This document discusses perturbations from a mixed inflaton-curvaton scenario of the early universe. It begins with an overview of perturbations from standard single-field inflation models. It then introduces the curvaton scenario, where a subdominant scalar field called the curvaton produces the primordial density perturbations after inflation ends. The document outlines how the curvaton scenario allows for non-Gaussian perturbations and explores constraints on curvaton-dominated theories. It concludes by discussing including perturbations from both the inflaton and curvaton fields in a mixed scenario.
Talk given at Cambridge DAMTP on Friday, 20 June 2008. Describes recent work on understanding what is necessary to embed accelerating cosmology in higher-dimensional theory.
Large scale coherent structures and turbulence in quasi-2D hydrodynamic modelsColm Connaughton
This document discusses turbulence in two-dimensional systems and the inverse energy cascade phenomenon. It begins with an overview of turbulence in 3D and 2D, describing the inverse energy cascade in 2D systems whereby energy is transferred to larger scales rather than smaller scales. It then discusses how finite size effects can generate large-scale coherent structures by blocking the inverse cascade. The document concludes by noting that extracting coherent flow from turbulent fluctuations is challenging and that diagnostics like the third-order structure function may not be reliable indicators of the energy cascade direction due to the presence of coherent structures.
This document summarizes key aspects of diffusion in solids:
1) Diffusion occurs due to a concentration gradient, which provides a driving force for atoms to move from high to low concentration regions.
2) Diffusion is an important part of materials processing techniques like case hardening and doping of semiconductors.
3) The rate of diffusion depends on factors like temperature, structure, and the diffusion mechanism (e.g. substitutional vs. interstitial). Fick's laws can be used to model and predict diffusion rates.
Feedback of zonal flows on Rossby-wave turbulence driven by small scale inst...Colm Connaughton
The document summarizes research on the interaction between large-scale zonal flows and small-scale Rossby wave turbulence. It describes how modulational instability can generate large-scale zonal jets from small-scale Rossby waves through an inverse cascade. The generated jets then provide negative feedback on the small-scale waves by distorting them and inducing spectral diffusion through a nonlocal turbulence theory. Numerical simulations demonstrate this generation of jets and spectral transport between scales.
1) Cosmological simulations of galaxy formation have improved greatly over the past few years due to increases in computational power and better modeling of physical processes. Simulations can now resolve disks and reproduce observed properties of galaxies like the Milky Way.
2) Feedback from supernovae is crucial for regulating star formation and producing realistic disk galaxies. It prevents overcooling and the formation of disks that are too compact. Higher resolution and feedback are both needed to match observations.
3) Gas accretes onto galaxies in two main modes - violent mergers at early times that build bulges, and smoother cold flows at late times that build disks. This two-phase assembly explains the formation of bulge and disk components in galaxies
Anderson localization, wave diffusion and the effect of nonlinearity in disor...ABDERRAHMANE REGGAD
This document discusses Anderson localization in disordered lattices and the effect of nonlinearity. It begins with an introduction to Anderson localization and how disorder can suppress diffusion due to interference effects. It then motivates studying this phenomenon experimentally using disordered waveguide lattices. The document describes measuring localized eigenmodes and observing the transition from diffusion to localization by exciting single sites. It finds that nonlinearity increases localization by affecting eigenmodes differently depending on their eigenvalue and enhancing localization of diffusing waves. In conclusion, the experiment provides direct observation of Anderson localization and characterization of diffusion regimes, revealing that nonlinearity generally increases the localization effects of disorder.
Evidence for a black hole remnant in the type iil supernova 1979 cSérgio Sacani
1) The Type IIL supernova SN 1979C has exhibited a remarkably constant X-ray luminosity of (6.5 ± 0.1) × 1038 erg s−1 over 12 years of observations from 1995 to 2007.
2) This steady luminosity is inconsistent with models of a supernova powered by a magnetar or expanding into a dense circumstellar wind, as the luminosity would be expected to decrease over time in these models.
3) The authors propose that the steady X-ray emission provides evidence for accretion onto a stellar-mass (5-10 solar mass) black hole remnant at the center of SN 1979C. Spectral modeling of the X-ray data is consistent with emission from
Talk given at Cambridge DAMTP on Friday, 20 June 2008. Describes recent work on understanding what is necessary to embed accelerating cosmology in higher-dimensional theory.
Large scale coherent structures and turbulence in quasi-2D hydrodynamic modelsColm Connaughton
This document discusses turbulence in two-dimensional systems and the inverse energy cascade phenomenon. It begins with an overview of turbulence in 3D and 2D, describing the inverse energy cascade in 2D systems whereby energy is transferred to larger scales rather than smaller scales. It then discusses how finite size effects can generate large-scale coherent structures by blocking the inverse cascade. The document concludes by noting that extracting coherent flow from turbulent fluctuations is challenging and that diagnostics like the third-order structure function may not be reliable indicators of the energy cascade direction due to the presence of coherent structures.
This document summarizes key aspects of diffusion in solids:
1) Diffusion occurs due to a concentration gradient, which provides a driving force for atoms to move from high to low concentration regions.
2) Diffusion is an important part of materials processing techniques like case hardening and doping of semiconductors.
3) The rate of diffusion depends on factors like temperature, structure, and the diffusion mechanism (e.g. substitutional vs. interstitial). Fick's laws can be used to model and predict diffusion rates.
Feedback of zonal flows on Rossby-wave turbulence driven by small scale inst...Colm Connaughton
The document summarizes research on the interaction between large-scale zonal flows and small-scale Rossby wave turbulence. It describes how modulational instability can generate large-scale zonal jets from small-scale Rossby waves through an inverse cascade. The generated jets then provide negative feedback on the small-scale waves by distorting them and inducing spectral diffusion through a nonlocal turbulence theory. Numerical simulations demonstrate this generation of jets and spectral transport between scales.
1) Cosmological simulations of galaxy formation have improved greatly over the past few years due to increases in computational power and better modeling of physical processes. Simulations can now resolve disks and reproduce observed properties of galaxies like the Milky Way.
2) Feedback from supernovae is crucial for regulating star formation and producing realistic disk galaxies. It prevents overcooling and the formation of disks that are too compact. Higher resolution and feedback are both needed to match observations.
3) Gas accretes onto galaxies in two main modes - violent mergers at early times that build bulges, and smoother cold flows at late times that build disks. This two-phase assembly explains the formation of bulge and disk components in galaxies
Anderson localization, wave diffusion and the effect of nonlinearity in disor...ABDERRAHMANE REGGAD
This document discusses Anderson localization in disordered lattices and the effect of nonlinearity. It begins with an introduction to Anderson localization and how disorder can suppress diffusion due to interference effects. It then motivates studying this phenomenon experimentally using disordered waveguide lattices. The document describes measuring localized eigenmodes and observing the transition from diffusion to localization by exciting single sites. It finds that nonlinearity increases localization by affecting eigenmodes differently depending on their eigenvalue and enhancing localization of diffusing waves. In conclusion, the experiment provides direct observation of Anderson localization and characterization of diffusion regimes, revealing that nonlinearity generally increases the localization effects of disorder.
Evidence for a black hole remnant in the type iil supernova 1979 cSérgio Sacani
1) The Type IIL supernova SN 1979C has exhibited a remarkably constant X-ray luminosity of (6.5 ± 0.1) × 1038 erg s−1 over 12 years of observations from 1995 to 2007.
2) This steady luminosity is inconsistent with models of a supernova powered by a magnetar or expanding into a dense circumstellar wind, as the luminosity would be expected to decrease over time in these models.
3) The authors propose that the steady X-ray emission provides evidence for accretion onto a stellar-mass (5-10 solar mass) black hole remnant at the center of SN 1979C. Spectral modeling of the X-ray data is consistent with emission from
Solar Cells Lecture 3: Modeling and Simulation of Photovoltaic Devices and Sy...Tuong Do
The document provides information about a summer school on modeling and simulation of photovoltaic devices and systems being held in July 2011. It outlines the course, which will cover objectives of PV modeling and simulation, device modeling, fundamental limits, system modeling of multijunction devices, and detailed numerical simulation. The instructor is Prof. Jeffery L. Gray of Purdue University and the material is provided under a Creative Commons license.
Talk given at the workshop "Multiphase turbulent flows in the atmosphere and ocean", National Centre for Atmospheric REsearch, Boulder CO, August 15 2012
Sergey Sibiryakov "Galactic rotation curves vs. ultra-light dark matter: Impl...SEENET-MTP
The document discusses ultra-light dark matter and its implications for galactic rotation curves. It begins by providing theoretical background on ultra-light dark matter and how it can form soliton cores within dark matter halos. It then discusses how the properties of these soliton cores, such as their mass and size, relate to the properties of the ultra-light dark matter particle. Finally, it discusses how measurements of galactic rotation curves could provide insights into ultra-light dark matter models by probing the presence and characteristics of these soliton cores.
1) The gamma-ray burst GRB 101225A is explained as being caused by the tidal disruption of a minor body (such as an asteroid or comet) falling onto an isolated neutron star.
2) The light curves and spectra observed across multiple wavelengths are consistent with the predictions of the tidal disruption model.
3) A minor body passing within 105-106 km of a neutron star would be disrupted by the star's tidal forces, with the debris falling back to form an accretion disk around the star and emitting radiation.
An R-matrix approach for plasma modelling and the interpretation of astrophys...AstroAtom
This document provides a 3-sentence summary of an expert presentation on plasma modeling and interpretation using an R-matrix approach:
The presentation discussed comprehensive plasma modeling capabilities using R-matrix calculations of electron-impact ionization, excitation, and photoionization of mid-Z elements, which have been parallelized to efficiently utilize modern high performance computing architectures. Scripted R-matrix calculations along iso-nuclear sequences automate the calculation of effective collision strengths. Examples were given of parallel calculations of electron-impact excitation of Fe III and photoionization of Kr II and Xe II using the Dirac Atomic R-matrix Codes that agree well with experimental results.
