Summer 2024

Below are the abstracts presented during the 2024 Boulder Solar Alliance REU Symposium, held during the final week of the program.

The Partners Across the Sky (PAARE) are also included, as they present at the poster session during Symposium week.

Student name in BOLD

Understanding the Variability of Mars’ Upper Atmosphere  

Spencer Biske1, Quan Gan2, Xiaohua Fang2

1University of California Santa Barbara, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

Atmospheric waves play a pivotal role in the variability of Mars’ thermosphere-ionosphere
(TI) system. Upward-propagating tides (a prominent type of global-scale oscillation) from the lower
and middle atmosphere are an important driver of the dynamics that contribute to processes such as
thermospheric heating and atmospheric loss. The Mars Atmosphere Volatile EvolutionN (MAVEN)
mission’s NGIMS instrument takes in situ measurements of number density across a wide range of
latitudes, altitudes, solar longitudes, and local solar times (LSTs), which offers an unparalleled
opportunity for studying the impact of atmospheric tides on the Martian thermosphere. Previous
studies of Mars’ upper atmosphere have consistently shown strong tidal signatures in zonal
wavenumber-2 and wavenumber-3. In this study, we perform spectral analysis of NGIMS data for
CO2, Ar, N2, and O number density, as well as temperature, at four solar longitudes (60o, 90o, 180o,
and 340o). These segments of the mission were chosen because they have similar LST and latitude.
Out spectral analysis aims to determine the relative significance of zonal wavenumbers 1-6 in the
observed longitudinal variations. We report for the first time significant contributions from zonal
wavenumber-6. This wave peaks at higher altitudes during aphelion seasons (60o, 90o) and at lower
altitudes during equinox seasons (180o, 340o). It is also seen to propagate vertically below 170km in
all seasons, though it becomes a standing wave at higher altitudes. In general, most of the tidal
signatures follow a similar pattern: they propagate at lower altitudes, but they stop at various points.
Our analysis of these propagations significantly advances the understanding of the role that the
lower atmospheric waves play in the longitudinal variations of the thermosphere at Mars.

Martian Atmospheric Escape Through Foreshock Transient Events

Alexandros Cooke-Politikos1, Sergey Shuvalov Ph.D2, Yaxue Dong Ph.D2, Yi Qi Ph.D2

1University of Hartford, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

Foreshock transient events are phenomena that occur upstream of a planetary bowshock and have
the potential to affect a planet’s magnetosphere both globally and locally. The Hot Flow Anomaly
(HFA) is a type of foreshock transient event that is caused by the interaction of an interplanetary
current sheet with a planet’s bow shock. Unlike Earth, Mars’ lack of intrinsic global magnetic field
results in the observation of HFAs much closer to the planet. This critical distinction means that
HFAs can reach into the ionosphere and accelerate heavy planetary ions (O+ and O2+) via first order Fermi acceleration to several keV energies. This effect allows these ions to escape, which we suggest contributes to atmospheric loss. This mechanism may be at play at all unmagnetized bodies with atmospheres directly exposed to stellar winds such as Venus. We explore the ways in which this phenomenon may act as an additional (and unexplored) channel for Martian atmospheric loss. Data from the Mars Atmospheric and Volatile EvolutioN (MAVEN) probe is studied in the shock upstream region to qualitatively identify HFA events. The dataset analyzed is limited to solar maximum and MAVEN orbits with high solar wind coverage. Events are identified by a combination of solar wind characteristics indicative of an HFA, including magnetic field rotation, solar wind disturbances, and decreases in solar wind density and velocity. More than sixty events have been selected for analysis spanning roughly fourteen months of observations. Through this process, we estimate the occurrence rate of HFA events at Mars to be approximately 1 per day, and roughly 50% of events exhibit heavy-ion acceleration. Additionally, we utilize MAVEN data to calculate various HFA characteristics such as event size, duration, propagation speed, and escaping fluxes of heavy ions. This broadly improves understanding of HFAs at Mars and allows for the assessment of the significance of this effect on Martian atmospheric loss. This work bolsters scientific understanding of the mechanisms of Mars’ atmosphere and solar wind interactions which is important in understanding Martian atmospheric and planetary history.

