This document discusses the relationship between cosmic rays, solar activity, and climate/weather patterns. It outlines that solar wind modulates cosmic rays entering the atmosphere, which act as cloud condensation nuclei and affect cloud formation. Studies have found correlations between cosmic ray flux decreases during solar events and decreases in cloud cover. The document then discusses how this proposed mechanism may influence climate through impacts on cloud radiative forcing. It analyzes links between various climate patterns like the North Atlantic Oscillation and weather types with rainfall and temperature in Galicia, Spain, and how these correlations have changed over time with solar activity levels.
Herman mosquera2011 nonlinear electrodynamics and the pioneer 1011 spacecraftSOCIEDAD JULIO GARAVITO
1) The document discusses the unexplained "Pioneer anomaly" - an anomalous blueshift in radio signals from the Pioneer 10/11 spacecraft that suggests they are accelerating under an unexplained force.
2) Conventional explanations like gravitational effects, solar radiation pressure, and modified dynamics have been ruled out. The anomaly appears to be related to the electromagnetic sector rather than gravity.
3) The document proposes that nonlinear electrodynamics (NLED), where the electromagnetic field depends nonlinearly on the field strength, could explain an anomalous frequency shift in photons as they propagate through space without interacting with matter. This effect is called "photon acceleration".
- Simple harmonic motion describes oscillatory or back-and-forth motion caused by a restoring force proportional to displacement from equilibrium.
- Examples of objects that exhibit simple harmonic motion include springs, pendulums, and waves.
- The period and frequency of oscillation depend on attributes like the spring constant, length, or mass in the case of springs and pendulums.
This document discusses signal coupling in multi-conductor highly inhomogeneous HF environments like multi-strip timing RPC detectors. It summarizes simulations and measurements of cross-talk and time resolution in multi-strip RPC detectors of various lengths from 20cm to 100cm. Optimization techniques like differential signaling and shielding were able to reduce cross-talk to below 3% and achieve cluster sizes of around 1, with a modest degradation of time resolution to 110ps mainly affecting the first neighbor strips. Further optimization may still be possible.
1. Timtrack is a tracking algorithm that uses a least squares method to estimate the parameters of tracks (called SAETAs) passing through detector planes.
2. A SAETA contains 6 parameters that define a track: two coordinates at a reference plane, two projected slopes, time at the reference plane, and velocity.
3. Timtrack works directly with detector measurements like coordinates and times. It allows the SAETA parameters to vary to minimize the difference between measured and predicted values across detector planes.
The document discusses calibration of the tanks at the Pierre Auger Observatory. It describes a three step calibration process: 1) adjusting PMT voltages to equalize signals, 2) setting trigger thresholds to achieve 100Hz single rates at 150 channels, and 3) using charge histograms to determine peak charge values accurately. Understanding the tank response to inclined muons is important for analyzing inclined showers, which provide additional statistics and composition information. Measuring muon flux and properties directly is needed to validate simulation models used in the analysis of inclined events.
TimTrack is a software for tracking charged particles. It uses C language for its speed and flexibility. Previous versions used LAPACK or Intel IPP libraries for linear algebra operations. The newest version TimTrack v2.0 uses LAPACK and is 23.6 seconds faster than earlier versions for tracking 1 million particles. Future plans include parallelizing with OpenMP, MPI, and implementing on GPUs using CUDA.
The document discusses field-programmable gate arrays (FPGAs) and their potential use as tracking devices. It provides an overview of FPGA technology, including programmable logic blocks, interconnects, embedded memory and hard processor cores. The document compares FPGAs to application-specific integrated circuits (ASICs) and discusses performance, design effort required, and example applications of FPGAs.
The document summarizes the development of a large area sealed RPC detector for use in cosmic ray experiments and outreach activities. A 1 square meter first prototype was built in August 2009 using a modular design of 4mm acrylic and 2mm glass layers with external readout electrodes. Initial performance testing shows a background current that is hypothesized to come from trapped air or material outgassing that is expected to reduce after further cleaning cycles.
