft such as the Energetic Particle Detector aboard the Solar Orbiter and/or the AMS aboard the International Space Station, for example, and indirect observations using ground-based detectors such as neutron monitors and muon telescopes that measure secondary particles produced through the interaction between cosmic rays and solar energetic particles with atmospheric nuclei.
An ideal ground-based detector to investigate the solar-terrestrial relationship should provide the flux of energetic particles, their energy, their identity and their spatial distribution. Neutron monitors and muon telescopes are the usual instruments for this purpose. Neutron monitors can give the neutron count rate although they may have some response to protons and muons. Although direct measurement of the energy/rigidity of energetic particles is not possible, the combination of several neutron monitor stations at different geomagnetic latitudes can provide a spectrum for these particles and the isotropy of energetic particles in the sky. A rough estimate of this energy can also be provided by a single neutron monitor if it can detect multiplicities by recording the time between successive neutron detections or by capturing height pulses. Muon telescopes provide count rates of charged particles, mainly muons, entering the detector; their configuration usually allows estimation of incoming particle directions and a better estimate can be achieved if several geographically well separated muon telescopes are used. However, due to the energy threshold for muon production, these detectors are less sensitive to solar energetic particles than neutron monitors. In recent years, our group has developed and deployed a type of detectors that can provide both neutron and muon count rates, some information about the cosmic and solar particle spectra, and the arrival directions of muons in the detector volume. This is a combination of a neutron monitor and a muon telescope that share the same structure. At the moment, one of them is operating at the Spanish Antarctic Base Juan Carlos I and a second one is operating at the Izaña Observatory, on the slope of Mount Teide, on the island of Tenerife. We present our ground based detectors, including our first neutron monitor, CaLMa, and our minineutron monitor, miniCaLMa, a multipurpose neutron monitor, as well as our latest results on solar events and the response of neutron monitors as a function of altitude.

Speaker: Dr Juan José Blanco Ávalos (University of Alcalá)

10:30 Neutron Monitors at Jungfraujoch

Two neutron monitors, an 18-IGY since 1958 and a 3-NM64 since 1986, are in operation at the High Altitude Research Station Jungfraujoch in Switzerland. Both neutron monitors are located close to each other but with a difference in altitude of about 100 m (IGY: 3570 m asl, NM64: 3475 m asl). Due to their locations in a high alpine environment, the two neutron monitors are exposed to high winds and snow accumulation on and around the detector housing. Updated readout electronics are in operation since end of 2022 at both neutron monitors. In this presentation, we give a status overview of the continuous cosmic ray measurements at Jungfraujoch.

Speaker: Lukas Baeni (University of Bern)

Baeni-Neutron_Monitors_Jungfraujoch-handout.pdf

10:50 FORBUSH EFFECTS AND THEIR CONNECTION WITH SOLAR, INTERPLANETARY AND GEOMAGNETIC PHENOMENA

Forbush decrease (or, in more wide sense, Forbush effect) - it is a storm in cosmic rays, which is a part of heliospheric storm and is very often observed simultaneously with a geomagnetic storm. All these three kinds of perturbations: disturbances in the solar wind, magnetosphere and cosmic rays are closely interrelated and caused by the same active processes on the Sun. In the report, they will be considered in common.

Speaker: Dr Maria Abunina (IZMIRAN)

Abunina FEs and IPDs.pptx

11:20 miniTRASGO: A Compact RPC Tracker for Global Cosmic Ray and Space Weather Monitoring

miniTRASGO is a compact and cost-effective detector for secondary charged cosmic rays, designed for research in solar activity, cosmic ray modulation, and atmospheric physics. Utilizing Resistive Plate Chambers (RPCs), it ensures stable detection rates and high sensitivity, as demonstrated by the observation of Forbush Decreases in March and May 2024 at the Madrid station ($40.4^\circ\mathrm{N},\ 7\ \mathrm{GV}$), where the first operational miniTRASGO unit successfully measured these events despite its small active area of $0.1\ \mathrm{m^{2}}$.

