Haleakalā Neutron Monitor Workshop and Ribbon Cutting Ceremony

5 Jan 2025, 15:00 → 9 Jan 2025, 17:00 Pacific/Honolulu

Nikolay Nikonov, Veronica Bindi (University of Hawai'i at Manoa (US))

This workshop commemorates the installation of two new neutron monitors, THIMON and HLEA, at the summit of Haleakalā on Maui, Hawaii. Designed for scientists, engineers, and students, the event will feature plenary sessions and interactive discussions.

Event Highlights:

• Ribbon-Cutting Ceremony at the Haleakalā Summit in Maui
• Plenary Sessions and Technical Talks 
• Focused Discussions
• Networking Opportunities 
• Poster Presentations

 

Funding Available for Early-Career Scientists!
Limited travel and registration grants are available for graduate students and postdocs. Present your research in plenary sessions and build collaborations with leaders in the field.

Workshop Objectives

• Integrate the new THIMON and HLEA neutron monitors with the global neutron monitor network
• Advance our understanding of the Sun-Earth space weather system
• Explore innovative approaches to studying radiation hazards, space weather forecasting, and cosmic ray physics

 

Registration Fee

The anticipated registration fee depends on your attendance type:

• Attendance in person Jan 5 to 9 -           $300
• Remote attendance Jan 6 to 9 -                 $60
• DKIST splinter meeting only on Jan 9 -     free

The collected fees will help support the following workshop expenses:

• Conference room facilities and audio-visual equipment
• Coffee breaks
• Lunch on workshop days
• Transportation to the Pau Hana Welcome reception and for the field trip to the summit of Haleakalā

 

Please use this reference to proceed with payment

Location and Dates

The workshop will be held across various locations on Oahu and Maui, combining professional sessions with Hawaii’s natural beauty.

• Welcome Pau Hana Reception and Poster Session at Hawaii Kai Marina (January 5):
  The workshop begins in the afternoon with a welcome Pau Hana and poster session at the Hawaii Kai Marina, offering a relaxed setting for attendees to introduce their research and network informally.

• University of Hawaii at Mānoa, Oahu (January 6-7 - Workshop Sessions at East-West Center):
  January 6 and 7 will feature full-day plenary and technical sessions at the East-West Center on the Mānoa campus. 

• One-Day Field Trip to Haleakalā Summit, Maui (January 8):
  A field trip to the Haleakalā summit on Maui is scheduled for January 8, where participants will visit the HLEA and THIMON neutron monitors. After a short flight from Oahu to Kahului Airport, a chartered bus will transport us to the summit. The day includes a ribbon-cutting ceremony and a tour of the Daniel K. Inouye Solar Telescope (DKIST), showcasing the research potential of these facilities.

• Splinter Meeting at UH Mānoa Physics and Astronomy Department (January 9):
  The workshop concludes on January 9 with a splinter meeting session at the UH Physics and Astronomy Department Manoa campus (walking distance from teh East-West center), focusing on synergies between neutron monitor data and DKIST’s solar science objectives. This session, led by NSO scientists, aims to align neutron monitor research with DKIST’s observational capabilities, addressing key questions in space weather impacts and cosmic ray physics.

This multi-location setup ensures a well-rounded experience, supporting scientific exchanges and productive partnerships.

Suggested Accommodations

For those seeking accommodation, we recommend the following options for convenient access to the workshop venues:

1. Lincoln Hall Dormitory (On-Campus)
   Located directly on the University of Hawaii campus, Lincoln Hall provides convenient, budget-friendly lodging for attendees. Just a few minutes’ walk from the East-West Center, this option offers easy access to all on-campus activities.

2. Hotels in Waikiki
   Waikiki offers a range of accommodation options, from budget-friendly hotels to luxury resorts, and is approximately 15 minutes by car or 20 minutes by bus from the University of Hawaii campus. Staying in Waikiki provides attendees with access to a variety of dining, shopping, and recreational options.

