Summer 2023

Student name in BOLD

Using Flare Ribbons to Understand Magnetic Reconnection in Solar Flares

Rose Sosa1, Ryan French2, Marcel Corchado2,3, Cole Tamburri2,3

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

Poster

Magnetic reconnection is a fundamental process within solar flares, resulting in a change
in local magnetic topography. Magnetic reconnection involves the release of magnetic free
energy as particle acceleration, light, and plasma heating. Although magnetic reconnection is a
crucial process in solar flare dynamics, it is not yet fully understood. During a solar flare, flare
ribbons mark the intersection between the chromosphere and flaring corona. Due to their
magnetic connectivity to the reconnection site, flare ribbons must be imprinted with information
of the flare reconnection dynamic. This study utilized this connectivity to investigate the process
of magnetic reconnection by analyzing flare ribbon behavior of multiple solar flares. We used
image and time series analysis of data from NASA’s Interface Region Imaging Spectrograph
(IRIS) Slit-Jaw Imager (SJI) data to study oscillations in flare ribbon position, intensity,
separation velocity, and physical width. Finally, we compared our results with expectations from
different models of magnetic reconnection in solar flares, in particular the tearing-mode
instability.

Space Weather Datasets for NOAA’s Science on a Sphere

Ethan Balderrama1, Mark Miesch2, Rodney Viereck2

1Pennsylvania State University, 2CIRES/Univ. Colorado, NOAA Space Weather Prediction Center

 

NOAA’s Science on a Sphere (SOS) is a room-sized, spherical projection system that
allows for the visualization of planetary data in an exciting and interactive way. Sitting at
over six feet in diameter, this powerful tool uses computers and video projectors to create
various eye-catching animations. The SOS is a powerful outreach tool that we at NOAA’s
Space Weather Prediction Center use to display awe-inspiring and pertinent space weather
datasets. This space weather includes aurora and solar images, providing useful
information and an educational experience to the viewer. The OVATION Prime model uses
solar wind to forecast the aurora with a 20–50-minute lead time and is used to create aurora
loops from the past, as well as nowcast and forecasts. Extreme Ultraviolet (EUV) images
from the Solar Ultraviolet Imager (SUVI) on NOAA’s GOES satellite are used to produce
solar images and loops on the SOS. As we develop more advanced technology and rely on
it more continually, the impacts of space weather continue to grow, making the
understanding of this data more important. SOS is an ideal vessel for allowing experience
via visualization, with minimal distortion of data, as its spherical nature aligns with the true
shape of the Earth and Sun. Future exploits include getting real-time data and forecasts
onto the SOS, giving viewers even more resources to learn about space weather.

Preparing for the 2024 Citizen Continental-America Telescopic Eclipse (CATE) project

Amelia Bettati1, Amir Caspi2, Dan Seaton2

1Elon University, 2Southwest Research Institute

Poster

The CATE 2024 project will produce next-generation polarized observations of the solar
corona during the April 8th, 2024, total solar eclipse (TSE) that will cross the continental U.S.
These observations will be made by 35 teams of citizen scientists along the path who will gather
continuous images of the lower and middle solar corona. The recruited teams will consist of
students and amateurs whose collective observations will be combined into a 1-hour-long movie
of the solar corona. The polarization data collected will answer questions such as determining
connectivity in the solar corona, measuring the nascent solar wind flow, and identifying and
characterizing reconnection in the middle corona. During the summer of 2023, we mapped out potential rural, urban, and tribal communities surrounding target CATE 2024, observing sites as possible citizen scientists for our project. We focused on underrepresented communities. We also tested and characterized observing setups, specifically cameras that will be distributed to the teams along the path of the TSE, as well as telescope equipment and software. During analysis, we characterized each of the cameras’ four polarization channels to analyze their performance and suitability for the high dynamic range imaging required for the CATE 2024 project. Based on the individual performance of different camera models, one will be chosen to be distributed in bulk across the teams. We found that the camera and telescope equipment meet all requirements, approving them for the 2024 TSE. Currently, we are preparing to begin recruitment for the community teams and are creating teaching materials that will be used as a universal training curriculum for our volunteer observers. We will present the results of our outreach planning and recruiting plans and expand on the characterization process of our equipment and plans for the CATE 2024 project.

