nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron Stars from an Amazing Mission 111 – WIYN Observatory - Building on the 210 – Bridging Laboratory and Astrophysics: 313 – Outer Limits of the Milky Way Past, Looking to the Future: pODI and Plasmas 314 – Evolution of Galaxies Instrumentation 211 – Outer Limits of the Milky Way II: Star 315 – Ground Based, Airborne Observations 112 – The Secret Life of Globular Clusters Formation 316 – Instrumentation: Space Missions 113 – Supernovae and Their Diversity 212 – Computation as a Bridge between the 317 – Stellar Evolution 114 – Laboratory Astrophysics Laboratory and Astrophysics 318 – Galaxy Observations 115 – Binaries, Variable Stars and White 213 – The X-ray Background and the Cosmic 400 – Current Perspectives on the Spiral Dwarfs History of Black Hole Growth Structure of the Milky Way 116 – Stars, Stellar Evolution and 214 – WIYN Observatory - Building on the 401 – Bridging Laboratory and Astrophysics: Atmospheres, Circumstellar Disks Past, Looking to the Future Particles 117 – Young Stellar Objects, Star Formation, 215 – AGN, QSO, Blazars 402 – Instrumentation, Data Handling, Surveys and Star Clusters 216 – The ISM and Objects Therein 403 – Stellar Evolution and Binary Stars 118 – Supernovae and Supernova Remnants 217 – Extrasolar Planets & Tools 404 – The Bridged Gap: Transients in the 119 – Cosmology and Associated Topics 218 – Pulsars and Neutron Stars Local Universe 120 – Astronomy Education & Public 300 – The Latest Results from the NASA 101 – Kavli Foundation Lectureship: The Search for Habitable Worlds ultra-precise radial velocities needed for confirming and characterizing the planets with 101.01 – The Search for Habitable Worlds mass determinations. HARPS-N has recently come into operation at the Telescopio David W. Latham1 Nazionale Galileo on La Palma and is now contributing to the follow up of Kepler 1. Harvard-Smithsonian, CfA, Cambridge, MA, United States. candidates, but we need better ways to correct for astrophysical effects that distort the radial velocities, and still better velocity precision if we hope to reach the level of 9 cm/s We live at a very special time in the history of astronomy. We are poised to discover and induced by a true Earth twin in a one-year orbit around a star like the Sun. Kepler looks characterizes exoplanets enough like the Earth that we can imagine life as we know it at only one four hundreth of the sky. We need all-sky surveys for transiting planets to could arise and be comfortable. We are seeking rocky planets at the right distances from find the nearest and brightest examples for radial-velocity follow up and studies of their host stars for water to be liquid on the surface, and with a secondary atmosphere planetary atmospheres with missions like the James Webb Space Telescope and that might even show evidence for biogenic gases. Transiting planets are where the G-CLEF spectrograph on the Giant Magellan Telescope. Our long-range goal is to see if present action is, because they can provide masses and radii for planets, and thus the the atmospheres of any potentially habitable planets actually show evidence for biogenic bulk properties such as density and surface gravity that constrain our models of their gases that have been produced in large enough quantities to impact the biosphere and be interior structure and composition. Are they ice giants like Uranus and Neptune, or detected remotely. If we detect spectroscopic biomarkers that can only be present if rocky worlds like the terrestrial planets, or maybe something in between with lots of they are continually replenished by life, then we can point at that star and speculate that water or extended atmospheres of hydrogen and helium? NASA's Kepler mission has we may not be alone in the universe. provided lots of small planet candidates, but the bottleneck for characterizing them is the 102 – Bridging Laboratory and Astrophysics: Atoms which the intense x-ray flux emitted at the collapse of a z-pinch implosion conducted at 102.01 – Atomic Data Applications for Supernova the Z pulsed-power machine is employed to produce a neon photoionized plasma. The Modeling broadband x-ray radiation flux from the z-pinch is used to both create the photoionized Christopher J. Fontes1 plasma and provide a source of backlighting photons to study the atomic kinetics through K-shell line absorption spectroscopy. The plasma is contained in a cm-scale gas cell that 1. Los Alamos National Laboratory, Los Alamos, NM, United can be located at different distances from the z-pinch, thus effectively controlling the States. x-ray flux producing the plasma. Time-integrated and gated transmission spectra are The modeling of supernovae (SNe) incorporates a variety of disciplines, including recorded with a spectrometer equipped with two elliptically-bent KAP crystals and a set hydrodynamics, radiation transport, nuclear physics and atomic physics. These efforts of slits to record up to six spatially-resolved spectra per crystal in the same shot. The require numerical simulation of the final stages of a star's life, the supernova explosion transmission data shows a rich line absorption spectrum that spans over several phase, and the radiation that is subsequently emitted by the supernova remnant, which ionization stages of neon including Be-, Li-, He- and H-like ions. Modeling calculations can occur over a time span of tens of thousands of years. While there are several are used to interpret the transmission spectra recorded in the Z experiments with the different types of SNe, they all emit radiation in some form. The measurement and goal of extracting the charge- state distribution, electron temperature and the radiation interpretation of these spectra provide important information about the structure of the flux driving the plasma, as well as to determine the ionization parameter of the plasma. exploding star and the supernova engine. In this talk, the role of atomic data is This work is sponsored in part by the National Nuclear Security Administration under highlighted as iit pertains to the modeling of supernova spectra. Recent applications [1,2] the High Energy Density Laboratory Plasmas grant program through DOE Grant involve the Los Alamos OPLIB opacity database, which has been used to provide DE-FG52-09NA29551, and the Z Facility Fundamental Science Program of SNL. atomic opacities for modeling supernova plasmas under local thermodynamic equilibrium (LTE) conditions. Ongoing work includes the application of atomic data generated by the 102.03 – Spectroscopic Measurements of Collision-less Los Alamos suite of atomic physics codes under more complicated, non-LTE conditions Coupling Between Laser-Produced, Super-Alfvénic Debris [3]. As a specific, recent example, a portion of the x-ray spectrum produced by Tycho's Plasmas and Magnetized, Ambient Plasmas supernova remnant (SN 1572) will be discussed [4]. [1] C.L. Fryer et al, Astrophys. J. 1 1 1 707, 193 (2009). [2] C.L. Fryer et al, Astrophys. J. 725, 296 (2009). [3] C.J. Fontes et Anton Bondarenko , Erik Everson , Derek Schaeffer , Carmen al, Conference Proceedings for ICPEAC XXVII, J. of Phys: Conf. Series 388, 012022 Constantin1, Steve Vincena1, Bart Van Compernolle1, S. Eric (2012). [4] K.A. Eriksen et al, Presentation at the 2012 AAS Meeting (Austin, TX). 1 1 (This work was performed under the auspices of the U.S. Department of Energy by Clark , Christoph Niemann Los Alamos National Laboratory under Contract No. DE-AC52-06NA25396.) 1. Physics and Astronomy, University of California at Los Angeles, Los Angeles, CA, United States. 102.02 – Photoionized Plasmas in the Z Facility and in Emission spectroscopy is currently being utilized in order to assess collision-less Astrophysics momentum and energy coupling between super-Alfvénic debris plasmas and Roberto Mancini1 magnetized, ambient plasmas of astrophysical relevance. In a recent campaign on the 1. University of Nevada, Reno, Reno, NV, United States. Large Plasma Device (LAPD) utilizing the Phoenix laboratory