Exploring the Impact of Sulfur and Chlorine Chemistry on the Dynamics and Escape of Hydrogen Isotopes on Venus

Simon Correra1, Eryn Cangi2, Michael Chaffin2, Roger Yelle3, Bethan Gregory2, Jusin Deighan2

1University of Connecticut, 2Laboratory for Atmospheric and Space Physics (LASP), 3Lunar and Planetary Laboratory

Poster

Modern Venus contains only a small amount of water, ~3cm global equivalent layer. It used to
contain much more with a similar content to Earth, which raises the question of why and how Venus lost
its water. Understanding the processes that lead to water loss improves our understanding of planetary
evolution and what makes different planets unique. On Venus, water loss can be studied through the rates of escape of its light components, hydrogen (H) and deuterium (D). Energy from the sun is able to set off chemical reactions that result in the destruction of the water molecules, and the escape of H, D, H2, and HD. Bluejay, a photochemical model developed for Mars, was adapted for the Venusian atmosphere above 90km. Chlorine and sulfur provide important H and D chemical pathways–e.g. aerosol adsorption or deuteration of the sulfuric acid droplets. We have added species including HCl, DCl, Cl, ClO, ClCO, S, SO, SO2, SO3, H2SO4, and HDSO4 to the model to improve our representation of the real atmosphere. The product of this study is an understanding of the sinks and escape pathways of H and D, with a focus on the effects of the newly added species. We will present the effects of chlorine and sulfur chemistry on H and D escape and make comparisons to previous iterations of the model and other similar studies.

Analysis of subsurface flows from GONG Doppler observations during solar cycles 23-25

Sumner Cotten1, Sushanta Tripathy2

1College of St. Scholastica, 2National Solar Observatory

Poster

 

Helioseismology is a powerful tool in understanding the overall nature of the Sun’s interior dynamics using the acoustic oscillations observed at the surface. In this work, we have focussed on the behavior of subsurface flows up to a depth of 30 Mm below the surface.
Using Doppler velocity data obtained from the Global Oscillation Network Group (GONG) and ring-diagram technique, we analyse zonal and meridional flows as functions of latitude and depth, over solar cycles 23 through 25. The flow measurements have several systematic variations with disk positions and indicate a centre-to-limb variation as the underlying cause. Following earlier methods, corrections were implemented to account for periodic changes in the sun’s inclination angle toward Earth, and geometric distortion effect caused by the limited resolution of the instrument. We use a linear fit in inclination angle to correct the flow velocities. Assuming that the systematic variations due to the geometric
effect vary only with the distance from the disk centre, we use radial components of Zernike polynomials to correct the zonal and meridional flows. After compensating for these systematic effects, we compare flow velocities for different solar cycles up to approximately 5% of the solar radius from the solar surface.

Magnetic Tomography of a Solar Active Region

Eric Dunnington1, João da Silva Santos Ph.D2, Serena Criscuoli Ph.D2

1Rensselaer Polytechnic Institute, 2National Solar Observatory

Poster

Solar chromospheric heating and dynamics are contested topics. The reasons behind the
excessive temperatures in the chromosphere are still not understood. Determining the magnetic
and velocity fields from observations in the chromosphere can shed light on the mechanisms
behind the heating, especially above active regions where the magnetic field and dynamics are
particularly intense relative to the quiet Sun. We use the advanced capabilities of the Visible
Spectro-Polarimeter (ViSP) instrument in NSF’s Daniel K. Inouye Solar Telescope (DKIST) to
obtain high-resolution spectra in three different passbands, providing multi-height magnetometry
of the photosphere and chromosphere. Using inversion techniques and multiline analysis, we
determine the magnetic field and plasma velocities at varying heights in the solar atmosphere
over an active region. The Ca II 854.2 nm spectral range shows strong evidence for large
velocity gradients and complex dynamics, suggesting multiple line-of-sight velocity components
in the spectral range. These high-velocity flows may be due to interactions of opposite magnetic
polarities in the photosphere or higher in the solar atmosphere. Understanding the relationship
between the observed chromospheric plasma flows and magnetic fields will allow us to make
stronger conclusions about chromospheric heating and dynamics in active regions. Additionally,
this knowledge will impact the greater field of solar weather, as chromospheric dynamics
directly impact solar winds and other solar events.

