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January[0]=["14","Wick Haxton","Berkeley","Solar Chemical Anomalies and Late Accretion","One of the last problems that John Bahcall considered was the solar abundance problem, the conflict between helioseismology, which indicates a high-metallicity solar core, and improved analyses of photospheric absorption lines, which favor a low surface metallicity. I will present some qualitative arguments to show that the metal segregation accompanying planetary formation is sufficient to account for both results, and some quantitative ones that suggest that it may be difficult to identify a specific low-metallicity accretion scenario capable of accommodating all of the data. I will describe a solar neutrino experiment that could help us make progress, allowing us to directly determine components of the Sun's core metallicity.","",""];

January[1]=["21","Ray Carlberg","U Toronto","Gaps in Galactic Stellar Streams","The LCDM paradigm predicts that the Milky Way dark halo has nearly 10% of its mass in the form of thousands of sub-halos, far more than can be accounted for with the known dwarf galaxies.  Globular clusters dissolving in the tidal field of the galaxy create long, thin stellar stream. Sub-halos that orbit through a stream will create a density gap in the stream. The visibility of the gap depends on the stream dynamics and the size of the sub-halo.  Observers have noted that star streams have significant density variations along their length. The degree to which the observed stream density variations may be quantitatively consistent with the presence of a rich dark matter sub-halo population is considered.","",""];

January[2]=["28","Nick Scoville","Caltech","ALMA Observations of Galaxy Evolution and Nuclear Activity","In the COSMOS survey we have now imaged the large scale structures out to redshift 3 using 200,000 galaxies with precision photometric redshifts. The evolution of the galaxies, their stellar masses and star formation activity is found to be strongly differentiated by environment. ALMA observations now also reveal strong evolution in the ISM masses as a function of redshift using a sample of 110 galaxies at z = 0.3 to 3. I also describe ALMA observations and theoretical work on ultra-luminous IR galaxies to determine the levels of starburst and AGN activities.","",""];

February[0]=["4","Paul Steinhardt","Princeton","","","",""];

February[1]=["11","Mark Phillips","Carnegie","On the Source of the Dust Extinction in Type Ia Supernovae","Echelle observations can be used as an independent means of probing the dust extinction of SNe Ia. I show that the extinction of the objects where the diffuse interstellar band at 5780 Angstroms is detected is consistent with the visual extinction derived from the supernova colors. This strongly suggests that the dust is predominantly located in the interstellar medium of the host galaxies and not in circumstellar material associated with the progenitor system. However, the echelle spectra also reveal that one quarter of the supernovae display anomalously large Na I column densities in comparison to the amount of dust extinction derived from their colors. Remarkably, all of the cases of unusually strong Na I D absorption correspond to Blueshifted profiles in the classification scheme of Sternberg et al. (2011). This coincidence suggests that outflowing circumstellar gas is responsible for at least some of the cases of anomalously large Na I column densities.","",""];

February[2]=["18","Ethan Vishniac","University of Saskatchewan","Driving the Dynamo Via Magnetic Helicity Flux: How Differential Rotation Makes Large Scale Magnetic Fields.","Large scale magnetic fields are found everywhere in the universe, from the scales of planets to galactic disks (or larger). Understanding their generation and maintenance has proven to be unexpectedly difficult.  I will discuss topological constraints on the growth of such fields, and argue that they are inconsistent with kinematic dynamo theory.  Instead, I propose a modified version of mean field dynamo theory in which field growth is not exponential, but can grow from infinitestimal seeds in a very short time.  I compare the predictions of the model to observations of stellar magnetic fields.","",""];

February[3]=["25","Mark Devlin","U Penn","Studying the Largest Objects in the Universe Undergoing the the Most Energetic Collisions in the Universe with the World's Biggest (moveable) Telescope","Clusters of Galaxies are the largest gravitationally-bound objects in the Universe.  They form via mergers with energetics that are only rivaled by the Big Bang.  The study of these objects and collisions can reveal the complex processes that govern the interactions. Observations at 90 GHz with the MUSTANG instrument on the GBT provide high (9 arcsec) resolution of the Sunyaev-Zel'dovich effect inside the clusters. Initial observations with the MUSTANG instrument have yielded very promising observations of a few clusters.    We are now in the midst of an upgrade which will allow us to observe hundreds of clusters (assuming we can keep the GBT open!).","",""];

