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 Cham : Springer, c2020.
 Description
 Book — 1 online resource ( 437 p..) : Digital: text file; PDF.
 Summary

 Intro; Foreword: Welcome to the NotSoSpherical Cow; Preface; References; Contents; Editors and Contributors; Abbreviations; 1 The Art and Science of Trajectory Modelling; 1.1 Introduction; 1.2 Trajectory Models; 1.3 A Gallery of Geodetic Trajectories; 1.4 Automatic Signal Decomposition Using GrAtSiD; 1.5 Conclusions; References; 2 Introduction to Geodetic Time Series Analysis; 2.1 Gaussian Noise and the Likelihood Function; 2.2 Linear Models; 2.3 Models for the Covariance Matrix; 2.4 Power Spectral Density; 2.5 Numerical Examples; 2.6 Discussion; References
 3 Markov Chain Monte Carlo and the Application to Geodetic Time Series Analysis3.1 Introduction; 3.2 Markov Chain Monte Carlo as a Parameter Estimation Method; 3.2.1 Fundamentals; 3.2.2 The RandomWalk MetropolisHasting Algorithm; 3.2.3 The Markov Chain Monte Carlo Algorithm; 3.3 General Considerations for Markov Chain Monte Carlo; 3.3.1 The Equilibrium State; 3.3.2 The Acceptance Rate; 3.3.3 The Spectrum of the Markov Chain; 3.4 Applications; 3.4.1 Position Time Series; 3.4.2 Plate Motion Models; 3.4.3 Gravity Time Series; 3.4.4 Mean Sea Level Time Series; 3.5 Summary; References
 4 Introduction to Dynamic Linear Models for Time Series Analysis4.1 Introduction to Dynamic Linear Models; 4.2 State Space Description; 4.2.1 Example: Spline Smoothing; 4.3 DLM as Hierarchical Statistical Model; 4.4 State and Parameter Estimation; 4.5 Recursive Kalman Formulas; 4.6 Simulation Smoother; 4.7 Estimating the Static Structural Parameters; 4.8 Analysing Trends; 4.9 Examples of Different DLM Models; 4.9.1 The Effect of Level and Trend Variance Parameters; 4.9.2 Seasonal Component; 4.9.3 Autoregressive Process; 4.9.4 Regression Covariates and Proxy Variables
 4.10 Synthetic GNSS Example4.11 Computer Implementation; 4.12 Conclusions; References; 5 Fast Statistical Approaches to Geodetic Time Series Analysis; 5.1 Introduction; 5.2 Motivation and Statistical Impact of Temporal Correlations; 5.3 The FirstOrder GaussMarkov Extrapolation (FOGMEX) Algorithm; 5.3.1 Weighted LeastSquares Algorithm; 5.3.2 Kalman Filter Extension; 5.3.3 Impact of Flicker Noise; 5.3.4 Dependence of Results on Data Duration and Noise Ratios; 5.3.5 Time Series Data Weighting; 5.4 Comparisons to Hector Results; 5.4.1 Comparison for Time Series with no Breaks
 5.4.2 Comparison for Time Series with Breaks5.5 Performance Using Real Data; 5.5.1 Comparison of LeastSquares and Kalman Filter Estimates; 5.5.2 Comparison of FOGMEX and Hector; 5.5.3 Comparison of Run Times; 5.6 Conclusions; References; 6 Least Squares Contribution to Geodetic Time Series Analysis; 6.1 Introduction and Background; 6.2 Univariate Geodetic Time Series Analysis; 6.2.1 Functional Model; 6.2.2 Stochastic Model; 6.3 Multivariate Geodetic Time Series Analysis; 6.3.1 Functional Model; 6.3.2 Stochastic Model; 6.4 Simulated Results on GPS Time Series
 Vermeer, Martin, author.
 Boca Raton : CRC Press, 2020
 Description
 Book — 1 online resource ( xvi, 273 pages) : illustrations.
 Summary