Machine Learning for Understanding Mars Global Magnetic Field Distributions

Benjamin Goldman1, Xiaohua Fang2, Xiangning Chu2, Xin Cao2

1Columbia University, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

The magnetic field environment near Mars is complex, driven by the interplay between the intrin-
sic, inhomogeneously-distributed crustal magnetic field and the impinging solar irradiance and solar wind conditions. The intrinsic magnetic field component rotates with Mars and is best described using the planetary frame, while the external magnetic field component is driven by the Mars-solar wind interaction and is more organized in the Sun-Mars reference frame. This combination creates intricate spatio-temporal variations in satellite measured magnetic field distributions, posing great challenge for our understanding. Recent efforts to separate these two components using empirical crustal field models have yielded promising results, significantly improving our understanding of the Mars magnetic field environment by focusing on the external field distribution and elucidating the Mars-solar wind interaction. Machine learning algorithms have emerged as powerful tools in planetary and space physics, demonstrating remarkable capabilities in analyzing vast datasets. In this study, we develop a decision tree-based regression model to process about 10 years of magnetic field data acquired by NASA’s Mars Atmosphere and Volatile EvolutioN (MAVEN) mission, with a focus on characterizing the external magnetic field. Unlike traditional statistical methods, the machine learning approach inherently captures nonlinear relationships between diverse driving factors and the observed magnetic field. These driving factors encompass not only upstream solar wind parameters (density, velocity, and IMF), but also solar irradiance (which determines the ionosphere) and Mars’ seasonal and rotational effects on crustal field orientation. By disentangling and assessing the relative importance of each driving factor, this study offers valuable insights into the distribution and variability of the magnetic field at Mars.

Identifying Undisturbed Solar Wind with Plasma
Measurements in the Inner Solar System

Nadia Gonzales1, Robin Ramstad Ph.D2, Yaxue Dong Ph.D2

1University of Texas at Austin, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

 

The solar wind drives a variety of processes in the Martian induced magnetosphere, measuring the upstream solar wind at Mars is thus critical for understanding Mars’ response to variations in the solar wind. The Mars Atmosphere and Volatile Evolution (MAVEN) mission was launched in 2014 and has been collecting data to study how the solar wind interacts with Mars’ upper atmosphere and ionosphere. MAVEN’s Solar Wind Ion Analyzer (SWIA) and Solar Wind Electron Analyzer (SWEA) measure the energy and angular distributions of ions and electrons. Here, we test an indicator to determine which MAVEN measurements are in undisturbed solar wind, as opposed to magnetospheric plasma. We utilize derived moment data from SWIA & SWEA to calculate the ion dynamic pressure and the electron thermal pressure. We expect the ratio of these pressures to be a potential indicator of undisturbed solar wind. To determine the validity of this indicator, we analyze how this ratio compares between the magnetosheath and undisturbed solar wind, and how it changes with various solar wind conditions. To determine the applicability of this indicator at other planets, we compare the ratio with other solar wind
measurements from spacecraft (e.g. WIND and Venus Express) varying in heliocentric distance.

Finding Solar Storms with MAVEN data

Ethan Grant1, Shannon Curry, Ph.D2, Phil Chamberlin, Ph.D2

1Palomar College, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

 

On the sun, highly twisted magnetic field structures realign into less tense
configurations and release plasma, causing it to travel out into the solar system. This is
known as an Interplanetary Coronal Mass Ejections (ICME). Fast solar winds emit from
coronal holes on the Sun, which are open magnetic fields, and slow solar winds stay
near the heliospheric current sheet. Plasma converges between the two when the fast
solar wind overtakes the slow solar wind, which is called a stream interaction region
(SIR). Both of these events affect the flow of the solar wind at Mars. The Mars
Atmosphere and Volatile EvolutioN (MAVEN) mission has been observing solar events
headed towards Mars since late 2014 using the Solar Wind Ion Analyzer (SWIA) and
Magnetometer (MAG). Solar wind interactions at Mars are especially unique due to it
being 1.5 AU away from the sun, causing the interactions on Mars to be different from
Earth’s interactions with the solar wind. The constant streams of solar wind and coronal
mass ejections have the potential to erode Mars atmosphere and thus remove the
oceans of water it once had.
When identifying these solar events through MAVEN data, the total thermal and
magnetic pressure is used as an indicator. This is because it has a simpler temporal
variation to identify and show events when they aren’t smooth, like a shock from an
ICME. When an ICME creates a shock, it can be seen as a simultaneous spike across
the measurements. When identifying an SIR, typically the magnetic field and density
spike, followed by a delay in increase from the temperature and velocity. Currently, there
is no catalog of these solar transient events at Mars. We will present an algorithm to sort
through the MAVEN data in order to classify these natural events. We will present a full
catalogue of events as well as statistics for CME’s and SIR’s, including the velocity,
temperature, density, magnetic field, and magnetic/thermal pressure. This could be
especially useful for future human space endeavors, as understanding these solar
events could further implement safety measures.