With deployments in Warsaw, Puebla, and Monterrey by early 2025, miniTRASGO will expand coverage across latitudes ($52^\circ\mathrm{N},\ 19^\circ\mathrm{N},\ 25^\circ\mathrm{N}$) and cutoff rigidities ($2.5\ \mathrm{GV},\ 8.2\ \mathrm{GV},\ 8.5\ \mathrm{GV}$), forming a scalable global muon monitoring network, even though it can also complement NMDB stations, such as CaLMa, which is near the Madrid station.

Beyond flux monitoring, miniTRASGO enables angular-resolved studies of cosmic ray variations, geomagnetic effects, and solar modulation, reinforcing its role in multi-site research.

Speaker: Dr Alberto Blanco (Laboratorio de Instrumentacao e Fisica Experimental de Particulas (LIP))

Soneira_NMDB2025_Template_eposter.pdf

11:30 ARTEMIS–JEAN LOUIS STEINBERG (ARTEMIS-IV/JLS) MULTICHANNEL SOLAR RADIO SPECTROGRAPH UPGRADING THE INSTRUMENT & A STUDY OF TYPE III BURSTS

Sun's radiospectroscopy, at different wavelengths, provides information on many phenomena, which extend through the interplanetary medium upto Earth.The ARTEMIS solar radiospectrograph records the dynamic spectrum of solar radio bursts on a daily basis.It is located at the Satellite Communication Center station(SCC)of COSMOTE at Thermopylae,Greece.
The HERON LAB has undertaken its upgrade and operation,in collaboration with the Universities of Athens and Ioannina.We present the work that has been done so far and our plans for the future.
The facilities hardware and software improvements will incorporate ground-based radio measurements into the broader community,introducing a new era of the instrument.This will add to the ongoing research on already-acquired radio data of active solar phenomena.
An important aspect of ARTEMIS is its synergy with other ground and space instruments.As ESA's Solar Orbiter mission and NASA's Parker Solar Probe mission will continue to observe the sun until 2025/2027, the new ARTEMIS can provide ground coverage.

Speaker: FANIS SMANIS (HERON LAB/UNIVERSITY OF THESSALY)

NMDB_2025 _abstract_SMANIS_final.pdf

NMDB_Radiospectrograph ARTEMIS-IV-JLS-fasma_final.pdf

11:50 → 12:30 Poster Session - Coffee Break

12:30 → 13:10 Cosmic Ray Detection Instrumentation: Session 4

Methods and instruments in the service of cosmic ray detection. Innovations, renovations, alterations, repairs and upgrades of the existing neutron monitor detectors that improve their operation and functionality.

12:30 On the usability of small-scale scintillation muon telescopes

A small-scale (under 1 square meter) scintillation muon telescope experiment was started at IZMIRAN a few years ago. It turned out, that despite small surface area, the count rate was big enough to provide statistically supported results. For example, several Forbush-effects were observed in the data.

The talk will cover details of the instrument construction, data collection and processing. Special attention will be given to temperature correction as its very important for muon component of cosmic rays. The perspective of using such instruments data for global modelling methods will also be discussed.

Speaker: Semyon Belov (IZMIRAN)

nmdb2025_belov.pdf

12:50 HLEA and THIMON: Enhancing Neutron Monitor Data from the Summit of Haleakalā

The recent deployment of two new neutron monitors, HLEA and THIMON, at the summit of Haleakalā, Hawaii, represents a significant advancement in the global neutron monitor network. Positioned at 3,055 meters above sea level, these monitors benefit from reduced atmospheric interference, providing high-quality measurements of galactic cosmic rays (GCRs) and solar neutrons. Operational since December 2024, HLEA and THIMON are filling a critical geographical gap in the Pacific Ocean region. Their strategic location offers unique opportunities to compare measurements with other neutron monitors, aiding in cross-calibration efforts and enhancing the reliability of the global network. This presentation will cover the technical specifications of HLEA and THIMON, their initial performance metrics, and the first scientific results. We will also discuss their integration into the neutron monitor database. As part of the broader scientific community’s efforts to maintain and expand neutron monitor capabilities, HLEA and THIMON underscore the importance of investing in new stations, maintaining robust data repositories, and fostering international collaboration.