 A brief history of mapping
 Popular conformal map projections
 The complex plane and conformal mappings
 Conformal mappings
 Transversal Mercator projections
 Spherical trigonometry
 The geometry of the ellipsoid of revolution
 Threedimensional coordinates and transformations
 Coordinate reference systems
 Coordinates of heaven and Earth
 The orbital motion of satellites
 The surface theory of Gauss
 Riemann surfaces and charts
 Map projections in light of surface theory
 Astronomical Data Analysis Software and Systems (Conference) (26th : 2016 : Trieste, Italy)
 First edition.  San Francisco : Astronomical Society of the Pacific, [2019]
 Description
 Book — 1 online resource (xxxiii, 788 pages) : illustrations (some color). Digital: text file.
 Summary

 Longterm management of data archives
 Surveys for transient objects in the era of gravitational wave astronomy
 Management of scientific and data analysis projects
 Reduction and analysis algorithms for large databases and viceversa
 Data models in astrophysics
 Python in astronomy
 New trends in HPC and distributed computing
 Miscellanea
 BoF sessions, demo booths and focus demo.
 Astronomical Data Analysis Software and Systems (Conference) (28th : 2018 : College Park, Md.), author.
 First edition.  San Francisco : Astronomical Society of the Pacific, [2019]
 Description
 Book — 1 online resource (xxxiv, 753 pages) : illustrations (some color).
 Summary

 Astrophysical data visualization from line plots to augmented and virtual reality
 Machine learning in astronomy
 Data science: workflows, hardware, software, humanware
 Management of large science projects
 Science platforms: tools for data discovery and analysis from different angles
 Quality assurance of science data
 DevOps practices in astronomy software
 Databases and archives: challenges and solutions in the big data era
 Software for solar system astronomy
 Time domain astronomy
 Multimessenger astronomy
 Algorithms
 Miscellaneous
 Tutorials
 Focus talks and demo booths
 Birds of a feather
 Ancillary meetings.
 Di Matteo, Tiziana, author.
 Berlin, Germany : Springer, 2019.
 Description
 Book — 1 online resource (xiii, 212 pages) : illustrations (some color).
 Lüst, Dieter, author.
 Cham, Switzerland : Springer, [2019]
 Description
 Book — 1 online resource.
 Summary

 Special relativity. Riemannian geometry. Introduction to general relativity. General relativity. Einstein's equations. Black holes. KruskalSzekeres coordinates and geodesics of the Schwarzschild black hole. Conformal compactifications and Penrose diagrams. Penrose diagrams of charged & rotating black holes. Rotating black holes and black hole mechanics. Black hole mechanics and thermodynamics. Black hole thermodynamics . Black holes and entropy. Hawking and Unruh radiation. Quantum field theory in curved spacetime backgrounds. Unruh und Hawking effect. Information loss paradox. Solitons in String Theory. Brane solutions. Dimensional reduction and black holes. Black holes in string theory from p/Dbranes. Black hole microstate counting. Asymptotic symmetries in general relativity and black hole hair. Asymptotic symmetries of 4D spacetime geometries. BMS charges. The gravitational memory effect. Current research on BMSlike transformations and charges of black holes. Quantum hair and quantum black hole vacua.
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 Lawrence, J. L. (Jackie L.), author.
 Cambridge : MIT Press, 2019. [Piscataqay, New Jersey] : IEEE Xplore, [2019]
 Description
 Book — 1 online resource (392 pages).
 Summary

How to predict and calculate the positions of stars, planets, the sun, the moon, and satellites using a personal computer and high school mathematics. Our knowledge of the universe is expanding rapidly, as space probes launched decades ago begin to send information back to earth. There has never been a better time to learn about how planets, stars, and satellites move through the heavens. This book is for amateur astronomers who want to move beyond pictures of constellations in star guides and solve the mysteries of a starry night. It is a book for readers who have wondered, for example, where Saturn will appear in the night sky, when the sun will rise and set, or how long the space station will be over their location. In Celestial Calculations, J. L. Lawrence shows readers how to find the answers to these and other astronomy questions with only a personal computer and high school math. Using an easytofollow stepbystep approach, Lawrence explains what calculations are required, why they are needed, and how they all fit together. Lawrence begins with basic principles: unit of measure conversions, time conversions, and coordinate systems. He combines these concepts into a computer program that can calculate the location of a star, and uses the same methods for predicting the locations of the sun, moon, and planets. He then shows how to use these methods for locating the many satellites we have sent into orbit. Finally, he describes a variety of resources and tools available to the amateur astronomer, including star charts and astronomical tables. Diagrams illustrate the major concepts, and computer programs that implement the algorithms are included. Photographs of actual celestial objects accompany the text, and interesting astronomical facts are interspersed throughout. Source code (in Python 3, JAVA, and Visual Basic) and executables for all the programs and examples presented in the book are available for download at https://CelestialCalculations.github.io.
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 Fegan, D. J., author.
 Singapore ; Hackensack, NJ : World Scientific Publishing Co. Pte. Ltd., [2019]
 Description
 Book — 1 online resource.
 Summary

