Below are the abstracts of all projects that were presented during the 2025 Boulder Solar Alliance REU Symposium, held during the final week of the program. Partners Across the Sky student posters are also included.
Student name in BOLD
Modeling Orbital Debris Impacts: Visualization and Analysis Tools for the Debris and meteoroid ENvironment Sensor (DENtS)
Andrea Borlovan1,2, David Malaspina1,2, Zoltan Sternovsky1,2, Timothy Hellickson2, Stacy Wade2, Lauren Christenson1,2, Justin Astalos1,2, Laila Andersson2, David Martin2
1University of Colorado Boulder, 2Laboratory for Atmospheric and Space Physics
*poster session only
The Debris and Meteoroid ENvironment Sensor (DENtS) project addresses a critical gap in our understanding of the Low Earth Orbit (LEO) small debris environment. While spacecraft’ face increasing risks from orbital debris, particularly particles smaller than 3mm, current observation techniques fail to capture the full scope of these threats. DENTS proposes an in-situ detection system, integrating PVDF foils, impact plates, and electric field antennas to characterize debris populations and their effects on spacecraft operations. In support of this mission, this project develops computational tools to simulate debris trajectories, visualize orbital intersections, and analyze detection geometries. These tools provide key insights into impact probabilities, detection coverage, and velocity components, serving as a foundation for validating the DENtS design and informing future hardware deployment. By providing predictions and visualizations, this work strengthens the foundation for DENtS’ continued development and its role in addressing critical observational gaps.
2D Pattern of Total Electron Content day-to-day Variability during Quiet Days of Solar Minimum
Jaylem Kai Cheek and Xuguang Cai
Laboratory for Atmospheric and Space Physics (LASP)
Currently, observed day-to-day variations in ionospheric Total Electron Content (TEC) during quiet periods (Kp < 3) are primarily attributed to lower atmospheric forcing. However, recent studies using two-dimensional (2D) images suggested that geomagnetic forcing may contribute significantly even during quiet periods, particularly near solar minimum. We systematically investigated this phenomenon through a three-stage analysis. First, we identified all geomagnetically quiet days in 2018 (solar minimum transition year) using the Auroral Electrojet Index data from SuperMAG, a global network of nearly 600 ground-based magnetometers. Strict selection criteria were applied to isolate subtle geomagnetic fluctuations. These quiet days were grouped into quiet cases, defined as sequences of two or more consecutive quiet days. Next, we calculated TEC percentage differences for each day within every quiet case, focusing on spatial (latitude-longitude) patterns and temporal evolution over the North American continent. Finally, we conducted a comprehensive statistical analysis of these differences to identify recurring patterns and anomalies. Our results reveal measurable geomagnetic contributions to TEC variability during quiet conditions, especially in the form of persistent spatial and temporal patterns. These findings challenge current models that overlook minor geomagnetic forcing, indicating the need for revisions to improve ionospheric characterization. The study demonstrates that even during periods of minimal geomagnetic activity, TEC variability can still be impacted, with implications for improving space weather prediction accuracy.
SpinSpotter in a Solar Context: Evaluating Rotation Across Spectral Bands
Raven Mercer1, Rae Holocomb2, Serena Criscuoli3
1University of Colorado Boulder, 2University of California Irvine, 3National Solar Observatory
*poster session only
The way a star spins holds clues to its magnetic behavior, surface evolution, and the environments of its orbiting planets. SpinSpotter, a code originally built to analyze Kepler and TESS data, detects stellar rotation by identifying repeating light curve features. While effective for distant stars, adapting SpinSpotter to study the Sun introduces new challenges; particularly its complex surface and wavelength-dependent irradiance. In this project, we repurposed SpinSpotter to study daily irradiance data from NASA’s Solar Radiation and Climate Experiment (SORCE) mission across 240–1000 nm. We created custom solar light curves from UV, visible, and IR bands, and evaluated rotational signal clarity using autocorrelation and Fourier-based methods.To maintain solar data accuracy while improving rotation period detection, we modified smoothing and peak-finding techniques to preserve sunspot-related anomalies. UV bands show strong periodic signals and consistent autocorrelation peaks, indicating high sensitivity to solar rotation. IR bands yield poor results, likely due to surface noise. Visible bands provide moderate detection accuracy, particularly during quiet solar periods with minimal sunspot interference. These results suggest that SpinSpotter’s effectiveness is highly wavelength-dependent and that UV irradiance provides the best path for measuring solar rotation. This work establishes a framework for applying this stellar tool to solar data and informs future extensions to solar-type stars with similar variability.
