Summer 2020

Student Name in BOLD

*Not all students made a poster

*Not all students submitted an abstract, but made a poster

Plasmaspheric dynamics studied using a three-dimensional machine learning based plasma density model in the inner magnetosphere

Hannah Ace1, Xiangning Chu1, Jacob Bortnik2, Richard Denton3

1Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, 2Department of Atmospheric and Oceanic Sciences, University of California, 3Department of Physics and Astronomy, Dartmouth College

Poster

Plasmaspheric density and composition strongly influence wave growth and propagation, as well as energetic particle scattering. Previous statistical, empirical plasma density models of the inner magnetosphere have limited capability to make accurate predictions. Consequently, these models cannot be used to adequately quantify complex global processes and nonlinear responses to driving conditions, factors of critical importance during storms. Recent advancements in machine learning techniques have enabled a more dynamic study of the space environment. Here we present a three-dimensional dynamic electron density model based on an artificial neural network. This model uses a feedforward neural network which was generated using electron densities from satellite missions of CRRES, ISEE, IMAGE, POLAR, and Van Allen Probe. The three-dimensional electron density model takes spacecraft location and time series of solar wind and geomagnetic indices (flow speed, SYM-H, AL, and AE) obtained from NASA’s OMNI database as inputs. When compared with the out-of-sample data, the three-dimensional model predicts equatorial and field-aligned density profiles from satellite measurements with an error of less than 0.16. When the three-dimensional model is applied to a number of magnetic storms, successful reconstruction of the expected plasmaspheric dynamics, such as the plasmaspheric erosion, plume formation in three dimensions was achieved.

Spectroscopic Inversions & Calibrations for DKIST Coronal Observations

Aatiya Ali1,2, Alin Paraschiv2, Philip Judge2, Kevin Reardon3

1University of Florida, 2National Solar Observatory, 3National Center for Atmospheric Research, High Altitude Observatory (HAO)

Poster

The Cryo-NIRSP’s (Cryogenic Near-IR Spectro-Polarimeter) is one of the DKIST instruments capable of sensitive imaging of faint infrared coronal solar spectra, and its primary goal is to measure the full polarization state (Stokes I, Q, U and V) of spectral lines originating on the Sun at different wavelengths. Producing data products from off-limb solar coronal observations from the DKIST telescope is essential when trying to study its future observations. Quantifying the accuracy of spectral inversion procedures based on its spectral comparisons to absorption and telluric calibrated spectra will give insight to interpreting valid DKIST observations and its ultimate findings. Using simulated contaminated data of both pure and noisy data sets has allowed us to compare the wavelength shifts and broadening properties to help pinpoint where contamination would affect the data set as a whole, and by how much. In doing so, we developed code that will eventually be integrated in the DKIST Level-2 pipeline. Working to compare these findings to absorption and telluric readings will further help minimize the uncertainties read in through observations, and give direction on how to reduce the original coronal data in hopes to refine it. Understanding the origins and magnitude of the contamination would therefore help refine the original coronal data and make it compatible for data processing, and would assist the automation of processing the data observed by the DKIST telescope.

The effect of solar observables on magnetic reconnection activity in the solar wind.

Bjorn Larsen1,2, Stefan Eriksson1

1Laboratory for Atmospheric and Space Physics, University of Colorado, 2California State University

Poster

It is well-known that current sheets within the turbulent structure of the solar wind can support the creation of plasma jets by magnetic reconnection. These reconnection jets have been measured in various sizes from just a few to over 106 kilometers and play a large role in determining the solar wind structure, energy distribution, and resulting temperature. We are currently using a large sample of reconnection jets found using data from the Wind spacecraft to empirically investigate how their commonality may be affected by behaviors present and observable on the Sun. A simple estimation we employ also confirms that these jets detected at 1 AU originate from locations in the solar wind nowhere near the Sun. This also means that the reconnection activity of the solar wind can provide a direct link towards better understanding the underlying solar wind structure and how its dynamics are driven. We use Wind plasma and magnetic field data to identify the cross-sectional signatures of these jets, consisting of a rotation of the in-plane magnetic field coupled with a velocity spike at the local Alfvén speed. In our correlation analysis we distinguish and categorize these jets by factors such as their current sheet normal widths and solar wind conditions when the jet was formed. Then, we use correlation analysis to look for relationships between the various jet distributions and the solar sunspot number, GOES X-ray flux data, and solar wind speed. Initial results show there is no correlation between reconnection activity and sunspot number or X-ray flux, but a weak inverse relation between jets generated outside of ICMEs and local solar wind speed