 Cosmic [gamma]ray timeline
 A serendipitous observation
 Photography, simulations, detectors
 Detection strategies
 Prototyping a TeV imager
 Image compactness selection
 Ongoing data fidelity issues
 Crab
 first TeV source, 1989
 Dedicated workshops
 XRB Rayleigh powers
 Imaging refinements
 Supercuts
 Markarian 421
 [Gamma]/Hadron in perspective
 TeV [gamma]ray astronomy in 2018.
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 CapuzzoDolcetta, Roberto, author.
 Cham, Switzerland : Springer, [2019]
 Description
 Book — 1 online resource
 Summary

 Chapter 1. Elements of Vector Calculus. 1.1 Vector Functions of Real Variables. 1.2 Limits of vector Functions. 1.3 Derivatives of Vector Functions. 1.3.1 Geometrie Interpretation. 1.4 Integrals of Vector Functions. 1.5 The Formal Operator Nabla, . 1.5.1 in Polar Coordinates. 1.5.2 in Cylindrical Coordinates. 1.6 The Divergence Operator. 1.7 The Curl Operator. 1.8 Divergence and Curl by Means of . 1.8.1 Spherical Polar Coordinates. 1.8.2 Cylindrieal Coordinates. 1.9 Vector Fields. 1.9.1 Field Lines. 1.10 Divergence Theorem. 1.10.1 Velocity Fields. 1.10.2 Continuity Equation. 1.10.3 Field Lines of Solenoidal Fields.
 Chapter 2 Potential Theory. Discrete mass distributions. 2.1 Single particle gravitational potential. 2.2 The gravitating N body case. 2.3 Mechanical Energy of the N bodies. 2.4 The Scalar Virial Theorem. 2.4.1 Consequenees of the Virial Theorem. 2.5 Newtonian Gravitational Force and Potential. 2.6 Gauss Theorem. 2.7 Gravitational Potential Energy. 2.8 Newton's Theorems. Chapter 3. Central Force Fields. 3.1 Force and Potential of a Spherical Mass Distribution. 3.2 Circular orbits. 3.2 Potential of a Homogeneous Sphere. 3.3.1 Quality of Motion. 3.3.2 Particle Trajectories. 3.4 Periods of Oscillations. 3.4.1 Radial and Azimuthal Oscillations. 3.4.2 Radial Oscillations in a Homogeneous Sphere. 3.4.3 Radial Oscillations in a Point Mass Potential. 3.5 The Isochrone Potential. 3.6 The Inverse Problem in Spherical Distributions. Chapter 4. Potential Series Developments. 4.1 Fundamental Solution of Laplace'sChapter 1. Elements of Vector Calculus. 1.1 Vector Functions of Real Variables. 1.2 Limits of vector Functions. 1.3 Derivatives of Vector Functions. 1.3.1 Geometrie Interpretation. 1.4 Integrals of Vector Functions. 1.5 The Formal Operator Nabla, . 1.5.1 in Polar Coordinates. 1.5.2 in Cylindrical Coordinates. 1.6 The Divergence Operator. 1.7 The Curl Operator. 1.8 Divergence and Curl by Means of . 1.8.1 Spherical Polar Coordinates. 1.8.2 Cylindrieal Coordinates. 1.9 Vector Fields. 1.9.1 Field Lines. 1.10 Divergence Theorem. 1.10.1 Velocity Fields. 1.10.2 Continuity Equation. 1.10.3 Field Lines of Solenoidal Fields.
 Chapter 2 Potential Theory. Discrete mass distributions. 2.1 Single particle gravitational potential. 2.2 The gravitating N body case. 2.3 Mechanical Energy of the N bodies. 2.4 The Scalar Virial Theorem. 2.4.1 Consequenees of the Virial Theorem. 2.5 Newtonian Gravitational Force and Potential. 2.6 Gauss Theorem. 2.7 Gravitational Potential Energy. 2.8 Newton's Theorems. Chapter 3. Central Force Fields. 3.1 Force and Potential of a Spherical Mass Distribution. 3.2 Circular orbits. 3.2 Potential of a Homogeneous Sphere. 3.3.1 Quality of Motion. 3.3.2 Particle Trajectories. 3.4 Periods of Oscillations. 3.4.1 Radial and Azimuthal Oscillations. 3.4.2 Radial Oscillations in a Homogeneous Sphere. 3.4.3 Radial Oscillations in a Point Mass Potential. 3.5 The Isochrone Potential. 3.6 The Inverse Problem in Spherical Distributions. Chapter 4. Potential Series Developments. 4.1 Fundamental Solution of Laplace's Equation. 4.2 Harmonic Functions. 4.3 Legendre's Polynomials. 4.4 Recursive Relations. 4.4.1 First Recursive Relation. 4.4.2 Second Recursive Relation. 4.5 Legendre Differential Equation. 4.6 Orthogonality of Legendre's Polynomials. 4.7 Development in Series of Legendre's Polynomials. 4.8 Rodrigues Formula Chapter 5. Harmonic and Homogeneous Polynomials. 5.1 Spherical Harmonics. 5.2 Solution of the Differential equations for Sm( , ). 5.3 The Solution in . 5.4 A note on the Associated Legendre Differential Equation. 5.5 Zonal, Sectorial and Tesseral Spherical Harmonics. 5.5.1Orthogonality Properties. Chapter 6. Series of Spherical Harmonics. 6.1 Potential Developments Out of a Mass Distribution. 6.2 The External Earth Potential. 6.3 Exercises.
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10. The cosmic mystery tour [2019]
 Mee, Nicholas, author.
 First edition.  Oxford ; New York, NY : Oxford University Press, 2019.
 Description
 Book — 1 online resource.
 Summary

