Bulletin of the American Physical Society
Bridge Program and National Mentoring Community Conference
Volume 63, Number 14
Friday–Sunday, November 16–18, 2018; Google HQ and Stanford University, CA
Session PS1: Undergraduate Poster Session (11:00AM - 12:30PM) |
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Room: Tressider Oak Lounge |
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PS1.00001: Wearable textile-based energy harvester designed for human motion. Rebeca Gurrola, Janna Eaves, Cary Pint While there are many different methods of generating sustainable energy, small quantities of energy otherwise wasted in the pursuit of everyday activities are often overlooked. Recently, electrochemical energy harvesters joined the ranks of piezoelectric and triboelectric harvesters to convert mechanical energy into electrical energy. Here, we use materials with mechanochemical response to seamlessly integrate motion harvesting into textiles for wearable applications. This study presents a novel class of safe and non-toxic ``smart'' energy harvesters which can be activated via sweat, simulated here by a solution of NaCl. The harvester comprised of a sodium tin alloy on copper fabric exploits ambient motion at frequencies of 0.1 Hz. In bend tests, the harvester generates a peak power of \textasciitilde 36.4 $\mu $W/cm$^{\mathrm{2}}$ and energy of \textasciitilde 131.1$\mu $J/cm$^{\mathrm{2}}$ with each bend. Additionally, it is sensitive to changes in salt concentration, suggesting applications in hydration-monitoring. These results emphasize the exciting possibilities for a new class of wearable harvesters. [Preview Abstract] |
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PS1.00002: Robotics with Humanoid Robot NAO and Hexapod (Robotic Spider) Carlos Galindo, Muhammad Saleem, Akhtar Mahmood Robotics is an exciting field. Various types of robotics devices are being used in many sectors of the industry, in NASA's Mars missions, hospitals and movies, among others. Since robotics technology has witnessed a remarkable growth, there is a need to educate the next-generation undergraduate STEM students in robotics. We have been conducting research in fully-autonomous robotics with our Humanoid-Robot NAO and in semi-autonomous robotics with Hexapod in our Robotics Lab. We have programmed a humanoid robot, called NAO that has the ability to detect the surroundings and can hear, communicate, carry out conversations with humans and can even sense/detect being touched. We have programmed NAO in Python to become fully-autonomous. NAO has 25 degrees of freedom and has multiple touch sensors, and hence is able to carry out specific tasks in the lab and can work alongside with students. NAO is controlled by a specialized Linux-based Operating System, called NAOqi, which allows NAO to interpret and understand data received by its sensors. NAOqi powers the robot's hardware, which includes four microphones (for voice recognition and sound localization), two speakers (for multilingual text-to-speech synthesis) and two HD cameras (for vision, including facial and shape recognition). Natural and human-created disasters often leave search-and-rescue missions reliant on human efforts in dangerous scenarios. We have experimented with applying semi-autonomous functionality by building a Hexapod robot using a PlayStation-2 controller that can be used to aid human operators in search-and-rescue operations. Using this controller, we are able to investigate the movements of the hexapod and understand its physical capabilities, which is necessary to determine whether a hexapod could function in diverse environments. We will highlight the advantages of implementing semi-autonomous human-operated robotics [Preview Abstract] |
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PS1.00003: Calibrating Mass Accretion Rates in Pre-Main Sequence Stars using Brackett Alpha Emission, and Pitfalls in Low Accretion Rate Systems Dakotah Tyler Using calibrations derived from correlations between luminosities of Hydrogen Line emissions, we can calculate Mass Accretion Rates for particular stars. Calibrations for the emission line strengths of Paschen Beta (1.28 microns) and Brackett Gamma (2.16 microns) are well known already. By analyzing correlations between the relative strengths of these emission lines and that of Br A (4.06 microns) we can calibrate Br A emission for producing Mass Accretion Rates as well. This is useful when extracting data from an observation that does not contain Pa B or Br G, but does contain Br A. It is important to be able to produce Accretion Rates on all observations, as variability in Low Accretion Rate Systems is a point of interest. In this presentation, we also look at some pitfalls associated with analyzing emission in these Low Accretion Rate Systems. Variability is defining characteristic of these systems, but this high level of variability can result in massive fluctuations in observations made in as little as weeks apart. Some of these observations even reveal negative fluxes at times when absorption seems to be stronger than emission from certain Hydrogen Lines. [Preview Abstract] |