Solar Cycle Variation of High Latitude Torsional Oscillations
Alexander Moncello1,2, B. Lekshmi2, Sushanta Tripathy2, Kiran Jain2
1Chatham University, 2National Solar Observatory
Solar torsional oscillations are alternating bands of faster- and slower- than-average flows that migrate from mid-latitudes to low- and high- latitudes. The bands that propagate towards the equator emerge one to two years prior to the solar cycle and have been shown to exhibit a strong correlation with the sunspot activity. The poleward-propagating bands develop near the maximum of the previous cycle and are still poorly understood. With nearly 24 years of helioseismic analysis from the Global Oscillation Network Group (GONG) Doppler velocity observations, we study these bands of residual east-west (zonal) flows along the surface and subsurface layers. We examine the migration of the equatorial branch of torsional oscillation and its connection with the low-latitude magnetic activity, as well as the temporal variation of the poleward branch and its relationship with the corresponding polar field observations. Finally, we explore the possibility of high-latitude flows to serve as potential indicators for the strength of the upcoming solar cycle.
Determining Properties of Solar Eruptions to Improve Space Weather Forecasting Using UCoMP Spectroscopic Data
Chloe Pistelli1, Momchil Molnar2, Joseph Plowman2
1Taylor University, 2Southwest Research Institute
Forecasting space weather depends critically on understanding coronal mass ejections (CMEs) as they evolve through the corona and heliosphere. While previous studies have relied on imaging to track solar eruptions, our work proposes complementary spectroscopic diagnostics based on the He I 1083 nm line observed with the Upgraded Coronal Multichannel Polarimeter (UCoMP). The He I 1083 nm line is Hanle-sensitive to the typical coronal magnetic field strengths, making it a potential diagnostic tool for the cooler component of the coronal magnetic environment. Complementary to available imaging data, we present hyperspectral He I 1083 of CME datasets from the UCoMP observations, which allow for the 3D velocity understanding of the CME evolution, including the line-of-sight component from the Doppler effect. Our results demonstrate that solar prominence eruptions are clearly detected in UCoMP’s He I 1083 nm observations, complementing the extreme ultraviolet and white light observations widely used. This confirms the utility of UCoMP for probing the dynamics of the middle corona, ultimately enhancing space weather prediction by improving our ability to detect and characterize Earth-directed eruptions earlier and more accurately.
A Novel Method for Cross-Calibrating Polar Field Measurements between WSO and HMI
Stephanie Puckett1, Bibhuti Kumar Jha2, Lisa Upton2
1University of Colorado Boulder, 2Southwest Research Institute
Accurate prediction of space weather and its effects on our technological infrastructure is of growing importance. Space weather events are dictated by solar activity. One of the most reliable precursors of future solar activity is the strength of the Sun’s polar magnetic fields at the end of the cycle, which acts as the seed for the subsequent solar cycle. A major challenge is the limited precision of polar magnetic field measurements, caused by observational constraints, such as the
Earth-Sun vantage point, which hinders our ability to reliably use them. The Wilcox Solar Observatory (WSO) has recorded polar fields continuously at low resolution since 1976, while the Helioseismic Magnetic Imager (HMI) has provided much higher resolution measurements since 2010. Significant discrepancies exist between the two data sets, largely due to these differing resolutions, observation techniques, and spectral wavelengths. All of these factors complicate our ability to create a long-standing and homogeneous data set, a requirement for the future cycles forecast. By accounting for key variables such as instrumental offsets, the Sun’s B-angle tilt, and the evolution of polar field strength, we developed a technique to establish the relationship between HMI and WSO measurements. This study aims to cross-calibrate WSO and HMI polar field data to create a cohesive data set which capitalizes on the strengths of both sets of observations. After our cross-calibration, preliminary results suggest that polar field measurements between these two instruments can be aligned. This uniform data set will be an ideal resource for solar cycle forecasts and will enhance our theoretical understanding of the solar dynamo process responsible for solar cycle variability.
