// Enter speaker information here. The format is:
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// ["Date","Name","Affiliation","Title","Abstract","Day","Time"]
//
// In the Abstract field you must escape double quotes (\"). Some HTML
// is possible (like <br>, <b>, etc.).
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// ** Edited to add color change for special day/time.
// ** If Day or Time field is not empty, special day/time
// ** is/are added in date column in red.
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// Note: the format is as follows:
//September[0] =["20" ,"Name","Institution","Title","Abstract","",""];
September[0] = ["22","Michael Fall","STSCI","Formation of the Hubble Sequence","This talk explains the formation of galaxies of different morphological types (aka the Hubble Sequence): spirals vs ellipticals, disks vs spheroids.  The talk includes theory, observation, and simulation, and is aimed at a general astrophysics audience.  Some highlights of the talk are the following: (1) The morphologies of galaxies are closely related to their specific angular momenta.  (2) Disk-dominated galaxies have about the same specific angular momenta as their dark-matter halos; spheroid-dominated galaxies have about five times less.  (3) Feedback by young stars (stellar radiation and winds, supernovae, etc) and active galactic nuclei is crucial for understanding the angular momenta of galaxies and hence their morphologies and hence the Hubble sequence. (4) The relations between the specific angular momenta and sizes of galaxies and their halos are nearly constant over the redshift range 0 < z < 3; galaxies and halos grow together nearly homologously.","",""];

September[1] = ["29","Dong Lai","Cornell","Chaotic Dances of Vectors: Misaligned Exoplanets, Disks/Rings and Planet IX","I will discuss several problems in (exo)planetary dynamics, all involving somewhat surprising behaviors of vectors tugging one another.  (1) Binary-disk-star interaction leading to the formation of misaligned protoplanetary disks; (2) Gentle gravitational purturbation from a binary companion on planets leading to the formation misaligned hot Jupiters; (3) Extented transiting disks and rings around exoplanets and brown dwarfs; (4) Hidding planets in multi-planet systems; (5) Solar obliquity induced by planet IX.","",""];

October[0]   = ["6","David Radice","IAS/Princeton","Turbulent Lives: Tales of Neutron Stars","Neutron stars live interesting and mysterious lives: from the moment they are created in core-collapse supernovae, to the moment some of them collapse to black-holes. In this talk, I will cover some aspects of their lives. I will discuss their birth in core-collapse supernovae, focusing on the key role of hydrodynamic turbulence in triggering the explosion. Then, I will talk about the ultimate fate of neutron stars born in close binaries. I will discuss the gravitational-wave emission during their last orbits and in the first milliseconds after merger. Finally, I will present results from recent studies of the neutron-rich outflows launched during neutron star mergers and discuss some of their implications for multimessenger astronomy and galactic chemical evolution.","",""];

October[1]   = ["13","Robert Penna","Columbia","The membrane paradigm and black hole astrophysics","The membrane paradigm gives an alternate description of black hole physics, in which the black hole is replaced by a fluid membrane living on the horizon.  In asymptotically flat spacetimes, the boundary at null infinity also has a membrane description.  I will explain how this reformulation is useful for understanding black hole astrophysics.  The universal scaling of black hole jet power with black hole spin, observed in GRMHD simulations, can be explained by a simple impedance matching argument between the membranes at the horizon and at infinity.  The membrane picture is also useful for understanding jet power from boosted black holes.  Finally, I will discuss the close relationship between the membrane paradigm and the Bondi-Metzner-Sachs (BMS) invariance of gravitational scattering.","",""];

October[2]   = ["20","Ra\xFAl Angulo","CEFCA","Simulating dark matter","Numerical simulations have played a crucial role in the development of modern cosmology and in the establishment of LCDM. In this talk, I will review the main results and the fundamental assumptions behind dark matter simulations. I will focus on the internal structure of halos and report on recent results on the formation and evolution of the very first halos to form in neutralino dark matter cosmologies. Then, I will discuss on attempts to model and study dark matter in the continuum limit. I will show how such methods help to overcome known problems of N-body simulations, and also how it is possible to get new insights into dark matter dynamics.","",""];

October[3]   = ["27","Jia Liu","Princeton","Large Scale Structure Cross-Correlations","","",""];

November[0]  = ["3","Jim Fuller","Caltech","Asteroseismology reveals strong magnetic fields in the cores of red giant stars","Internal stellar magnetic fields are inaccessible to direct observations and little is known about their amplitude, geometry and evolution. I will discuss how strong magnetic fields in the cores of red giant stars can be identified with asteroseismology. The fields manifest themselves via depressed dipole stellar oscillation modes, which arises from a magnetic greenhouse effect that scatters and traps oscillation mode energy within the core of the star. The Kepler satellite has already observed hundreds of red giants with depressed dipole modes, which may be stars with strongly magnetized cores. Field strengths larger than roughly 10^5 G can produce the observed depression, and in one case a core field strength of 10^7 G is inferred. Strong core fields may be present in roughly 50% of stars above 1.5 solar masses, suggesting that long-lived convective core dynamo-generated fields are common within these stars. Strong core fields are nearly absent in stars less than 1.2 solar masses, indicating that Sun-like stars do not harbor strong fields within their cores.","",""];

November[1]  = ["10","","","","","Seminar canceled",""];

November[2]  = ["17","Alexander Hubbard","AMNH","Chondrules: Constraining Protoplanetary Disks","While observations of extra-solar protoplanetary disks have been improving by leaps and bounds, they still cannot probe the early stages of planet formation. The best data we have for the sub-micron to cm phase of the planet formation process, which plays an essential role in setting the chemistry of terrestrial planets, is the meteoritical record itself. In particular the sub-mm melted glassy beads known as chondrules testify to the environment in which solids grew and were processed. I will give an overview of several interesting oddities in the meteoritical record which all point to a fundamental framework of vertically stratified protoplanetary disks; with chondrules melted in active, hot upper layers and planetesimals formed at the cool mid-plane.","",""];

November[3]  = ["24 (Thanksgiving)","","","","","No Seminar",""];

December[0]  = ["1","Adrian Price-Whelan","Princeton","Chaos, Stellar Streams, and the Galactic Bar","","",""];

December[1]  = ["8","Marilena Loverde","SUNY Stonybrook","Cosmic Neutrinos and Large-scale Structure","","",""];

December[2]  = ["15","Daniel Grin","Haverford","Perturbations are no spectator sport","I will give a tour through a variety of results on how precision cosmological data can test for the consequences of a light scalar in the early universe, such as an axion or a curvaton. Observable consequences could include altered CMB peak structure, suppressed matter power on small scales, and isocurvature perbturbations. I'll discuss constraints from Planck and WiggleZ, the prospects for a future CMB-S4 type experiment. I will conclude with a snapshot of ongoing work with undergraduate students at Haverford college, including work to forecast the prospects of large galaxy surveys for constraining axions, and separate work to improve the treatment of axion perturbation evolution in cosmological Boltzmann codes.","",""];