March[0]=["4","Daisuke Nagai","Yale","Cosmology and Astrophysics with Galaxy Clusters","Galaxy clusters are among the largest gravitationally bound objects in the universe, whose formation is driven by dark energy and dark matter. The majority of the baryonic mass in clusters resides in the hot X-ray emitting plasma, which also leaves imprints in the cosmic microwave background radiation. Recent X-ray and microwave observations have revealed detailed thermodynamic structure of the hot X-ray emitting plasma from their cores to the virial radii, making comparisons of baryonic component in simulations to observations a strong cosmological probe. In this talk, I will review recent advances in our understanding of cluster astrophysics and discuss future prospects, opportunities and challenges for the use of galaxy clusters as a precision cosmological probe.","",""];

March[1]=["11","Peter Meszaros","Penn State","Gamma-ray Bursts: the standard model and beyond","I will review the recent ultra-bright GRB 130427A data and the puzzles (as well as non-puzzles) raised by its intepretation both in terms of the standard model and in terms of previous plausible extensions of this model. I then discuss the implications of the Icecube TeV neutrino non-detection of either this particular burst nor, so far, of the expected cumulative diffuse flux from many bursts, in terms of the standard model and the extended-standard model of the prompt emission, including photospheric and hadronic models. This is followed by a general discussion of the physics and issues behind the introduction of such extensions of the model, which have been motivated by the need to address the prompt gamma-ray spectra.","",""];

March[2]=["18","Daniel Eisenstein","Harvard","Measuring the Cosmic Distance Scale with SDSS-III","I will discuss how sound waves racing through the cosmos during the first million years of the Universe provide a robust method for measuring the low-redshift cosmological distance scale and thereby the properties of dark energy.  The distance that the sound can travel can be computed to high precision and creates a signature in the late-time clustering of matter that serves as a standard ruler.  Galaxy clustering results from the Sloan Digital Sky Survey and SDSS-III reveal this feature and allow us to measure distances to high accuracy, including a new 1% measurement to z=0.57.","",""];

March[3]=["25","Eli Waxman","Weizmann","IceCube's neutrinos: A new era in neutrino and cosmic-ray astrophysic","","",""];

April[0]=["1","Bhuvnesh Jain","U Penn","Lensing by Galaxies, Filaments and Voids","","",""];

April[1]=["8","Meg Urry","Yale University","Galaxy Evolution and the Growth of Supermassive Black Holes","Multiwavelength surveys like GOODS and COSMOS indicate that most actively growing black holes are heavily obscured, and this fraction increases in the young Universe and in lower luminosity AGN. Most black holes grow in moderate luminosity AGN, which dominate the X-ray .background,. rather than in luminous quasars. In the peak epoch of black hole growth, at z~1-3, such AGN are hosted in galaxies with significant disks, and thus cannot have undergone a recent major merger. Using morphological classifications from Galaxy Zoo (at z~0), we identify two distinct modes of galaxy evolution, with mergers and AGN feedback affecting only a minority.","",""];

April[2]=["15","Richard Ellis","Caltech","Observations of Star Forming Galaxies in the Heart of the Reionization Era","Deep exposures with the Hubble Space Telescope (HST) have provided the primary evidence that star-forming galaxies were present in the first billion years of cosmic history. Sometime during this early period the intergalactic medium transitioned from a neutral gas to one that is fully ionized. How did this `cosmic reionization' occur and were star-forming galaxies responsible? The electron scattering optical depth inferred from cosmic microwave background observations suggests that reionization occurred sometime in the redshift interval z=20 to z=6 so probing the abundance, luminosity distribution and spectral properties of galaxies during this uncharted period holds the key to addressing these fundamental questions. Recent imaging with HST's Wide Field Camera 3 in conjunction with Spitzer photometry and Keck spectroscopy has provided important new insight into understanding when reionization occurred and the role of early galaxies in the process.  I will review this progress and discuss the remaining challenges ahead of future facilities such as TMT and JWST.","",""];