Herman mosquera2011 nonlinear electrodynamics and the pioneer 1011 spacecraftSOCIEDAD JULIO GARAVITO
1) The document discusses the unexplained "Pioneer anomaly" - an anomalous blueshift in radio signals from the Pioneer 10/11 spacecraft that suggests they are accelerating under an unexplained force.
2) Conventional explanations like gravitational effects, solar radiation pressure, and modified dynamics have been ruled out. The anomaly appears to be related to the electromagnetic sector rather than gravity.
3) The document proposes that nonlinear electrodynamics (NLED), where the electromagnetic field depends nonlinearly on the field strength, could explain an anomalous frequency shift in photons as they propagate through space without interacting with matter. This effect is called "photon acceleration".
- Simple harmonic motion describes oscillatory or back-and-forth motion caused by a restoring force proportional to displacement from equilibrium.
- Examples of objects that exhibit simple harmonic motion include springs, pendulums, and waves.
- The period and frequency of oscillation depend on attributes like the spring constant, length, or mass in the case of springs and pendulums.
This document discusses signal coupling in multi-conductor highly inhomogeneous HF environments like multi-strip timing RPC detectors. It summarizes simulations and measurements of cross-talk and time resolution in multi-strip RPC detectors of various lengths from 20cm to 100cm. Optimization techniques like differential signaling and shielding were able to reduce cross-talk to below 3% and achieve cluster sizes of around 1, with a modest degradation of time resolution to 110ps mainly affecting the first neighbor strips. Further optimization may still be possible.
1. Timtrack is a tracking algorithm that uses a least squares method to estimate the parameters of tracks (called SAETAs) passing through detector planes.
2. A SAETA contains 6 parameters that define a track: two coordinates at a reference plane, two projected slopes, time at the reference plane, and velocity.
3. Timtrack works directly with detector measurements like coordinates and times. It allows the SAETA parameters to vary to minimize the difference between measured and predicted values across detector planes.
The document discusses calibration of the tanks at the Pierre Auger Observatory. It describes a three step calibration process: 1) adjusting PMT voltages to equalize signals, 2) setting trigger thresholds to achieve 100Hz single rates at 150 channels, and 3) using charge histograms to determine peak charge values accurately. Understanding the tank response to inclined muons is important for analyzing inclined showers, which provide additional statistics and composition information. Measuring muon flux and properties directly is needed to validate simulation models used in the analysis of inclined events.
TimTrack is a software for tracking charged particles. It uses C language for its speed and flexibility. Previous versions used LAPACK or Intel IPP libraries for linear algebra operations. The newest version TimTrack v2.0 uses LAPACK and is 23.6 seconds faster than earlier versions for tracking 1 million particles. Future plans include parallelizing with OpenMP, MPI, and implementing on GPUs using CUDA.
The document discusses field-programmable gate arrays (FPGAs) and their potential use as tracking devices. It provides an overview of FPGA technology, including programmable logic blocks, interconnects, embedded memory and hard processor cores. The document compares FPGAs to application-specific integrated circuits (ASICs) and discusses performance, design effort required, and example applications of FPGAs.
The document summarizes the development of a large area sealed RPC detector for use in cosmic ray experiments and outreach activities. A 1 square meter first prototype was built in August 2009 using a modular design of 4mm acrylic and 2mm glass layers with external readout electrodes. Initial performance testing shows a background current that is hypothesized to come from trapped air or material outgassing that is expected to reduce after further cleaning cycles.
TimTrack is a software for tracking charged particles that uses C language for its speed and flexibility. It uses linear algebra libraries like LAPACK and Intel IPP for numerical computations like solving systems of linear equations. TimTrack version 2.0 implements a new algebra version for faster variance-covariance matrix calculations. Future versions will parallelize computations using OpenMP, MPI, and GPUs with CUDA to further improve performance for large particle datasets.
1. The document discusses methods for estimating and analyzing saetas (linear models). It proposes estimating a saeta under a new reference frame by applying the appropriate transformation to the estimated saeta coefficients.
2. Once a saeta is estimated, it can be restricted to pass through the origin by applying a linear restriction to the model estimation. The restriction can be tested with an F-test.
