“ Fitting Supernova Spectra using SYNOW ”
Sara Paugh- University of Oklahoma
Mentor: Dr. Eddie Baron
SN 2021fxy is a recently discovered supernova with magnitude 16.9 and redshift 0.0094. It features a strong red absorption line produced by singly ionized silicon (Si
II), classifying it as a type Ia. Using SYNOW, a program developed by David Branch, we can produce synthesized supernova spectra and compare it with the actual spectra
of SN 2021fxy. We attempt to produce synthesized spectra that matches the actual spectra as best as possible by adding on different ions (silicon, iron, calcium, etc.),
one at a time and manipulating their parameters such as optical depth, velocities, temperature, and more. Once every absorption line is fit, we will be able to
understand SN 2021fxy’s properties in greater detail as well as determine its Branch group: core-normal, cool, shallow-silicon, or broad-line.
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“ AU Mic ”
Jacob Monahan - University of Nebraska at Omaha
Mentor: Dr. John Wisniewski
Observing variability in the lightcurve of a star during a planetary transit removes degeneracies in determining starspot distribution. AU Mic is a nearby
very young M dwarf star with at least two transiting planets and large flux variations due to starspots. We will study and characterize the distribution and size
of those starspots on AU Mic via in-transit and out-of-transit starspot modeling.
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“ Improved Magnetic Field Control for Experiments with Sodium Bose-Einstein Condensates ”
Nathaniel Gunter - University of Oklahoma
Mentor: Dr. Arne Schwettmann
This summer, I am designing and manufacturing a current controller intended to improve the magnetic field uniformity of our sodium vapor magneto-optical trap.
Doing so will reduce noise introduced by uncontrolled Zeeman shifts and allow for faster and finer control of any gradients that may be necessary for future
experiments.
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“ Characterization of Microwave Cavity ”
Kellan Brown - East Central University
Mentor: Dr. Alberto Marino
I took a spectrum analyzer and connected its output through a circulator. The output labelled
two connected to the microwave cavity, and output three back to the spectrum analyzer.
Through the spectrum analyzer, I send a sweeping signal with a range of frequencies to the
cavity, which was reflected back to the spectrum analyzer after interacting in the cavity. I found
the resonant frequency of the cavity of length 11.583 cm to be 3.0736 GHz. Then I increased
the length of the cavity by increments of 1 mm and recorded the change in resonant frequency
up to 11.35 mm. The peak resonant frequency shifted to 3.0302 GHz when fully extended. The
next few steps include heating the cavity to 50°C and 100°C and recording the resonant
frequency as the length is increased in increments of 1 mm.
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“ A dark matter study through the Higgs portal ”
Samantha Reisenauer - Northern Arizona University
Mentor: Dr. Kuver Sinha
Dark matter makes up close to 27% of our universe, and yet its precise nature is still unknown. To solve this mystery,
there are several methods being used to search for dark matter. These experiments are conducted based on calculations from
models of a theorist’s idea of how dark matter will interact with the Standard Model, highlighting the importance of these
theories and models. My research this summer will focus on an existing Higgs portal model. I will be analyzing this model
of dark matter and working to reproduce the plots created based on the calculations in the paper.
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“ Starspot Modeling ”
Simon Lowry - University of Oklahoma
Mentor: Dr. John Wisniewski
Modeling starspots on stars other than our Sun gives us a deeper understanding of the magnetic activity of those stars,
and allows us to study the radius and atmosphere of transiting exoplanets with much greater certainty. We look at data for
the binary KOI-340, which comprises a solar-type primary star and an M-dwarf companion. This data was captured by the
Kepler spacecraft over a period of 17 Quarters, and is accessed online as lightcurve files. We use the Lightkurve python
module to access and analyse the files. The aim of the research is to use these lightcurves to verify the size and
position of starspots on the surface of KOI-340; this is only possible with software that allows us to model starspots and
compare the lightcurve generated to that of the real world. Using existing models of starspot activity between the
latitudes eclipsed by the companion, we will use the software program STSP to model starspots, focusing on the
out-of-transit data. Keeping in mind the 12.96-day rotational period of the star, which has been found by running
periodograms on the various Quarters of data, we aim to find complete models for the starspots of KOI-340 over all
longitudes, for the duration of the Kepler mission. This is critical in advancing our understanding of stellar magnetic
activity.