 Part 1: The Laws of The Cosmos1: The Path to Immortality2: The Rosetta Stone and Quantum Waves3: We're Having a Field Day!4: Cosmic Ripples5: Lovely LISA6: Animated Atom Boy7: Twinkle, Twinkle Little Star8: Forces of the World Unite!9: Most of the Universe is Missing!Part II: The History, Geography and Architecture of the Cosmos10: From Genesis to Revelation!11: The Battle for the Cosmos12: Alchemical Furnaces of the Cosmos13: Diamonds in the Sky14: From the Leviathan to the Behemoth15: The Crab and the Jellyfish16: The Ultimate Heavy Metal Space Rock17: Pan Galactic Gargle Blaster18: Cosmic Spacequakes19: Doctor Atomic and the Black Hole20: Supermassive Black HolesPart III: The Biology of the Cosmos21: The Gorgon's Head!22: Raise Your Glasses to the Skies!23: Life, But Not as We Know It!24: To Boldly Go...25: Somewhere Over the Rainbow26: Where is Everybody?
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 Singapore ; Hackensack, NJ : World Scientific, [2019]
 Description
 Book — 1 online resource.
 Summary

Early Universe cosmology is an active area of research and cosmic inflation is a pillar of modern cosmology. Among predictions of inflation, observationally the most important one is the generation of cosmological perturbations from quantum vacuum fluctuations that source all inhomogeneous structures in the Universe, not to mention the largescale structures such as clusters of galaxies.Cosmological perturbation theory is the basic tool to study the perturbations generated from inflation. There are a few different approaches to primordial cosmological perturbations. In the conventional approach one perturbs the field equations and after quantizing the perturbations by the use of the corresponding action, one calculates the power spectrum of cosmological observables. This approach extends to higher order perturbations such as bispectrum etc., but the analysis becomes increasingly difficult.The delta N formalism, the topic of this book, is an alternative approach. The novelty of this approach is that, under the condition that the scale of interest is very large so that the spatial derivatives may be ignored in the dynamics, it can be applied to all orders in perturbation theory and has a rigorous foundation in general relativity. Thanks to the fact that one can evaluate perturbations with only the knowledge of background solutions, it is proved to be much easier than the conventional approach in evaluating higher order effects in many cases.
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 Wood, Jeremy.
 Cham : Springer, 2019.
 Description
 Book — 1 online resource (129 p.).
 Summary