3. When two saetas are estimated from different data sets, the best overall saeta can be determined by testing whether the two saetas are equal.
The document discusses the development of sealed resistive plate chambers (sRPCs) as a more flexible alternative to gas ionization detectors that do not require a gas system. Several prototype sRPCs were constructed and two were tested with radioactive sources, finding that signals and current increased over time but that high voltage had to be reduced to avoid streamers at the cost of gain. Further work is needed to characterize the resolution and efficiency of sRPCs over time and to improve their construction and evaluate different gas mixtures to reduce aging effects.
The document discusses the front-end electronics (FEE) developed for the timing RPCs used in the HADES experiment. The FEE consists of daughter boards (DBOs) connected to the RPC cells that amplify and digitize signals, and mother boards (MBOs) that interface between the DBOs and data acquisition system. The FEE achieves a time resolution of less than 17 ps using a charge-to-width algorithm to encode timing and charge information. Testing shows the FEE performs well and could be adapted for use in the TRASGO detector with some modifications to reduce power consumption.
The document discusses the development of sealed resistive plate chambers (sRPCs) as a more flexible alternative to gas ionization detectors that do not require a gas system. Several prototype sRPCs were constructed and two were tested with radioactive sources, though two failed on the first day with little response. Signals from the functioning chambers increased over time, and high voltage had to be decreased to avoid streamers but with reduced gain. Further testing is needed to evaluate resolution, efficiency, isolation, and alternative gas mixtures to better understand aging effects in sRPCs.
TimTrack is an algorithm for tracking charged particles using data from detectors. It estimates the parameters of a "SAETA", which defines a particle track using 6 parameters. TimTrack uses a least squares method to minimize the differences between measured and predicted values from a model. It can handle data from various detector geometries by defining appropriate configuration and data matrices. The method provides a matrix solution that is fast to compute and easy to implement.
This document discusses characteristics of extensive air showers initiated by cosmic rays, including:
1) Shower characteristics like size, timing, energies, densities, and rates are intrinsic properties that must be accounted for in cosmic ray detector design and interpretation of data.
2) Models can be used to understand shower development and determine physical parameters from air shower data, but depend on hadronic interactions and primary particle composition which introduce uncertainties.
3) The energy and altitude of detection affect what can be observed, with higher energy air showers penetrating further and being detectable at higher altitudes.
This document discusses the relationship between cosmic rays, solar activity, and climate/weather patterns. It begins by outlining how solar wind modulates cosmic rays, which influence cloud formation by acting as cloud condensation nuclei. Studies of Forbush decreases have provided evidence this mechanism works in the real atmosphere. The author then discusses how cosmic ray flux variations from our galactic position may have influenced past climate changes. Finally, the document analyzes correlations between solar activity and climate variability patterns like the NAO and weather types in Galicia, Spain. The overall evidence suggests solar activity modulates cosmic rays in ways that influence global and regional climate and weather patterns.
This document discusses signal coupling in multi-conductor timing RPC detectors. It provides theoretical models and experimental results on pad, strip, double-strip, and multi-strip detector configurations. Simulations show cross-talk levels below 3% and cluster sizes of 1 can be achieved in optimized multi-strip designs, with time resolutions around 110 ps even for double hits. Experimental measurements on long multi-strip detectors validated the simulations. Further optimization may still improve performance.
The document discusses the Trasgo Project, which aims to develop an affordable and high-performance timing and tracking detector. It describes the key aspects of Trasgo, including its use of timing resistive plate chambers for high time resolution, a timing and tracking board for data acquisition and reconstruction, and a fast track reconstruction algorithm. Potential applications of Trasgo that are mentioned include cosmic ray detection for research in astroparticle physics, dosimetry, and studying correlations between cosmic rays and climate change. Examples are given of how Trasgo could provide more accurate information about air shower properties compared to using surface detectors alone.
The document summarizes a simulation of extensive air showers (EAS) using the AIRES code. Key points:
1) Simulations were run for primaries of protons, carbon, iron, and gamma rays with energies of 1015 eV in the "knee" region to study EAS characteristics.
2) Variables like energy, arrival time, production height, and identity of secondaries were recorded. Results showed differences in lateral distribution and time profiles between primaries.