Tool and Asset Development for Occultation Full Dome Visualizations

Elizabeth Hamilton1, Mateo Vasquez2, John Keller3,4, Micah Acinpura3,4, Nick Conant3,4

1Towson University, 2University of North Georgia, 3Fiske Planetarium, 4University of Colorado at Boulder

Poster

 

 

Public outreach regarding stellar occultations (when an object of large angular size blocks
an object of a smaller angular size from an observer’s view) has increased in recent years
partially due to the Fiske Planetarium’s work on Science through Shadows. Through a
collaboration between the Fiske Planetarium and the American Museum of Natural History, we
aim to further occultation outreach by creating a visualization asset that will allow for users to
showcase past and possibly future occultations in the AMNH OpenSpace planetarium software.
Utilizing data from the NASA Lucy Mission occultation efforts, we ensure that the visual
representations of the events within the software are as accurate to life as possible. The
occultations we aim to visualize are of Lucy Mission target asteroids occulting stars. We will
create these visualization assets by using Lua programming language to code and develop these
assets within the Open Space platform. The resulting visuals will allow users to simulate
occultations for educational purposes. There will be a variety of perspectives of the occultations
that could be investigated through OpenSpace to understand occultations as a researcher and to
engage and educate the public about the geometry and workings of occultations and planetary
science. With the OpenSpace platform being open-source and free to use, the creation of these
assets will allow for a resource of learning for a wide audience.

Analyzing Short-term Solar Activity Bursts: Exploring the Capability for Predicting
next Burst’s Amplitude

Ainsley Helgerson1, Mausumi Dikpati Ph.D.2, Kiran Jain Ph.D.3

1Embry-Riddle Aeronautical University, 2NSF-NCAR High Altitude Observatory, 3National Solar Observatory

Poster

Within the sun’s 11-year solar cycle, there are short-term variabilities with periods typically
spanning 6-24 months, often called Rieger-type periodicity or quasi-biennial oscillations (QBOs).
These periodic bursts of solar activity are highly correlated with coronal mass ejections (CMEs)
and solar flares, which impact our technological society through space weather hazards. This
analysis seeks to determine whether specific patterns exist, such as correlations between the
periods of activity bursts and the amplitudes of the following bursts. We developed a code and
implemented it on long-term SILSO Hemispheric Sunspot Number Data to obtain running
averages with Gaussian smoothing. To derive short-term variability, we subtracted the mean or
basal solar cycle trend (i.e., 27 Carrington rotation Gaussian smoothed data) from smoothed daily
SSN. Three different averaging lengths (5, 7, and 9 rotations) were used to obtain the smoothed
daily SSN. Next, we developed an algorithm to derive the peak amplitude and Full Width at Half
Maximum (FWHM) of all these bursts, allowing us to determine the corresponding periods of
these bursts. We then computed the lag correlation between the periods and amplitudes of these
bursts in both hemispheres, plus, applied autocorrelation among the properties of these bursts. We
found a moderate inverse correlation (~50%) between the period of the n-th burst and the
amplitude of the (n+1)-th burst, implying that the shorter the burst duration, the stronger the next
burst is. Interestingly, we also found a very strong autocorrelation (~72%) among the periods of
the bursts. This indicates that the Sun has a short-term memory of 1-2 years, and hence the periods
from one burst to the next are not random but follow a pattern. Such memory has also been indicated through the exploration of SSN data by artificial intelligence (AI) and information-
theoretic (IT) approaches. The results from our analysis can be used to build a forecasting tool which will assess the nature of upcoming enhanced bursts of activity.

Experimentally Determining Minimum Power Threshold for Successful UHF Radio Commanding

Caleb Johnson1, Maggie Zheng1, Aimee Merkel1, Evan Bauch1

1Laboratory for Atmosphere and Space Physics (LASP)

Poster

The presentation will focus on one such REU project supported by the Laboratory for
Atmospheric and Space Physics (LASP). The conducted research utilizes Ultra High Frequency
(UHF) radio testing to support radio satellite communications for future LASP CubeSats.
CubeSats are small satellites that are less expensive and faster to develop, making CubeSats
exciting opportunities to train students. LASP CubeSats have been used for a variety of science
missions, such as studying space weather or extreme exoplanets. All LASP CubeSats utilize
UHF communications for vital functions such as commanding the spacecraft and receiving
spacecraft health and telemetry. Determining adequate power levels for the transmitting ground
station is important for Federal Communications Commission (FCC) licensing. The project
involves experimentally determining the minimum power threshold for 95% of commands sent
to a CubeSat to be successfully received. This presentation will discuss the experimental set-up,
which allows for incremental adjustment of power levels and determination of the number of
sent and received commands. The results of the experiment will be presented, as well as the
skills gained through this research project, such as lab safety, hands-on hardware experience,
satellite link budgets, and professional and science communication.