 Intro; Acknowledgments; Contents; List of Figures; List of Tables; 1 Introduction; 1.1 The Beginning; 1.2 What Is a Small Solar System Body?; Exercises; 2 The Science of Small Solar System Bodies; 2.1 Why Study Small Solar System Bodies?; 2.2 How Small Solar System Bodies Are Studied; 2.2.1 Probes; 2.2.2 Physical Samples; 2.2.3 Computer Simulations; 2.2.4 Telescopic Observations; 2.2.5 The Future Study of SSSBs; Exercises; 3 A Brief Review of Cosmological Models; 3.1 The Geocentric Model; 3.2 The Copernican Model; Exercises; 4 Modern Orbital Mechanics
 4.1 Kepler's Laws and Newton's Universal Law of Gravitation4.1.1 Kepler's First Law: The Law of Ellipses; 4.1.2 Kepler's Second Law: The Law of Equal Areas; 4.1.3 Kepler's Third Law: The Harmonic Law; 4.1.4 Newton's Universal Law of Gravitation; 4.1.5 Tidal Forces; 4.2 Orbits in a ThreeDimensional Coordinate System; 4.2.1 The 2Body Problem in the Solar System; 4.2.2 The Circular Restricted 3Body Problem; 4.3 Resonances; 4.3.1 Mean Motion Resonances; 4.3.2 Secular Resonances; 4.3.3 Secondary Resonances; 4.4 Chaos and Stability; Exercises; 5 Populations of Small Solar System Bodies
 5.1 Asteroids5.2 Comets; 5.3 Centaurs; 5.4 The Taxonomy of Comets and CometLike Bodies; 5.5 Other Small Body Populations; 5.6 The Effects of Planets on Small Body Populations; Exercises; 6 Ringed Small Bodies; 6.1 Chariklo; 6.2 Chiron; 6.3 Haumea; 6.4 The Detection of Rings; 6.5 Measuring the Severity of Close Encounters Between Ringed Small Bodies and Planets; 6.6 The Ring Limit; 6.7 The Future Study of Ringed Small Bodies; Exercises; Answer Key; Chapter One; Chapter Two; Chapter Three; Chapter Four; Chapter Five; Chapter Six; References
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 Carpathian Summer School of Physics (28th : 2018 : Sinaia, Romania), author.
 [Melville, New York] : AIP Publishing LLC, 2019.
 Description
 Book — 1 online resource : illustrations (some color). Digital: text file.
14. Extraterrestrial languages [2019]
 Oberhaus, Daniel, author.
 Cambridge : MIT Press, 2019.
 Description
 Book — 1 online resource (264 pages).
 Summary

If we send a message into space, will extraterrestrial beings receive it? Will they understand?The endlessly fascinating question of whether we are alone in the universe has always been accompanied by another, more complicated one: if there is extraterrestrial life, how would we communicate with it? In this book, Daniel Oberhaus leads readers on a quest for extraterrestrial communication. Exploring Earthlings' various attempts to reach out to nonEarthlings over the centuries, he poses some not entirely answerable questions: If we send a message into space, will extraterrestrial beings receive it? Will they understand? What languages will they (and we) speak? Is there not only a universal grammar (as Noam Chomsky has posited), but also a grammar of the universe? Oberhaus describes, among other things, a latenineteenthcentury idea to communicate with Martians via Morse code and mirrors; the emergence in the twentieth century of SETI (the search for extraterrestrial intelligence), CETI (communication with extraterrestrial intelligence), and finally METI (messaging extraterrestrial intelligence); the oneway space voyage of Ella, an artificial intelligence agent that can play cards, tell fortunes, and recite poetry; and the launching of a theremin concert for aliens. He considers media used in attempts at extraterrestrial communication, from microwave systems to plaques on spacecrafts to formal logic, and discusses attempts to formulate a language for our message, including the Astraglossa and two generations of Lincos (lingua cosmica).The chosen medium for interstellar communication reveals much about the technological sophistication of the civilization that sends it, Oberhaus observes, but even more interesting is the information embedded in the message itself. In Extraterrestrial Languages, he considers how philosophy, linguistics, mathematics, science, and art have informed the design or limited the effectiveness of our interstellar messaging.
15. Formation of the first black holes [2019]
 New Jersey : World Scientific, 2019.
 Description
 Book — 1 online resource.
 Summary