Nonequilibrium statistical mechanics of cluster-cluster aggregation, School o...Colm Connaughton
Colm Connaughton presented on nonequilibrium statistical mechanics models of cluster-cluster aggregation. He discussed simple models where particles move randomly and merge upon contact. More sophisticated models track the size distribution of clusters as they aggregate. The Smoluchowski equation describes this process. For certain collision kernels, clusters of arbitrarily large size can form in finite time, known as gelation. While some kernels mathematically describe instantaneous gelation, physical models avoid this with a cluster size cutoff. Stationary states can be reached with a particle source.
A rapidly spinning_supermassive_black_hole_at_the_centre_of_ngc1365Sérgio Sacani
1) XMM-Newton and NuSTAR observed the galaxy NGC 1365 simultaneously over 130 ks, detecting broadband X-ray emission from 3-79 keV.
2) The observations revealed variable absorption below 10 keV and prominent broad emission features between 5-7 keV and 10-30 keV, indicative of relativistic reflection from an accretion disk near a spinning supermassive black hole.
3) Time-resolved spectral analysis was able to disentangle the variable absorption component from the relativistic reflection component. Absorption-dominated models without reflection could be ruled out statistically and on physical grounds.
The document discusses a research project on 3D stacked chip architectures and interlayer cooling, including developing through-silicon vias for vertical electrical connections, using two-phase refrigerant cooling to remove heat from chip stacks more effectively than backside cooling, and experimental work on microchannel heat sinks, boiling visualization, and bubble dynamics simulation using an arbitrary Lagrangian-Eulerian technique.
This summary provides the key information from the document in 3 sentences:
The document discusses nuclear physics concepts such as nuclear structure, binding energy, mass defect, radioactive decay, and half-life. It includes examples calculating physical properties like mass, radius, binding energy, and activity for various nuclei. The examples analyze nuclear reactions and decays, and solve related problems involving time, mass, energy, and radioactive decay calculations.
Atmospheric aberrations in coherent laser systemswtyru1989
The document discusses atmospheric effects on coherent laser systems and compensation methods. It presents:
1) Simulations of atmospheric propagation using phase screens and analyzing phase distortion, beam wander, spreading, and scintillation.
2) Techniques for compensating atmospheric effects in coherent measurements, including phase compensation receivers and adaptive optics.
3) Modeling of beam projection in coherent lidars and analyzing compensation of speckle averaging using non-conjugated adaptive optics.
This document summarizes key concepts and equations related to wave motion from a physics textbook. It discusses transverse and longitudinal waves, and defines terms like amplitude, wavelength, frequency, period, and speed. It also covers topics like standing waves, harmonics, wave energy, and calculating the fundamental frequency and overtones of vibrating strings and ropes based on their tension, mass, and length. Sample problems are provided and worked through applying these concepts and equations to different scenarios.
The document discusses switchgear technology and circuit breaker operation. It covers several topics in 3 sentences or less:
Static welding of contacts can be overcome by increasing contact force and occurs at lower currents than dynamic welding. Arc interruption requires increasing plasma resistance at current zero and ensuring dielectric strength increases faster than electric stress. In a double frequency circuit, the voltages on the two circuits after opening will be proportional to the inductances in each circuit divided by the total inductance.
This document provides tables of constants, conversion factors, units, prefixes, values of trigonometric functions for common angles, and equations for Newtonian mechanics, electricity, and magnetism that are relevant for the 2002 AP Physics B exam. The tables include fundamental physical constants such as the speed of light, Planck's constant, electron mass, and more. Units covered include meters, kilograms, seconds, amperes, kelvins, and others. Prefixes from giga to pico are also listed.
Instantaneous Gelation in Smoluchwski's Coagulation Equation Revisited, Confe...Colm Connaughton
Invited talk given at "Boltzmann equation:
mathematics, modeling and simulations
In memory of Carlo Cercignani", Institut Henri Poincare, Paris, February 11, 2011.
1) The rotational Doppler effect describes a change in the resonant frequency of a system due to relative rotation between the emitter and observer. (Beginning sentence)
2) For magnetic resonance systems like ESR, NMR, and FMR, the resonant frequency is sensitive to magnetic fields and will shift due to the rotational Doppler effect caused by particle rotation.
3) For free magnetic nanoparticles with rotation rates of around 100 kHz, the rotational Doppler shift of around 100 kHz is measurable and on the same order as the linewidth for ESR and FMR, allowing determination of the maximum position with 100 kHz accuracy.
IJERA (International journal of Engineering Research and Applications) is International online, ... peer reviewed journal. For more detail or submit your article, please visit www.ijera.com
1) A changing magnetic flux induces an electromotive force (EMF) in a conductor according to Faraday's law of induction.
2) The direction of the induced current is such that the resulting magnetic field opposes the original change in flux according to Lenz's law.
3) For a conducting loop, the induced electric field is uniform and can be calculated from the rate of change of magnetic flux through the loop.
The document discusses how electrical signals propagate through the heart. It begins by introducing the heart model as involving electricity, mechanics, elasticity and fluids. It then discusses how the electrical signal propagates as a non-decremental traveling wave through the heart tissue. The document notes that the heart tissue is strongly anisotropic, conducting electrical signals faster along fiber directions than across fibers. It proposes using the method of moving frames to simulate electrophysiology phenomena on complex anisotropic heart geometries.
This document discusses inhomogeneous cosmological models as an alternative to the standard cosmological model. It begins by outlining the standard model and some of its variations proposed to address issues like dark energy. It then introduces the Lemaitre-Tolman-Bondi metric, which allows for spherical symmetry and spatial variations. Key aspects of inhomogeneous models using this metric are that they have two expansion rates and three free functions of spatial position that describe the matter profile, initial positions, and expansion rates. These models can evolve from an initially homogeneous early state to a currently inhomogeneous one.
Solar Cells Lecture 3: Modeling and Simulation of Photovoltaic Devices and Sy...Tuong Do
The document provides information about a summer school on modeling and simulation of photovoltaic devices and systems being held in July 2011. It outlines the course, which will cover objectives of PV modeling and simulation, device modeling, fundamental limits, system modeling of multijunction devices, and detailed numerical simulation. The instructor is Prof. Jeffery L. Gray of Purdue University and the material is provided under a Creative Commons license.
Talk given at the workshop "Multiphase turbulent flows in the atmosphere and ocean", National Centre for Atmospheric REsearch, Boulder CO, August 15 2012
Sergey Sibiryakov "Galactic rotation curves vs. ultra-light dark matter: Impl...SEENET-MTP
The document discusses ultra-light dark matter and its implications for galactic rotation curves. It begins by providing theoretical background on ultra-light dark matter and how it can form soliton cores within dark matter halos. It then discusses how the properties of these soliton cores, such as their mass and size, relate to the properties of the ultra-light dark matter particle. Finally, it discusses how measurements of galactic rotation curves could provide insights into ultra-light dark matter models by probing the presence and characteristics of these soliton cores.
1) The gamma-ray burst GRB 101225A is explained as being caused by the tidal disruption of a minor body (such as an asteroid or comet) falling onto an isolated neutron star.
2) The light curves and spectra observed across multiple wavelengths are consistent with the predictions of the tidal disruption model.
3) A minor body passing within 105-106 km of a neutron star would be disrupted by the star's tidal forces, with the debris falling back to form an accretion disk around the star and emitting radiation.
An R-matrix approach for plasma modelling and the interpretation of astrophys...AstroAtom
This document provides a 3-sentence summary of an expert presentation on plasma modeling and interpretation using an R-matrix approach:
The presentation discussed comprehensive plasma modeling capabilities using R-matrix calculations of electron-impact ionization, excitation, and photoionization of mid-Z elements, which have been parallelized to efficiently utilize modern high performance computing architectures. Scripted R-matrix calculations along iso-nuclear sequences automate the calculation of effective collision strengths. Examples were given of parallel calculations of electron-impact excitation of Fe III and photoionization of Kr II and Xe II using the Dirac Atomic R-matrix Codes that agree well with experimental results.
Nonequilibrium statistical mechanics of cluster-cluster aggregation, School o...Colm Connaughton
Colm Connaughton presented on nonequilibrium statistical mechanics models of cluster-cluster aggregation. He discussed simple models where particles move randomly and merge upon contact. More sophisticated models track the size distribution of clusters as they aggregate. The Smoluchowski equation describes this process. For certain collision kernels, clusters of arbitrarily large size can form in finite time, known as gelation. While some kernels mathematically describe instantaneous gelation, physical models avoid this with a cluster size cutoff. Stationary states can be reached with a particle source.
A rapidly spinning_supermassive_black_hole_at_the_centre_of_ngc1365Sérgio Sacani
1) XMM-Newton and NuSTAR observed the galaxy NGC 1365 simultaneously over 130 ks, detecting broadband X-ray emission from 3-79 keV.
2) The observations revealed variable absorption below 10 keV and prominent broad emission features between 5-7 keV and 10-30 keV, indicative of relativistic reflection from an accretion disk near a spinning supermassive black hole.
3) Time-resolved spectral analysis was able to disentangle the variable absorption component from the relativistic reflection component. Absorption-dominated models without reflection could be ruled out statistically and on physical grounds.
The document discusses a research project on 3D stacked chip architectures and interlayer cooling, including developing through-silicon vias for vertical electrical connections, using two-phase refrigerant cooling to remove heat from chip stacks more effectively than backside cooling, and experimental work on microchannel heat sinks, boiling visualization, and bubble dynamics simulation using an arbitrary Lagrangian-Eulerian technique.
This summary provides the key information from the document in 3 sentences:
The document discusses nuclear physics concepts such as nuclear structure, binding energy, mass defect, radioactive decay, and half-life. It includes examples calculating physical properties like mass, radius, binding energy, and activity for various nuclei. The examples analyze nuclear reactions and decays, and solve related problems involving time, mass, energy, and radioactive decay calculations.
Atmospheric aberrations in coherent laser systemswtyru1989
The document discusses atmospheric effects on coherent laser systems and compensation methods. It presents:
1) Simulations of atmospheric propagation using phase screens and analyzing phase distortion, beam wander, spreading, and scintillation.
2) Techniques for compensating atmospheric effects in coherent measurements, including phase compensation receivers and adaptive optics.