Seasonality in CO2 gas jet eruptions on Mars

Chelsey Drake1, K.-M. Aye2, and G. Portyankina2

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

Poster

Every winter, a layer of CO2 ice forms at the poles of Mars. When spring comes, solar energy penetrates this layer and sublimes CO2 from underneath. This gas is under high pressure and is looking for ways to escape the CO2 ice layer, and eventually breaks the ice at the weakest point in the area, erupting into a CO2 gas jet. While moving below the ice towards the vent, CO2 gas erodes substrate and picks up loose regolith particles. It brings this material out to the atmosphere and deposits it on top of the ice layer forming dark blotches and fan-shaped deposits. Repeated eruptions erode the underlying substrate, producing the so called araneiform terrain (colloquially called martian “spiders”). These processes are not found on Earth. The High Resolution Imaging Science Experiment (HiRISE) camera of the Mars Reconnaissance Orbiter mission is monitoring araneiforms and yearly seasonal re-appearance of related fans and blotches. The data from this mission is providing information on spatial and temporal distribution of eruptions, and on the activity levels in different regions of interest around the martian south pole.
Using data from HiRISE, we are investigating how topography, solar energy input, and time-dependent shadowing influence the distribution of the activity that leads to araneiform formation. According to the currently accepted models, CO2 jet activity and subsequent araneiform formation is driven mainly by the solar energy. We use high-resolution digital terrains models (DTMs) produced from HiRISE stereo images together with precise SPICE calculations of the Sun position in the local sky to create insolation maps at regions of interest around the martian south pole. These insolation maps account for local surface angles (tilt and aspect) as well as time-dependent shadowing due to topographical features. Spatial scale of insolation maps is equal to the one of the used DTM, i.e. up to 1m/pixel. This high resolution allows us to investigate energy distribution resolving smallest topographical features, for example, araneiform troughs and isolated boulders. We are able to correlate amount of energy that a feature receives over martian hours, days, or a complete season to the CO2 jet activity nearby. Thus, we determine why some areas are more active/have higher density of araneiforms than the others.
We will discuss the computational pipeline for production of insolation maps. We will show insolation maps calculated for several HiRISE monitored regions of interest (ROIs) and compare them with the spatial distribution of araneiforms. Doing so we aim to determine if the current insolation is correlated with density of araneiform terrains in different ROIs. This project improves our understanding of CO2-related seasonal processes unknown to Earth, and how they currently modify martian surfaces, and thus how the geological record is preserved in the top surface of the polar areas of Mars.

Understanding the Connection Between Dimmings and CMEs through Quadrature Observations