April[3]=["22","Pavel Kroupa","Bonn","The Vast Polar Structures Around the Milky Way and Andromeda, and the Implications Thereof for Fundamental Physics","The current cosmological model rests on Einstein's theory of general relativity. In order for it to be consistent with large-scale structure data, the existence of cosmologically relevant physical processes need to be postulated: inflation, cold or warm dark matter particles and dark energy. Each of these is not well understood, but assuming the resulting standard mathematical description is a representation of cosmological reality, this representation can be tested in a different regime, namely on the scales of the Local Volume of galaxies down to individual galaxies. It is found that each test which has been designed shows the standard description to fail such that the currently standard model of cosmology is difficult to be upheld. In particular, the Dual-Dwarf-Galaxy Theorem, which must be true in the standard model, is falsified. The arrangement of satellite galaxies in rotating disk-like vast near-polar structures around both, the Milky Way and Andromeda, support this conclusion. As suggested by Milgrom, scale-invariant dynamics may be showing a new direction for the understanding of the astrophysics of galaxies. A successful final description of cosmology is yet to be found though.","",""];

April[4]=["29","Joshua A Frieman","Fermilab","Probing Cosmic Acceleration with the Dark Energy Survey","The Nobel Prize in Physics for 2011 was awarded for the discovery that the expansion of the Universe is accelerating. Yet the physical origin of cosmic acceleration remains a mystery. The Dark Energy Survey (DES) aims to address the questions: why is the expansion speeding up? Is cosmic acceleration due to dark energy or does it require a modification of General Relativity? If dark energy, is it the energy density of the vacuum (Einstein's cosmological constant) or something else? DES is addressing these questions by measuring the history of cosmic expansion and of the growth of structure through four complementary techniques: galaxy clusters, the large-scale galaxy distribution, weak gravitational lensing, and supernovae. The DES collaboration has built a new, 570-megapixel, digital camera for the Blanco 4-meter telescope at Cerro Tololo Inter-American Observatory in Chile to carry out a deep, wide-area sky survey of 300 million galaxies and a time-domain survey that will discover 3500 supernovae over 525 nights. I will overview the DES project, which achieved `first light' in September 2012 and which just finished its first survey season in early February 2014, and describe early science results.","",""];

May[0]=["6","Matt Holman","CfA","Confirming and Constraining Kepler Planets via Transit Timing Variations","Of the Kepler planets that have been reported to date, a significant fraction are in systems with multiple transiting planet.  In some cases, the signature of the gravitational interactions between planets in these systems can be seen in the variations of their times of transit. By carefully modeling the transit times, as well as investigating long-term stability, we are able to measure or constrain the masses and orbits of the transiting bodies in some of these systems, verifying that they are indeed planets. Although this approach is particularly effective for closely packed and near-resonant systems, it has also been applied to a broad range of systems. These include circumbinary planets, as well as systems with additional non-transiting planets. I review the process of using transit timing variations to confirm Kepler planets, highlighting some examples of dynamically interesting systems.","",""];

May[1]=["13","Shlomi Kotler","NIST","Quantum Information in experiments: there and back again","The field of experimental quantum information started with the first realization of an entangling gate in 1995. Tools originally developed for precision spectroscopy, turned out extremely useful for generating Bell pairs and storing quantum superposition states for seconds. At the level of very few quantum bits, we can quantum compute. A real large-scale quantum computer, however, is nowhere near to be found. We do not know how to scale the very few to the tens and hundreds. Yet.","",""];


September[0]=["16","Nir Shaviv","University of Jerusalem/IAS","Various aspects of the MW disk’s vertical structure","","",""];
September[1]=["23","David Eichler","Ben Gurion University","Gamma Ray Bursts from a Different Angle: The Sequel","A classic problem posed by long gamma ray bursts (GRB) is that the energy output requires  gravitational energy release so deep within the host star that the prompt gamma rays should, upon naive consideration, have been obscured. It is suggested that photons emitted along the direction of the emitting plasma's motion are indeed  geometrically blocked by optically thick baryonic matter, and that we usually see the photons that are emitted nearly backward in the frame of the emitting plasma.  Many puzzling observations concerning GRB then fall into place.","",""];
September[2]=["30","Mansi Kasliwal","Caltech","See the Sound: Transients in the Local Universe","The advent of wide-field synoptic imaging has re-invigorated the venerable field of time domain astronomy. Our framework of optical transients no longer has a wide six-magnitude luminosity gap between the brightest novae and faintest supernovae. Multiple new and distinct classes of very rare explosions have been uncovered just in the past few years. I review the surge of excitement (and debate) on the physics of these transients with unprecedented explosion signatures. Gap transients represent missing pieces in two fundamental pictures: the fate of massive stars and the evolution of compact binaries. Calcium-rich gap transients may even be the key to solving a long standing abundance problem in the intra-cluster medium. Two classes of gap transients are extremely red motivating a systematic exploration of the dynamic infrared dynamic sky. I will present new, mysterious discoveries of infrared transients from a Spitzer search that just began called SPIRITS. I will conclude with the next frontier in gap transients - discovering elusive binary neutron star mergers, a goal which may soon be within reach with coordination between the next generation Zwicky Transient Facility and advanced gravitational wave interferometers. This search may literally be the 21st century gold rush!","",""];