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PS1.00004: Background Spectrum Analysis of the PULSTAR Reactor using a HP Ge Detector Elon Price, Albert Young {Background radiation can often be a significant issue with large scale nuclear physics experiments. A background spectrum for the PULSTAR reactor can be vital information for ongoing projects like UCN nEDM, Neutron Activation Analysis, and }\textit{Neutron Radiography of turbine blades for jet engine manufacturing (to name a few). High-purity germanium detectors are used for gamma-ray spectroscopy and are more efficient and sensitive than standard 3'' x 3'' Na(Tl) detectors. I used a 2001A Canberra HP Ge detector and conducted several 24 hour runs in the reactor bay. Using ROOT, I generated a smoothed histogram and fitted the data with a Guassian and linear model. Using the known }\textit{Ar-41 and K-40 peaks (energies 1293 keV and 1460 keV), I was able to produce a calibrated spectrum which allowed me to find other gammas like Na-24 and Th-232. Currently I'm working with Geant4, to subtract the compton scattering portion of the spectrum. The resulting product will be a well-calibrated background spectrum of the reactor including the total and peak efficiency.} [Preview Abstract] |
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PS1.00005: Patterned Fabrication of Dielectric Nanowaveguides Chelsea Howard, Patrick DeLear, Huizhong Xu Strong transmission of visible light through dielectric nanowire waveguides has been previously demonstrated with 40-nm-diameter zinc oxide waveguides in a silver film. However, the chemical synthesis methods used to fabricate the waveguides prevent the controllability of size and distribution, within the nanowaveguide arrays. In this work, we utilize Electron Beam Lithography (EBL) and Reactive Ion Etching (RIE), to fabricate dielectric nano pillars of titanium dioxide and silicon nitride. The optical properties of these nano pillar waveguides will be used to make devices for nanoscale imaging and spectroscopy applications. [Preview Abstract] |
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PS1.00006: Adapting Pion Mentorship Program to Prepare Students for Post-Graduation Kathryn Mendez To support undergraduate students at Florida International University's Physics Department, the Pion Mentorship program has been adapted to incorporate peer mentorship, faculty mentorship, and professional development. This program is run by the Sigma Pi Sigma chapter at FIU, who's students are primarily from historically underrepresented groups in physics like women and ethnic minorities. The program's first aim pairs freshmen and sophomore students with their peers who are in upper division courses so they can receive guidance in their classes and advice for getting involved. Secondly, students and faculty are paired with the goal of facilitating a relationship where students learn about research and faculty learn how to be better mentors. Lastly, students attend various professional development workshops specifically tailored to their needs. The Pion Mentorship program has improved students' preparedness for their post-graduation plans. Further details of the program including methods of obtaining student feedback, changes, and challenges that need to be overcome will be shared. [Preview Abstract] |
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PS1.00007: Visualizing Binary Black Hole Collisions and Gravitational Waves Teresita Ramirez Aguilar, Geoffrey Lovelace Gravitational waves are ripples in the fabric of space and time, traveling at the speed of light predicted by Einstein’s theory of relativity. One of the best sources of gravitational waves is binary black hole mergers, which are among the most violent events in the universe. On September 14 2015, Advanced LIGO (Laser Interferometer Gravitational-wave Observatory) successfully made the first gravitational wave detection. Since then, LIGO and Virgo have published four additional observations of gravitational waves from merging black holes. This poster presents a visualization of the merging black holes that LIGO and Virgo have observed so far, created by solving Einstein's equations of general relativity on supercomputers. This is the only way to model merging black holes, because all approximations fail near the time of merger. The video shows calculations of the black holes’ horizons and the emitted gravitational waves during the final few orbits as they spiral inwards, merge and ring down. Each calculation is consistent with one of the LIGO-Virgo observations. [Preview Abstract] |
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PS1.00008: Simulating Black Hole-Neutron Star Mergers Jennifer Sanchez Gravitational waves are ripples in space and time predicted by Einstein’s theory of relativity; in 2015, Advanced LIGO observed these waves passing through Earth for the first time. Looking forward, we hope to observe black hole-neutron star mergers as they are the most exciting sources of gravitational waves since they are “multi-messengers,” emitting both electromagnetic and gravitational waves. Highly accurate mathematical descriptions of these waves are crucial for helping experiments to detect as many gravitational waves from merging black holes and neutron stars as possible, and to help determine whether observed gravitational waves are from merging black holes or from a black hole-neutron star merger. Using the Spectral Einstein Code, we are modeling black hole-neutron star mergers for different binaries, computing the emitted gravitational waves, the properties of the black hole before, during, and after the merger, and the behavior of the neutron-star matter as it is torn apart, forming a disk around the black hole. So far, we have focused on low-mass mergers with non-spinning black holes, a case where tidal effects on the emitted gravitational waves are especially strong. In the future, we will extend this work to rapidly spinning merging black holes. [Preview Abstract] |