Tracking Halo CME across 1 Astronomical Unit with PUNCH
Kieran Russell1, Sam Van Kooten2, Craig DeForest2 and the PUNCH development team
1Michigan State University, 2Southwest Research Institute
The Polarimeter to UNify the Corona and Heliosphere (PUNCH) mission acts as a “virtual coronagraph” with a very wide 90° field of view. On May 31st, 2025, PUNCH tracked a large halo CME as it crossed the entire distance from Sun to Earth, losing sight of the leading edge less than 3 hours before impact with the GOES satellites. This is the first CME tracked directly from Sun to Earth using visible light observations on the Sun-Earth line. We have conducted a 2-D leading edge analysis of the CME and its trajectory, building on the existing “ice-cream cone” model of the geometry. We compare the simple model geometry to the far more complex evolution of the cloud as it crosses the void and show that the large cloud is composed of multiple distinct structures moving at different speeds.
Martian Discrete Aurora Analysis during MAVEN and EMM Conjuctions
Elijah Smith1, K. Chirakkil2, R. Lillis3, J. Deighan2, S.Xu3, J. Gérard4, L. Soret4, Y. Harada5, M. Chaffin2, S. Jain2, D. Brain2, M. Fillingim3, G. Holsclaw2, N. Schneider2, N. Al Saeed6
1Fort Lewis College, 2Laboratory for Atmosphere and Space Physics, 3Space Science Laboratory/UC Berkeley, 4Université de Liége, 5Kyoto University, 6UAE Space Agency
The Discrete Martian Aurora, known on Earth as the Northern or Southern Lights is not well understood. Previous work revealed discrete aurora form when suprathermal electrons from the solar wind interact with the Martian crustal magnetic field and atmosphere, resulting in ultraviolet oxygen (OI) emissions at 130.4 nm. To improve the understanding of the formation of discrete aurora, in-situ data from the Mars Atmosphere and Volatile EvolutioN (MAVEN) Particles and Fields instruments, along with ultraviolet imaging from the Emirates Mars Ultraviolet Spectrometer (EMUS) on board the Emirates Mars Mission (EMM), were analyzed during conjunction events. A conjunction event in this study is defined as when MAVEN and EMUS made near-simultaneous observations and MAVEN flew directly over a discrete aurora. Conjunction events leveraged the EMUS ability to look at the whole nightside of Mars to see discrete auroras when OI emissions were detected. Simultaneously, MAVEN recorded data on the suprathermal electron flux and pitch angle distribution, magnetic field strength and orientation, ionospheric densities and temperatures angle, temperature, and density of a discrete aurora. The combination of MAVEN and EMUS provides an in-depth look into the properties and formation of discrete aurora.
Empirical Studies of Increased Measurement Integration Time on Modeling Solar Irradiance Variability in the Near-Infrared
Raven Stribling1, Odele Coddington2, Courtney Peck2
1Northwest Vista College, 2Laboratory for Atmospheric and Space Physics
Understanding solar irradiance is essential to understanding how Earth’s atmosphere and climate respond to diJerent solar variabilities. Current models of solar irradiance, particularly in the near-infrared, remain underdeveloped. Precise observations and measurements are crucial towards improving accurate models and to better understand the eJects of solar irradiance on Earth. The variability of solar spectral irradiance (SSI) at near-infrared wavelengths longer than 1600 nm remains poorly understood due to both small irradiance magnitude as well as small short- and long-term variability, theoretically estimated to be of order 10x smaller than the variability of the total solar irradiance (TSI) over the solar cycle. This challenging combination imposes stringent requirements on instrument precision and accuracy. Since September 2024, a research experiment with the Spectral Irradiance Monitor (SIM) instrument on the Total and Spectral Solar Irradiance Sensor-1 (TSIS-1) mission has been undertaken to evaluate the impact of longer measurement integration times on measurement precision for two near-infrared spectral regions from approximately 1800 nm to 1850 nm and from approximately 2000 nm to 2050 nm.