October[0]=["7","Bruce Draine","Princeton University","Andromeda's Dust","Infrared observations from Spitzer Space Telescope and Herschel Space Observatory are used to study the interstellar dust in M31.  A physical dust model is used to map the dust surface density, dust/gas ratio, starlight heating intensity, and the PAH abundance, out to R=25 kpc from the center of M31. The dust/gas ratio declines smoothly with increasing galactocentric radius, decreasing by almost a factor of ten from R=0 to R=20 kpc, following the metallicity of the gas. The dust serves as a photometer to measure the intensity of the starlight heating the dust.  Within the central kpc the starlight intensity estimated from the observed dust SED is in good agreement with the directly-observed bulge starlight -- a validation of the dust model. The dust model predicts the extinction through the disk. Nature has kindly placed an AGN behind the dusty disk of M31. Dust-scattered X-ray photons from this AGN could be used to get a geometric distance to M31.","",""];
October[1]=["14","Dragan Huterer","University of Michigan","How to Falsify a Dark Energy Paradigm","The physical mechanism behind the acceleration of the universe remains one of the great mysteries of modern cosmology. Given the proliferation of dark energy models on the market, an obvious question is: How can we rule out whole classes of dark energy models?  And what quantities, at what redshift, and with what accuracy, should be measured in order to rule out these classes of models? I present answers to these questions by presenting results from several interrelated analyses whose motivation is to compare the geometrical quantities with the growth of structure using current or future cosmological observations.","",""];
October[2]=["21","Eric Blackman","Rochester","Explaining the Stellar Magnetic Activity-Rotation Relation: A Context for Some Broadly Applicable Principles","X-ray luminosity in low mass stars has long been recognized as a signature of coronal magnetic activity.  Understanding such activity and its evolution as a function of rotation and  field strength is of broad interest for the connection of these features to basic stellar evolution and structure, as a potential  tracer of stellar age, and even potential consequences for habitability.   A particularly long-standing observation that has not yet  been explained is the curious dependence of stellar X-ray luminosity  on rotation:  For slow rotators, the X-ray to bolometric luminosity increases strongly with rotation, whereas for fast rotators, this ratio is nearly independent of rotation. Why?  Since magnetic activity depends on the generation of magnetic fields from dynamos, we must look at what has missing from previous attempts to associate of the two. I will suggest how the incorporation of two missing physical concepts, even in simple models, looks promising in the effort to explain the aforementioned observational puzzle. I hope give a flavor for the diversity, richness, and opportunities in the overall subject, but also highlight a few take-away physical ideas.","",""];
October[3]=["28","Rachel Mandelbaum","Carnegie Mellon Univeristy","Intrinsic galaxy alignments and the cosmic web","Intrinsic alignments of galaxy shapes with cosmological large-scale structure include a great deal of information about galaxy formation and evolution in a cosmological context, while also serving as a contaminant to weak gravitational lensing measurements (which assume that all coherent galaxy alignments are due to gravitational lensing).  In this talk, I will discuss recent progress in our understanding of galaxy intrinsic alignments on both the observational side and the computational side, using SDSS-III BOSS data and SPH simulations, respectively.  Recent work using massive BOSS galaxies has permitted a study of how galaxy intrinsic alignments vary from small scales (within massive halos) to cosmological scales, and how the level of the alignments scales with the galaxy environment (for brightest group galaxies, satellites in groups, and field galaxies).  Among these new observational results is the fact that the level of small-scale alignments (<1 Mpc/h) correlates more tightly with the large-scale galaxy bias (from >10 Mpc/h) than with the galaxy luminosity.  On the computational side, high-resolution SPH simulations with 100 Mpc/h box sizes are able to make predictions for how galaxy intrinsic alignments scale with galaxy properties, as well as to make verifiable predictions for the intrinsic alignment 2-point correlation functions of massive galaxies that are observed by existing galaxy redshift surveys.  I will discuss challenges for using and interpreting simulated intrinsic alignment signals, and the latest results for their comparison with observations, as well as the implications for future weak lensing surveys.","",""];