3. Ala Moana Hotels
   The Ala Moana area is another excellent choice, located close to shopping and dining options, and around 20 minutes by bus to the campus. 

Transportation to the Campus:

• Bus 13 from Waikiki and Bus 6 from Ala Moana both provide direct service to the University of Hawaii campus in approximately 18 minutes.

 

Haleakala Visit Key Details

1. Airfare to Maui
   Each participant will need to organize and purchase their own flights to Kahului Airport (OGG), Maui. Both Hawaiian Airlines and Southwest Airlines offer flights from Honolulu (HNL) that align with our revised schedule. Hawaiian Airlines is a convenient option as it allows changes with no fees, even on the day of the flight. Southwest might have the same flexibility but I am not sure.

   Suggested Flight on January 8 (for reference):

   • Honolulu (HNL) to Kahului, Maui (OGG)
     Hawaiian Airlines Flight HA 166 • Depart 8:00 am • Arrive 8:42 am
   • Return: Kahului (OGG) to Honolulu (HNL)
     Hawaiian Airlines Flight HA 355 • Depart 5:10 pm • Arrive 5:50 pm

   Southwest Airlines has similar timing for these flights if preferred.

2. Updated Meeting Time
   Our original plan was to meet in Maui by 10:00 AM, but we have moved the meeting time up to 9:15 AM to better align with flight schedules. Please arrive promptly at Kahului Airport, as we will depart shortly afterward.

3. Revised Schedule for the Day

   • Meet at Kahului Airport: 9:15 AM
   • Arrive at Haleakalā Summit: Approximately 11:15 AM
   • Lunch: Around 1:15/1:30 PM at a nearby restaurant
   • Return to Airport: 3:00-3:30 PM

   The suggested return flight for 5:10 PM, but there is an option at 4:45 PM as well. Since Hawaiian Airlines allows changes at the airport, you have flexibility if needed.

4. Transportation on Maui
   We’ll have two buses at Kahului Airport to ensure everyone can reach the summit comfortably, with extra space to accommodate any unexpected delays.

Please refer to timetable for all the details of January 8 travel and Ribbon Cutting Ceremony.

We look forward to welcoming you to Hawaii!

Local Organizers at the University of Hawaii:

 

Chair  Prof. Veronica Bindi

Dr. Nikolay Nikonov 

Dr. Abhinandan Dass 

Dr. Cristina Consolandi 

Dr. Claudio Corti (NASA GSFC CCMC & University of Hawaii)

Sunday 5 January

17:00 → 20:00 Welcome Pau Hana Reception and Poster Session

he workshop begins in the afternoon with a welcome Pau Hana and poster session at the Hawaii Kai Marina, offering a relaxed setting for attendees to introduce their research and network informally.

Monday 6 January

08:30 → 09:00 Registration

09:00 → 09:40 Welcome: Introduction and NSF talks

09:00 Welcome

Speaker: Veronica Bindi (UH Manoa)

09:10 NSF talk

Speaker: Roman Makarevich

09:20 Opening talk

Speaker: Roald Sagdeev (UMD)

09:40 → 10:30 Simpson Network and Facilities

09:40 HLEA and THIMON NM deployment

Speaker: Veronica Bindi (UH Manoa)

10:10 HLEA and Thimon NM deployment

Speaker: Nikolay Nikonov (UH Manoa)

NN_Workshop.pdf

10:30 → 10:45 Coffee

10:45 → 11:20 Simpson Network and Facilities

10:45 New HLEA and THIMON facility on Maui

Speaker: James Ryan (UNH)

Honolulu workshop talk 1.pdf

11:20 → 12:20 NM Design / Hardware / Electronics

11:20 University of Delaware and the Formation of Spaceship Earth

Speaker: Paul Evenson (UDEL)

SpaceShip Earth.pdf

11:50 Overview of UNH neutron monitors

Speaker: Andrew Kuhlman (UNH)