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PS1.00009: Neutron Star Measurements in Third Generation Gravitational Wave Observatories Isabella Molina, Jocelyn Read, Eric Flynn, Erick Leon Gravitational waves were detected from a binary neutron star merger giving us more insight into neutron stars. Future detectors are being investigated that will be better equipped to make these detections and help us learn more about the neutron stars themselves. Proposals for future gravitational-wave detectors were analyzed to determine their capabilities in detecting binary neutron-star mergers and measuring their properties.This research compares the future detectors A$+$, A$++$, Cosmic Explorer1 and 2 Wide and Narrow, Einstein Telescopes B and D, Vrt, and Voyager to the current Advanced LIGO. The inspiral analysis aimed to determine the optimal frequency range for the detectors to observe the inspiral of two neutron stars. The post merger analysis used several equations of state and determined the frequency range that gave the clearest SNR and best results for making analysis on the EOS's. SNR values indicate whether the post merger is distinguishable after the inspiral. This analysis will determine which detector configurations are best for measuring properties of neutron stars. [Preview Abstract] |
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PS1.00010: Simulating the Lyman-alpha Forest in Self-Interacting Dark Matter Models Sergio Garcia, Anson D'Aloisio The cold dark matter model successfully accounts for all~observations on super-galactic scales. However, it is unclear whether simulations of collision-less dark matter (CDM) can be reconciled with astronomical observations on sub-galactic scales.~ In addition, null results from terrestrial experiments have motivated the exploration of alternatives to the Weakly Interacting Massive Particle.~ It has been shown that self-interacting dark matter (SIDM) models in which a dark photon mediates the self-interaction can alleviate the sub-galactic tensions while at the same time evading direct detection experiments.~ ~These models generally yield a suppression of cosmological density fluctuations on scales below \textasciitilde 1 Mpc, making them constrainable by current Lyman-alpha forest observations.~ Previous studies have constrained SIDM models in an approximate way using cosmological perturbation theory. However, because the Lyman-alpha forest is sensitive to nonlinear scales, obtaining accurate constraints requires the use hydrodynamic simulations.~ I will discuss results from hydrodynamic simulations of the Lyman-alpha forest in SIDM cosmologies.~ Specifically, I will discuss the effects of SIDM on the Lyman-alpha forest flux power spectrum and our efforts to obtain accurate constraints from observational measurements.~ [Preview Abstract] |
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PS1.00011: An Efficient Search for Gravitational Waves from Primordial Black Holes Phoebe McClincy, Ryan Magee, Anne-Sylvie Deutsch, Chad Hanna, Christian Horst, Duncan Meacher, Cody Messick, Sarah Shandera, Madeline Wade There is increasing interest in sub-solar mass black holes regarding the possibility that they are a component of dark~ matter, due to the limited knowledge regarding its composition. ~We are able to test the primordial black hole theory of dark matter by running a targeted sub-solar mass search using LIGO data. The range and difficulty of the search depends on certain parameters (defined below). We aim to define parameters that produce a search which simultaneously maximizes relative sensitivity and minimizes computational cost. We tested template bank size dependence on several parameter sets, including minimum/maximum frequency, minimum mass, and spin. ~As the template bank size increased, the overall computational cost of the project also increased.~ We determined that larger magnitudes of spin, wider frequency ranges, and smaller masses produce a larger template bank, and subsequently a higher computational cost. ~To obtain the lowest computational cost for this project, we would need to constrain the search parameters as much as possible.~ In the future, we will construct a search such that our parameters are as extensive as possible without substantial computational cost. [Preview Abstract] |
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PS1.00012: Circularly-Polarized Light Signatures in Nature Daniela Marin, Yitian Ding, Stanley Pau Polarized light is ubiquitously found across the globe. Circularly polarized light (CPL) on the other hand, is seldom found. Traces of CPL have been detected in the reflection of the exoskeleton of certain species of beetles, bird feathers, and the lanterns of firefly larvae. The structure of the beetle cuticle can serve as a biological model for cholesteric liquid crystals, crystals that respond to stimuli with a change in color. Moreover, humans are not able to distinguish the differences between polarization states, but studies have shown that some animals exhibit polarization vision. This type of vision has the capability of producing light information used in contrast enhancement, camouflage breaking and object recognition. This project aimed to contribute to the understanding of CPL in the biological sciences and to further investigate the functionality of CPL in organisms. Many types of animals, plants, and landscapes were imaged, and it was found that CPL was absent in several species under the categories, reinforcing CPL's infrequent appearance in nature. [Preview Abstract] |