November[0]=["4","Rachel Somerville","Rutgers","Think Globally, Act Locally: Physical Models of Galaxy Formation in a Cosmological Framework","Galaxies mark the nexus between the micro scales of individual stars and black holes, and the macro scales of the cosmic web, the large scale structure in which galaxies are embedded. Modeling the physics of galaxy formation is therefore one of the greatest challenges in astrophysics today because of the enormous range of scales involved and the diversity of physical processes that are important. However, models have made enormous progress in the past few years towards explaining a variety of observations and identifying a set of essential physical processes that shape the observable properties of galaxies. I will review the successes and some of the failures of state-of-the-art cosmological models of galaxy formation when confronted with an array of observations and discuss what we have learned from these results about the physics that drive galaxy evolution. I will focus on understanding the link between the structural and morphological properties of galaxies and their formation histories.","",""];
November[1]=["11","Rashid Sunayev","MPA Munich / Space Research Institute Moscow / IAS","Two milestones in the history of the Universe: last scattering surface and black body photosphere of the Universe. Unavoidable spectral distortions of the CMB.","Hydrogen recombination at redshifts  z ~ 1100 - 1500 leads to a rapid decrease of the optical depth due to Thomson scattering. As a result the CMB photons, previously strongly coupled with baryonic matter, become free and can reach us. The observed acoustic peaks in the CMB angular distribution and the shape of BAOs are formed in the vicinity of the last scattering surface.<br> The question remains how and at which redshifts the observed practically ideal black body spectrum of the CMB was formed. Why do we hope that proposed space missions like PIXIE will be able to detect traces of any significant energy release in our Universe at redshifts smaller than 2 million? Why can the spectral distortions not originate behind the black body photosphere or at redshifts higher than 2 million?<br> I plan to describe the nature of the black body photosphere of the Universe, the physical processes leading to the formation of characteristic spectral distortions of CMB and to discuss in detail the unavoidable spectral distortions of CMB due to cosmological recombination, Silk damping and presence of hot gas in the early Universe. It will be mentioned why we will never observe the traces of electron-positron annihilation in the early Universe or due to decay of tritium and conversion of Be-7 to Li-7 at z ~ 30000 in the spectrum of the CMB.","",""];
November[2]=["18","Dave Charbonneau","Harvard/CfA","The Compositions of Small Planets","The NASA Kepler Mission has demonstrated that planets with radii larger than Earth yet smaller than Neptune are common around Sun-like stars. Although Kepler has determined the physical sizes of hundreds of such planets, we know virtually nothing about their masses and, by inference, their compositions. HARPS-N is an ultra-stable fiber-fed high-resolution spectrograph optimized for the measurement of very precise radial velocities. Using HARPS-N we have measured to high precision the masses of several of these so-called super-Earths. I will report on the resulting constraints on the planetary compositions, and address the transition from rocky planets, composed of rock and iron, and Neptune-like worlds, which have accreted and retained an envelope of primordial H/He gas. I will then explain the future role of the NASA Transiting Exoplanet Survey Satellite (TESS), scheduled for launch in 2017.","",""];
November[3]=["25","Catherine Espaillat","Boston University","Tracking Planet Footprints in Dusty Disks","We know that most stars, if not all, were once surrounded by protoplanetary disks.  How these young disks evolve into planetary systems is a fundamental question in astronomy. Observations of T Tauri stars (TTS) may provide insights into this question, particularly a subset of TTS with transitional disks. The spectral energy distributions of these objects feature an infrared dip, indicating that they have developed holes or gaps in their dust disk. For many transitional disks, the inward truncation of the outer dust disk has been confirmed, predominantly through (sub)millimeter interferometric imaging. Many researchers have posited that these holes and gaps are the footprints of planets given that theoretical simulations predict that a young, forming planet will clear the material around itself, leaving behind a cavity in the disk. In this talk, I will review the key observational constraints on the dust and gas properties of transitional disks and examine these in the context of theoretical planet-induced disk clearing models. I will also discuss possibilities for future work in this field in the era of ALMA.","",""];

