Bulletin of the American Physical Society
Joint Spring 2013 Meeting of the Texas Sections of the APS and AAPT and Zone 13 of the SPS
Volume 58, Number 3
Thursday–Saturday, April 4–6, 2013; Stephenville, Texas
Session N1: Astrophysics II |
Hide Abstracts |
Chair: Michael Hibbs, Tarleton State University Room: Science Building 102 |
Saturday, April 6, 2013 10:30AM - 10:42AM |
N1.00001: Estimating the viscous potential value using SuperDARN data Michael Mishler, Denver Scott, Aaron Baca, Shree Bhattarai, Ramon Lopez The solar wind flowing around the magnetosphere causes tail-ward dragging of the magnetospheric plasma, which in turn causes a return flow deeper inside the magnetosphere, thus producing a circulation pattern called the viscous circulation pattern. This plasma circulation pattern gets mapped into the ionosphere via magnetic field lines, thus imposing an electric field in the ionosphere. This field can be measured in terms of an electric potential which is known as the viscous potential. In this paper, we will use the electric potential values obtained from SuperDARN (Super Dual Auroral Network) during weak IMF (Interplanetary Magnetic Field) conditions (\textbar By\textbar \textless 1 , and -0.5 \textless Bz \textless 0) to estimate the viscous potential value. [Preview Abstract] |
Saturday, April 6, 2013 10:42AM - 10:54AM |
N1.00002: Interaction of space, time, mass relation -- constant of LIZI Yongquan Han One, definition 1, LIZI: the material which is reasonable to exist, from the basic to the universe 2, the universe, the outer space and is a constant size of space, is the foundation of space; space including non vacuum part ( the internal space ) and the vacuum part ( the universe outer space), non vacuum part as far as possible to occupy the whole vacuum part into non vacuum. 3, LIZI space: refers to the visible, not visible management sub can radiate to the field. 4, feeling space: in addition to the LIZI space outside the space. 5, if and only if the universe ( LIZI ) mass will not change Two, LIZI constant The product of the mass of LIZI, time, feeling space is a constant, we can express it by a math equation, N$=$(V-v)MT, N is the LIZI constant, V refers to the summation of the inside and outside universe is a constant, v is the space which LIZI takes, (V-v)is the feeling space, M is the mass of the LIZI, T refers to time. [Preview Abstract] |
Saturday, April 6, 2013 10:54AM - 11:06AM |
N1.00003: Analyzing the Parameters of Corotating Interaction Regions and Their Relationships with Geomagnetic Storms Phu Nguyen, Soha Aslam, Kyle Van Zuiden, Kevin Pham, Ramon Lopez A corotating interaction region (CIR) forms when a low speed solar wind stream is compressed by a high speed solar wind stream (HSS) behind it, creating a region of higher pressure and density. This interaction region rotates along with the Sun, hence the name ``corotating interaction region.'' It is observed that HSSs occur after CIRs. CIRs and the following HSSs are often associated with geomagnetic storms. We have collected CIRs followed by HSSs from the period of the years 2000-2005. We will analyze the relationship between the average parameters of CIRs and HSSs to determine which parameters affect the size of geomagnetic storms. [Preview Abstract] |
Saturday, April 6, 2013 11:06AM - 11:18AM |
N1.00004: Evaluation of Two Transit Algorithms Matt Heuser, Richard Olenick, Arthur Sweeney, James Meier, Jeff Schneiderjan Crucial in the data pipeline for transit searches are dependable algorithms which hunt for transits in accumulated light curves. We used C$++$ versions of EEBLS (Edge Enhanced Box Least Squares) and QATS (Quasi Automated Transit Search) algorithms to search for possible transits in the STExT group database of light curves of approximately 2500 stars. The outputs of these two programs were compared and a list of potential binary candidates was determined. We will compare the algorithms and discuss possible candidates for transits. [Preview Abstract] |
Saturday, April 6, 2013 11:18AM - 11:30AM |
N1.00005: Big Bang Nucleosynthesis with a non-Maxwellian distribution John Fuqua, Carlos Bertulani, Mahir Hussein I will present results on the abundances of light elements based on the big bang nucleosynthesis model calculated using the Tsallis non-extensive statistics. The impact of the variation of the non-extensive parameter q from the unity value is compared to observations and to the abundance yields from the standard big bang model. We find large differences between the reaction rates and the abundance of light elements calculated with the extensive and the non-extensive statistics. We found that the observations are consistent with a non-extensive parameter q = 1+0.05-0.12, indicating that a large deviation from the Boltzmann-Gibbs statistics (q = 1) is highly unlikely. [Preview Abstract] |
Saturday, April 6, 2013 11:30AM - 11:42AM |
N1.00006: Comparisons between observations and simulations of solar wind magnetic field reversals Brett Schock, Spencer Durrenberger, Robert Bruntz, Ramon Lopez Computer simulations are essential to our pursuit of a greater understanding of the space that surrounds our planet, including the interaction of the solar wind and the Earth's magnetic field -- the magnetosphere. These simulations incorporate years of knowledge obtained by physicists on the nature of the solar wind, a plasma of particles streaming from the sun that can greatly affect the satellites and power grids that we depend on for much of modern life. Testing of the simulations with observed data helps to validate existing theories and refine the computer models to better simulate reality and provide physicists, commercial and governmental satellite operators with critical information on the potential negative effects of ``space weather.'' Several quick and significant reversals in the predominant direction of the magnetic field carried by the solar wind, events that can cause dramatic changes in the magnetosphere which satellite operators must be aware of, were identified in otherwise steady observational data. These data were compared to simulations of the same events, using the Lyon-Fedder-Mobarry (LFM) magnetohydrodynamic (MHD) simulation. The ionospheric states during periods of steady conditions were also compared to simulation results to determine correspondence. [Preview Abstract] |
Saturday, April 6, 2013 11:42AM - 11:54AM |
N1.00007: The Effects of Modifying the Solar Wind Input into an MHD Simulation of the Whole Heliosphere Interval Kevin Pham, Ramon Lopez As high speed solar wind catches up to slower solar wind, it compresses the slower solar wind. This compressed region, called a corotating interaction region (CIR), has higher density, magnetic field magnitude, and temperature. CIRs interact with the Earth's magnetosphere and can cause geomagnetic storms. It has been suggested that the fluctuation in the magnetic field of the CIR and the following high speed stream play a large role in geomagnetic storm strength. We will be using the Lyon-Fedder-Mobarry global 3D magnetohydrodynamic(MHD) simulation to simulate the Whole Heliosphere Interval (March 20 -- April 16, 2008) which contains two CIRs. Various modifications will be done to the solar wind input to determine the relative geoeffectiveness due to the average magnetic field and due to the fluctuation in the magnetic field. [Preview Abstract] |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700