Validating Solar atmosphere models using high spectral resolution, center-to-limb
observations of solar Balmer lines

Tyler Case1, Serena Criscuoli2, Odele Coddington3

1Lycoming College, 2National Solar Observatory, 3Laboratory for Atmospheric and Space Physics

Poster

The variations in solar irradiance have an effect on the Earth’s atmosphere and climate.
Irradiance variations occur at different temporal scales (second to millennia), and their
amplitude largely depend on the spectral region. This variability is driven by magnetic activity
on the solar surface such as sunspots, facula, etc. Continuous monitoring of solar irradiance
only started in the late 1970s (other indicators of solar activity were monitored prior to this
date), therefore, in order to estimate irradiance variability over long temporal scales (decades to
millennia), we resort to using synthetic models of the solar spectrum. These synthetic spectra
may also be used to model stellar atmospheres that could help characterize exoplanets’
atmospheres and their habitability, as well as help validate assumptions about magnetic
features on the solar surface. We are validating several quiet Sun synthetic spectra obtained with atmosphere models that are commonly used to describe properties of the Sun and sun-like stars. This is done by comparing them to recent spatially resolved, high spectral resolution, center-to-limb observations from the Institut für Astrophysik (IAG), Germany, and the FTS quiet Sun reference spectrum. We focus on the alpha, beta, and gamma Hydrogen Balmer lines, which sample different depths of the solar atmosphere.

Spatio-temporal Variability in Acoustic Mode Parameters of Solar Oscillations

Nicholas Cebula1, Sushanta Tripathy2, Kiran Jain2

1Macalester College, 2National Solar Observatory

 

Helioseismology measures acoustic oscillating waves that are observed on the surface
of the Sun to learn about the interior dynamics. In this investigation we use a local
helioseismic technique of ring diagrams to study the power, energy and damping rates
of local high degree solar acoustic modes. Our data is derived from the Global
Oscillations Network Group (GONG) and covers the period 2001-2022 i.e. starting from
the maximum phase of solar cycle 23 to the ascending phase of cycle 25. The goal is
to examine the variations in the mode parameters, e.g., mode amplitude, line width,
with solar activity as well as the differences and similarities between different cycles
since each solar cycle behaves differently. For this, we use different proxies of solar
activity. In particular, we use 10.7 radio flux measurements and a local measure of
magnetic flux known as magnetic activity index calculated from magnetograms.
The current results of this project have so far confirmed the correlation between
intensity of magnetic flux and mode width which is proportional to the damping rate.
Thus we find that the modes are damped during the period of maximum solar activity.
with periods of high magnetic flux leading to higher values of mode width. We further
confirm that the mode amplitude is in anti-phase with magnetic flux, where amplitude
values are found to be decreasing during periods of high magnetic flux. This relation
has held true for the majority of the years analyzed here. However there are a few
anomalous periods of time where the amplitude values appear to be in phase with
magnetic flux. While the exact reason for this has not been found yet, we do not rule out
an instrumental origin. We will explore the reasons for this anomaly. We will further investigate variations in the northern and southern hemispheres to characterize the progress of the solar cycle and to highlight the differences between the two hemispheres.

Exploring the Effect of a Faint Young Sun on Venus’ Cloud Structure

Grace Fassio1, Dr. Kevin McGouldrick2, Dr. Erika Barth3

1Whitman College, 2Laboratory for Atmospheric and Space Physics, 3Southwest Research Institute

Poster

Sulfuric acid clouds entirely cover Venus today. The production of this sulfuric acid is
caused by a photochemical reaction that consumes sulfur dioxide, water vapor, and
sunlight. Venus has been exposed to varying amounts of solar intensity throughout its
history due to a fainter young Sun. During the Archean eon (3.8 to 2.5 billion years ago),
it is believed that the Sun was 20-25% less luminous. We explored the effects of this
“Faint Young Sun” on Venus’ cloud structure by using a microphysics model.
PlanetCARMA is a model for atmospheres that simulates physical processes, including
nucleation, condensation, and evaporation. We mimicked the effects of the Faint Young
Sun by varying the photochemical production and loss rates. Our expectation was that the
reduced insolation would result in lower sulfuric acid production hence fewer clouds; in this presentation we report on the findings of our simulations.