Drew Manning1, Larisza D. Krista2

1Colorado College, 2University of Colorado/CIRES, NOAA/NCEI

Poster

The goal of our project is to investigate the relationship between two solar phenomena: coronal dimmings and the associated coronal mass ejections (CMEs). Solar eruptions often lead to mass evacuation visible in EUV images (i.e. dimmings) as well as CMEs in off-disk images. Using images from the STEREO and SOHO satellites during their quadrature period in 2010, we achieved optimal observation of both phenomena, allowing for a more accurate computation of their properties. The SECCHI/EUVI instruments aboard STEREO A and B were used to observe dimmings in the 195 Angstrom wavelength, while the SOHO/LASCO instrument was used to create base-difference images to observe CMEs. Dimmings were processed using the Coronal Dimming Tracker (CoDiT, Krista 2017). This semi-automated tool tracks dimmings through their lifetime, allowing us to observe dimming evolution from its beginning to its end. The dimming observations were paired with the associated CME to identify a correlation between their observed properties and hence, better understand their relationship. In a study of Krista and Reinard (2017), poor correlation was found between dimming and CME properties. We hypothesize that the lack of correlation could have been due to errors in CME mass measurements. For this reason, we studied the above mentioned quadrature period where CMEs and dimmings were observed at right angles. Our study in this period allowed for a more accurate measurement of the CME masses, and as a result, we found significant correlation between CME masses and certain dimming properties: dimming area (Pearson correlation = 0.677), mean EUV intensity (-0.718), and dimming lifetime (0.529).

 

Polarization Of Astronomical Objects

Eden Ashebo1, Dmitry Vorobiev2

1Metropolitan State University of Denver, 2Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder

Poster

The overall scientific goal of the study is to identify post-AGB (asymptotic giant branch
star phase) by using RIT Polarization Imaging Camera (telescope). Particularly, the transition
phase from red giant to planetary nebula in the life cycle of low mass stars. From the observed
12 stars we analyzed data of 5 stars so far. We analyzed the polarization state of the 5 stars that
were observed in different filters, in Blue, Red, and green. It was enabled by MATLAB image
processing technique and calculating error propagation of the measurement. Based on the
information that we gathered from analyzed stars, we found high polarization for some of the
stars. This polarization state would let us study the physical properties of the stars and as well as
to identify their phase. Stars that have strong polarization in our sample are good candidates for
further observation.

A statistical study on the ULF wave-driven ultrarelativistic electron flux oscillations in the
outer radiation belt

Isabela Huckabee1, Hong Zhao2

1Arizona State University, 2LASP, University of Colorado at Boulder

Poster

The objective of this study is to assess the relation between ultrarelativistic electron flux
oscillation events in the outer radiation belt and the solar wind/geomagnetic conditions
that underlie these events. Ultimately, this will aid in revealing the role of radial diffusion
by ultralow frequency (ULF) waves on the ultrarelativistic electrons in the outer radiation
belt by using their flux oscillations as observed by the Relativistic Electron Proton
Telescope on NASA’s Van Allen Probes. Previous research has shown that radial
diffusion is the result of magnetic and electric field fluctuations and can be characterized
in this way (Schulz and Lanzerotti, 1974), and more recently Sarris et al., 2017 has
shown that using Van Allen Probe measurements, oscillation in flux amplitude on
energetic particles’ drift period can also act as an indicator for radial diffusion. This
investigation utilizes Fast Fourier Transform (FFT) analyses on electron fluxes to
automatically identify the flux oscillation events for ultrarelativistic electrons. We identify
272 events of 3.4 MeV electrons throughout the year of 2017. We then take this
collection of events and conduct a statistical analysis to observe the relationship
between electron flux oscillation events and parameters such as solar wind and
geomagnetic activity. The results help gain a more in-depth understanding of the
relation between electron flux oscillations and radial diffusion for ultrarelativistic
electrons in the radiation belts and shed light on the role of radial diffusion on the
ultrarelativistic electron dynamics.

Analysis of DKIST Adaptive Optics Jitter Control

Iris Wang1, Luke Johnson2, Andy Ferayorni2

 