3) Further analysis of observables like particle counts, arrival times, and azimuthal/zenith angles at different distances from the core is planned to better understand correlations with primary properties. Multivariate analysis techniques may help reveal hidden
This document contains 25 multiple choice questions from a GATE EE exam, along with explanations for each answer. The questions cover topics such as probability, complex variables, circuit analysis, differential equations, and electric machines. For each question, the correct answer is identified and a brief explanation of the solution steps is provided.
The TRB was developed as a general purpose platform for time-to-digital converters (TDCs) and fast data acquisition for nuclear physics experiments with thousands of channels. It provides integrated TDC, data acquisition, and local computing capabilities in a modular design that can be directly mounted on detectors. Measurements showed time resolutions of 40 picoseconds for 128 channels and 16 picoseconds for 32 channels. The TRB has been successfully used in several experiments and more developments are planned to further improve performance and reduce costs.
Here are the key details about the voltmeter and circuit:
- Voltmeter has sensitivities of 20 kΩ/V
- It has ranges of 5 V, 10 V, and 50 V
- It is connected across resistor RA in the circuit
The question is asking to calculate:
1) The voltage reading on the 5 V range
2) The voltage reading on the 10 V range
3) The voltage reading on the 50 V range
4) The percentage loading error for each reading
Given these details, the appropriate calculations using the voltmeter loading effects equations can be done to solve the problem.
Isotopic evidence of long-lived volcanism on IoSérgio Sacani
Jupiter’s moon Io hosts extensive volcanism, driven by tidal heating. The isotopic composition of Io's inventory of volatile chemical elements, including sulfur and chlorine, reflects its outgassing and mass loss history, and thus records information about its evolution. We used millimeter observations of Io’s atmosphere to measure sulfur isotopes in gaseous SO2 and SO, and chlorine isotopes in gaseous NaCl and KCl. We find 34S/32S = 0.0595 ± 0.0038 (equivalent to δ34S = +347 ± 86‰), which is highly enriched compared to average Solar System values and indicates that Io has lost 94 to 99% of its available sulfur. Our measurement of 37Cl/35Cl = 0.403 ± 0.028 (δ37Cl = +263 ± 88‰) shows that chlorine is similarly enriched. These results indicate that Io has been volcanically active for most (or all) of its history, with potentially higher outgassing and mass-loss rates at earlier times.
Bright features have been recently discovered by Dawn on Ceres, which extend
previous photometric and Space Telescope observations. These features should produce
distortions of the line profiles of the reflected solar spectrum and therefore an apparent
radial velocity variation modulated by the rotation of the dwarf planet. Here we report
on two sequences of observations of Ceres performed in the nights of 31 July, 26-
27 August 2015 by means of the high-precision HARPS spectrograph at the 3.6-m
La Silla ESO telescope. The observations revealed a quite complex behaviour which
likely combines a radial velocity modulation due to the rotation with an amplitude of
⇡ ±6 m s
The Sun is a dynamic star whose activity and variability directly influence conditions on Earth. The Sun's atmosphere, including the photosphere, chromosphere, and corona, undergo continuous changes driven by the Sun's magnetic field and interior dynamics. Small-scale magnetic features and energetic events throughout the solar atmosphere, such as spicules in the chromosphere and nanoflares in the corona, are thought to play an important role in heating the Sun's million-degree outer atmosphere through dissipation of magnetic energy. Observatories such as SOHO, STEREO, and Hinode provide continuous monitoring of the Sun to improve understanding of its complex variability and influence.
The document describes various NMR techniques including:
1) 2D NMR experiments like COSY and NOESY that provide information on through-bond and through-space couplings between nuclei to determine chemical structure and conformation.
2) The nuclear Overhauser effect (NOE) which allows measurement of internuclear distances below 5 Angstroms and is proportional to r^-6.
3) Pulse sequences like TOCSY that transfer magnetization between all spins within a coupled network to resolve overlapping signals in NMR spectra.
4 radio wave propagation over the earthSolo Hermelin
Describes the Electromagnetic Wave Propagation over the Earth Surface. Please send comments to solo.hermelin@gmail.com.