December[0]=["2","Amaya-Moro Martin","STSCI","Herschel studies of extrasolar Kuiper belt-like systems","Planetesimals are the building blocks of planets. They can be traced by the dust they produce in collisions or sublimation that forms a debris disk. In the solar system, such a dust disk is produced by the asteroids, comets and Kuiper Belt objects, with a dust production rate that has changed significantly with time, being higher in the past when the planetesimal belts were more densely populated. The Herschel DEBRIS, DUNES, and GT programs observed 37 extrasolar planetary systems within 25 pc. With a sensitivity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the current solar system’s Kuiper belt, these surveys identified 11 debris disks, indicating the presence of planetesimals. We discuss the general characteristics of these Kuiper belt-like disks and the correlations between the stellar, planetary, and debris components. We also present results from an unbiased subsample of the Herschel surveys consisting of 204 FGK stars, located at distances <20 pc,  with ages > 100 Myr, and with no binary companions at <100 AU, and discuss whether the presence of planets affect the frequency and properties of extrasolar Kuiper belts. Is there evidence that debris disks are more common, or more dusty, or have a different characteristic temperature around stars harboring high-mass or low-mass planets compared to a control sample without identified planets? Are debris disks more or less common, or more or less dusty, around stars harboring multiple planets compared to single-planet systems? The study of extrasolar Kuiper belt-like disks can shed light on planet formation and migration scenarios. It can also help assess whether terrestrial planet detection might be feasible in these systems. The debris dust can cause an important observational issue for direct detection, with the level of zodiacal light being one of the parameters that defines the design of future telescopes like ATLAST, that have a goal of detecting biosignatures. From our unbiased subsample, we find that 14% of solar-type stars harbor dust-producing planetesimals at 10s of AU from the star with a distribution of fractional luminosity (L_dust /L_star ) that can be reproduced by a Gaussian centered at the solar-system’s level. A Gaussian distribution centered at 10×the solar-system’s value can be ruled out. Because this dust would drift into the terrestrial planet region under PR drag, this indicates that there are good prospects for finding a large number of debris-disk systems—with evidence of harboring planetesimals—with zodi emission low enough to be appropriate targets for terrestrial-planet searches.","",""];
December[1]=["9","Tom Abel","Stanford","Dark Matter Dynamics","Computational Physics allows us to study extremely non-linear systems with fidelity. In astrophysical hydrodynamics and studies of galaxy formation much of the last two decades we have explored various discretization techniques and found subtle differences in some applications. Interestingly numerical studies of collisionless fluids such as e.g. the collapse of cold dark matter to form the large scale structure of the Universe has only been studied meaningfully with one approach; N-body Monte Carlo techniques. I will introduce a novel simulation approach, and demonstrate its feasibility, that can study a collisionless system in the continuum limit in multi-dimensions. I will also show this new technique opens a new window in making sense of structure formation as well as plasma physics.<br>In an application to Landau damping of a collisionless plasma in one dimension we obtain the same accuracy as standard particle in cell codes with 40 times fewer particles.<br>For multi-dimensional applications we have developed a novel rasterization/voxelization algorithm applicable in computational geometry, computational physics, CAD design and other fields. I show how these approaches allow also for much improved predictions for  gravitational lensing, dark matter annihilation and properties of cosmic velocity fields.","",""];
December[2]=["16","Clifford Will","University of Florida","Incorporating post-Newtonian effects in N-body dynamics","The increasing role of general relativity in the dynamics of stellar systems with central massive black holes, in the generation of extreme mass-ratio inspirals, and in the evolution of hierarchical triple systems inspires a close examination of how post-Newtonian effects are incorporated into N-body dynamics.  Most approaches incorporate relativity by adding to the Newtonian N-body equations the standard two-body post-Newtonian terms for a given star around the black hole or for the close binary in a triple system.   We argue that, for calculating the evolution of such systems over timescales comparable to the relativistic pericenter advance timescale, it is essential to include ``cross terms'' in the equations of motion.  These are post-Newtonian terms that represent a coupling between the potential of the central black hole or the inner binary system and the potential due to the other star(s) in the system.  Over pericenter precession timescales, the effects of such terms can actually be ``boosted'' to amplitudes of Newtonian order. We display the post-Newtonian N-body equations of motion including a central black hole in a truncated form that includes all the relevant cross terms, in a format ready to use for numerical implementation.   For hierarchical triple systems, we show explicitly the effects of cross terms on the orbit-averaged equations for the orbit elements of the inner binary for the special case where the third body is on a circular orbit, and present the results of numerical integrations of those equations. ","",""];