Physics and Astronomy REU 2021

June 1 - July 31

 

 

 

Projects

 

“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


Final talk


“ 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. ​

5 minute talk


Final talk


“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


“ 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.

5 minute talk


Final talk


“ 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.

5 minute talk


Final talk


 

 

 

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