Multi-Instrument Views of the Sun in H-alpha: The Eclipse and Beyond

Aiza Kenzhebekova1, Kevin Reardon2, Sarah Bruce2,3

1University of Edinburgh, 2National Solar Observatory, 3University of Colorado at Boulder

Poster

The corona, the outermost layer of the solar atmosphere, exhibits unexpectedly hot
temperatures—reaching millions of Kelvin—while the Sun’s surface is only around 6,000K. To study the driver for this heating phenomenon, measurements of the Sun in the Hydrogen-alpha
(Hα) line from the April 8th, 2024, total solar eclipse are displayed, processed, and aligned with
coronal images from the same time period. Hα represents the first Balmer series transition of the
Hydrogen atom, which emits light at a wavelength of 6562.8 Å, and is distinctly suited to solar
observations due to its accessibility within the visible spectrum as well as its sensitivity to
temperature and velocity. Using observations from GONG (Global Oscillation Network Group),
Chinese H-alpha Solar Explorer (CHASE), and a Celestron C-8 telescope with an attached
spectrograph, we aligned and analyzed solar images taken around the time of the eclipse. Using
SunPy to process maps of the Sun in Hα with the corresponding metadata, we flattened images
by subtracting their radial profiles to emphasize features near the limb and analyze spectral lines,
facilitating multi-instrument comparisons. This allowed us to examine correlations between
spectral-line-profile parameters and filtergram intensities. Using these findings, we will be able
to better understand the structure of the chromosphere, the conditions during the total eclipse,
and provide insight into the mechanisms behind coronal heating.

Comparison of Real-time WAM-IPE Neutral Wind with ICON/MIGHTI Satellite Observations

Colton Koenig1, Astrid Maute2, Tzu-Wei Fang2, Adam Kaubaryk2

1Colorado School of Mines, 2NOAA Space Weather Prediction Center

Poster

The NOAA Space Weather Prediction Center (SWPC) provides real-time monitoring and
forecasting of the Earth’s space environment. NOAA’s Whole Atmosphere Model – Ionosphere
Plasmasphere Electrodynamics (WAM-IPE) uses an extension of the NOAA Global Forecast
System model to include the upper atmosphere, up to ~600 km, coupled to a model of the plasma
environment. An important part of the model’s evaluation is their validation with real data. This
provides information about the accuracy and biases under various conditions, and can guide
future improvement. WAM simulates the neutral wind in the atmosphere. The neutral wind in the
upper mesosphere and thermosphere (above ~ 90 km) is important for determining the neutral
composition and neutral density as well as the plasma density distribution, for which the
ionospheric electrodynamics and direct wind impact has to be considered. These neutral winds
are a driving factor of the movement of plasma in the ionosphere.
In this project, neutral winds from WAM will be compared with the NASA Ionospheric
Connection Explorer (ICON) satellite mission, launched in 2019. We focus on the comparison of
the year 2020, which had low solar and geomagnetic forcing. WAM is driven by observed
3-hourly Kp and the solar radio flux F10.7. The ICON satellite can be flown through WAM for a
direct comparison with the model output by using simple linear interpolation methods in space
and time to infer the model at the observed location and time. We compare the WAM model in
the 110 km and 250 km regions with ICON observations and illustrate the captured seasonal and
solar local time variations in the zonal and meridional neutral wind. In addition, we evaluate the
height variation of the WAM neutral wind for specific months, for example in the 110km region,
upward propagating atmospheric tides (global scale waves) play a key role in the neutral wind
variation. We will analyze variation in solar local time and longitude of the neutral wind for
specific periods to extract information about dominant tides. We will conclude by discussing
follow up investigations.