3) Modeling of beam projection in coherent lidars and analyzing compensation of speckle averaging using non-conjugated adaptive optics.
This document summarizes key concepts and equations related to wave motion from a physics textbook. It discusses transverse and longitudinal waves, and defines terms like amplitude, wavelength, frequency, period, and speed. It also covers topics like standing waves, harmonics, wave energy, and calculating the fundamental frequency and overtones of vibrating strings and ropes based on their tension, mass, and length. Sample problems are provided and worked through applying these concepts and equations to different scenarios.
The document discusses switchgear technology and circuit breaker operation. It covers several topics in 3 sentences or less:
Static welding of contacts can be overcome by increasing contact force and occurs at lower currents than dynamic welding. Arc interruption requires increasing plasma resistance at current zero and ensuring dielectric strength increases faster than electric stress. In a double frequency circuit, the voltages on the two circuits after opening will be proportional to the inductances in each circuit divided by the total inductance.
This document provides tables of constants, conversion factors, units, prefixes, values of trigonometric functions for common angles, and equations for Newtonian mechanics, electricity, and magnetism that are relevant for the 2002 AP Physics B exam. The tables include fundamental physical constants such as the speed of light, Planck's constant, electron mass, and more. Units covered include meters, kilograms, seconds, amperes, kelvins, and others. Prefixes from giga to pico are also listed.
Instantaneous Gelation in Smoluchwski's Coagulation Equation Revisited, Confe...Colm Connaughton
Invited talk given at "Boltzmann equation:
mathematics, modeling and simulations
In memory of Carlo Cercignani", Institut Henri Poincare, Paris, February 11, 2011.
1) The rotational Doppler effect describes a change in the resonant frequency of a system due to relative rotation between the emitter and observer. (Beginning sentence)
2) For magnetic resonance systems like ESR, NMR, and FMR, the resonant frequency is sensitive to magnetic fields and will shift due to the rotational Doppler effect caused by particle rotation.
3) For free magnetic nanoparticles with rotation rates of around 100 kHz, the rotational Doppler shift of around 100 kHz is measurable and on the same order as the linewidth for ESR and FMR, allowing determination of the maximum position with 100 kHz accuracy.
IJERA (International journal of Engineering Research and Applications) is International online, ... peer reviewed journal. For more detail or submit your article, please visit www.ijera.com
1) A changing magnetic flux induces an electromotive force (EMF) in a conductor according to Faraday's law of induction.
2) The direction of the induced current is such that the resulting magnetic field opposes the original change in flux according to Lenz's law.
3) For a conducting loop, the induced electric field is uniform and can be calculated from the rate of change of magnetic flux through the loop.
The document discusses how electrical signals propagate through the heart. It begins by introducing the heart model as involving electricity, mechanics, elasticity and fluids. It then discusses how the electrical signal propagates as a non-decremental traveling wave through the heart tissue. The document notes that the heart tissue is strongly anisotropic, conducting electrical signals faster along fiber directions than across fibers. It proposes using the method of moving frames to simulate electrophysiology phenomena on complex anisotropic heart geometries.
This document discusses inhomogeneous cosmological models as an alternative to the standard cosmological model. It begins by outlining the standard model and some of its variations proposed to address issues like dark energy. It then introduces the Lemaitre-Tolman-Bondi metric, which allows for spherical symmetry and spatial variations. Key aspects of inhomogeneous models using this metric are that they have two expansion rates and three free functions of spatial position that describe the matter profile, initial positions, and expansion rates. These models can evolve from an initially homogeneous early state to a currently inhomogeneous one.
Optimization of Multi-Object Spectroscopy in AstronomyCosmoAIMS Bassett
The document discusses optimizing multi-object spectroscopy (MOS) field configuration through simulated annealing. MOS involves using fiber optic cables or slit masks to obtain spectra from hundreds of celestial objects simultaneously. Properly configuring the fibers/slits is challenging due to constraints like limited reach and avoiding collisions. The author details how simulated annealing, a probabilistic technique inspired by physical processes, can be applied to find high-quality MOS configurations. It was shown to significantly outperform previous methods in terms of target yield and flexibility. The author proposes adapting this approach to optimize slit mask configuration for the MOS instrument being developed on the Southern African Large Telescope.
Literacy and Numeracy week concluded with family members visiting classes to see students make roosters based on the story "Kip". It was a great end to a successful Literacy and Numeracy week. Students and teachers had a wonderful time during the week's activities.
A short introduction to massive gravity... or ... Can one give a mass to the ...CosmoAIMS Bassett
1. The document discusses massive gravity and proposes that giving the graviton a small mass could potentially explain dark matter and dark energy without needing to introduce those concepts.
2. It reviews several models of massive gravity, including the Dvali-Gabadadze-Porrati model, which produces cosmic acceleration similar to dark energy. Kaluza-Klein theory is also discussed as producing massive gravitons.
3. Nonlinear extensions of the Pauli-Fierz theory are examined, finding solutions only with singularities. The "Goldstone" description of massive gravity is introduced as a way to better understand nonlinear effects like the Vainshtein mechanism.
- The government deficit and debt of the euro area and EU27 increased in 2009 compared to 2008 due to falling GDP.
- The government deficit as a percentage of GDP increased to 6.3% in the euro area and 6.8% in the EU27. Government debt as a percentage of GDP increased to 78.7% in the euro area and 73.6% in the EU27.
- Several countries had government deficits over 10% of GDP including Ireland, Greece, the UK, Spain, and Portugal. No country had a government surplus in 2009.
The document discusses Coulomb's law and its application to calculate the electric field and force between point charges. It also introduces the concepts of electric field intensity and field lines to visualize electric fields. Continuous charge distributions such as line, surface, and volume charges are described. The electric field of an infinite line charge is derived using calculus by treating the line as an integral of point charges.
Second Order Perturbations During Inflation Beyond Slow-rollIan Huston
This document outlines research on second-order perturbations during inflation beyond the slow-roll approximation. It discusses perturbation theory at first and second order, and presents results on the source term and second-order perturbations for inflation models with features. The document also describes Pyflation, an open-source Python code for numerically calculating inflationary perturbations up to second order, and outlines future goals for the code including calculating the three-point function and incorporating multi-field models.
The document provides an overview of bonding, molecular vibrations, and lattice vibrations in crystals. It discusses different types of bonding including ionic, covalent, metallic, and secondary bonding. It examines the periodic table and how elements form bonds. It also covers crystal structures, unit cells, X-ray diffraction, and how bonding influences material properties like melting temperature and elastic modulus. Finally, it summarizes vibrational frequencies of molecules and lattice vibrations in crystals using the harmonic approximation.
The document discusses the field of magnetism from 1990-2010, including topics such as quantum magnetism, single-domain particles, molecular magnets, magnetic deflagration, and the rotational Doppler effect in magnetic resonance systems which can be used to detect the rotation of nanoparticles.
1. A correction factor FB is proposed to consider the effect of bending in the stress intensity factor calculation for fatigue cracks in welded joints. FB is derived based on the principle of superposition.
2. Fatigue tests were conducted on welded joint specimens under bending. Crack shapes agreed well with predictions using the proposed FB factor. Cracks propagated until the a/t ratio reached 0.78.
3. Finite element analysis was used to derive stress concentration correction factors FG for different weld geometries. Predictions using the proposed approach agreed well with fatigue test results.
Introduction to Scanning Tunneling Microscopynirupam12
This document provides an overview of scanning tunneling microscopy (STM) principles and applications. It begins with a general introduction and outlines the basic theoretical framework of STM operation. Specifically, it discusses how STM works by bringing a tip within atomic reach of a surface and measuring tunneling current. The document then covers various STM capabilities such as surface characterization, probing oxides and high-temperature superconductors, and atomic resolution imaging. It concludes by discussing advanced STM techniques including spectroscopy, momentum-space imaging, spin-polarized measurements, and time-resolved applications with picosecond resolution.
A comparison of VLSI interconnect modelshappybhatia
This document presents a comparative study of delay analysis for carbon nanotube and copper based VLSI interconnect models. It outlines the introduction, interconnect models, factors affecting interconnect performance, and comparison of CNT vs copper. It then discusses analytical delay estimation using the driver interconnect model and modified nodal analysis, as well as SPICE simulation results comparing CNT and copper. The goal is to analyze and compare the delay performance of CNT and copper interconnects.
A Comparison Of Vlsi Interconnect Modelshappybhatia
The document presents a comparative study of delay analysis for carbon nanotube and copper based VLSI interconnect models. It analyzes the performance of CNT and copper interconnects using analytical delay estimation techniques like the driver interconnect load model, modified nodal analysis, and the unified time delay model. Simulation results show that CNT bundle interconnects provide significant delay improvement over copper interconnects for certain parameters like repeater sizing and pitch ratio.
Further discriminatory signature of inflationLaila A
These are the slides of the talk I gave on discriminating between models of inflation using space based gravitational wave detectors, at KEK in Tskuba University, Japan.
1) Small particles in oscillatory flows with traveling waves tend to form ordered, low-dimensional structures known as particulate coherent structures (PAS).
2) The particles synchronize with the traveling waves, causing their individual motions to phase lock with the wave frequency and form the PAS.
3) Contrary to initial expectations, the mechanism behind PAS formation is quite simple - the inertial forces from the oscillatory flow and wave cause particles to synchronize with the wave, leading to the ordered structures.
This document discusses magnetic deflagration and detonation in nanomagnets and manganites. It summarizes previous work on magnetic avalanches in these materials and introduces the concept of quantum magnetic deflagration. Key findings include observing deflagration fronts propagating at resonant magnetic fields and a potential deflagration to detonation transition. The document also discusses using surface acoustic waves and high-frequency EPR to study spin dynamics, as well as observing magnetic deflagration and colossal resistivity changes in manganites.
Alfvén waves and their kinetic modifications like kinetic Alfvén waves play an important role in space weather and plasma energization processes. Kinetic Alfvén waves are able to dissipate energy and accelerate particles in various regions of space including the solar atmosphere, Earth's magnetosphere during substorms, and in forming features of the solar wind like proton beams. Open questions remain about the detailed theory and observations of kinetic Alfvén wave generation, propagation, and dissipation across different plasma environments.