For more presentations on different subjects pleade visit my website at http://www,solohermelin.com.
This presentation is in the Radar folder.
Heliospheric Modulation of CRI Due to Solar Activityijsrd.com
The main features of solar cycle 23, sun enters a period of intermediate and weak solar activity in terms of sunspot number. Based on the observation from Omniweb data centre for solar- interplanetary data , geomagnetic activity and monthly mean count rate of cosmic ray intensity (CRI) variation data from Oulu / Moscow/ Keil neutron monitors (Rc=0.80 GV , Rc=2.42 GV and Rc=2.29 GV,) during solar activity cycle 23 . The phase of minimum solar activity began in May 2005 and lasted for 4.5 years the unprecedented duration of the relative sunspot numbers falls. It is observed that the strength of the interplanetary magnetic field has been falling off to new low levels, and reduces the GCR entering inner- heliosphere and it is also found that SSN positive correlated with Kp and Ap and sunspot number, 10.7 cm solar radio flux, were inverse correlated with monthly mean count rate of cosmic ray intensity
TimTrack is a software for tracking charged particles that uses C language for its speed and flexibility. It uses linear algebra libraries like LAPACK and Intel IPP for numerical computations like solving systems of linear equations. TimTrack version 2.0 implements a new algebra version for faster variance-covariance matrix calculations. Future versions will parallelize computations using OpenMP, MPI, and GPUs with CUDA to further improve performance for large particle datasets.
1. The document discusses methods for estimating and analyzing saetas (linear models). It proposes estimating a saeta under a new reference frame by applying the appropriate transformation to the estimated saeta coefficients.
2. Once a saeta is estimated, it can be restricted to pass through the origin by applying a linear restriction to the model estimation. The restriction can be tested with an F-test.
3. When two saetas are estimated from different data sets, the best overall saeta can be determined by testing whether the two saetas are equal.
The document discusses the development of sealed resistive plate chambers (sRPCs) as a more flexible alternative to gas ionization detectors that do not require a gas system. Several prototype sRPCs were constructed and two were tested with radioactive sources, finding that signals and current increased over time but that high voltage had to be reduced to avoid streamers at the cost of gain. Further work is needed to characterize the resolution and efficiency of sRPCs over time and to improve their construction and evaluate different gas mixtures to reduce aging effects.
The document discusses the front-end electronics (FEE) developed for the timing RPCs used in the HADES experiment. The FEE consists of daughter boards (DBOs) connected to the RPC cells that amplify and digitize signals, and mother boards (MBOs) that interface between the DBOs and data acquisition system. The FEE achieves a time resolution of less than 17 ps using a charge-to-width algorithm to encode timing and charge information. Testing shows the FEE performs well and could be adapted for use in the TRASGO detector with some modifications to reduce power consumption.
The document discusses the development of sealed resistive plate chambers (sRPCs) as a more flexible alternative to gas ionization detectors that do not require a gas system. Several prototype sRPCs were constructed and two were tested with radioactive sources, though two failed on the first day with little response. Signals from the functioning chambers increased over time, and high voltage had to be decreased to avoid streamers but with reduced gain. Further testing is needed to evaluate resolution, efficiency, isolation, and alternative gas mixtures to better understand aging effects in sRPCs.
TimTrack is an algorithm for tracking charged particles using data from detectors. It estimates the parameters of a "SAETA", which defines a particle track using 6 parameters. TimTrack uses a least squares method to minimize the differences between measured and predicted values from a model. It can handle data from various detector geometries by defining appropriate configuration and data matrices. The method provides a matrix solution that is fast to compute and easy to implement.
This document discusses characteristics of extensive air showers initiated by cosmic rays, including:
1) Shower characteristics like size, timing, energies, densities, and rates are intrinsic properties that must be accounted for in cosmic ray detector design and interpretation of data.
2) Models can be used to understand shower development and determine physical parameters from air shower data, but depend on hadronic interactions and primary particle composition which introduce uncertainties.
3) The energy and altitude of detection affect what can be observed, with higher energy air showers penetrating further and being detectable at higher altitudes.