The formation of the first supermassive black holes is one of the main open questions in our understanding of highredshift structure formation. In this book, we aim to provide a summary of stateoftheart modern research on this topic, exploring the formation of massive black holes from a fluiddynamical, stellardynamical and chemical perspective. The book thus presents a solid theoretical foundation, a comparison with current observations and future observational perspectives with upcoming missions such as the Square Kilometre Array, the European Extremely Large Telescope, the Euclid satellite as well as possible detections via gravitational waves.
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 Armitage, Philip J., 1971 author.
 Berlin, Germany : Springer, 2019.
 Description
 Book — 1 online resource (xxxiii, 260 pages) : illustrations (some color).
 Summary

 Intro; Preface; Acknowledgements; Contents; List of Figures; List of Tables; 1 Physical Processes in Protoplanetary Disks; 1.1 Preamble; 1.2 Observational Context; 1.2.1 The Classification of Young Stellar Objects; 1.2.2 Accretion Rates and Lifetimes; 1.2.3 Inferences from the Dust Continuum; 1.2.4 Molecular Line Observations; 1.2.5 LargeScaleStructure in Disks; 1.3 Disk Structure; 1.3.1 Vertical and Radial Structure; 1.3.2 Thermal Physics; 1.3.3 Ionization Structure; 1.4 Disk Evolution; 1.4.1 The Classical Equations; 1.4.2 Boundary Conditions; 1.4.3 Viscous Heating; 1.4.4 Warped Disks
 1.4.5 Disk Winds1.5 Turbulence; 1.5.1 Hydrodynamic Turbulence; 1.5.2 Selfgravity; 1.5.3 Magnetohydrodynamic Turbulence and Transport; 1.5.4 The Magnetorotational Instability; 1.5.5 Transport in the Boundary Layer; 1.6 Episodic Accretion; 1.6.1 Secular Disk Instabilities; 1.6.2 Triggered Accretion Outbursts; 1.7 Single and Collective Particle Evolution; 1.7.1 Radial Drift; 1.7.2 Vertical Settling; 1.7.3 Streaming Instability; 1.8 Structure Formation in Protoplanetary Disks; 1.8.1 Ice Lines; 1.8.2 Particle Traps; 1.8.3 Zonal Flows; 1.8.4 Vortices; 1.8.5 Rossby Wave Instability
 1.9 Disk Dispersal1.9.1 Photoevaporation; 1.9.2 MHD Winds; References; 2 Planet Formation and DiskPlanet Interactions; 2.1 Introduction; 2.1.1 The Solar System; 2.1.2 Properties of the Extrasolar Planets; 2.1.3 Pathways to Planets; 2.2 From Dust to Planetesimals; 2.2.1 Study the Initial Growth Phase; 2.2.2 How to Overcome Growth Barriers; 2.2.3 Dust Concentration; 2.3 Terrestrial Planet Formation; 2.3.1 Concepts; 2.3.2 Growth to Protoplanets; 2.3.3 Assembly of the Terrestrial Planets; 2.4 The Formation of Massive Planets by Core Accretion; 2.4.1 Background; 2.4.2 The Growth to a Giant
 2.4.3 The Final Mass2.4.4 Interior Structure of Planets; 2.5 Planets Formed by Gravitational Instability; 2.5.1 Background; 2.5.2 Linear Stability Analyses; 2.5.3 Fragmentation Conditions; 2.5.4 Nonlinear Simulations; 2.6 PlanetDisk Interaction; 2.6.1 Basic Concepts; 2.6.2 Type I Migration; 2.6.3 Type II Migration; 2.6.4 Other Regimes of Migration; 2.6.5 Eccentricity and Inclination; 2.7 Multibody Systems; 2.7.1 Resonances; 2.7.2 Dynamics; 2.7.3 Multiplanet Systems; 2.7.4 Circumbinary Planets; References
 Dainotti, Maria, author.
 Bristol [England] (Temple Circus, Temple Way, Bristol BS1 6HG, UK) : IOP Publishing, [2019]
 Description
 Book — 1 online resource (various pagings) : illustrations (some color).
 Summary

