Bulletin of the American Physical Society
81st Annual Meeting of the APS Southeastern Section
Volume 59, Number 18
Wednesday–Saturday, November 12–15, 2014; Columbia, South Carolina
Session JA: Nuclear/Hadronic Physics II |
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Chair: Simonetta Liuti, University of Virginia Room: Richland I |
Friday, November 14, 2014 2:00PM - 2:36PM |
JA.00001: TBD Invited Speaker: Keh-Fei Liu |
Friday, November 14, 2014 2:36PM - 3:12PM |
JA.00002: TBD Invited Speaker: Charles Hyde |
Friday, November 14, 2014 3:12PM - 3:24PM |
JA.00003: Nucleon Spin and Twist Three Distributions FNU Abha Rajan I will be talking about the significance of twist three distribution functions in our understanding of spin of protons and neutrons. When the EMC experiment in the 1980s at CERN showed the quark spin contribution to be extremely small, it presented us with the nucleon spin puzzle. I have been working on the angular momentum generated by the motion of quarks and gluons: the orbital angular momentum contribution (OAM). Transverse momentum distributions (TMDs) and generalised parton distributions (GPDs) are theoretical quantities that provide us with the frameowork to study many different properties of the nucleon including the partonic OAM. By looking at the helicity content of these objects we can make the connection to experimental observables. TMDs and GPDs are obtained by parameterizing the quark correlator between hadron states under different kinematical conditions. TMDs include quark transverse momentum while the GPDs involve momentum transfer between the hadron states. At leading order, the so called twist two limit, the correlator only involves two quarks but, at the next order a gluon needs to be included as well. I am trying to understand the physics of this limit and explore the new aspects of partonic OAM that these distributions shed light on. [Preview Abstract] |
Friday, November 14, 2014 3:24PM - 3:36PM |
JA.00004: Characterizing the Power of Supernova 2009nr through Photometry and Spectra Integration Jonathan Heath, Ginger Bryngelson A plot of a supernova's brightness over time produces a light curve. Due to the uniformity of their light curves, type Ia supernovae (SNe Ia) are valuable markers for determining the expansion of the universe and other cosmological parameters. Additional properties related to SNe Ia may also be better understood by examining their late-time light curves, such as their composition, magnetic field, etc. This study examines the behavior of SN 2009nr compared to additional normal SNe Ia at similar epochs. Regarding SN 2009nr, NIR (K, H, J) images using the FLAMINGOS IR Imaging Spectrometer and visible (B, V, R, I) images using the Mosaic 1 imager were taken with the 4m Mayall Telescope at Kitt Peak National-Observatory. In order to characterize the late behavior of SN 2009nr, the supernova's apparent magnitude for each night of observation (by filter) was found using the Image Reduction and Analysis Facility (IRAF). To characterize and relate the additional SNe Ia to SN 2009nr, a Python script capable of solving for fluxes and power contributions in given filters was written. The script uses the Savitzky-Golay filter to first smooth SNe Ia spectra data before integrating under the curves by filter. [Preview Abstract] |
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