Influence of Trap-Assisted Recombination on Polymer–Fullerene Solar Cells, Ca...disorderedmatter
The document discusses how trap-assisted recombination influences polymer-fullerene solar cells. It finds that:
1) Recombination in annealed P3HT:PCBM solar cells is reduced Langevin or higher order than second order, indicating the influence of traps.
2) Transient absorption measurements of P3HT also show recombination orders higher than second order at low temperatures, consistent with photo-CELIV results.
3) The disorder in pristine samples leads to even higher recombination orders, showing the influence of morphological factors like phase separation on recombination.
The document appears to be the syllabus for a 12th grade physics chapter on electrostatics. It includes 3 sections: 1) Key concepts related to electric charges, fields, potential, capacitance, and dielectrics, 2) Important formulas, and 3) Sample problems. The concepts cover topics such as Coulomb's law, electric fields, electric potential, capacitors, dielectrics, and more. Formulas provided include those for electric force, field, potential, capacitance, and other quantities. Sample problems demonstrate applications of the concepts and formulas to calculate values related to charges, fields, dipoles, capacitors, and more.
Spectroscopic ellipsometry is a technique for investigating the optical properties and electrodynamics of materials. It has several advantages over other optical techniques:
1) It provides an exact numerical inversion with no need for Kramers-Kronig transformations, allowing consistency checks.
2) Measurements are non-invasive and highly reproducible as they do not require reference samples.
3) It is very sensitive to thin film properties due to its ability to measure at oblique angles of incidence.
Ellipsometry has been used to study phenomena like superconductivity in cuprates and pnictides by measuring changes in spectral weight, and collective charge ordering in oxide superlattices.
This document discusses developing a pressure balance watt balance to redefine the kilogram in terms of the Planck constant. It would use two pressure balances in weighing mode for force comparison and oscillating coil motion in dynamic mode. Research is underway to improve pressure balance performance, measure coil motion and induced voltage, design magnets, and address ground vibration issues. The goal is to have an operational pressure balance watt balance by mid-2013 to contribute results in advance of a 2014 international dataset compilation.
Quadrupolar structures generated by chiral islands in freely suspended smecti...NunoSilvestre
This document describes a study of quadrupolar defect structures generated by chiral islands in freely suspended smectic C films. The researchers provide a quantitative model to describe interactions between topologically chiral islands that depend on the islands' chirality. Their model uses the Landau theory approach with an order parameter representing the smectic C layers. They find that as the separation between islands increases, the symmetric quadrupolar defect configuration breaks down and the defects begin to follow individual islands in a dipolar structure.
(1) Composite Inelastic Dark Matter models propose that dark matter is composed of bound states of new "dark" quarks that interact via a new dark force.
(2) The lightest dark matter state has a small mass splitting from another nearly degenerate state due to hyperfine interactions, analogous to atomic energy levels.
(3) This mass splitting of ~100 keV allows the model to explain apparent annual modulation seen by the DAMA experiment through inelastic dark matter scattering, while evading other direct detection constraints.
Similar to Non-Gaussian perturbations from mixed inflaton-curvaton scenario (20)
This document discusses machine learning concepts including supervised vs. unsupervised learning, clustering algorithms, and specific clustering methods like k-means and k-nearest neighbors. It provides examples of how clustering can be used for applications such as market segmentation and astronomical data analysis. Key clustering algorithms covered are hierarchy methods, partitioning methods, k-means which groups data by assigning objects to the closest cluster center, and k-nearest neighbors which classifies new data based on its closest training examples.
- The document discusses methods for characterizing dark energy and modified gravity models in a model-independent way using cosmological observations.
- Due to the "dark degeneracy" between dark matter and dark energy, it is not possible to separately measure the properties of dark matter and dark energy without assuming a specific model class.
- Observables like the Hubble parameter H(z) and gravitational potentials can be reconstructed from the data, but this does not break the degeneracy between dark matter and dark energy contributions.
- The scale-dependence of quantities like the gravitational potentials and growth rate can be used to test and constrain broad classes of dark energy and modified gravity models in a more model-independent way.
Seminar by Prof Bruce Bassett at IAP, Paris, October 2013CosmoAIMS Bassett
This document discusses the rise of machine learning and artificial intelligence in astronomy due to a massive increase in data from upcoming surveys. It will produce around an exabyte of data per day, far more than has been produced throughout human history. This raises issues around preparing students, and how science may be done. The document discusses using machine learning for tasks like supernova identification and classification. It also discusses challenges like ensuring machine learning results are trustworthy, and whether this can truly replace human genius. It explores the idea of a universal language for scientific theories that could be searched algorithmically.
The 21cm line from neutral hydrogen can be used to study cosmology during the first billion years of the universe. This includes the Dark Ages when no structures formed, the Cosmic Dawn when the first luminous objects formed, and the Epoch of Reionization when these objects reionized the intergalactic medium. Current and future 21cm experiments like LOFAR, MWA, PAPER, and HERA aim to detect the signal from these eras but face challenges in calibrating the instruments and subtracting bright foreground sources. Some progress has been made in placing upper limits on the signal and constraining the heating of the intergalactic medium by X-rays, but a clear detection of the signal is still needed
The document discusses the cosmic dawn and reionization period in the early universe. It describes the evolution from the dark ages after recombination to the epoch of reionization around z=6-20. Key aspects discussed include understanding the sources and sinks of ionizing photons that drove reionization, and challenges in modeling this period due to the large parameter space and scales involved, from single stars to the entire universe. Seminumerical simulations are presented as an efficient method to model reionization and predict 21cm signals.
This document summarizes recent research on how the sizes and densities of galaxies have changed over time. Studies have found that galaxies at high redshift had smaller sizes than present-day galaxies of the same mass, often by a factor of 2-3 within 1 kpc and over 100 times within the effective radius. Various mechanisms are discussed for how galaxies could have grown, including minor mergers which could increase size more than mass over time. The document also examines constraints on the amount of growth massive galaxies could have experienced through mergers between redshifts of 0.8 to 0.1 based on the luminosity and stellar mass functions remaining largely unchanged over this period.
Cluster abundances and clustering Can theory step up to precision cosmology?CosmoAIMS Bassett
This document discusses improvements to the Press-Schechter theory for modeling the abundances and clustering of dark matter halos. It proposes that modeling halo collapse as requiring the density to "step up" above a critical density threshold at progressively larger spatial scales provides a better approximation than assuming fully correlated or uncorrelated densities. This "stepping up" approach requires only 2-point statistics and can be applied to non-Gaussian fields. The document also suggests that modeling the distribution of density slopes at peak positions provides a way to match halo counts through an Excursion Set Peaks model.
This document discusses gravitational lensing and some of the challenges involved in measuring it. Gravitational lensing causes the apparent deflection of light from distant background sources as it passes massive foreground objects. Precise measurements of lensing effects can provide information about dark matter distributions and the geometry and growth of the universe. However, there are three main problems: accurately measuring galaxy shapes used to detect lensing distortions, determining reliable photometric redshifts for galaxies, and accounting for intrinsic alignments of galaxy orientations unrelated to lensing.
Testing cosmology with galaxy clusters, the CMB and galaxy clusteringCosmoAIMS Bassett
This document summarizes a presentation on testing cosmology using galaxy clusters, the cosmic microwave background, and galaxy clustering. It discusses combining measurements of cosmic growth and expansion from these sources to constrain departures from general relativity. Models are presented for linear, time-dependent departures from GR. Constraints on parameters like the growth index γ are shown from combinations of clusters, CMB, and galaxy data. Tightening constraints are achieved by adding baryon acoustic oscillation, supernova, and Hubble constant data. The document also briefly discusses using cluster counts to constrain primordial non-Gaussianity.
This document discusses galaxy formation and evolution from cosmological simulations and models. It summarizes that galaxy formation is driven by the hierarchical growth of dark matter halos, gas accretion via cold filamentary streams or hot spherical halos, and feedback regulating star formation. Galaxy properties like star formation rates and metallicities are set by the balance between gas inflow and outflow.
Spit, Duct Tape, Baling Wire & Oral Tradition: Dealing With Radio DataCosmoAIMS Bassett
The document discusses the process of creating radio interferometers and summarizing data from them. It begins with an overview of how a normal reflector telescope can be broken up and transformed into an interferometer by replacing the optical path with electronics and correlating signals between antenna elements. It then discusses some of the challenges in summarizing interferometer data, including missing information due to an incomplete coverage of the uv-plane, measurement errors that distort the signals, and direction-dependent effects that vary with time, antenna, and direction. The document introduces the concept of the Radio Interferometer Measurement Equation (RIME) to formally describe these direction-dependent distortions.
The document summarizes the MeerKAT radio telescope project in South Africa, including:
- MeerKAT will be the largest radio telescope in the southern hemisphere and one of the largest in the world, establishing a legacy for Africa. It is an SKA precursor project.
- The specifications for MeerKAT including the number of antennas, maximum baseline, bandwidth, frequency range, and survey plans.
- MeerKAT will initially consist of 64 antennas in 2016, expanding over time. It aims to carry out a number of surveys for HI, pulsars, galaxies, and fast/slow transients.
- Opportunities are outlined for students and faculty to get involved in radio astronomy research
This document provides guidance on reducing interferometric radio astronomy data from the Karoo Array Telescope (KAT-7) using the Common Astronomy Software Applications (CASA). It describes the multi-step process of calibration and imaging required to produce an image from the visibility measurements made by an interferometer. The key steps involve: 1) converting the raw data from HDF5 format to a measurement set, 2) loading and inspecting the data, 3) flagging bad or corrupted data, 4) solving for the complex gain calibration terms using calibrator sources, 5) splitting the data for source and calibrator, 6) deconvolving the dirty image using CLEAN to account for incomplete uv-coverage. Trouble
From Darkness, Light: Computing Cosmological ReionizationCosmoAIMS Bassett
1) Reionization occurred between redshifts of 10-6, beginning around 10 billion years ago and ending around 1 billion years ago.