Speakers: Nikolay Nikonov (University of Hawaii at Manoa), Veronica Bindi (Physics & Astronomy Department, The University of Hawaii at Manoa, USA)

Nikonov_HLEA_Thimon_2025.pdf

13:10 → 14:30 Lunch

14:30 → 15:50 Databases and Catalogues: Session 5

14:30 The ARTEMIS-IV\JLS free access database (ARTDB): Off to a Good Start-With Room for Improvement

Open-access data is vital for advancing solar and space physics, promoting collaboration and combination of diverse datasets. To this end, the ARTEMIS-IV/JLS free-access database (ARTDB), presented by the ARTEMIS-IV/JLS Group, provides extensive solar radio observations from the ARTEMIS-IV Multichannel Radiospectrograph, operated by the University of Athens at Thermopylae, Greece (Lat: 38° 49'N, Lon: 22° 41'E), since 1996.

ARTEMIS-IV records daily spectra (05:30–15:00 UT) across 20–650 MHz using two receivers:
1. The Global Spectral Analyser (ASG)–covering the full band at 10 samples per second.
2. The high resolution Acousto-Optic Spectrograph (SAO)–1.4 MHz, 100 samples/s in the 265–450 MHz range.

Generating ~1.5 GB of data per day, ARTDB provides FITS-formatted spectral recordings and daily overview images (“Quick Looks”). The website (http://artemis-iv.phys.uoa.gr) also features select radio burst spectra, scientific publications, and educational resources.

Future improvements of the ARTDB include expanding event catalogs and implementing automated data processing for enhanced calibration and quality control.

Speaker: Dr Spiridon Armatas (National and Kapodistrian University of Athens: Department of Astrophysics, Astronomy and Mechanics)

ARTDB_Presentation_Final1.pdf

14:50 Neutron background monitoring for the IAXO-D0 detector prototype

The International Axion Observatory (IAXO) is a planned gaseous detector helioscope designed to detect axions, theorised to be dark matter candidates. A baseline detector prototype, IAXO-D0, is at present undergoing tests in Zaragoza. This prototype is sensitive to background high-energy neutrons that could induce false positive axion detections.

A neutron monitor has been proposed as a way to provide a continuous measurement of ambient neutrons. A prototype neutron monitor was designed and assembled. It consists of three He-3 proportional counter tubes surrounded by several layers of HDPE and lead. It has been in operation since March 2024 inside the laboratory where IAXO-D0 is being commissioned.

We present Monte Carlo simulations performed to characterise the monitor and the first results of the neutron count rate during the Forbush decrease observed in May 2024, once noise and pile-up have been taken care of, and atmospheric pressure effects have been corrected for.

Speaker: Víctor Martínez Nouvilas (Universidad Complutense de Madrid)

15:10 NMDB Stations Report

Contribution from all NM operators

15:30 The current Status of NEST

I will be presenting the Nest tool (nest.nmdb.eu), dedicated to the representation of the data stored in the NMDB database. Nest has been around for a long time and has evolved over time with new features. As the latest changes to the historic web site are cosmetic in nature, I'd like to take a closer look, in the form of a live demonstration, at the pages that have been developed recently and which offer a more interactive experience with the data. Feedback from users is essential if these tools are to evolve towards greater usefulness and efficiency.

Speaker: Nicolas Fuller (LIRA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS, France)

NF_summary_slides_NMDB2025.pptx

15:50 → 16:50 Open Discussion & Closing