Historical Simulations of Magnetic Flux Data

Phoebe Mahlin1, Lisa Upton, Ph.D.2, Bibhuti Jha, Ph.D.2

1University of Texas at Austin, 2Southwest Research Institute

Poster

The ability to detect magnetic fields on astronomical bodies has only been possible since
the 1950s with the discovery of the Zeeman effect. Therefore, we only have around 3 solar
cycles worth of magnetic data to compare with centuries of solar observations. The Kodaikanal
Solar Observatory (KoSO) has imaged the sun from 1904 to 2017 with a white-light telescope.
By performing a comparative analysis of magnetic data with the KoSO data using machine
learning techniques we can approximate the polarity of sunspots photographed in white light for
ten continuous cycles. There are two characteristics of these active regions (AR) that are
important to calculate for this project: the sunspot surface area and the tilt between two AR
clusters. The surface area of the ARs is directly proportional to the amount of magnetic flux
contained within them. Secondly, ARs are spots of magnetic flux with fields in opposing
directions. These spots typically align according to Hale’s law, with the leading/more westward
sunspot’s polarity matching the hemispheric polar field at the start of that solar cycle, and the
following sunspot having the opposite polarity. Since the leading spots tend to be more
equator-ward, each group has a characteristic tilt between the leading and following spots
described by Joy’s law. Using the K-means clustering algorithm, we identify sunspot groups and
then cluster them into two regions for which we will assign their magnetic polarity. The AR data
we will obtain (including the magnetic flux strength, location, and tilt) will then be input into the
Advective Flux Transport model as parameters for simulating surface flux transport. With this
model, we will visualize the magnetic flux evolution of ARs imaged in white light over the past
100 years. Finally, we will use our KoSO data and simulations to enhance our understanding of
magnetism on the Sun and refine our ability to predict upcoming solar cycles.

Daily, Seasonal, and Solar Activity Variations of the Equatorial Ionization Anomaly (EIA) at Different Longitudes Using NASA’s GOLD (Global-Scale Observations of the Limb and Disk) Data

Sophia Marrone1, Deepak Karan2, Saurav Aryal2, Richard Eastes2

1Gettysburg College, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

The maximum plasma density of Earth’s ionosphere is produced at its sub-solar point;
however, at the geomagnetic equator, the interactions between the ionospheric zonal electric field
and the encompassing magnetic field create two bands of enhanced plasma on either side. This
double-peaked structure of ionospheric plasma density appears in the form of crests at around
±15° magnetic latitude. This structure is called the Equatorial Ionization Anomaly (EIA), or the
Appleton Anomaly. Due to its important role in trans-ionospheric radio wave propagation, the
EIA has become a prominent topic for further study in space research. Especially in the wake of
its unexpected features that have recently been revealed by the NASA GOLD (Global-Scale
Observations of the Limb and Disk) ultraviolet spectrograph’s improved sensitivity and
observing capabilities. Since October 2018, GOLD has observed the post-sunset EIA daily at
~10° E to ~80° W geographic longitude, and the data’s consistent temporal-spatial coverage
makes it ideal for identifying variations in the EIA. We have analyzed this GOLD data and
obtained the EIA crests’ peak brightness and latitude as well as their day-to-day, seasonal
(equinoxes vs solstices), and solar activity variations at three different longitudes (from South
America to Africa). In this study, we compare the analysis from 2022 and 2023 to present these
new findings regarding the variabilities of the EIA.

Investigation of Magnetic Mapping between the High-latitude Ionosphere and Equatorial Magnetosphere Using Conjugate Spacecraft Observations

Wilson Moyer1, Samuel Califf1

1NOAA National Centers for Environmental Information

Poster

Magnetic field models are critical tools for studying the Earth’s magnetosphere – they provide global context for sparse spacecraft observations of various phenomena such as the ring current and radiation belts. However, due to the dynamic interactions between the Earth’s magnetosphere and the Interplanetary Magnetic Field (IMF), these models are approximations at best. This work assesses the validity of magnetic field models in the inner magnetosphere using observations of Subauroral Polarization Streams (SAPS), which are broad features characterized by strong radial electric fields in the equatorial inner magnetosphere and corresponding fast westward ion flows in the mid-latitude ionosphere. Equatorial electric field measurements from Van Allen Probes are compared to mid-latitude ion flow measurements from Defense Meteorological Satellite Program (DMSP) probes by tracing magnetic field lines using existing magnetic field models. We focus on the radial extent of the SAPS to evaluate the models, ultimately enabling recommendations for improved magnetic field models.