UNH_NM_electronics_final.pdf

12:10 Development of CMU Master Board for Chang Van Mobile Neutron Detector

Chiang Mai University operates the "Chang Van" mobile neutron detector, a twin model
of the "Thimon" (Thailand-Hawaii Neutron Monitor). Over the years, we have successfully conducted multiple expeditions aboard icebreaker ships, supported by the Polar Research Institute of China and the Korea Polar Research Institute, to both the Arctic and Antarctic regions as part of the Latitude Survey Project. During our most recent expedition, we identified a significant challenge that the electronic board of Chang Van was found to be highly susceptible to harsh operating conditions, with no spare replacements available, posing risks to mission continuity. To overcome this limitation and ensure the detector's reliability in extreme environments, we are developing the CMU Master Board for the Chang Van mobile neutron detector. We aim to enhance its durability and performance by integrating cutting-edge technology and components.
This research work was supported by Pre-Technology Incubation Grant from Science
and Technology Park, Chiang Mai University.

Speaker: Thirasak Panyaphirawat (CMU)

CMU master board - Thirasak.pdf

12:20 → 13:30 Lunch

13:30 → 14:20 NM Design / Hardware / Electronics

13:30 Mexico City Cosmic Ray Observatory

An overview of the Mexico City Cosmic Ray Observatory (MX-CRO), located within University City, UNAM (19°19'47.9"N 99°10'41.6"W) is presented. The MX-CRO includes a 6-NM64 neutron monitor, a muon telescope, a weather station and an electric field monitor. The neutron monitor, its design and electronics, are the main focus of the presentation.

Speaker: Jania Newton-Bosch (UNAM)

Mexico City CRO.pdf

13:50 System overview and design justifications for the United Kingdom’s new neutron monitor, the NM-2023

Aspinall M1, Alton T1, Binnersley C3, Bradnam S2, Cazzaniga C4, Croft S1, Frost C4, Joyce M1, Mashao D1, Packer L2, Turner T2, Wild J1
1 Lancaster University, Lancaster, United Kingdom
2 United Kingdom Atomic Energy Authority, Abingdon, United Kingdom
3 Mirion Technologies (Canberra UK) Limited, Warrington, United Kingdom
4 STFC Rutherford Appleton Laboratory, Harwell Campus, Didcot, United Kingdom

This presentation explores the system design justification for the United Kingdom’s (UK) new ground-level neutron monitor, the NM-2023. Funded by UK Research & Innovation (UKRI), the project developed networkable instruments for ground-level neutron monitoring that are significantly cheaper, more compact, and capable of producing results comparable to existing neutron monitors. A core goal of the project was to provide the UK Met Office with operational instruments, the potential to increase monitoring worldwide and enhance existing global capabilities. Design decisions were influenced by this and the challenging application requirements of neutron monitoring. After evaluating boron-coated straw (BCS) neutron counters as an alternative to boron trifluoride (BF3) and helium-3 (He3) gas-filled counters, the choice settled on He3 proportional counters. While BCS counters avoid the toxicity of BF3 and the expense of He3, their counting efficiency—about one-third that of He3 at 4 atm for an equivalent size—proved insufficient for the application. The justification for the neutron counters used is complemented by an explanation of the data acquisition chain, leveraging the established nuclear safeguards supply chain and International Atomic Energy Agency (IAEA) approved-for-use technology. Key design aspects of the neutron monitor, including the support table, housing, uninterrupted power supply (UPS), heating, ventilation, air conditioning (HVAC), and data ingest, are also addressed.

Speaker: Michael Aspinall

ASPINALL NM-2023 System overview and design justifications, Haleakala, v2, 6 Jan 25.pdf

14:20 → 15:05 Physics / Space Weather, Data Analysis, and Results

14:20 Space Weather Monitoring with the Neutron Monitor Network

Speaker: Pierre-Simon Mangeard

NMworkshopJan2025_SpaceWeatherTalk_Mangeard.pdf

14:50 The Neutron Monitor of Mexico City as a tool for Space Weather Analysis

An overview of the space weather events observed by the Neutron Monitor of Mexico City is presented. The detector is located at the Mexico City Cosmic Ray Observatory (MX-CRO) and it has been operating since 1990. The relevance and scope of its data for space weather analysis is discussed.