This document discusses the relationship between cosmic rays, solar activity, and climate/weather patterns. It begins by outlining how solar wind modulates cosmic rays, which influence cloud formation by acting as cloud condensation nuclei. Studies of Forbush decreases have provided evidence this mechanism works in the real atmosphere. The author then discusses how cosmic ray flux variations from our galactic position may have influenced past climate changes. Finally, the document analyzes correlations between solar activity and climate variability patterns like the NAO and weather types in Galicia, Spain. The overall evidence suggests solar activity modulates cosmic rays in ways that influence global and regional climate and weather patterns.
This document discusses signal coupling in multi-conductor timing RPC detectors. It provides theoretical models and experimental results on pad, strip, double-strip, and multi-strip detector configurations. Simulations show cross-talk levels below 3% and cluster sizes of 1 can be achieved in optimized multi-strip designs, with time resolutions around 110 ps even for double hits. Experimental measurements on long multi-strip detectors validated the simulations. Further optimization may still improve performance.
The document discusses the Trasgo Project, which aims to develop an affordable and high-performance timing and tracking detector. It describes the key aspects of Trasgo, including its use of timing resistive plate chambers for high time resolution, a timing and tracking board for data acquisition and reconstruction, and a fast track reconstruction algorithm. Potential applications of Trasgo that are mentioned include cosmic ray detection for research in astroparticle physics, dosimetry, and studying correlations between cosmic rays and climate change. Examples are given of how Trasgo could provide more accurate information about air shower properties compared to using surface detectors alone.
The document summarizes a simulation of extensive air showers (EAS) using the AIRES code. Key points:
1) Simulations were run for primaries of protons, carbon, iron, and gamma rays with energies of 1015 eV in the "knee" region to study EAS characteristics.
2) Variables like energy, arrival time, production height, and identity of secondaries were recorded. Results showed differences in lateral distribution and time profiles between primaries.
3) Further analysis of observables like particle counts, arrival times, and azimuthal/zenith angles at different distances from the core is planned to better understand correlations with primary properties. Multivariate analysis techniques may help reveal hidden
This document contains 25 multiple choice questions from a GATE EE exam, along with explanations for each answer. The questions cover topics such as probability, complex variables, circuit analysis, differential equations, and electric machines. For each question, the correct answer is identified and a brief explanation of the solution steps is provided.
The TRB was developed as a general purpose platform for time-to-digital converters (TDCs) and fast data acquisition for nuclear physics experiments with thousands of channels. It provides integrated TDC, data acquisition, and local computing capabilities in a modular design that can be directly mounted on detectors. Measurements showed time resolutions of 40 picoseconds for 128 channels and 16 picoseconds for 32 channels. The TRB has been successfully used in several experiments and more developments are planned to further improve performance and reduce costs.
Here are the key details about the voltmeter and circuit:
- Voltmeter has sensitivities of 20 kΩ/V
- It has ranges of 5 V, 10 V, and 50 V
- It is connected across resistor RA in the circuit
The question is asking to calculate:
1) The voltage reading on the 5 V range
2) The voltage reading on the 10 V range
3) The voltage reading on the 50 V range
4) The percentage loading error for each reading
Given these details, the appropriate calculations using the voltmeter loading effects equations can be done to solve the problem.
Isotopic evidence of long-lived volcanism on IoSérgio Sacani
Jupiter’s moon Io hosts extensive volcanism, driven by tidal heating. The isotopic composition of Io's inventory of volatile chemical elements, including sulfur and chlorine, reflects its outgassing and mass loss history, and thus records information about its evolution. We used millimeter observations of Io’s atmosphere to measure sulfur isotopes in gaseous SO2 and SO, and chlorine isotopes in gaseous NaCl and KCl. We find 34S/32S = 0.0595 ± 0.0038 (equivalent to δ34S = +347 ± 86‰), which is highly enriched compared to average Solar System values and indicates that Io has lost 94 to 99% of its available sulfur. Our measurement of 37Cl/35Cl = 0.403 ± 0.028 (δ37Cl = +263 ± 88‰) shows that chlorine is similarly enriched. These results indicate that Io has been volcanically active for most (or all) of its history, with potentially higher outgassing and mass-loss rates at earlier times.
