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January[0] =["8","Maxwell Moe","Harvard","The All-Sky Automated Survey for Supernovae (ASAS-SN): Big Science with Small Telescopes","","",""];
January[1] =["15" ,"Jeffrey Fung","Toronto","Disk-Planet Interaction: From 2D to 3D","","",""];
January[2] =["22" ,"Daniel Foreman-Mackey","NYU","Inferring the Population of Exoplanets from Noisy, Incomplete Catalogs","","",""];
January[3] =["29" ,"Francesca Valsecchi","Northwestern","Stellar Tides As a Probe of Hot Jupiters’ Origin and Fate","Hot Jupiters constitute one of the many surprises of Exoplanet searches. Their tight, few-day orbits make them a challenge for commonly invoked planet formation scenarios and correspond to the onset of strong tidal dissipation. Hot Jupiters could have migrated inward in a disk, or they could have formed via tidal circularization of an orbit made highly eccentric following gravitational interactions with a companion. I will show how current observations coupled with a detailed treatment of tides can be used to constrain both hot Jupiter formation and tidal dissipation theories. Eventually, stellar tides will cause the orbits of many gas giants to decay down to their Roche limit. I will show how a hot Jupiter undergoing a phase of Roche-lobe overflow can lead to a hot super-Earth- or sub-Neptune-size planet. If correct, these results suggest that many Jovian planets have rocky cores that can now be studied directly. ","",""];
February[0]=["5" ,"Kengo Tomida","Princeton","Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Non-Ideal Magnetohydrodynamic Effects and Early Formation of Circumstellar Disks","The transport of angular momentum by magnetic fields is a crucial physical process in formation and evolution of stars and disks. Because the ionization degree in star forming clouds is extremely low, non-ideal magnetohydrodynamic (MHD) effects such as ambipolar diffusion and Ohmic dissipation work strongly during protostellar collapse. These effects have significant impacts in the early phase of star formation as they redistribute magnetic flux and suppress angular momentum transport by magnetic fields. We perform three-dimensional nested-grid radiation magnetohydrodynamic (RMHD) simulations including Ohmic dissipation and ambipolar diffusion. Without these effects, magnetic fields transport angular momentum so efficiently that no rotationally supported disk is formed even after the second collapse. Ohmic dissipation works only in a relatively high density region within the first core and suppresses angular momentum transport, enabling formation of a very small rotationally supported disk after the second collapse. With both Ohmic dissipation and ambipolar diffusion, these effects work effectively in almost the entire region within the first core and significant magnetic flux loss occurs. As a result, a rotationally supported disk is formed even before a protostellar core forms. The size of the disk is still small, about 5 AU at the end of the first core phase, but this disk will grow later as gas accretion continues. Thus the non-ideal MHD effects can resolve the so-called magnetic braking catastrophe while maintaining the disk size small in the early phase, which is implied from recent interferometric observations.","",""];
February[1]=["12" ,"James Owen","IAS","Astrophysical models for cosmochemical problems","I will discuss two cases where models of protoplanetary discs developed for astrophysical application can help understand problems in cosmochemistry. In the first I will show how accretion bursts through the gravo-magnetic limit cycle can control the D/H ratio in water. The bursts can thermally process a large fraction of water in the disc allowing isotopic exchange with Hydrogen at high temperatures. This processed water can then be transported to small radii by advection and larger radii by diffusion. Allowing the observed D/H water ratio distribution in the solar system to be qualitatively explained. Secondly, I will discuss models which aim to investigate the transport of the components of meteorites, using the constrains on the chemical composition of these components we can track the time and location of formation.","",""];
February[2]=["19","Daniel Jacobs","ASU","Chasing our Cosmic Dawn: Opening the 21cm cosmological window on the universe","The Epoch of Reionization (EoR) marks when the first stars ionized the primordial hydrogen half a billion years after the big bang.  Direct observation of cosmological hydrogen is possible via the 21cm line and is now being hotly pursued as a new cosmological probe. Danny Jacobs is helping to lead observations with both the Precision Array for Probing the Epoch of Reionization (PAPER) and the Murchison Widefield Array (MWA). PAPER currently holds the deepest limits on the epoch of reionization power spectrum, while the MWA is leading the charge towards understanding foregrounds at a level necessary for imaging large scale structure. The two intertwined themes in these new instruments are the degree to which experimentation is an essential component of the science process and the ascendance of the software pipeline. Experiments currently under-way to refine array sensitivity include high-bandwidth forward-modeling of instrumental response, developing high level heuristics for data flagging, accelerating imaging pipelines, pushing more analysis steps into real-time systems, and in-situ calibration with external drone-mounted transmitters. Lessons learned and systems developed for PAPER and the MWA are being incorporated into the next generation Hydrogen Epoch of Reionization Array (HERA) that will yield 20 times the sensitivity of first generation arrays, and into the upcoming Square Kilometer Array. ","",""];
February[3]=["26","Neal Dalal","University of Illinois at Urbana-Champaign","Structure formation with fast particles","","",""];