2) Observations of the CMB and galaxies at z>6 provide constraints but questions remain about the sources and topology of reionization.
3) Cosmological simulations of reionization must model structure formation, radiation transport, and non-equilibrium chemistry and physics to help address open questions.
WHAT CAN WE DEDUCE FROM STUDIES OF NEARBY GALAXY POPULATIONS?CosmoAIMS Bassett
Studies of nearby galaxy populations using large optical surveys like SDSS have provided insights into galaxy formation and evolution. Key findings include identifying characteristic scales where baryon conversion peaks at halo masses of ~10^12 solar masses and galaxies transition from blue to red at stellar masses of ~10^10 solar masses. While surveys have constrained stellar populations and traced dark matter halos, they have not well constrained gas accretion onto galaxies, gas outflows, or the influence of black holes on galaxy evolution.
Binary pulsars provide an excellent tool to test theories of gravity. The document describes several binary pulsar systems and how measurements of their orbital parameters over time have allowed for high-precision tests of general relativity in strong gravitational fields. Specifically, the double pulsar system PSR J0737-3039A/B has enabled measurements that agree with general relativity predictions to within 0.05% precision by measuring parameters like periastron advance and gravitational redshift effects.
Cross Matching EUCLID and SKA using the Likelihood RatioCosmoAIMS Bassett
1) The document discusses using a likelihood ratio technique to identify counterparts between low-resolution radio data from surveys like SKA and optical/infrared data from surveys like Euclid.
2) The likelihood ratio technique calculates probabilities that potential counterparts are true matches versus random alignments based on positional offsets and magnitude distributions.
3) Applying the technique to simulated lower-resolution radio data shows a 3-5% loss in identified counterparts compared to high-resolution data, with the worst effects for faint radio sources. However, the vast majority of identified counterparts remain the same.
The document discusses using machine learning techniques to classify astronomical objects from large surveys. It notes that surveys are producing huge amounts of data that conventional methods cannot fully process. Machine learning can be used to help classify objects and sort candidates. Specifically, the document discusses using machine learning on photometric data from the Sloan Digital Sky Survey (SDSS) to identify low-redshift quasars. It notes challenges including the large size and dimensionality of the data, and proposes using a boosted ensemble method to learn weights for different regions of feature space rather than trying to estimate probabilities. This would help classify objects from the SDSS into categories like quasars, stars or galaxies.
The document discusses results from the Planck space telescope. It describes how Planck mapped the cosmic microwave background (CMB) using instruments on board that observed at multiple frequencies. The high-quality CMB maps from Planck allowed for improved constraints on cosmological parameters like the age of the universe, matter/energy densities, and support for the standard Lambda CDM model. Planck was also able to probe large scale structure through CMB lensing, detect galaxy clusters via the Sunyaev-Zeldovich effect, and map the cosmic infrared background.
Ocean lotus Threat actors project by John Sitima 2024 (1).pptxSitimaJohn
Ocean Lotus cyber threat actors represent a sophisticated, persistent, and politically motivated group that poses a significant risk to organizations and individuals in the Southeast Asian region. Their continuous evolution and adaptability underscore the need for robust cybersecurity measures and international cooperation to identify and mitigate the threats posed by such advanced persistent threat groups.
Cosa hanno in comune un mattoncino Lego e la backdoor XZ?Speck&Tech
ABSTRACT: A prima vista, un mattoncino Lego e la backdoor XZ potrebbero avere in comune il fatto di essere entrambi blocchi di costruzione, o dipendenze di progetti creativi e software. La realtà è che un mattoncino Lego e il caso della backdoor XZ hanno molto di più di tutto ciò in comune.
Partecipate alla presentazione per immergervi in una storia di interoperabilità, standard e formati aperti, per poi discutere del ruolo importante che i contributori hanno in una comunità open source sostenibile.
BIO: Sostenitrice del software libero e dei formati standard e aperti. È stata un membro attivo dei progetti Fedora e openSUSE e ha co-fondato l'Associazione LibreItalia dove è stata coinvolta in diversi eventi, migrazioni e formazione relativi a LibreOffice. In precedenza ha lavorato a migrazioni e corsi di formazione su LibreOffice per diverse amministrazioni pubbliche e privati. Da gennaio 2020 lavora in SUSE come Software Release Engineer per Uyuni e SUSE Manager e quando non segue la sua passione per i computer e per Geeko coltiva la sua curiosità per l'astronomia (da cui deriva il suo nickname deneb_alpha).
Programming Foundation Models with DSPy - Meetup SlidesZilliz
Prompting language models is hard, while programming language models is easy. In this talk, I will discuss the state-of-the-art framework DSPy for programming foundation models with its powerful optimizers and runtime constraint system.
OpenID AuthZEN Interop Read Out - AuthorizationDavid Brossard
During Identiverse 2024 and EIC 2024, members of the OpenID AuthZEN WG got together and demoed their authorization endpoints conforming to the AuthZEN API
GraphRAG for Life Science to increase LLM accuracyTomaz Bratanic
GraphRAG for life science domain, where you retriever information from biomedical knowledge graphs using LLMs to increase the accuracy and performance of generated answers
In the rapidly evolving landscape of technologies, XML continues to play a vital role in structuring, storing, and transporting data across diverse systems. The recent advancements in artificial intelligence (AI) present new methodologies for enhancing XML development workflows, introducing efficiency, automation, and intelligent capabilities. This presentation will outline the scope and perspective of utilizing AI in XML development. The potential benefits and the possible pitfalls will be highlighted, providing a balanced view of the subject.
We will explore the capabilities of AI in understanding XML markup languages and autonomously creating structured XML content. Additionally, we will examine the capacity of AI to enrich plain text with appropriate XML markup. Practical examples and methodological guidelines will be provided to elucidate how AI can be effectively prompted to interpret and generate accurate XML markup.
Further emphasis will be placed on the role of AI in developing XSLT, or schemas such as XSD and Schematron. We will address the techniques and strategies adopted to create prompts for generating code, explaining code, or refactoring the code, and the results achieved.
The discussion will extend to how AI can be used to transform XML content. In particular, the focus will be on the use of AI XPath extension functions in XSLT, Schematron, Schematron Quick Fixes, or for XML content refactoring.
The presentation aims to deliver a comprehensive overview of AI usage in XML development, providing attendees with the necessary knowledge to make informed decisions. Whether you’re at the early stages of adopting AI or considering integrating it in advanced XML development, this presentation will cover all levels of expertise.
By highlighting the potential advantages and challenges of integrating AI with XML development tools and languages, the presentation seeks to inspire thoughtful conversation around the future of XML development. We’ll not only delve into the technical aspects of AI-powered XML development but also discuss practical implications and possible future directions.
Introduction of Cybersecurity with OSS at Code Europe 2024Hiroshi SHIBATA
I develop the Ruby programming language, RubyGems, and Bundler, which are package managers for Ruby. Today, I will introduce how to enhance the security of your application using open-source software (OSS) examples from Ruby and RubyGems.
The first topic is CVE (Common Vulnerabilities and Exposures). I have published CVEs many times. But what exactly is a CVE? I'll provide a basic understanding of CVEs and explain how to detect and handle vulnerabilities in OSS.
Next, let's discuss package managers. Package managers play a critical role in the OSS ecosystem. I'll explain how to manage library dependencies in your application.
I'll share insights into how the Ruby and RubyGems core team works to keep our ecosystem safe. By the end of this talk, you'll have a better understanding of how to safeguard your code.
Threats to mobile devices are more prevalent and increasing in scope and complexity. Users of mobile devices desire to take full advantage of the features
available on those devices, but many of the features provide convenience and capability but sacrifice security. This best practices guide outlines steps the users can take to better protect personal devices and information.
Have you ever been confused by the myriad of choices offered by AWS for hosting a website or an API?
Lambda, Elastic Beanstalk, Lightsail, Amplify, S3 (and more!) can each host websites + APIs. But which one should we choose?
Which one is cheapest? Which one is fastest? Which one will scale to meet our needs?
Join me in this session as we dive into each AWS hosting service to determine which one is best for your scenario and explain why!
Fueling AI with Great Data with Airbyte WebinarZilliz
This talk will focus on how to collect data from a variety of sources, leveraging this data for RAG and other GenAI use cases, and finally charting your course to productionalization.
How to Interpret Trends in the Kalyan Rajdhani Mix Chart.pdfChart Kalyan
A Mix Chart displays historical data of numbers in a graphical or tabular form. The Kalyan Rajdhani Mix Chart specifically shows the results of a sequence of numbers over different periods.
Monitoring and Managing Anomaly Detection on OpenShift.pdfTosin Akinosho
Monitoring and Managing Anomaly Detection on OpenShift
Overview
Dive into the world of anomaly detection on edge devices with our comprehensive hands-on tutorial. This SlideShare presentation will guide you through the entire process, from data collection and model training to edge deployment and real-time monitoring. Perfect for those looking to implement robust anomaly detection systems on resource-constrained IoT/edge devices.
Key Topics Covered
1. Introduction to Anomaly Detection
- Understand the fundamentals of anomaly detection and its importance in identifying unusual behavior or failures in systems.
2. Understanding Edge (IoT)
- Learn about edge computing and IoT, and how they enable real-time data processing and decision-making at the source.
3. What is ArgoCD?
- Discover ArgoCD, a declarative, GitOps continuous delivery tool for Kubernetes, and its role in deploying applications on edge devices.
4. Deployment Using ArgoCD for Edge Devices
- Step-by-step guide on deploying anomaly detection models on edge devices using ArgoCD.
5. Introduction to Apache Kafka and S3
- Explore Apache Kafka for real-time data streaming and Amazon S3 for scalable storage solutions.
6. Viewing Kafka Messages in the Data Lake
- Learn how to view and analyze Kafka messages stored in a data lake for better insights.
7. What is Prometheus?
- Get to know Prometheus, an open-source monitoring and alerting toolkit, and its application in monitoring edge devices.
8. Monitoring Application Metrics with Prometheus
- Detailed instructions on setting up Prometheus to monitor the performance and health of your anomaly detection system.
9. What is Camel K?
- Introduction to Camel K, a lightweight integration framework built on Apache Camel, designed for Kubernetes.