Speaker: Franando Monterde-Andrade (UNAM)

Neutron_Monitor_workshop_2025_slides.pdf

15:05 → 15:20 Coffee

15:20 → 17:00 Physics / Space Weather, Data Analysis, and Results

15:20 Investigating Cosmic Ray Variation with Semi-Leaded Neutron Monitors and Polar Surveys

This study presents notable progress in cosmic ray research through both semi-leaded (Changvan) and standard neutron monitor configurations, focusing on the Changvan latitude surveys (2018–2024) and altitude comparisons with the Princess Sirindhorn Neutron Monitor (PSNM). Our findings confirm the spectral crossover pattern in cosmic ray modulation, revealing rigidity-dependent phenomena—drifts at lower rigidities and helicity-driven diffusion at higher rigidities—and highlight the leader fraction as a key spectral indicator that clarifies structural influences on detector responses. Preliminary results from the 2023 Antarctic and 2024 Arctic voyages, conducted in collaboration with the Korea Polar Research Institute (KOPRI), further explain Galactic cosmic ray spectra and solar modulation. By improving our understanding of cosmic ray dynamics, this integrated approach ultimately enhances space weather forecasting and helps mitigate the potential impacts of cosmic rays on technology and human activities.

Speaker: Waraporn Nuntiyakul (CMU)

LatSur_Hawaii_Fhon.pdf

15:45 CMU-ESE Research Activities on Space Weather and Cosmic Rays and its impact

Chiang Mai University (CMU) has a longstanding history of astronomical research, beginning with the establishment of the Sirindhorn Observatory in the 1980s. Over the years, CMU has expanded its facilities to include advanced infrastructure for monitoring space weather and cosmic rays, such as the Chang Van neutron monitor and the CMU Space Weather War Room. In 2023, CMU launched the Research Group on Earth-Space Ecology (ESE), an interdisciplinary initiative to support and promote frontier research in space science. This group integrates expertise from various disciplines to innovate and explore the impacts of space weather on Earth, addressing challenges and opportunities in space-related studies. By fostering collaboration and innovation, the CMU-ESE group aims to position CMU as a leader in the field of space science research.

Speaker: Siramas Komonjinda (CMU)

02_Siramas_Hawaii2025_presentation.pdf

16:00 Ionospheric and Magnetospheric Responses to Space Weather

Thailand's awareness about space weather has grown significantly in the past decade. It is now commonly accepted that space weather, the dynamics of particles, and radiation outside the Earth can significantly affect human activities on Earth. We have looked at the ionospheric response using GNSS observations during geomagnetically quiet and disturbed times and disturbances produced by the Hunga Tonga volcano. Moreover, the investigation of magnetospheric responses let to the several studies, including the difference in waves’ characteristics in the plasma sheet during substorms and pseudosubstorms (pseudobreakups) and space-based observation of the auroral variability during substorm onset.

This research work was supported by Pre-Technology Incubation Grant from Science and Technology Park, Chiang Mai University

Speaker: Suwicha Wannawichian (CMU)

16:15 Low-Latitude Neutron Monitor Science: Solar Neutrons and Galactic Cosmic Rays at High Cutoff Rigidity

Speaker: David Ruffolo (U Mahidol)

Ruffolo-Hawaii.pdf

16:40 Real-time NM leader fractions

Speaker: Alejandro Sáiz (U Mahidol)

Real-Time NM Leader Fractions.pdf

Tuesday 7 January

09:00 → 09:20 NM Design / Hardware / Electronics

09:00 Overview of Univ. Oulu neutron monitors (OULU, DOMC, DOMB) and IGLED database

Speaker: Ilya Usoskin (OULU)

Usoskin_talk.pdf

09:20 → 09:40 Montecarlo simulations

09:20 OTSO - a new open-source magnetospheric particle trajectory and cutoff rigidity tool