1Swarthmore College, 2National Solar Observatory

The Daniel K. Inouye Solar Telescope (DKIST) is a 4-meter solar telescope currently under construction at Haleakala, Hawaii. Its science objectives include studying the dynamics of the outer solar atmosphere and magnetic structures of the Sun. In order to obtain high resolution images for scientific study, DKIST requires an accurate adaptive optics (AO) system that will correct atmospheric distortion of incoming wavefronts. By analyzing the jitter control system, which corrects image shift, we can identify and eventually eliminate sources of non-atmospheric vibration that cause jitter and reduce image resolution. In the present work, we constructed movies and used image cross-correlation techniques to corroborate jitter seen in images with jitter calculated using Python code. After quantifying the magnitude of jitter in images, we used power spectra of AO mirror command telemetry data to determine the strength of jitter vibrations at different frequencies. We also compared the response of the actual jitter control system to the response of a Matlab model of the system. Analysis indicates that the system correction is matched by the model in the 5 Hz to 100 Hz range, suggesting that the atmospheric simulation matches atmospheric data at lower frequencies. But we also observe continuum mid-frequency (40 – 150 Hz) jitter unexplained by atmospheric or telescope wind-shake modeling. By fitting the modelled system correction to the actual system response, we can identify input parameters, such as integral and proportional gain, that need to be adjusted to obtain a better correction. We present methods used to quantify the AO jitter performance and discuss ways to further mitigate jitter through mechanical damping or more advanced control algorithms.

Characterizing Solar Wind Dynamics in Coronagraph Data

Jake Wilson1, Barbara Thompson2, Craig DeForest3

1University of Maryland College Park, 2NASA Goddard, 3SwRI

The solar corona is the source of the solar wind that fills our solar system. The flow of the solar wind is far from steady, and noise-reduced coronagraph images from NASA’s STEREO mission show that the outer corona is a riotous torrent of visible features rather than a smooth flow. NASA’s upcoming mission PUNCH (Polarimeter to UNify the Corona and Heliosphere) will examine the young solar wind, which is the region from the middle of the solar corona to 1AU. PUNCH will be able to study how the solar wind evolves, allowing an unification of the Corona and Heliosphere.

This project focused on creating a Python data pipeline that will process the data coming out of PUNCH. The prototype data pipeline already exists in Perl Data Language (PDL). However, PDL lacks support from the broader data science and heliophysics fields, leading it to be ported into the more mainstream language of Python 3. In order to port the data pipeline into Python, PDL Transform also had to be ported into Python 3. PDL Transform is a library in PDL that takes in images or data and applies linear, and non-linear transforms to them. Unlike methods that already exist in Python, this allows for more freedom in what kind of transform you want to apply to your data.

In the end, this project successfully ported over PDL Transform and laid the groundwork for finishing the Python data pipeline.

Variation of Small-Scale Solar Magnetic Fields with Hinode

Jonathan Roberts1, Dr. Ricky Egeland2, Dr. Rebecca Centeno2

1University of Florida, 2HAO 

Poster

Since 2008 the Hinode spacecraft has been taking monthly synoptic high-resolution spectropolarimetric observations of the central meridian of the Sun. This data provides routine observations of small-scale magnetism from pole to pole. In this project we search this unique dataset for variation of the small-scale magnetic field from one solar minimum to the next. By doing so, we investigate whether the small-scale magnetism varies on the same time scales as the large-scale magnetic field, which is still an unanswered question. If detected, this could be evidence of a connection between the large-scale solar dynamo on local dynamo action, which is found in simulations. The multi-scale connection could have consequences for the overall magnetic behavior of the Sun during periods of extended low activity such as the Maunder Minimum of 1645–1715, and on the solar irradiance and Earth climate during these periods.

Deep Space Radiation Genomics: Magnetotail and Bow shock Affect

Kaiya Wahl1, Valerie Bernstein1, Delores Knipp1

1University of Colorado at Boulder

Poster

A Deep Space Radiation Genomics (DSRG) Yeast Experiment will be launching on Artemis 1 that will orbit the moon as it is flown past the Van Allen belts. The experiment needs to take place when the moon is outside of the magnetotail to ensure that it is exposed to a deep space radiation environment. To make sure the experiment takes place during an eligible time period information must be gathered about the moon’s position and the magnetotail. To accomplish this it is necessary to calculate the moon’s position over a three year launch window and compare its position to the position of Earth’s magnetotail and bow shock. Provide this information as a decision support table for the DSRG experiment. Determine if passage through Earth’s bow shock poses a concern for altering the ionizing radiation encountered by the yeast experiment. Provide examples of moderate-to-extreme conditions that could be encountered during the experiment.