10. Configuring Camel K Integrations for Data Pipelines
- Learn how to configure Camel K for seamless data pipeline integrations in your anomaly detection workflow.
11. What is a Jupyter Notebook?
- Overview of Jupyter Notebooks, an open-source web application for creating and sharing documents with live code, equations, visualizations, and narrative text.
12. Jupyter Notebooks with Code Examples
- Hands-on examples and code snippets in Jupyter Notebooks to help you implement and test anomaly detection models.
UiPath Test Automation using UiPath Test Suite series, part 6DianaGray10
Welcome to UiPath Test Automation using UiPath Test Suite series part 6. In this session, we will cover Test Automation with generative AI and Open AI.
UiPath Test Automation with generative AI and Open AI webinar offers an in-depth exploration of leveraging cutting-edge technologies for test automation within the UiPath platform. Attendees will delve into the integration of generative AI, a test automation solution, with Open AI advanced natural language processing capabilities.
Throughout the session, participants will discover how this synergy empowers testers to automate repetitive tasks, enhance testing accuracy, and expedite the software testing life cycle. Topics covered include the seamless integration process, practical use cases, and the benefits of harnessing AI-driven automation for UiPath testing initiatives. By attending this webinar, testers, and automation professionals can gain valuable insights into harnessing the power of AI to optimize their test automation workflows within the UiPath ecosystem, ultimately driving efficiency and quality in software development processes.
What will you get from this session?
1. Insights into integrating generative AI.
2. Understanding how this integration enhances test automation within the UiPath platform
3. Practical demonstrations
4. Exploration of real-world use cases illustrating the benefits of AI-driven test automation for UiPath
Topics covered:
What is generative AI
Test Automation with generative AI and Open AI.
UiPath integration with generative AI
Speaker:
Deepak Rai, Automation Practice Lead, Boundaryless Group and UiPath MVP
TrustArc Webinar - 2024 Global Privacy SurveyTrustArc
How does your privacy program stack up against your peers? What challenges are privacy teams tackling and prioritizing in 2024?
In the fifth annual Global Privacy Benchmarks Survey, we asked over 1,800 global privacy professionals and business executives to share their perspectives on the current state of privacy inside and outside of their organizations. This year’s report focused on emerging areas of importance for privacy and compliance professionals, including considerations and implications of Artificial Intelligence (AI) technologies, building brand trust, and different approaches for achieving higher privacy competence scores.
See how organizational priorities and strategic approaches to data security and privacy are evolving around the globe.
This webinar will review:
- The top 10 privacy insights from the fifth annual Global Privacy Benchmarks Survey
- The top challenges for privacy leaders, practitioners, and organizations in 2024
- Key themes to consider in developing and maintaining your privacy program
Webinar: Designing a schema for a Data WarehouseFederico Razzoli
Are you new to data warehouses (DWH)? Do you need to check whether your data warehouse follows the best practices for a good design? In both cases, this webinar is for you.
A data warehouse is a central relational database that contains all measurements about a business or an organisation. This data comes from a variety of heterogeneous data sources, which includes databases of any type that back the applications used by the company, data files exported by some applications, or APIs provided by internal or external services.
But designing a data warehouse correctly is a hard task, which requires gathering information about the business processes that need to be analysed in the first place. These processes must be translated into so-called star schemas, which means, denormalised databases where each table represents a dimension or facts.
We will discuss these topics:
- How to gather information about a business;
- Understanding dictionaries and how to identify business entities;
- Dimensions and facts;
- Setting a table granularity;
- Types of facts;
- Types of dimensions;
- Snowflakes and how to avoid them;
- Expanding existing dimensions and facts.
Non-Gaussian perturbations from mixed inflaton-curvaton scenario
1. Non-Gaussian perturbations from mixed
inflaton-curvaton scenario
José Fonseca - University of Portsmouth
Based on a paper with David Wands arxiv:1101.1254/Phys. Rev. D 83, 064025 (2011) and
current work
13-Feb at AIMS
Quarta-feira, 15 de Fevereiro de 12
2. The Plan
• Motivation;
• Perturbations from inflation in a nutshell;
• Curvaton Scenario;
• Mixed perturbations;
• Constraints on curvaton dominated theories;
• Including inflation perturbations;
• Summary
Quarta-feira, 15 de Fevereiro de 12
3. This is a pic of the Cosmic Microwave Background, aka CMB!
Power Spectrum of
primordial density
perturbations
✓ ◆ns (k0 ) 1
k
P⇣ (k) = ⇣ (k0 )
2
k0
1
k0 = 0.002Mpc
2 +0.091 9
(k0 ) = (2.430 0.091 ) ⇥ 10
+0.012
ns (k0 ) = 0.968 0.012
E. Komatsu et al, Seven-year
WMAP Observations:
Cosmological Interpretation
- arXiv:1001.4538v1
Quarta-feira, 15 de Fevereiro de 12
4. This is a pic of the Cosmic Microwave Background, aka CMB!
Power Spectrum of
Bispectrum from quadratic
primordial density
corrections
perturbations
✓ ◆ns (k0 ) 1
k 3
P⇣ (k) = ⇣ (k0 )
2
⇣ = ⇣1 + fnl (⇣1
2 2
h⇣1 i)
k0 5
1
k0 = 0.002Mpc
2 +0.091 9
(k0 ) = (2.430 0.091 ) ⇥ 10 10 < fnl < 74
+0.012
ns (k0 ) = 0.968 0.012
E. Komatsu et al, Seven-year
WMAP Observations:
Single field inflation is
Cosmological Interpretation
perfectly fine but...
- arXiv:1001.4538v1
Quarta-feira, 15 de Fevereiro de 12
5. Perturbations from
inflation in a nutshell
Quarta-feira, 15 de Fevereiro de 12
6. INFLATON
3H ˙ ⇥ V
SCALAR FIELD LIVING IN A FRW UNIVERSE THAT
DRIVES INFLATION. 2 V( )
H '
3m2 l
P
PERTURBATIONS FROM INFLATION IN A NUTSHELL
STANDARD INFLATION = INFLATON + SLOW ROLL
Quarta-feira, 15 de Fevereiro de 12
7. INFLATON
3H ˙ ⇥ V
SCALAR FIELD LIVING IN A FRW UNIVERSE THAT
DRIVES INFLATION. 2 V( )
H '
3m2 l
P
SLOW ROLL
✓ ◆2
THE FIELD HAS AN OVER-DAMPED EVOLUTION, I.E., IT
1 2 V
✏ ⌘ mP l ⌧1
ROLLS DOWN THE POTENTIAL SLOWLY. 2 V
THE EXPANSION IS ALMOST EXPONENTIAL.
KINETIC ENERGY DOES NOT VARY WITHIN 1 HUBBLE 2 V
TIME.
|⌘ |⌘ mP l ⌧1
V
THE POTENTIAL NEEDS TO BE FLAT.
PERTURBATIONS FROM INFLATION IN A NUTSHELL
STANDARD INFLATION = INFLATON + SLOW ROLL
Quarta-feira, 15 de Fevereiro de 12
8. SPLIT QUANTITIES BETWEEN BACKGROUND AND 1ST
O R D E R P E R T U R B AT I O N ( G A U S S I A N VA C U U M ⇥(t, x) = ⇥(t) + ⇥(t, x)
FLUCTUATIONS)
✓ ◆
EQ. OF MOTION FOR THE FIELD PERTURBATIONS (IN ¨ ˙
⇥k + 3H ⇥k +
k2
+ m2 ⇥k = 0
FOURIER SPACE) FOR A “MASSLESS” FIELD. a2
⇥ ⇤2
POWER SPECTRUM OF FIELD PERTURBATIONS AT H
P ⇥
HORIZON EXIT 2 k=aH
PERTURBATIONS FROM INFLATION IN A NUTSHELL
POWER SPECTRUM OF PERTURBATIONS FOR A MASSLESS FIELD DURING INFLATION
Quarta-feira, 15 de Fevereiro de 12
9. 0
THE “SEPARATE UNIVERSE” PICTURE SAYS 2 SUPER-
HORIZON REGIONS OF THE UNIVERSE EVOLVE AS IF t2
THEY WERE SEPARATE FRIEDMANN-ROBERTSON-
W A L K E R U N I V E R S E S W H I C H A R E L O C A L LY
-1
cH s
HOMOGENEOUS BUT MAY HAVE DIFFERENT DENSITIES
AND PRESSURE. t1
a b
Wands et al., astro-ph/0003278v2
THE CURVATURE PERTURBATION ZETA IS THEN GIVEN
BY THE DIFFERENCE OF THE INTEGRATED EXPANSION ⇥ = N
FROM A SPATIALY-FLAT HYPERSURFACE TO A
UNIFORM-DENSITY HYPERSURFACE .