Bright features have been recently discovered by Dawn on Ceres, which extend
previous photometric and Space Telescope observations. These features should produce
distortions of the line profiles of the reflected solar spectrum and therefore an apparent
radial velocity variation modulated by the rotation of the dwarf planet. Here we report
on two sequences of observations of Ceres performed in the nights of 31 July, 26-
27 August 2015 by means of the high-precision HARPS spectrograph at the 3.6-m
La Silla ESO telescope. The observations revealed a quite complex behaviour which
likely combines a radial velocity modulation due to the rotation with an amplitude of
⇡ ±6 m s
The Sun is a dynamic star whose activity and variability directly influence conditions on Earth. The Sun's atmosphere, including the photosphere, chromosphere, and corona, undergo continuous changes driven by the Sun's magnetic field and interior dynamics. Small-scale magnetic features and energetic events throughout the solar atmosphere, such as spicules in the chromosphere and nanoflares in the corona, are thought to play an important role in heating the Sun's million-degree outer atmosphere through dissipation of magnetic energy. Observatories such as SOHO, STEREO, and Hinode provide continuous monitoring of the Sun to improve understanding of its complex variability and influence.
The document describes various NMR techniques including:
1) 2D NMR experiments like COSY and NOESY that provide information on through-bond and through-space couplings between nuclei to determine chemical structure and conformation.
2) The nuclear Overhauser effect (NOE) which allows measurement of internuclear distances below 5 Angstroms and is proportional to r^-6.
3) Pulse sequences like TOCSY that transfer magnetization between all spins within a coupled network to resolve overlapping signals in NMR spectra.
4 radio wave propagation over the earthSolo Hermelin
Describes the Electromagnetic Wave Propagation over the Earth Surface. Please send comments to solo.hermelin@gmail.com.
For more presentations on different subjects pleade visit my website at http://www,solohermelin.com.
This presentation is in the Radar folder.
Heliospheric Modulation of CRI Due to Solar Activityijsrd.com
The main features of solar cycle 23, sun enters a period of intermediate and weak solar activity in terms of sunspot number. Based on the observation from Omniweb data centre for solar- interplanetary data , geomagnetic activity and monthly mean count rate of cosmic ray intensity (CRI) variation data from Oulu / Moscow/ Keil neutron monitors (Rc=0.80 GV , Rc=2.42 GV and Rc=2.29 GV,) during solar activity cycle 23 . The phase of minimum solar activity began in May 2005 and lasted for 4.5 years the unprecedented duration of the relative sunspot numbers falls. It is observed that the strength of the interplanetary magnetic field has been falling off to new low levels, and reduces the GCR entering inner- heliosphere and it is also found that SSN positive correlated with Kp and Ap and sunspot number, 10.7 cm solar radio flux, were inverse correlated with monthly mean count rate of cosmic ray intensity
Atmospheric flows are governed by the equations of fluid dynamics. These equations are nonlinear. But because atmospheric flows are inhomogeneous and anisotropic, the nonlinearity may manifest itself only weakly through interactions of non-trivial mean flows with disturbances or eddies. In such situations, the quasi-linear (QL) approximation, that retains eddy-mean flow interactions but neglect eddy-eddy interactions, hold promise in resolving large-scale atmospheric dynamics. The statistics of the QL system corresponds to closing the hierarchy of statistical moments at the second order.
Hence, exploring QL dynamics paves the way for the development of direct statistical simulations of geophysical flows.
Using a hierarchy of idealized general circulation models, we identify when the QL approximation captures large-scale dynamics. We show that the QL dynamics fails to capture the flow when the dissipation of large-scale eddies occurs through strongly nonlinear eddy-eddy interactions in upper tropospheric surf zones, as it is often the case on Earth. But we demonstrate that the QL approximation captures eddy absorption when it arises from the shearing by the mean flow, for example when the eddy amplitude is small enough or the planetary rotation rate is large enough.