Exploring Thermospheric Response to Magnetospheric Forcing Using Principal Component Analysis

Kristian Mrazek1, Clayton Cantrall2, Tomoko Matsuo2

1Augustana College, 2CU Boulder Aerospace Engineering Sciences Department

Poster

The NASA Global-scale Observations of the Limb and Disk (GOLD) mission provides a unique, global perspective of Earth’s ultraviolet emission from space. The GOLD observations are sensitive to both the composition and temperature in Earth’s upper atmosphere. Measuring these states is important for understanding and predicting the effects of space weather in Earth’s atmosphere. We present a case study into the global-scale response of the thermosphere during a period of heightened geomagnetic activity in November 2018. GOLD observations of temperature and composition are compared to a simulation by NOAA’s Whole Atmosphere Model (WAM)2. Principal Component Analysis (PCA) on the WAM simulation is used to explore the global modes of thermospheric variability during this period. The modes associated with geomagnetic activity are identified using cross-correlations between the time series of PCA coefficients and geomagnetic drivers. We find that while global temperature responds rapidly to geomagnetic forcing, composition displays a significant lag time.

Comparisons of Novel Imaging and Spectroscopic Infrared Eclipse Observations in 2017

Lauryn Williams1, Amir Caspi2, Dan Seaton3, Jenna Samra 4

1University of Missouri – Columbia, 2Southwest Research Institute, 3CU/NOAA & SwRI, 4Harvard-Smithsonian CfA

Poster

The 2017 total solar eclipse was a valuable opportunity to make unique observations in the Mid-Wave Infrared (3–5 μm) passband at high altitudes to study organized structures in the corona in an under-observed wavelength range. Using two NASA WB-57 research aircraft at 52,000 feet, we observed about 7.5 minutes of totality. We compared our images to measurements taken by the Airborne Infrared Spectrometer (AIR-Spec) on the NSF HIAPER Gulfstream V flying at 47,000 feet and observations from the Solar Ultraviolet Imager (SUVI) on the GOES-16 spacecraft. Directly comparing these data allows us to interpret our broadband images in the context of these new spectral measurements that highlight the physical processes in the corona. Overlaying the AIR-Spec spectra at their four slit positions on our broadband MWIR images reveal the IR spectral lines contributing from a solar prominence and an active region that we focus on. SUVI gives us a calibrated reference against which to compare our two experimental data sets. Comparison of the spectral data from AIR-Spec with high-resolution filter imaging from WB-57 and SUVI provides temperature diagnostics and spatial context not available from existing EUV and visible light observations to probe the physical nature of the structures. This study is a pathfinder for future coordinated observations with upgraded instrumentation to measure key spectral lines, sampling temperatures and ionization states largely inaccessible in other wavelengths, to improve understanding of heating and evolution of coronal structures.

Examining Neutral Line Properties And Their Connection To Flare Activity

Leah Kiser1,2, Alexei Pevtsov3

1Northland College, 2Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, 3National Solar Observatory

Poster

The impacts of space weather have been a concern to many sectors and have recently become an important topic of research. Because more and more technology has been developed with the potential to be affected by geomagnetic activity, it has become critical to improve space weather forecasts. Both timing and accuracy require improvement to prevent interruptions in communications, GPS, and other important systems. This project seeks to better understand magnetic neutral line properties and the connections to flare activities in the hopes of better understanding flares. Flares are often a precursors to eruptive events that may cause space weather impacts on Earth. A deeper knowledge of flares could be used to better predict events. This research utilized IDL to analyze magnetograms and determine three key properties of neutral lines, their total length, their maximum gradient, and the length of neutral lines with a gradient of 10 G/degree or more. Flare data from the Hinode missions was also included. A primary relationship between magnetic flux and flare activity was found. However, secondary relationships between neutral line properties and flare activity were not present. It was found that on full solar disks during one carrington rotation, neutral line properties have little to no relationship to flare activity. It is likely that further research is needed on a smaller scale. Looking at specific active regions may show a better relationship between neutral line properties and flare activity. If relationships can be found, flare activity may be better understood and easier to predict. This would improve space weather predictions on Earth.