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“ Quantum Periodic Cavity Systems ”
Claire Kvande - Kalamazoo College
Mentor: Dr. Doerte Blume
In order to design a system with a specific response on the quantum level, we will link together finite square well potentials (cavities) into rings and observe
how the population density of these cavities changes over time, particularly with the introduction of one or more two-level emitters at the intersection between
rings. These systems would have applications in computing because as technology advances and demands smaller infrastructure, quantum effects will eventually have
to be accounted for.
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“ Optical Cavity for Raman Laser ”
Jalen Crutchfield - East Central University
Mentor: Dr. Grant Biedermann
The spin states of ultra-cold neutral atoms can be coherently manipulated with magnetic and optical
fields to form complex many-body quantum states. This research builds upon previous work with entangling
interactions with ultra-cold Rydberg atoms that were controlled via optical tweezers. This summer, I
will be working with an optical cavity as a part Raman laser system to control the quantum states of
single cesium atoms. The purpose of this optical cavity research is to stabilize the frequency of light
exiting the laser via laser locking, and filtering out unwanted sidebands that are byproducts of a phase
modulator that generates the Raman tones on the optical field.
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“ Going Beyond the Shockley-Queisser Limit ”
John Mahoney - College of New Jersey
Mentor: Dr. Ian Sellers
The Shockley-Queisser Limit states the upper bound of efficiency of a single junction photovoltaic is roughly thirty percent; this is obtained through
accounting for the five intrinsic losses of photovoltaics. The process of thermalization is an intrinsic loss that results in the loss of power due to
thermal relaxations of electrons in the upper regions of the conduction band known as hot carriers. We will study possible candidate materials that could
allow for the capturing of these hot carriers and further increase the efficiency of single junction photovoltaics.
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“ H->WW* ”
Greg McNamara - St. John's University
Mentor: Dr. Mike Strauss
I will be working on Higgs Boson decay with Dr. Strauss through the CERN ATLAS
Experiment this summer. The creation of CERN and the findings will be talked about in order to
provide background knowledge on the subject matter. Higgs Boson production and decay will be
demonstrated where all the necessary tools to look at such an event will as well be explained. In
the last section I will go over how in the summer my goal is to eliminate as many background
processes on a graph using MVAs giving it the highest amount of WW purity as possible.
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“ Looking Past the Standard Model ”
Ryan Parsons - University of Oklahoma
Mentor: Dr. Brad Abbott
Particle physics has developed quickly over the last twenty years. The Large Hadron Collider (LHC) started hunting for particles in 2008. Since then, the
LHC has been at the leading front of high-energy particle physics. In 1964, Peter Higgs predicted a particle that supplied mass to all particles, and in
2012 it was confirmed at the LHC. While this discovery was very significant, it is time to look to the future. Throughout the physics community (Snow
Mass), there is a push for a new particle accelerator to drive the current known frontier of particle physics. There are two main focuses: a linear
accelerator (CLIC) that utilizes collisions 𝑒+ 𝑡𝑜 𝑒−And the other is a circular collision of 𝜇+ 𝑡𝑜 𝜇−. CLIC and the circular 𝜇+ 𝑡𝑜 𝜇− both
have their advantages and disadvantages; however, being that they are both fundamental particles, this will significantly reduce the prominent background
at the LHC. By running simulations and then comparing them to the standard model, we can look for new physics that we are sensitive to with 95% certainty.
By doing this, we can better understand which collider produces the best results for future physics.
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“ Gas Properties and Star Formation as an indicator of AGN activity ”
Anna Engelhardt - Grinnell College
Mentor: Dr. Ferah Munshi
It is not precisely known on what scale environmental mechanisms and galactic properties stimulate the growth of central super massive black holes (SMBH)
to produce active galactic nuclei (AGN). Using cosmological N-Body + SPH simulations it is possible to track galaxy properties over the age of the
universe and attain a deeper understanding of galaxy evolution. Previous investigation using the ROMULUS simulations found a tight correlation between the
Star Formation Rates (SFR) and the Black Hole Accretion Rates (BHAR) of galaxies and their central black holes (Ricarte et. al 2019). This implies that
SMBH and stellar populations grow in tandem (Ricarte et. al 2019). The goal of this research is to further investigate the scale at which the properties
of galaxies matter to BHAR by analyzing SFR and gas content as a function of radius from the center of halos. The gas properties explored in this research
are the fractions of gas, cool gas and HI gas.
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