Speaker: Nicholas Larsen (OULU)

Larsen_Presentation.pdf

09:40 → 10:30 Physics / Space Weather, Data Analysis, and Results

09:40 Neutron Monitor yield functions: applications and perspectives

Speaker: Alexander Mishev (OULU)

Mishev_Hawai_2025.pdf

09:55 Calibrating NM on Ground with AMS in Space

Speaker: Cristina Consolandi (UH Manoa)

Consolandi_AMS_NM.pdf

10:30 → 10:45 Coffee

10:45 → 12:05 Physics / Space Weather, Data Analysis, and Results

10:45 Investigation of Neutron Monitor Response to Cosmic Ray Air Showers.

Speaker: Chloe Heifner (UDEL)

Heifner_NMwksp_Jan25.pdf

11:15 Unusually long scattering mean-free path of suprathermal ions in the turbulent interplanetary magnetic field

Speaker: Joe Giacalone (University of Arizona)

04_Hawaii-NM-2025-Giacalone-final.pdf

11:35 Transport of GV Rigidity Solar Energetic Particles in Turbulent and Non-turbulent Interplanetary Magnetic Field and SEP profiles at 1 AU

Ground-level enhancement (GLE) is triggered by GV rigidity solar energetic particles (SEPs). In such high energies (a few hundred MeV/n to a few GeV/n), the characteristic of an SEP events differs from the more common low-energy SEPs at 1 au. We present several numerical studies on how the characteristics of an SEP event depend on parameters of the interplanetary magnetic field (IMF), pitch-angle scattering, energy, and ion mass charge ratio. We present that the large-scale turbulent IMF due to the random walk of the IMF footpoints can drastically change the time-intensity profiles and the pitch-angle distributions at 1 au. The GLEs characteristics will strongly depend on the location of the Earth or spacecraft. We provide another explanation for the unusual time-intensity profile and the pitch-angel distribution of the unusual GLE#44 on 1989 October 22 and conclude that such double-spike profiles are more common, however, the Earth was at the right place at the right time on 1989 October 22. We also investigate the importance of the mass-charge ratio on the onset time and decay phase of the intensity profiles of 4He, He3 and H ions at 1 au in both magnetically well-connected and weakly connected observers at 1au. We show that the HCS has the greatest impact on the observed He4 to H ratios at 1au and the asymptotic direction of the SEPs entering the magnetosphere.

Speaker: Ashraf Moradi (University of Arizona)

05_2024_NM_opening_Ashraf_2.pdf

12:15 → 13:30 Lunch

13:30 → 14:15 Montecarlo simulations

13:30 Monte-Carlo simulations of Neutron Monitor

Speaker: Pierre-Simon Mangeard (UDEL)

06_NMWorkshopJan2025_SimulationTalk_Mangeard.pdf

14:00 Monte Carlo Simulations of Neutron Monitors: Fixed Stations and Portable Monitors from CMU Research

This study presents Monte Carlo simulations using the FLUKA 4-4 package coupled with
the DMPJET model to analyze the response of neutron monitors at the Princess
Sirindhorn Neutron Monitor (PSNM) in Thailand, the South Pole Neutron Monitor, and a
mobile semi-leaded neutron monitor (Changvan) during a latitude survey. The
atmospheric and detector simulations accounted for deadtime corrections and employed
monthly solar modulation parameters alongside galactic cosmic ray (GCR) models to
calculate count rates and yield functions. Key results include the comparison of actual
and simulated count rates at PSNM from September 2022 to October 2023 and time-
series analysis of count rate trends at the South Pole, covering data from 1977 to the
present with a detailed focus on trends from 2010 onwards. Differential and integral
response functions were also determined for varying rigidity cutoffs, including the
Changvan monitor. Future work aims to enhance the simulation accuracy by
incorporating more frequent solar modulation parameters and increasing statistical
precision.
This research work was partially supported by Chiang Mai University, CMU Proactive
Researcher [grant number 905/2567] and the Seed International Initiatives.