In this work, we quantify improved measurement precision in the research scans relative to the precision of the standard operational measurements in these wavelength ranges. Furthermore, we quantify an improved ability to relate enhanced precision, near-infrared, SSI measurements to proxies of solar magnetic activity evidenced in faculae and sunspots and, by doing so, demonstrate the importance of enhanced near-infrared SSI measurement precision to irradiance model development. We compare and contrast estimates of SSI variability developed from using multiple linear regression models of SSI with solar proxies (faculae and sunspots), for standard operation TSIS-1 SIM data versus extended integration data. Our findings contribute to refining SSI models and improving understanding of how solar proxies influence near-infrared SSI and impact Earth’s climate and to informing the operational planning for near-infrared observations of the future TSIS-2 SIM instrument.
Evaluation of Thermospheric Density Simulated by TIEGCM during 2014-2024
Antonio Hernandez Torres1, Haonan Wu2, Kevin Pham2, Wenbig Wang2, Jordi Vila-Pérez2
1Front Range Community College, 2High Altitude Observatory, National Center for Atmospheric Research
The growing number of satellites in low Earth orbit (LEO) demands improved upper atmospheric modeling to ensure accurate trajectory prediction and collision avoidance. Atmospheric drag, largely determined by the density of the upper atmosphere, plays a key role in shaping satellite orbits. This study evaluates the long-term performance of the NSF NCAR Thermosphere-Ionosphere-Electrodynamics General Circulation Model (TIEGCM) in simulating atmospheric density. The project focuses on data-model comparisons using in-situ neutral mass density observations from multiple LEO satellite missions, including Swarm and GRACE (including GRACE-FO). The study employs NSF NCAR TIEGCM 3.0 driven by the Heelis high-latitude potential model. Modeled densities are compared to satellite observational densities, derived from accelerometer data or precise orbit determination, for a full solar cycle, from 2014 to 2024. The model accuracy is evaluated and correlated to varying seasonal, solar activity, and geomagnetic conditions. The effects of geomagnetic activity, driven by the Kp index, are studied over short timescales ranging from hours to days. Results indicate that solar activity (the F10.7 solar radio flux is used as a proxy for solar EUV radiation to drive the model) significantly influences prediction accuracy throughout the 11-year solar cycle. Simulations display a better performance during periods of high solar activity. Additionally, the impact of seasonal variations is reflected on a yearly scale, with improved performance during solstices, compared to equinoxes.
Visualizing the Solar Corona in 3D using PUNCH
Jack Vogel1, Ritesh Patel2, Anna Malanushenko2, Elena Provornikova2, Craig DeForest2
1University of North Georgia, 2Southwest Research Institute
The solar corona and heliosphere are visible via sunlight that is Thomson-scattered off free electrons and detected by coronagraphs and heliospheric imagers. The Polarimeter to Unify the Corona and Heliosphere (PUNCH) mission utilizes polarization properties of Thomson-scattering to glean 3D information about the structure of plasma and magnetic fields associated with the free electrons. We demonstrate several visualization methods to make these unusual images accessible and intuitive for visual analysis. In particular we explored using color to represent polarization data directly, following early development by the PUNCH mission team. We also developed pseudo color schemes to represent derived quantities such as the out of sky plane angle. We apply these schemes to forward modeled CME image data from the PUNCH pre-launch CME challenge and illustrate how they might be used for visual analysis of PUNCH images.
Listening to Plasma Waves in Earth’s Magnetosphere
Lucy Williams1, Lauren Blum2, Tiffany Costello2, Xueling Shi3,4, Michael Hartinger5,6
1Smith College, 2Laboratory for Atmospheric and Space Physics, 3Virginia Tech, 4Clemson University, 5Space Science Institute, 6University of California Los Angeles
Electromagnetic ion cyclotron waves, or EMIC waves, are thought to play a crucial role in the dynamics of high energy electrons in the Earth’s magnetosphere. Typical techniques for studying EMIC waves have relied on visual detection and automated algorithms, however this project seeks to employ sonication techniques, in which numerical data is transformed into sound, to identify and understand waves in the complex near-Earth environment. Using data from the GOES spacecraft, this project explores different methodology within the sonification process to better understand how different data handling, audio mixing, and listening speeds impact the detection of EMIC waves. Using sonification methods, we explore listening to month- to year-long timescales of data in a way that traditional visual methods had not previously allowed, in order to better recognize patterns in EMIC wave occurrence and their relationship to geomagnetic activity.