Evaluation of the Dynamics of Ion Populations Upstream of Quasi-Perpendicular Shocks Using Spacecraft Measurements

Julia Hand1,2, Hadi Madanian2, Li-Jen Chun3

1Grand Canyon University, 2Laboratory for Atmospheric and Space Physics, 3Goddard Space Flight Center, National Aeronautics and Space Administration

Poster

Earth’s bow shock lies against the continuous flow of supersonic, magnetized solar wind.
Understanding the particle activity around shock crossings drives a broader understanding of the
physical processes of the bow shock. This project assesses ion populations upstream of Earth’s
bow shock with a quasi-perpendicular geometry using satellite data from NASA’s
Magnetospheric Multiscale (MMS) mission. Spacecraft measurements taken in regions of
supercritical crossings are used to analyze upstream activity, which comprise magnetic field
amplification and ion energy scattering. To better understand the fate and trajectories of assorted
ion populations, multipoint 3-D ion distributions are analyzed by projecting the measurements on
2-D planes parallel and perpendicular to the shock surface. From these planes can various
distributions of ions be defined, aiding to establish the dynamics of interaction with magnetic
enhancement. The investigation of these ion populations allows a broader understanding of the microphysics occurring at quasi-perpendicular shocks.

GPS Satellite Observations of a Radiation Belt Dropout Event in the Post-RBSP Era

Alexis Hensley1, Harriet George2, David Malaspina2, Milla Kalliokoski3

1Berea College, 2Laboratory for Atmospheric and Space Physics, 3Japan Aerospace Exploration Agency

Poster

The Earth’s radiation belts present a space weather hazard to satellites and astronauts in orbit. The gold-standard radiation belt observations were provided by the Van Allen probes (RBSP) from 2012 to 2018. We demonstrated the use of the Global Position System (GPS) satellite data to investigate a radiation belt dropout event, thus examining the feasibility of using GPS satellites to continue to monitor the radiation belts in a post-RBSP era. A dropout of relativistic electrons from Earth’s outer radiation belt occurred on 14 May 2019 and was analyzed using the GPS constellation.Most GPS satellites carry a Combined X-Ray Dosimeter (CXD) instrument that provides electron count data. These count data have been cross-calibrated with RBSP electron flux observations to calculate electron fluxes from the GPS observations. We analyzed this dropout event using electron flux data provided by 19 different GPS satellites to investigate the driving mechanism and timescales of the losses. Electron flux losses of an order of magnitude were observed at all evaluated L-shell in the 4 MeV population. These flux losses were rapid and closely corresponded with a strong compression of the magnetopause. The magnetopause was abruptly compressed from its nominal location by ∼ 2RE, with the inward
incursion starting at approximately 4 AM. Analysis of the phase space density (PSD) calculated from GPS fluxes showed a total loss of the 3433 MeV /G and
0.11 G1/2RE population at L∗ > 4.5 was observed between the inward pass of ns65 satellite at 3:20 AM and its outbound at 4:50 AM. Further examination of the PSD revealed that radial diffusion transported particles across the mag-
netopause after the initial compression, moreover contributing to the dropout event. This analysis demonstrates the feasibility of using GPS data to evaluate
rapid changes in the radiation belts, especially in the post-RBSP era.