1 00 2
DIFFERENT PATCHES OF THE UNIVERSE WILL HAVE N = 0
N ⇤⇤ + N ⇤⇤
DIFFERENT EXPANSION HISTORIES DUE TO DIFFERENT 2
INITIAL CONDITIONS
PERTURBATIONS FROM INFLATION IN A NUTSHELL
DELTA N FORMALISM AND THE SEPARATE UNIVERSE PICTURE
Quarta-feira, 15 de Fevereiro de 12
10. POWER SPECTRUM AND SCALE DEPENDENCE
✓ ◆2
POWER SPECTRUM OF CURVATURE PERTURBATIONS
1 H⇤
P⇣ ⇤
'
W H I C H R E M A I N S C O N S TA N T F O R A D I A B AT I C 2✏⇤ 2⇡mP l
PERTURBATIONS ON LARGE SCALES
d ln P⇣
TILT n⇣ 1⌘
d ln k
ns 1⇥ 6 + 2⇥
dn⇣
RUNNING ↵⇣ ⌘ s ⇥ 24⇥2 + 16⇥ ⇤ 2⌅ 2
d ln k
PERTURBATIONS FROM INFLATION IN A NUTSHELL
OBSERVATIONAL PREDICTIONS FOR SINGLE FIELD
Quarta-feira, 15 de Fevereiro de 12
11. POWER SPECTRUM AND SCALE DEPENDENCE
✓ ◆2
POWER SPECTRUM OF CURVATURE PERTURBATIONS
1 H⇤
P⇣ ⇤
'
W H I C H R E M A I N S C O N S TA N T F O R A D I A B AT I C 2✏⇤ 2⇡mP l
PERTURBATIONS ON LARGE SCALES
d ln P⇣
TILT n⇣ 1⌘
d ln k
ns 1⇥ 6 + 2⇥
dn⇣
RUNNING ↵⇣ ⌘ s ⇥ 24⇥2 + 16⇥ ⇤ 2⌅ 2
d ln k
GRAVITATIONAL WAVES
✓ ◆2
2 H⇤
TENSOR-TO-SCALAR RATIO rT ⌘ PG /P⇣ rT =
m2 l P⇣
P 2⇡
PERTURBATIONS FROM INFLATION IN A NUTSHELL
OBSERVATIONAL PREDICTIONS FOR SINGLE FIELD
Quarta-feira, 15 de Fevereiro de 12
12. POWER SPECTRUM AND SCALE DEPENDENCE
✓ ◆2
POWER SPECTRUM OF CURVATURE PERTURBATIONS
1 H⇤
P⇣ ⇤
'
W H I C H R E M A I N S C O N S TA N T F O R A D I A B AT I C 2✏⇤ 2⇡mP l
PERTURBATIONS ON LARGE SCALES
d ln P⇣
TILT n⇣ 1⌘
d ln k
ns 1⇥ 6 + 2⇥
dn⇣
RUNNING ↵⇣ ⌘ s ⇥ 24⇥2 + 16⇥ ⇤ 2⌅ 2
d ln k
GRAVITATIONAL WAVES
✓ ◆2
2 H⇤
TENSOR-TO-SCALAR RATIO rT ⌘ PG /P⇣ rT =
m2 l P⇣
P 2⇡
NON-GAUSSIANITY
CONSERVED CURVATURE PERTURBATION REMAINS 5
GAUSSIAN
fnl = (2 ⇤ ⇥ )⌧1
6
PERTURBATIONS FROM INFLATION IN A NUTSHELL
OBSERVATIONAL PREDICTIONS FOR SINGLE FIELD
Quarta-feira, 15 de Fevereiro de 12
14. IT IS AN INFLATIONARY MODEL.
THE INFLATON DRIVES THE ACCELERATED EXPANSION Lyth&Wands: hep-th/0110002
Enqvist&Sloth: hep-ph/0109214
WHILE THE CURVATON PRODUCES THE STRUCTURE IN Moroi&Takahashi: hep-ph/0110096
THE UNIVERSE.
THE CURVATON IS A LIGHT FIELD DURING INFLATION,
WEAKLY COUPLED AND LATE DECAYING, I.E., DECAYS H⇤ > m >
INTO RADIATION AFTER INFLATION.
CURVATON SCENARIO
MAIN PRINCIPLES
Quarta-feira, 15 de Fevereiro de 12
15. IT IS AN INFLATIONARY MODEL.
THE INFLATON DRIVES THE ACCELERATED EXPANSION Lyth&Wands: hep-th/0110002
Enqvist&Sloth: hep-ph/0109214
WHILE THE CURVATON PRODUCES THE STRUCTURE IN Moroi&Takahashi: hep-ph/0110096
THE UNIVERSE.
THE CURVATON IS A LIGHT FIELD DURING INFLATION,
WEAKLY COUPLED AND LATE DECAYING, I.E., DECAYS H⇤ > m >
INTO RADIATION AFTER INFLATION.
DURING INFLATION
SUBDOMINANT COMPONENT ⌧1
SINCE IT IS EFFECTIVELLY MASSLESS IT IS IN AN
OVER-DAMPED REGIME. THEREFORE OBEYS TO THE ⌧1 , ⇥ ⌧1
SLOW-ROLL CONDITIONS
✓ ◆2
AND ACQUIRES A SPECTRUM OF GAUSSIAN FIELD H⇤
PERTURBATIONS AT HORIZON EXIT P
2
CURVATON SCENARIO
MAIN PRINCIPLES
Quarta-feira, 15 de Fevereiro de 12
16. AFTER INFLATION
THE CURVATON IS AN ENTROPY DIRECTION, SO THE
CURVATURE PERTURBATION ON UNIFORM DENSITY ˙ 6= 0
⇣
HYPER-SURFACES IS NO LONGER CONSERVED
CURVATON SCENARIO
MAIN IDEAS
Quarta-feira, 15 de Fevereiro de 12
17. AFTER INFLATION
THE CURVATON IS AN ENTROPY DIRECTION, SO THE
CURVATURE PERTURBATION ON UNIFORM DENSITY ˙ 6= 0
⇣
HYPER-SURFACES IS NO LONGER CONSERVED
THE FIELD STARTS COHERENT OSCILLATIONS IN THE
BOTTOM OF THE POTENTIAL AND BEHAVES LIKE A H'm
MATTER FLUID.
CURVATON SCENARIO
MAIN IDEAS
Quarta-feira, 15 de Fevereiro de 12
18. AFTER INFLATION
THE CURVATON IS AN ENTROPY DIRECTION, SO THE
CURVATURE PERTURBATION ON UNIFORM DENSITY ˙ 6= 0
⇣
HYPER-SURFACES IS NO LONGER CONSERVED
THE FIELD STARTS COHERENT OSCILLATIONS IN THE
BOTTOM OF THE POTENTIAL AND BEHAVES LIKE A H'm
MATTER FLUID.
DECAYS INTO RADIATION AND TRANSFERS ITS
PERTURBATIONS
H'
CURVATON SCENARIO
MAIN IDEAS
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19. DURING AND AFTER INFLATION, THE CURVATON IS AN
S ⌘ 3 (⇣ ⇣ )
ENTROPY PERTURBATION
ZETA IS THE CURVATURE PERTURBATION ON UNIFORM H ⇢
⇣=
DENSITY HYPERSURFACES ⇢
˙
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
20. DURING AND AFTER INFLATION, THE CURVATON IS AN
S ⌘ 3 (⇣ ⇣ )
ENTROPY PERTURBATION
ZETA IS THE CURVATURE PERTURBATION ON UNIFORM H ⇢
⇣=
DENSITY HYPERSURFACES ⇢
˙
LOCAL CURVATON ENERGY DENSITY ⇢ = ⇢ eS = m2
¯ 2
osc
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
21. DURING AND AFTER INFLATION, THE CURVATON IS AN
S ⌘ 3 (⇣ ⇣ )
ENTROPY PERTURBATION
ZETA IS THE CURVATURE PERTURBATION ON UNIFORM H ⇢
⇣=
DENSITY HYPERSURFACES ⇢
˙
LOCAL CURVATON ENERGY DENSITY ⇢ = ⇢ eS = m2
¯ 2
osc
EXPAND LOCAL VALUE OF THE FIELD DURING 1 00
0 2
OSCILLATION IN TERMS OF ITS VEV AND FIELD osc 'g+g ⇤+ g ⇤
FLUCTUATIONS DURING INFLATION 2
G ACCOUNTS FOR NON-LINEAR EVOLUTION OF CHI osc ⌘ g( ⇤)
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
22. DURING AND AFTER INFLATION, THE CURVATON IS AN
S ⌘ 3 (⇣ ⇣ )
ENTROPY PERTURBATION
ZETA IS THE CURVATURE PERTURBATION ON UNIFORM H ⇢
⇣=
DENSITY HYPERSURFACES ⇢
˙
LOCAL CURVATON ENERGY DENSITY ⇢ = ⇢ eS = m2
¯ 2
osc
EXPAND LOCAL VALUE OF THE FIELD DURING 1 00
0 2
OSCILLATION IN TERMS OF ITS VEV AND FIELD osc 'g+g ⇤+ g ⇤
FLUCTUATIONS DURING INFLATION 2
G ACCOUNTS FOR NON-LINEAR EVOLUTION OF CHI osc ⌘ g( ⇤)
✓ ◆
1 gg 00 2
S = SG + 1 SG
4 g 02
THE ENTROPY PERTURBATION IS
g0
SG ⌘ 2 ⇤
g
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
23. THE FINAL CURVATON POWER SPECTRUM COMES ✓ 0
◆2
FROM THE MODES EXCITED DURING INFLATION AND g H⇤
FROM NON-LINEAR EVOLUTION OF THE FIELD UNTIL PS = 4
DECAY.
g 2⇡
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
24. THE FINAL CURVATON POWER SPECTRUM COMES ✓ 0
◆2
FROM THE MODES EXCITED DURING INFLATION AND g H⇤
FROM NON-LINEAR EVOLUTION OF THE FIELD UNTIL PS = 4
DECAY.
g 2⇡
⇥
AT DECAY ON UNIFORM TOTAL ENERGY DENSITY
(1 ⌦ ) e4(⇣ ⇣)
+
HYPERSURFACES WE HAVE ⇢ = ⇢r + ⇢ ⇤
+⌦ e3(⇣ ⇣)
=1
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
25. THE FINAL CURVATON POWER SPECTRUM COMES ✓ 0
◆2
FROM THE MODES EXCITED DURING INFLATION AND g H⇤
FROM NON-LINEAR EVOLUTION OF THE FIELD UNTIL PS = 4
DECAY.
g 2⇡
⇥
AT DECAY ON UNIFORM TOTAL ENERGY DENSITY
(1 ⌦ ) e4(⇣ ⇣)
+
HYPERSURFACES WE HAVE ⇢ = ⇢r + ⇢ ⇤
+⌦ e3(⇣ ⇣)
=1
AFTER THE DECAY ZETA IS CONSERVED ON SUPER- R2
HORIZON SCALES. WE DEFINE R AS THE TRANSFER P⇣ = P⇣ + PS
EFFICIENCY AT DECAY. 9
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
26. THE FINAL CURVATON POWER SPECTRUM COMES ✓ 0
◆2
FROM THE MODES EXCITED DURING INFLATION AND g H⇤
FROM NON-LINEAR EVOLUTION OF THE FIELD UNTIL PS = 4
DECAY.