March[0]   =["5" ,"Jon Blazek","OSU","Galaxy intrinsic alignments and precision cosmology","The relationship between large-scale struture and the intrinsic shapes of galaxies is an important element of observational cosmology. These intrinsic alignments (IA) are the most significant source of astrophysical uncertainty in weak lensing measurements and must be understood if current and upcoming lensing surveys are to reach their full potential. I will present recent developments in understanding IA, including a model based on galaxy alignment with the tidal field. I will discuss efforts to probe IA through observation and simulation. I will show estimates of IA contamination in future lensing surveys and discuss our ability to remove it. Beyond its presence as a systematic uncertainty, IA can be a powerful probe of large-scale structure as well as the formation and evolution of galaxies and dark matter halos.","",""];
March[1]   =["12" ,"Marko Simonovic","IAS","B-mode cosmology","","",""];
March[2]   =["19","Philip Chang","UWM","The Physics and Cosmology of TeV Blazars","The universe is teeming with very high energy gamma ray sources (> 100 GeV), but it is generally thought that their impact on the universe is minor at best. On energetic grounds, this assumption seems well-founded because the energy density in TeV photons is 0.2% of that of ionizing photons from quasars.  However, as I hope to show in this talk, this is not the case. Rather, the greater efficiency by which TeV photons can be converted to heating in the intergalactic medium (IGM) allows TeV blazars dominate the heating of the IGM at low redshift.  I will discuss the nature of this conversion via beam instabilities.  I will then discuss how the resultant heating from these TeV sources makes dramatic differences in the formation of structure in the universe and the implications of these beam instabilities on the redshift evolution of TeV blazars.  I will also discuss how it gives rise to the inverted temperature-density profile of the IGM, the bimodality of galaxy clusters, and the paucity of dwarf galaxies in galactic halos and voids.","",""];
March[3]   =["26","Matthew Hasselfield","Princeton","The Atacama Cosmology Telescope: Recent results and future prospects","","",""];
April[0]   =["2" ,"Til Birnstiel","CfA","Early Stages of Planet Formation - Bridging Theory and Observations","Planets are formed out of sub-micrometer sized solid particles that orbit young stars in their accretion disks. The growth of these particles, their transport, and the structure and dynamics of the gaseous accretion disk are tightly interlinked. Dust continuum emission provides a powerful tracer of the dynamical processes that drive disk evolution and dispersal. The size evolution of solids is an important piece of this physical puzzle that is often left out for convenience. In this talk, I will present our recent efforts to probe the physical structure of disks and their evolution by comparing detailed physical models of growth and transport of solids to current resolved and unresolved observations.","",""];
April[1]   =["8","Andrei Beloborodov","Columbia","Mechanism of magnetar activity","","Wednesday","11:00am"];
April[2]   =["16","Eli Waxman","Weizmann"," IceCube and the future of HE neutrino astronomy","","",""]; 
April[3]   =["28","Alex Geringer-Sameth","CMU","A search for dark matter annihilation in the newly discovered dwarf galaxy Reticulum 2","I will present results from a search for gamma-ray emission in nine Milky Way satellites recently discovered in the Dark Energy Survey. The nearest of these, Reticulum 2, shows evidence for a signal in public Fermi data. The detected emission is consistent with annihilating dark matter with a particle mass less than a few hundred GeV. Different ways of treating the background yield different significances -- ranging from 2.3 sigma to greater than 3.7 sigma (after trials) -- and I will discuss the caveats involved. Spectroscopic observations of member stars are used to infer the density profile of Reticulum 2, showing that its annihilation signal should be among the largest of the known dwarfs. Finally, I will discuss tests that a dark matter interpretation must pass. ","Tuesday","2:00pm"];
April[4]   =["30","Chang-Goo Kim","Princeton","Feedback Regulated Turbulence, Magnetic Fields, and Star Formation Rates in Galactic Disks","We use local three-dimensional magnetohydrodynamic simulations to investigate the quasi-equilibrium states of galactic disks regulated by star formation feedback. We incorporate effects from massive-star feedback via time-varying heating rates and supernova (SN) explosions. We find that the ISM disks in our simulations rapidly approach a quasi-steady state that satisfies vertical dynamical equilibrium. The SFR surface density self-adjusts to provide the total momentum flux (pressure) in the vertical direction that matches the weight of the gas. The final (time-averaged) state is insensitive to initial conditions and vertical boundary conditions. We quantify feedback efficiency by measuring ``feedback yields’’ defined by the ratio between different pressure components and the SFR surface density. For both magnetized and unmagnetized models, the turbulent and thermal yields are the same. In magnetized models, turbulent magnetic fields are rapidly generated by the small-scale turbulence dynamo, and saturate at a level corresponding to the equipartition with the turbulent kinetic energy. The presence of magnetic fields enhances the total feedback yield and therefore reduces the SFR, since the same vertical support can be supplied at a smaller SFR. Since additional vertical support can be provided by mean magnetic fields in the azimuthal direction, the SFRs are even more reduced in strongly magnetized models.","",""];
May[0]     =["7" ,"Christopher Hirata","OSU","Circular polarization of redshifted 21 cm radiation: Another futuristic idea for detecting primordial gravitational waves.","","",""];
May[1]     =["14","Jenny Greene","Princeton","MASSIVE Galaxies and Small Supermassive Black Holes","","",""];
May[2]     =["21","Kaitlin Kratter","Arizona","What we can learn from planets in binary systems","","",""];