Variation of Solar Flare Properties During Solar Cycles 24 and 25

Maheen Khan1,3, Dr. Larisza Krista2,3

1Pikes Peak State College, 2Cooperative Institute for Research in Environmental Sciences (CIRES), 3National Oceanic and Atmospheric Administration (NOAA)

Poster

Solar flares are phenomena that can occur any time during the solar cycle. Flares can interfere with
modern life by affecting power grids, telecommunication and GPS navigation. Our goal is to better
understand the evolution of solar flare properties in the ascending phase of the current solar cycle 25.
Using the HEK flare catalog (an online server providing solar flare data from GOES and SDO), we
study the duration, magnitude, and heliographic latitude of solar flares between 2017 and 2023. We find
that the duration of solar flares is typically in the range of 14 to 16 minutes, and is independent from the
X-ray magnitude. Our results also indicate that larger flares (specifically X class flares) coincide with
increased solar activity associated with the ascending phase of the solar cycle. Further research will
involve analyzing the latitudinal location of flares, and how they correlate with the ascending phase of
solar cycle 25.

The Characteristics of Active Regions and its Relevance to Space Weather Forecast
Research Focus: Space Weather, Active Regions, and Space Exploration

Ysabella Marie Lopez1, Andres Munoz2

1Spelman College, 2Southwest Research Institute(SWRI)

 

Active Regions occur throughout areas on the Sun’s surface where there is an abundance of magnetism.
Extensive understanding and research on the properties of active regions is imperative to the future of
space exploration and aerospace machine innovation. In this research journey, we extracted the data from files that recorded the activity of active regions over the span of about 40 years. The extracted data was converted from IDL files to Python to modernize it and make it accessible to a new generation of
scientists. With this data, we used the contents to create a set of data features/high-level quantities to
enable space weather forecast. These features were then input into a logistic regression to output
predictions of solar flares.

Building an AI-Ready Calibrated and Denoised Dataset of Magnetic Anomalies using Citizen Science Contributed CrowdMag Measurements

Emma Opper1, Manoj C. Nair2, Rob Redmon3,4

1University of California, Santa Barbara, 2Cooperative Institute for Research in Environmental Sciences (CIRES), 3NOAA National Centers for Environmental Information (NCEI), 4NOAA Center for AI

Poster

Deviations in local magnetic field strengths from what is expected are known as magnetic
anomalies, whose proper detection can reveal various geophysical features and help understand
geological history. NOAA’s current magnetic anomaly map is known as EMAG2_v3, which is a
compilation of data from airborne, shipborne, and satellite measurements. However, the
resolution of this map is limited by the spacing between these measurements. To improve its
magnetic reference models and maps, NOAA introduced CrowdMag, a citizen science project
that harnesses data contributed by the public through a mobile app that utilizes the
magnetometers embedded in modern smartphones. But because the magnetometers in
smartphones are lower quality and therefore influenced by surrounding magnetic interference,
the collected data is extremely noisy. To overcome this challenge, a type of deep neural network
known as an autoencoder (AE) is employed to denoise the data. An AE learns to reconstruct its
input data by effectively compressing the information into a lower-dimensional representation
and then reconstructing it to remove noise. This artificial intelligence (AI) technique is trained
using intentionally noised and masked EMAG2_v3 data (Figure 1b) and its hyperparameters
optimally tuned before being applied to the noisy CrowdMag data. This tuning includes but is
not limited to, altering input size, epoch size, loss function, masking and randomization level,
and compression ratio. Once the optimal parameters are established, an AI-ready calibrated and
denoised dataset of magnetic anomalies is produced. To the best of our knowledge, this is the
first time autoencoders have been applied to this sector of geoscience. The outcomes of this
project can be extended to other fields of science where noisy datasets are prevalent.
Additionally, this initiative promotes the utilization of citizen science-collected measurements,
fostering greater public involvement in scientific research.