Speaker: Achara Seripienlert (CMU)

07_Kim_CMU_MC_Sim.pdf

14:15 → 14:45 Montecarlo simulations

14:15 Monte Carlo design optimization for the United Kingdom’s new neutron monitor, the NM-2023

Aspinall M1, Alton T1, Binnersley C3, Bradnam S2, Cazzaniga C4, Croft S1, Frost C4, Joyce M1, Mashao D1, Packer L2, Turner T2, Wild J1
1 Lancaster University, Lancaster, United Kingdom
2 United Kingdom Atomic Energy Authority, Abingdon, United Kingdom
3 Mirion Technologies (Canberra UK) Limited, Warrington, United Kingdom
4 STFC Rutherford Appleton Laboratory, Harwell Campus, Didcot, United Kingdom

This presentation focuses on the extensive Monte Carlo N-Particle (MCNP) simulations used to design and optimize the United Kingdom’s (UK) new ground-level neutron monitor, the NM-2023. Through MCNP parameter optimizations and the use of 1-inch diameter, 4-atm helium-3 (He3) gas-filled proportional counters, the monitor achieves a 64% smaller footprint, 80% smaller volume, and 55% of the mass of the 6-NM-64, while delivering equivalent counting performance. The design also allows for potential cost reductions in fabrication and deployment through a simpler slab configuration, reduced volume and cost of raw materials, and smaller housing and infrastructure requirements. The presentation details the derived environmental radiation source, the development of a 6-NM-64 benchmark model, and the creation of parameterized ‘cavity’ and ‘slab’ models. The ‘cavity’ design closely resembles the NM-64, while the ‘slab’ design is more akin to the IGY monitor. A randomized parameter scan of the ‘cavity’ model demonstrates that the NM-64 is highly optimized for large-volume boron trifluoride (BF3) counters in terms of lead (Pb) mass relative to total count rate. Parameter optimization of the ‘slab’ design evaluates configurations based on constant volume, equal Pb thickness, constant Pb mass, and detector placement, resulting in a more compact design with equivalent counting performance to the 4-NM-64. Several experimental campaigns validate the simulation results, providing a robust foundation for the new monitor’s design.

Speaker: Michael Aspinall (U Lancaster)

08_ASPINALL NM-2023 Monte Carlo design optimization for the United Kingdom’s new neutron monitor, Haleakala, v1, 7 Jan 25.pdf

14:45 → 15:05 Operations and Housekeeping

14:45 Data processing of the Bartol Neutron Monitors

Speaker: Pierre-Simon Mangeard (UDEL)

09_NMWorkshopJan2025_DataProcessingTalk_Mangeard.pdf

15:05 → 15:20 Coffee

15:20 → 15:50 Computing Infrastructure and Data Transfer

15:20 Influence of Solar Emissions on the Cosmic Ray Observatory at Sierra Negra, Puebla, México

Speaker: Stephanie de la Torre (UNAM)

Haleakalā Neutron Monitor Workshop.pdf

15:50 → 16:30 OPEN DISCUSSION

Wednesday 8 January

07:00 → 07:30 Meeting at Honolulu Airport (HNL)

07:30 → 09:15 Flights to Maui Kahului Airport (OGG)

Hawaiian airlines and Southwest airlines departs every half an hour. Duration of the flight is 45 minutes.

09:15 → 09:45 Meeting at Kahului Airport, picking up the bus

09:45 → 11:15 Bus travel from Maui Airport to the summit of Haleakala

11:15 → 12:45 HLEA and THIMON ribbon cutting ceremony / DKIST tour

12:45 → 13:30 Bus travel from the summit

13:30 → 14:30 Early dinner at Kula Bistro

14:30 → 15:00 Bus travel to Maui Airport

15:00 → 17:00 Flights to Honolulu (HNL)

Thursday 9 January

09:00 → 10:30 Splinter meetings

10:30 → 10:45 Coffee

10:45 → 12:15 Splinter meetings