Understanding the Solar Corona Using Ground-Based Observations of the 2024 Total Solar Eclipse with Citizen CATE 2024

Ellianna Nestlerode1, Sarah Kovac2, Amir Caspi2

1University of Washington, 2Southwest Research Institute

Poster

The Citizen CATE 2024 Experiment deployed 35+ teams of community scientists along the 2024
total solar eclipse (TSE) path of totality from Texas to Maine to capture a 60-minute continuous
set of high-cadence observation of the solar corona in polarized light. Each team was extensively
trained on the equipment and procedures provided, including a telescope, camera, laptop, and
supporting observing equipment. This novel dataset allows for examination of the dynamics and
magnetic structure of the lower and middle corona. The middle corona is a region of transitions
between surface magnetic field structures and the outflowing solar wind, however, the connections between the inner and outer corona are not well understood.
CATE 2024 had 100% team participation on eclipse day, capturing over 2TB of data. One of the initial steps in the data analysis is to assess image quality by evaluating the focus, calculated
using image sharpness. Data that can be used to meet CATE 2024’s science goals are sharp and
free of major obstructions, like clouds. Here, we present the methodology for image evaluation,
which includes finding the gradient of a region of interest, such as a sunspot or, during partial
eclipse phases, the limb of the Moon. Once the gradient is calculated, we can categorize images
into sharp or blurred based on whether the gradient metrics are above or below a predicted
threshold.
Once all 2 TB of polarized light observations are properly categorized and calibrated, they will
be compiled into a 60-minute movie illustrating the evolution and dynamics of the solar corona
during the 2024 TSE. Using this movie, we will analyze the fine structures of the middle corona,
make measurements of the flow of nascent solar wind, and characterize magnetic reconnection in
the middle corona.

A Back-to-Back Validation of Spectropolarimetric Inversions for Solar Coronal Magnetic Fields using Global MHD Models

Emma Porter1, Alin Paraschiv2, Tom Schad2

1Brigham Young University, 2National Solar Observatory

Poster

The corona is the outermost layer of the solar atmosphere and is composed of plasma that
is still inexplicably hot, with a temperature greater than one million Kelvin. Remote sensing the
physical state of the hot solar corona is critical to addressing the source of its heat as well as the
energy that it expels towards Earth, which has many negative terrestrial impacts. Despite its high temperature, the corona is extremely dim, and therefore difficult to observe directly. In this work, we utilize state-of-the-art global coronal magnetohydrodynamic models provided by Predictive Sciences (PSImas) to study the emission from the corona and forward synthesize coronal observables applicable to the April 8th, 2024, total solar eclipse. Spectropolarimetry of forbidden coronal emission lines offers a wealth of information about solar density, temperature, and the coronal magnetic field, as compared to more routine intensity- only measurements.

Forward synthesis and inversion techniques applicable to coronal structures and magnetic
fields are still in their infancy. We present key findings from our analysis, as well as insight
gained while performing a back-to-back interpretation and validation of inversions using two
newly developed open-source python packages, PyCELP and CLEDB. These tools enable us to
forward synthesize and then invert the polarized radiation coming from the Sun’s corona when
considering the ground-truth input provided by the PSImas model. Our goal is to better establish
remote methods for extracting the state of the coronal plasma, and further constrain spectropolarimetric observations collected during and after the solar eclipse.

Comparison of the Sun in Hydrogen-α Versus Calcium-H Wavelengths

Finn Rogers1, Scott Sewell

1South Dakota School of Mines and Technology, 2NSF-NCAR High Altitude Observatory

Poster

Solar imaging is an essential study in astrophysics, providing data that helps predict solar flares. These flares, once severe enough, can disrupt aircraft communications and damage electrical systems. Predicting them accurately can save time, money, and prevent extensive damage. In this context, the High Altitude Observatory (HAO) is developing a tunable birefringent optical filter. This filter, designed to work with a camera and telescope, can select specific wavelengths of light, eliminating the need for multiple filters. The aim is to prove this setup’s feasibility for space missions, where there is no atmospheric interference and the imaging is clearer. In our project, we studied solar imaging from Earth using Hydrogen-α (656.26 nm) and Calcium-H (396.9 nm) filters with an 8-inch Schmidt-Cassegrain telescope. We sharpened images with the Lucy-Richardson deconvolution algorithm and aligned them to solar north for consistency, following practices of other research institutions. We compared H-α and Ca-H images to gain additional insights into chromospheric features such as sunspot depth and shape. This study is a first step towards future work on the tunable filter, paving the way for further advancements in solar imaging.