An Investigation of the Vertical Properties of Thermospheric Gravity Waves Using FUV
Stellar Occultation SORCE Data

Pepper Rivera1, Josh Elliott2, Ed Thiemann2

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

Poster

Atmospheric gravity waves play an important role in the dynamics of the Earth’s
atmosphere, facilitating the transfer of energy and momentum throughout all atmospheric layers.
Observing gravity waves in the thermosphere, the layer of Earth’s atmosphere above 90 km, is
especially challenging. The horizontal component of these waves has been studied using
primarily satellite accelerometer data at altitudes above 200 km but their vertical properties are
poorly understood. The region in Earth’s atmosphere from 100 km to 200 km is called the
‘thermospheric gap’ because of the lack of study of waves in this region. This presentation
outlines the process of attempting to find thermospheric gravity waves within this gap region
from 120 km to 200 km. This was done using stellar occultation data collected from the Solar
Stellar Irradiance Comparison Experiment (SOLSTICE) aboard the Solar Radiation and Climate
Experiment (SORCE) spacecraft. In particular, the vertical properties of these waves were
considered. As far ultraviolet (FUV) stellar light passes through the atmosphere, a percentage of the light is absorbed by O2 in the atmosphere creating the occultation profiles used in the study. Stellar irradiance measurements from the instrument were then used to calculate the density of the thermosphere at various altitudes, at which point efforts were made to find statistically significant vertical oscillations which indicate the presence of thermospheric gravity waves. This stellar occultation approach has been recently used with great success by the Mars Atmosphere and Volatile Evolution mission (MAVEN) to study atmospheric waves in Mars’ atmosphere. Finally, we performed comparison tests between the data observed and theoretical models for gravity waves in this region of the Earth’s atmosphere.

Minor Pick-up Ions from the Martian Corona

Martina Salichs1,2, Robin Ramstad1, Yaxue Dong1, Shannon Curry1,3

1Laboratory for Atmospheric and Space Physics, 2University of Puerto Rico at Mayagüez, 3University of California Berkeley

Poster

 

The SupraThermal and Thermal Ion Composition (STATIC) instrument onboard the Mars
Atmosphere and Volatile EvolutioN (MAVEN) spacecraft measures angular, energy, and mass
distributions of suprathermal ions over a range of altitudes near Mars. We studied pick-up ions that
are created and escape when neutrals in Mars’ exosphere get ionized and accelerated by the solar wind’s motional electric field. We analyzed mass-energy spectra to identify minor species of pick-up ions, i.e. ions other than O+ or H+. For this project, we analyzed time intervals when the spacecraft was in the solar wind and excluded ions that were co-moving with the solar wind. We successfully detected minor pick-up ion species by statistical analysis to determine signal significance. We report the confirmed minor ion species, their spatial distributions, and abundances. The prevalence of these minor pick-up ions constrains the ongoing escape of Mars’ upper atmosphere and its evolution over time.

The Lost Art of Harnessing: Designing for Optimization

Jordan Richardson1, Dr. Amie Merkel1

1Laboratory for Atmospheric and Space Physics (LASP)

Poster

The purpose of this study is to research the next genera>on of harnessing
techniques and configura>ons to op>mize overall system performance poten>ally extending the
opera>onal mission life of CubeSats and create a no>onal design for the DYNAGLO CubeSat
harnessing system. Harnessing is an oQen-overlooked subject in the world of engineering. Much of this aspect of engineering is oQen reduced to a second thought, when it should be a key design performance
parameter. Due to this priori>za>on, wiring complica>ons may occur causing more problems later in the system lifecycle. This is not the case for DYNAGLO, DYNamics Atmosphere GLObal-Connec>on (DYNAGLO). It is the first-of-its-kind two 6U CubeSat that provides global thermosphere gravity waves (GW) measurements along with characteris>cs for correla>on with known GW sources both terrestrial and geomagne>c to the science community. Funded by NASA’s Heliophysics Division, DYNAGLO aims to achieve NASA’s mission goal to contribute to the fundamental understanding of how ver>cal coupling by atmospheric waves relate to the energy and momentum balance in the thermosphere. Using Draw.io and SolidWorks CAD designs, the research study will show modest low-cost modifica>ons to a satellite’s harness and wiring design can not only increase power output but poten>ally extend the mission lifespan of a satellite. Concluding results and expected outcomes include baseline of current CubeSat design configura>ons and the poten>al areas of focus for future next-gen harness and wiring designs. The new CAD model no>onal design created shows a new low-cost approach and the poten>al to increase power and extend satellite mission lifespan on orbit.

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