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// ["Date","Name","Affiliation","Title","Abstract"]
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September[0]=["11","Lars Bildsten","KITP","Faint Ia Supernovae from Ultracompact Binaries","","",""];
September[1]=["18","Nima Arkani-Hamed","Harvard/IAS","Physics, Cosmology and the Large Hadron Collider","","",""];
September[2]=["25","Re'em Sari","Caltech","Binaries, Rubble-Piles and Tidal Evolution","","",""];


October[0]=["2","Andrei Gruzinov","NYU","Pulsar Theory","","",""];
October[1]=["9","Shri Kulkarni","Caltech","An explosion of explosions","","",""];
October[2]=["16","Avi Loeb","Harvard","Three Astrophysical Laboratories for Particle Physics","The Universe offers environments with extreme physical conditions that cannot be realized in laboratories on Earth. These environments provide unprecedented tests for extensions of the Standard Model.  I will describe three such \"astrophysical laboratories\", which are likely to represent new frontiers in cosmology and astrophysics over the next decade. One provides a novel probe of the initial conditions from inflation and the nature of the dark matter, based on 3D mapping of the distribution of cosmic hydrogen through its resonant 21cm line. The second allows to constrain the metric around supermassive black holes based on direct imaging or the detection of gravitational waves. The third involves the acceleration of high-energy particles in cosmological shock waves.  I will describe past and future observations of these environments and some related theoretical work.","",""];
October[3]=["23","Alice Shapley","Princeton","The Metallicities and Physical Conditions in Star-forming Galaxies at High-Redshift","The abundance of heavy elements in the ISM of star-forming galaxies represents a fundamental metric of the galaxy formation process. This metallicity reflects the gas reprocessed by stars, and the metals returned to the ISM by supernova explosions. Furthermore, galaxies display universal correlations among luminosity, stellar mass, and metallicity.  The form and evolution of these correlations as a function of redshift lend insight into the infall and outflow of gas in galaxies as they build up their stellar populations, and provide important constraints on the nature of star-formation \"feedback,\" a crucial ingredient in models of galaxy formation. Here we present evidence, based on rest-frame optical spectroscopy of galaxies at z~1.0-2.5, that the physical conditions in star-forming regions at high redshift are qualitatively different from those in the local universe. These differences have implications for understanding galaxy metallicities and, perhaps more fundamentally, star formation, itself, during an important epoch when the properties of today's galaxy population were still in the process of coming into place.","",""];
October[4]=["30","Felix Aharonian","MPIK","Very High Energy Gamma-Ray Sources","","Canceled",""];


November[0]=["6","Andy Gould","Ohio State","Degeneracy and Confidence in Planetary Microlensing","When microlensing planet searches were proposed, it was expected that only one physical parameter of the system could be accurately measured: the planet/star mass ratio.  15 years and 7 planet detections later, we have often been able to measure the planet mass, the distance and transverse velocity of the system, the planet-star projected separation, and even in some cases, orbital properties.  The additional information is teased out of higher-order effects, often in the face of a bewildering proliferation of model degeneracies.  I analyze the physical origin of these higer-order effects and the degeneracies they bring with them, and discuss how modelers are overcoming these obstacles to derive new types of information about extrasolar planets.","",""];
November[1]=["13","Edmund Bertschinger","MIT","Spiral Waves in Accretion Disks","The X-ray flux of accreting black holes occasionally shows a pair of quasi-periodic oscillations with frequencies in a 3:2 ratio having values comparable to the orbital frequency at the innermost stable circular orbit.  The cause and nature of these oscillations is not understood.  One proposed explanation is that they are caused by waves in the accretion disk.  For a thin disk, the matter can be approximated as a cold collisionless fluid provided that orbits to not intersect.  Long-lived perturbations can exist only where the pattern speed is approximately a constant, independent of radius.  The resulting waves are analogous to the Lindblad-Kalnajs kinematic density waves in galactic disks.  In the case of black holes, while several pairs of modes have frequencies close to a 3:2 ratio, the predicted frequencies are either too high or too low by about a factor of two to explain the observed oscillations.  Thus an alternative explanation, perhaps involving parametric resonance, is required to explain the X-ray oscillations of accreting black holes.","",""];
November[2]=["27","Bill Matthaeus","Univ. of Delaware","MHD Turbulence and Some of Its Effects in the Solar Wind","","",""];


December[0]=["4","Alessandro Morbidelli","CNRS, France","Crucial dynamical phases in solar system formation","The formation and evolution of the giant planets of our Solar System presents several problems: the cores of the planets should have been driven into the Sun by Type I migration, faster than they could accrete their massive gaseous atmosphere; once formed, Jupiter and Saturn should have suffered Type-II migration towards the Sun, becoming hot or warm giants, like most of the extra-solar planets known so far; the planets most likely underwent a late reorganization of their orbital architecture, as indicated by the Late Heavy Bombardment (LHB) of the Moon, which suggests that a massive reservoir of small bodies suddenly became unstable.<br>Without pretension of providing any definitive answer, I will present a scenario of the formation and evolution of the giant planets that addresses these problems. More specifically I will present simulations of the dynamics of planetary cores in the vicinity of a 'planet trap', which can exist at the transition between the active and the dead zones of the disk. I will illustrate how the dynamics of the fully formed planets in the gas disk leads to one of 6 possible mutual configurations, that are stable and avoid significant migration towards the Sun. Finally I will describe our model for the origin of the LHB and how it connects with some of these mutual stable configurations.","",""];
December[1]=["11","Bhuvnesh Jain","UPenn","Testing Gravity Theories with Lensing and Other Large-Scale Probes","","",""];