Numerical Simulations of the Interaction of Jupiter’s Magnetospheric Plasma with the Atmosphere of Europa

Emily Simpson1, Vincent Dols2, Fran Bagenal2, Rob Wilson2

1Florida Institute of Technology, 2Laboratory for Atmospheric and Space Physics (LASP)

Poster

Since the existence of Europa’s salty subsurface ocean was established by many Galileo
flybys in the late 1990s, Europa has been a prominent topic of interest in planetary science.
However, Galileo instruments did not provide any compelling plasma observations to constrain
Europa’s atmospheric composition and distribution, and thus its atmosphere is still poorly
known. Juno’s flyby of Europa in September 2022 with a closest approach altitude of 353 km
made the first close observations of Europa since then, as well as the first measurements with
instruments capable of detecting the plasma composition (electrons, H2+, H+, O2+, heavy ions).
Thus, despite only making one flyby, Juno data provides valuable context to guide future
missions to Europa like NASA’s Europa Clipper launching October 2024 and JUICE’s approach
in 2032.
For the first time based on Juno’s unique observations rather than Galileo’s, we study the
plasma composition at Europa with numerical simulations of the plasma-atmosphere interaction.
We apply a multi-species physical chemistry code that computes the electron-impact ionizations,
dissociations, charge exchanges, and recombinations taking place in the atmosphere of Europa
considering all ion species in the plasma sheet (sulfur and oxygen multi-charge ions) and a
prescribed atmosphere of O2 and H2. In the simulation, a plasma parcel upstream of Europa with
known composition and temperature is carried along flow lines (calculated analytically or with
an MHD code) into the moon’s atmosphere. The new plasma properties are then collected along
a spacecraft trajectory close to Europa and compared to Juno’s instrument observations. With
these simulations, we infer Europa’s neutral atmosphere distribution and composition.
Additionally, we compute the neutral loss that feeds the neutral clouds extending along Europa’s
orbit, suggested by Juno observations.

Glider-Driven Precision: Optimizing Atmospheric Instrument Deployment

Julia Zamora1, Sergio Vidal-Luengo, Ph.D.1, Lauren Blum, Ph.D.1

1Laboratory for Atmosphere and Space Physics (LASP)

Poster

Balloon probe launches are a highly economical approach for gathering data from Earth’s
upper atmosphere using deployed instrumentation. Yet, a lack of control due to unpredictable
weather patterns often complicates successful payload recovery. GPS tracking alone does not
prevent payloads from frequently landing in remote or inaccessible locations such as forests
rivers, or lakes. Consequently, scientists who are faced with the risk of losing the payload may
resort to using inexpensive, low-quality instrumentation which may affect the quality of their
overall results. This project seeks to tackle this challenge through the development of an
unmanned aerial vehicle (UAV) glider designed to autonomously return to a predetermined
location for safe retrieval and enabling researchers to deploy higher-quality instruments. We
utilized Aircraft Intuitive Design (AID) in MATLAB to define flight parameters and model the
glider. We estimated the functionality and assessed the glider performance under standard
atmospheric conditions. Our objective is to deliver a prototype and fine tune necessary flight and
landing systems to enhance control and reliability in payload recovery. Furthermore, we aim to
deliver navigation, flight control, and recovery systems for the glider, providing an open source
and adjustable platform that will allow scientists and students to deploy instrumentation of their
own for lower and upper atmospheric observations without the need to fully develop a glider
platform. Additionally, an online platform will be created to facilitate the exchange of UAV
designs customized to meet specific mission requirements in atmospheric studies (e.g.,
chemistry, weather, aerosols) and magnetospheric physics (e.g., high-energy particle
precipitation).

Partners Across the Sky

Characterizing the Plasma Environment Around Callisto and Ganymede Using JADE-I Data from Juno

Reign Pagaran1,2, Fran Bagenal1,2, Jian-Zhao Wang1,2

1Laboratory for Atmospheric and Space Physics (LASP), 2University of Colorado, Boulder

Changes in Density on Opposite Sides of the Plasmasphere

R.A. Iker1,2, Tyler Bishop2,3, Lauren Blum2,3

1Fort Lewis College, 2University of Colorado Boulder, 3LASP

Examining Plasma Waves Through Spectrograms and Audio Using Parker Solar Probe Data

Degen McCabe1, Peter Tatum1,2, David Malaspina1,2

1Laboratory for Atmospheric and Space Physics, 2University of Colorado at Boulder

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