g 2⇡
⇥
AT DECAY ON UNIFORM TOTAL ENERGY DENSITY
(1 ⌦ ) e4(⇣ ⇣)
+
HYPERSURFACES WE HAVE ⇢ = ⇢r + ⇢ ⇤
+⌦ e3(⇣ ⇣)
=1
AFTER THE DECAY ZETA IS CONSERVED ON SUPER- R2
HORIZON SCALES. WE DEFINE R AS THE TRANSFER P⇣ = P⇣ + PS
EFFICIENCY AT DECAY. 9
3
FOR A SUDDEN DECAY APPROXIMATION R ,dec =
4 dec
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
27. 2
THE WEIGHT OF THE CURVATON CONTRIBUTION TO R /9 P⇣
THE FINAL POWER SPECTRUM
w ⌘
P⇣
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
28. 2
THE WEIGHT OF THE CURVATON CONTRIBUTION TO R /9 P⇣
THE FINAL POWER SPECTRUM
w ⌘
P⇣
✓ ◆2
CRITICAL EPSILON FOR THE CURVATON. DEFINES THE 9 1 H⇤
FRONTIER BETWEEN RELEVANT CONTRIBUTIONS OF ✏c ⌘
2 R P⇣ 2⇡
THE CURVATON TO THE TOTAL POWER SPECTRUM
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
29. 2
THE WEIGHT OF THE CURVATON CONTRIBUTION TO R /9 P⇣
THE FINAL POWER SPECTRUM
w ⌘
P⇣
✓ ◆2
CRITICAL EPSILON FOR THE CURVATON. DEFINES THE 9 1 H⇤
FRONTIER BETWEEN RELEVANT CONTRIBUTIONS OF ✏c ⌘
2 R P⇣ 2⇡
THE CURVATON TO THE TOTAL POWER SPECTRUM
✓ ◆✓ ◆2
T H E P O W E R S P E C T R U M O F C U R V AT U R E 1 1 1 H⇤
P⇣ = +
PERTURBATIONS IN TERMS OF EPSILON CRITICAL 2 ✏⇤ ✏c 2⇡mP l
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
30. 2
THE WEIGHT OF THE CURVATON CONTRIBUTION TO R /9 P⇣
THE FINAL POWER SPECTRUM
w ⌘
P⇣
✓ ◆2
CRITICAL EPSILON FOR THE CURVATON. DEFINES THE 9 1 H⇤
FRONTIER BETWEEN RELEVANT CONTRIBUTIONS OF ✏c ⌘
2 R P⇣ 2⇡
THE CURVATON TO THE TOTAL POWER SPECTRUM
✓ ◆✓ ◆2
T H E P O W E R S P E C T R U M O F C U R V AT U R E 1 1 1 H⇤
P⇣ = +
PERTURBATIONS IN TERMS OF EPSILON CRITICAL 2 ✏⇤ ✏c 2⇡mP l
T H E C U R V AT O N I S T H E M A I N S O U R C E O F
PERTURBATIONS IF
✏⇤ ✏c
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS
Quarta-feira, 15 de Fevereiro de 12
31. SCALE DEPENDENCE OF POWER
SPECTRUM
n⇣ 1 = w (nS 1) + (1 w )(n⇣ 1)
TILT = 2✏⇤ + 2⌘ w + (1 w )( 4✏⇤ + 2⌘ )
2
RUNNING ↵⇣ = w ↵S + (1 w )↵⇣ + w (1 w ) nS n⇣
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS: OBSERVABLE QUANTITIES
Quarta-feira, 15 de Fevereiro de 12
32. SCALE DEPENDENCE OF POWER
SPECTRUM
n⇣ 1 = w (nS 1) + (1 w )(n⇣ 1)
TILT = 2✏⇤ + 2⌘ w + (1 w )( 4✏⇤ + 2⌘ )
2
RUNNING ↵⇣ = w ↵S + (1 w )↵⇣ + w (1 w ) nS n⇣
GRAVITATIONAL WAVES
TENSOR-TO-SCALAR RATIO rT = 16w ✏c = 16✏⇤ (1 w )
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS: OBSERVABLE QUANTITIES
Quarta-feira, 15 de Fevereiro de 12
33. SCALE DEPENDENCE OF POWER
SPECTRUM
n⇣ 1 = w (nS 1) + (1 w )(n⇣ 1)
TILT = 2✏⇤ + 2⌘ w + (1 w )( 4✏⇤ + 2⌘ )
2
RUNNING ↵⇣ = w ↵S + (1 w )↵⇣ + w (1 w ) nS n⇣
GRAVITATIONAL WAVES
TENSOR-TO-SCALAR RATIO rT = 16w ✏c = 16✏⇤ (1 w )
NON-GAUSSIANITY
5N ✓ ◆
5 gg 00 (g/g 0 )R0 2R
FNL fnl = w2 fnl = 1 + 02 + w2
6 N2 4R g R
⌧nl 36
TNL 2 = 25w
fnl
MIXED PERTURBATIONS
TRANSFER OF LINEAR PERTURBATIONS: OBSERVABLE QUANTITIES
Quarta-feira, 15 de Fevereiro de 12
34. CONSTRAINS ON
CURVATON
DOMINATED THEORIES
Fonseca & Wands
arxiv:1101.1254
Quarta-feira, 15 de Fevereiro de 12
35. Numerical Studies
Solve the Friedmann and the curvaton field evolution equations
prior to decay for diferent potential;
Ensure that the curvaton starts subdominant and overdamped;
We match it with fluid description of the curvaton decay studied by
Malik et al (2003) and Gupta et al (2004).
m
In principle there are 4 free parameters: ⇤ ✏⇤ H⇤
But the COBE normalisation of the power spectrum fixes the Hubble
scale during inflation.
In the curvaton limit the observables becomes independent of epsilon.
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36. Curvaton Limit 18.5
18 -1
Quadratic potential 17.5
1
1
rT
10
1 2 2 17 30 0.1
V( )= m
/GeV
100
2 16.5 0.01
fN L
*
Tensors and non-
10
16 0.001
log
linearities can be used 15.5
in a complementary 15
way to constrain the 14.5
model parameters. 14
3 4 5 6 7 8
log
9
m/
10 11 12 13 14
10
( 4
4.7 ⇥ 10 q⇤ for ⇤ ( /m)1/4 mP l
H⇤ ' 3 m2 l 1/4 < 5.7 ⇥ 1017 GeV
1.5 ⇥ 10 P
for ⇤ ⌧ ( /m) mP l ⇤
(
m ⇤ ✓ ◆2
5/4 for ( /m)1/4 mP l ⇤
q ⇤ < 0.023
fN L ' m2 l 1/4
m mP l
3.9 m P2 for ⇤ ⌧ ( /m) mP l
⇤
Quarta-feira, 15 de Fevereiro de 12
37. rg . 0.1
Curvaton Limit 18.5
18 -1
Quadratic potential 17.5
1
1
rT
10
1 2 2 17 30 0.1
V( )= m
/GeV
100
2 16.5 0.01
fN L
*
Tensors and non-
10
16 0.001
log
linearities can be used 15.5
in a complementary 15
way to constrain the 14.5
model parameters. 14
3 4 5 6 7 8 9 10 11 12 13 14
log
10
m/ fnl . 100
( 4
4.7 ⇥ 10 q⇤ for ⇤ ( /m)1/4 mP l
H⇤ ' 3 m2 l 1/4 < 5.7 ⇥ 1017 GeV
1.5 ⇥ 10 P
for ⇤ ⌧ ( /m) mP l ⇤
(
m ⇤ ✓ ◆2
5/4 for ( /m)1/4 mP l ⇤
q ⇤ < 0.023
fN L ' m2 l 1/4
m mP l
3.9 m P2 for ⇤ ⌧ ( /m) mP l
⇤
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42. Limits of Epsilon critical
✓ ◆2 Quadratic Potential
1 H⇤
✏c
18.5
P⇣ =
2✏c 2⇡mP l 18
1
✓ ◆2 17.5
9 g 1
✏c = 17
8 g 0 mP l R2
/GeV
0.01
16.5
*
10
16
Curvaton limit
log
0.0001
15.5
✏⇤ ✏c 15
Inflaton contributions 14.5
✏⇤ . ✏c 14
3 4 5 6 7 8
log
10
9
m/
10 11 12 13 14
We need to fix the first slow-roll parameter to identify each region.
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43. For ✏⇤ ⌘ ⌘ and w ' 1 we expect ✏⇤ = 0.02 from n⇣
17.5
0.24
17
✏c = 0.02
0.1
−1
16.5
0
0.01 In the curvaton
/GeV
1
16
limit region
*
0.001
10
15.5 10
rT ' 16✏c
log
30 2
15
✏⇤ = 0.02 ↵⇣ ' 2 (n⇣ 1)
100
14.5
fN L rT
14
7 8 9 10 11 12 13 14
log m/
10
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44. For ✏⇤ ⇠ ⌘ and w ' 1 we expect (✏⇤ ⌘ ) ' 0.02 from n⇣
17.5
✏c = 0.1
17
This case requires fine
0.24
−1
0
0.1 tuning of the slow roll
16.5
0.01 parameters
/GeV
16
*
0.001
No inflation
10
15.5
log
1
dominated power
15
✏⇤ = 0.1 10
spectrum allowed
14.5 30
fN L rT 100
14
6 7 8 9 10 11 12 13 14
log m/
10
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46. Summary
• The curvaton is an inflation model to
source structure in the universe and
predicts non-Gaussianities;
• The tensor-to-scalar ration and fnl can be
used in a complementary way to constrain
the curvaton model;
• Studied inflation contributions to the
power spectrum and in which regimes are
important.
Quarta-feira, 15 de Fevereiro de 12
47. Summary
• The curvaton is an inflation model to
source structure in the universe and
predicts non-Gaussianities;
• The tensor-to-scalar ration and fnl can be
used in a complementary way to constrain
the curvaton model;
• Studied inflation contributions to the
power spectrum and in which regimes are
important.
Thanks!
Quarta-feira, 15 de Fevereiro de 12