 3. GRB correlations between prompt parameters
 3.1. Why are standard candles and sirens important for cosmology?
 3.2. Notations, nomenclature and abbreviations
 3.3. The GRB correlations between prompt parameters
 4. Selection effects on prompt correlations
 4.1. Introduction to selection effects
 4.2. Selection effects for peak energy
 4.3. Selection effects for the isotropic energy
 4.4. Selection effects for the isotropic luminosity
 4.5. Selection effects for the peak luminosity
 4.6. Selection effects for the lag time and the rise time
 5. Redshift estimators and cosmology for prompt relations
 5.1. Redshift estimator for correlations between prompt parameters
 5.2. Cosmology
 5.3. Statistical approaches related to SN Ia cosmology
 6. The afterglow relations
 6.1. The correlations between afterglow parameters
 6.2. The LO, 200sαO, >200s correlation and its physical interpretation
 7. Correlations between prompt and afterglow parameters
 7.1. The EX, afterglowEγ, prompt correlation and its physical interpretation
 7.2. The LX, afterglowEγ, prompt correlation and its physical interpretation
 7.3. The LX, aLO, a correlation and its physical interpretation
 7.4. The LX, aLγ, iso correlation
 7.5. The LX, aLX, peak correlation
 7.6. The LOF, peakTO*F, peak correlation and its physical interpretation
 8. Selection effects in the afterglow and promptafterglow correlations
 8.1. Redshift induced correlations
 8.2. Redshift induced correlations through the Efron and Petrosian method
 8.3. Evaluation of the intrinsic slope
 8.4. Selection effects for the optical and Xray luminosities
 8.5. Selection effects in the LO, 200sαO, >200s correlation
 9. Redshift estimator
 10. Applications of GRB afterglow correlations
 10.1. Summary and conclusion.
 1. Introduction
 1.1. The phenomenology of GRBs
 1.2. The phenomenological Willingale model
 1.3. The past and current missions observing GRBs
 1.4. The historical background of SNe
 2. GRB models
 2.1. The compactness problem
 2.2. The fireball model
 2.3. The jet opening angle
 2.4. The central engine models
 2.5. Additional models
 2.6. The SN Ib/c models
 Belgiorno, Francesco, author.
 Singapore ; Hackensack, NJ : World Scientific Publishing Co. Pte. Ltd., [2019]
 Description
 Book — 1 online resource.
 Summary

 A short scrapbook on classical black holes
 The seminal paper
 Thermality of Hawking radiation: from HartleHawking to Israel and Unruh
 The tunneling approach
 The anomaly route to Hawking radiation
 The Euclidean section and Hawking temperature
 Rigorous aspects of Hawking radiation
 The roots of analogue gravity
 Hawking radiation in a nondispersive nonlinear Kerr dielectric
 Hawking radiation in a dispersive Kerr dielectric
 Hawking radiation in the lab.
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 Linsky, J. L. (Jeffrey L.), 1941 author.
 Cham, Switzerland Springer [2019]
 Description
 Book — 1 online resource
 Summary

 Why are Host Stars Important for Understanding Exoplanet Atmospheres?. Stellar activityphenomenology and general principles. Magnetic Fieldsthe Source of Stellar Activity. Stellar Chromospheresthe Source of UV Emission. Stellar Coronaethe Source of Xray Emission. Reconstructing the Missing Stellar Emission. Stellar Winds. Correlations of Observables with Stellar Age and Rotation. Stellar Space WeatherConnecting Host Stars to Their Exoplanets  Host Star Driven Exoplanet Mass Loss. Host Star Driven Photochemistry in Exoplanet Atmospheres. StarPlanet Interactions (SPI)Real or Imaginary?. Final Comments and Speculation.
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20. Hypersonic meteoroid entry physics [2019]
 Colonna, Gianpiero, author.
 Bristol [England] (Temple Circus, Temple Way, Bristol BS1 6HG, UK) : IOP Publishing, [2019]
 Description
 Book — 1 online resource (various pagings) : illustrations (chiefly color).
 Summary