Time Analysis of the SORCE and TSIS similaritY (TASTY)

Peter Breslin1 ,Stéphane Béland2, Steven Penton2

1Trinity College Dublin, 2Laboratory for Atmospheric and Space Physics – LASP

By almost 4 orders of magnitude, solar irradiance is the primary source of natural forcing operating on the Earth’s atmosphere. There are two critical aspects to the measurement of solar irradiance: 1) measuring the solar irradiance traceable to international radiometric standards, and 2) understanding and correcting long-term instrument degradation for the determination of full-spectral solar variability. The Total Solar Irradiance Sensor (TSIS) on the International Space Station measures spectral irradiance with the Spectral Irradiance Monitor (SIM). This was launched in 2017 and was built on heritage and lessons-learned from the SORCE-SIM (Solar Radiation and Climate Experiment), a satellite which was launched in 2003. Almost 2 years of overlapping observations were collected from both instruments before the SORCE mission ended in February 2020. We present the analysis of the solar  irradiances  as  measured  by both instruments throughout the overlap period in which we quantify the wavelength dependent long-term stability. Moreover, we provide a late mission absolute flux correction for SORCE-SIM which was launched with an absolute irradiance scale less accurate than TSIS by almost a factor of 10. This will help to ensure the continuous data record of solar variability is maintained and kept to the required degree of accuracy, and will therefore help to lower uncertainties when constructing composite data sets.

Modeling the solar corona: testing nonlinear force-free methods with a magneto-hydrostatic test case

Santiago Rodriguez, Stuart Gilchrist, KD Leka, Karin Dissauer

The solar corona is the outer atmosphere of the Sun and it is where highly energetic solar events take place, e.g. solar flares. The coronal magnetic field is thought to be in a force- free state, meaning that the magnetic Lorentz force is self-balanced. Furthermore, we don’t get reliable vector magnetic data at the corona. This motivates Nonlinear Force-Free Field (NLFFF) extrapolations of the coronal magnetic field using photospheric magnetic data as boundary conditions. Photospheric data is not in a force-free state, which leads to an inconsistency between the boundary conditions and the assumptions of the model. However, by using a Linear Magneto-HydroStatic model (LMHS), which deliberately takes into account gravity and gas pressure forces, as boundary conditions to a force free model we can examine the effect of this inconsistency in the modeling. In the LMHS model, the non-magnetic contribution to the forces is controlled by a single parameter . We consider several test cases with different values of this parameter. It is hypothesized that NLFFF model will not experience much change when this parameter is set to zero, providing a consistent control test case. Nevertheless, by increasing non-magnetic contributions, we seek to test the limits of the NLFFF model and determine the deviation from the original LMHS model using various methods of comparison (point-wise comparison, field line tracings, magnetic energy calculations, Lorentz force calculations).
This material is based upon work supported by the National Science Foundation under Grant No. 1841962. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation.

Variability of H-alpha Line Observed at High Spectral Resolution in the Solar Atmosphere

Rudy Parra1, Serena Criscuoli2

1Central New Mexico Community College, 2 NSO

Poster

We analyzed temporal variations of the properties of the Hα alpha line in sun-as-a-star observations. The goal is to understand how magnetic photospheric and chromospheric features modulate the variations of the Hα core-to-wing ratio at the 27-days rotational time-scale. We find that sunspot area modulates the shape of Hα the most, while faculae and filaments have little or negligible effects. These results are of relevance to understand chromospheric variability in solar-like stars.

 

Katy Luttrell

Poster

Jeffery Dulaney

Poster
Kate DeMarsh
 
Poster
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