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PS1.00013: Quantifying Chromatin Compaction in HL-60/S4 Cells Cristopher Thompson The concepts of chromatin compaction is to measure the level of compaction of complex macromolecules found in the cells. The each set of cells were treated with sucrose or trichostatin. Sucrose condenses the DNA of the cell nucleus together, and trichostatin decondenses the DNA of the cell nucleus. The chromatin compaction method in this experiment measured and observed how DNA compacts around histones during the cell replication cycle. Our data set contained samples coated in sucrose (mM) and trichostatin (ng/ml) for levels 0, 50, 100, 200. With fluorescence microscopy, we can study the involved structural organization of DNA in a cell nuclei using antibodies. We used antibodies to mark different components of the nucleus, H1.5, FAB, DAPI, and PL2.6. These antibodies were to mark histones, nucleosomes, and DNA. We use a fixative formaldehyde and glyoxal to fix the cells in place. We used SP8 microscope to image the cells in interphase and mitosis. The tools that were used were multicrop function, open source R package nucim, and bioimagetools. The R package analysis of the crop data creates a compaction tables. This table is classes of compaction for the DNA within the nucleus. [Preview Abstract] |
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PS1.00014: Parameter Estimation of Gravitational Waves of Binary Neutron Star Mergers Using Lalinference Erick Leon The first gravitational waves emitted by a neutron star binary coalescence was detected on August 17, 2017. Being able to estimate the parameters of such a system including mass, and tidal deformation is an important factor in understanding the physics of neutron stars. Lalinference is a parameter estimation tool used to estimate parameters from gravitational wave signals. By using other computational methods to create fake gravitational wave signals we can test the capability of Lalinference to predict the correct parameters of these gravitational waves for some given noise spectrum. In my project, I ran Lalinference parameter estimation on several fake gravitational wave signals and compared the predicted parameters with the ones used to create the fake signals. This research can be used to predict the scientific capabilities of future observing runs for advanced interferometers. [Preview Abstract] |
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PS1.00015: Feasibility and Life Cycle Studies of Dolomites for Carbon Capture Mc Ben Joe Charles, Dominic Dodson, Shirley Garcia, Scott Wallen, Gary Albarelli, Brian Birky, Sesha Srinivasan Dolomites (CaMg(CO$_{\mathrm{3}})_{\mathrm{2}})$ are the minerals present in large quantities and are currently not used by the phosphate mining industry in Florida. This project seeks to utilize Dolomites~as a medium for carbon capture. Thermogravimetric (TG) measurement of high concentration dolomite phosphatic pebbles received from our collaborating partners from Florida Industrial and Phosphate Research Institute (FIPR) were examined under Nitrogen (N$_{\mathrm{2}})$ ambient environment between 300\textdegree C to 800\textdegree C. The structure and chemical composition of each sample were investigated using X-Ray Fluorescence (XRF), Fourier Transform Infrared Spectroscopy (FTIR) and X-Ray Diffraction (XRD). TG data shows that the amount of CO$_{\mathrm{2}}$ lost on the first initial decomposition can't be gained; however, the amount of CO$_{\mathrm{2}}$ that the samples gain and loss stabilize as more cycles are performed. We will describe and discuss the life cycle analysis of both commercial and handpicked dolomite samples for carbon capture applications. [Preview Abstract] |
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PS1.00016: Feasibility Studies of Using Dolomite as Thermal Energy Storage for CSP Applications Dominic Dodson, Mc Ben Joe Charles, Shirley Garcia, Scott Wallen, Gary Albarelli, Brian Birky, Katharina Pfaff, Sesha Srinivasan Dolomite, calcium magnesium carbonate (CaMg(CO$_{\mathrm{3}})_{\mathrm{2}})$, is considered an undesirable mined resource for phosphoric acid production in Florida; as such, large quantities of the mineral are available. This study characterized phosphatic high concentration dolomite pebbles received from the Florida Industrial and Phosphate Research Institute (FIPR) and investigated their feasibility for carbon dioxide (CO$_{\mathrm{2}})$ sequestration and thermochemical energy storage (TCES). The chemical composition of the dolomite minerals was studied using X-ray Fluorescence (XRF), Fourier-transform infrared spectroscopy (FTIR), and Scanning electron microscopy with energy dispersive x-ray spectroscopy (SEM, EDS), which confirmed the phosphatic pebbles received from FIPR contained high percentages of dolomite. Thermogravimetric analysis (TGA) was used to calculate the dolomite mineral activation energy for carbonation and calcination of the dolomite pebbles in Nitrogen (N$_{\mathrm{2}})$ ambient and CO$_{\mathrm{2}}$ ambient conditions, respectively, and with temperatures up to 800\textdegree C. Values important for thermochemical energy storage such as heat capacity and enthalpy of reaction were also calculated using this TGA data. Changes in crystal structure after calcination, carbonation, and wet ball milling of the dolomite minerals were observed using X-ray diffraction (XRD). The effects of wet ball milling to reduce particle size were observed on the cyclic stability and carbonation of the dolomite pebbles. Particle size and surface area were measured using XRD and N$_{\mathrm{2}}$ adsorption BET methods. [Preview Abstract] |
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