 1. Considerations on meteoroid entry physics. part I. Meteoroid and meteorite science.
 2. The trajectory, structure and origin of the Chelyabinsk impactor
 2.1. Trajectory
 2.2. Structure
 2.3. Origin
 2.4. Implications
 3. Properties of meteoroids from forward scatter radio observations
 3.1. Radio meteor theory
 3.2. The BRAMS project
 3.3. Conclusions
 4. The flux of meteoroids over time : meteor emission spectroscopy and the delivery of volatiles and chondritic materials to Earth
 4.1. The meteor phenomenon and the origin of Earth's volatiles
 4.2. Meteor spectroscopy : an added value to Meteoritica
 4.3. Relative elemental abundances and cosmochemical ratios from photographic, video and CCD spectroscopy
 4.4. The Na overabundance : clues on the delivery of volatiles from fragile meteoroids and IDPs
 4.5. Astrobiological implications of the continuous arrival of chondritic components to Earth's surface
 4.6. Conclusions and future work
 5. Compositional, mineralogical and structural investigation of meteorites by XRD and LIBS
 5.1. The XRD technique
 5.2. The LIBS technique
 5.3. Conclusions and perspectives
 part II. Hypersonic entry physics.
 6. Radiation gas dynamics of centimeter meteoric bodies at an altitude of 80 km
 6.1. Computer RadGD model
 6.2. Numerical simulation results
 6.3. Conclusion
 7. Superorbital entry of artificial asteroids (Apollo, Hayabusa) and CFD/radiation/thermal analysis of the entry of the Chelyabinsk meteorite
 7.1. A simplified model for meteoroid entry
 7.2. Entry of large meteoroids
 7.3. Heating
 7.4. Thermal analysis
 7.5. Conclusions
 8. Highenthalpy ionized flows
 8.1. Modeling of nonlocal thermodynamic equilibrium plasmas
 8.2. Selfconsistent statetostate approach
 8.3. The selfconsistent model in hypersonic flows
 9. Precursor ionization during highspeed Earth entry
 9.1. Langmuir probe analysis
 9.2. Experimental setup
 9.3. Test conditions
 9.4. Results
 9.5. Conclusions
 10. Response of the meteoroid/meteorite to aerodynamic forces and ablation
 10.1. Ablation models
 10.2. An example
 10.3. Porosity
 10.4. The presence of a fluid phase
 10.5. Creation of surface patterns
 10.6. Fragmentation processes
 10.7. Chemically reacting surfaces
 11. Experimental investigation of meteorites : ground test facilities
 11.1. The CP50 plasma torch facility at CentraleSupélec
 11.2. The PWT facility for testing meteorites at CIRA
 11.3. Optical emission spectroscopy (OES)
 11.4. Laser induced fluorescence spectroscopy (LIF)
 11.5. Ion beam analysis (IBA) on meteorites
 11.6. Infrared thermography
 11.7. The HEAT facility at SITAEL
 12. Advanced statetostate and multitemperature models for flow regimes
 12.1. General kinetic theory method for nonequilibrium flow modeling
 12.2. Stateto state theoretical model of kinetics and transport properties
 12.3. Multitemperature models for reacting air flows
 12.4. Multitemperature models for flows containing CO2
 12.5. Conclusions
 13. Statetostate kinetics in CFD simulation of hypersonic flows using GPUs
 13.1. Physical model
 13.2. Numerical method
 13.3. Computational approach and hardware specifications
 13.4. Results
 part III. Elementary processes in hypersonic flows.
 14. Thermodynamic and transport properties of reacting air including ablated species
 14.1. The EquilTheTA code
 14.2. Thermodynamics and equilibrium
 14.3. Transport properties
 14.4. Conclusions
 15. Electronmolecule processes
 15.1. Nonresonant inelastic eH2 collision processes
 15.2. Resonant inelastic eH2 processes
 15.3. Resonant electroninduced reaction cross sections in Earth atmosphere molecules
 15.4. Nonresonant vibronic excitations in Earth atmosphere molecules
 15.5. Conclusion
 16. Heavyparticle elementary processes in hypersonic flows
 16.1. The quasiclassical method
 16.2. Energy transfer and dissociation of N2
 16.3. Specifics of O2N2 collisions
 17. Nonempirical analytical model of nonequilibrium dissociation in hightemperature air
 17.1. Description of the MacheretFridman model
 17.2. MacheretFridman model for CFD
 17.3. MacheretFridman model for DSMC
 17.4. Concluding remarks
 18. The role of vibrational activation and bimolecular reactions in nonequilibrium plasma kinetics
 18.1. Reactive channels promoted by heavyparticle collisions
 18.2. The plasma kinetic model
 18.3. Conclusions.