These results illustrate different classes of nonlinear processes that can control wave dissipation in the upper troposphere and show that in some parameter regimes the QL approximation is accurate to resolve large-scale dynamics.
Solar limb darkening_function_from_baily_beads_observationsSérgio Sacani
This document presents a new method for measuring the solar limb darkening function using observations of Baily's beads during solar eclipses. The method involves analyzing the light curve profiles of emerging and disappearing Baily's beads to determine the surface brightness profile of the outer solar atmosphere with high resolution. The method is applied to eclipse videos from 2010, yielding constraints on the position of the limb darkening function inflection point between -0.190 and +0.050 arcseconds. The results suggest reconsidering evaluations of historical eclipses that assumed a step function profile for the limb darkening.
The document discusses the appraisal of solar resources. It covers topics such as solar radiation characteristics, the classical evaluation of solar radiation, the interaction of solar radiation with the atmosphere, and the study of direct solar radiation. The document provides information on measuring and estimating solar radiation data from satellites and numerical weather prediction models. It also discusses generating time series for simulation and databases of solar radiation data available online.
This document summarizes the structure and magnetic properties of the Sun. It describes the core, radiative zone, and convective zone in the Sun's interior. It also discusses the photosphere, chromosphere, corona, and heliosphere that make up the Sun's atmosphere. The document then focuses on the Sun's magnetic field and how sunspots and solar activity vary in a approximately 11-year cycle. It introduces the alpha-omega dynamo model to explain how differential rotation and plasma currents generate and maintain the Sun's magnetic field through self-exciting dynamo action.
Small magnetic elements like bright points are ubiquitous in the solar photosphere and low chromosphere. They are highly dynamic, evolving through fragmentation, merging and cancellation. High resolution and cadence observations are needed to study their structure and role in solar irradiance. Solar active regions interact with surrounding granulation. The transition of pores into sunspots and their formation and decay involve interactions between plasma and magnetic fields. It is unclear what subsurface flows are responsible for pore formation. Filamentary structures and inward plasma flows are observed around sunspots.
This document discusses the need for a reconciled ozone dataset for trend analysis. It outlines several goals for the dataset including assessing the state of the ozone layer, evaluating trends in ozone-depleting substances, and analyzing interactions between tropospheric and stratospheric ozone. The document also describes challenges with combining ozone profile records from different satellite instruments and the need for a workshop to develop a work plan for creating the reconciled ozone dataset.
Study of Solar Interplanetary and Geomagnetic Disturbances in Solar Cycle 23ijsrd.com
The most specific of solar cycle 23, sun enters a period of intermediate and weak solar activity in terms of sunspot number. Based on the observation from Omniweb data centre for solar- interplanetary data, geomagnetic activity and monthly mean count rate of cosmic ray intensity (CRI) variation data taken from neutron monitors during solar activity period 23/24. The phase of minimum solar activity began in May 2005 and lasted for 4.5 years the unprecedented duration of the relative sunspot numbers falls. It is observed that the strength of the interplanetary magnetic field has been falling off to new low levels, and reduces the GCR entering inner- heliosphere and it is also found that SSN positive correlated with Kp and Ap and sunspot number, 10.7 cm solar radio flux, were inverse correlated with monthly mean count rate of cosmic ray intensity.
- The rings of Jupiter show vertical corrugations resembling patterns detected in Saturn's rings, which are caused by the rings being tilted and slowly twisting into spirals due to planetary gravity.
- Galileo images from 1996 and 2000 of Jupiter's rings revealed two spiral pattern wavelengths that are associated with the Shoemaker-Levy 9 comet impacts in 1994 and another event in 1990.
- New Horizons images of the rings in 2007 continued to show the pattern from 1994, demonstrating the longevity of these imprints from comet impacts.
2020-02-12 Theory of Application of Synthetic Aperture RadarYosuke Aoki
The document provides an overview of synthetic aperture radar (SAR) theory and applications for measuring earthquake and volcano deformation. It discusses how SAR can detect millimeter-scale surface changes from space using interferometry techniques. Examples are given of SAR being used to map coseismic deformation from past earthquakes, as well as interseismic, postseismic and creeping motions on faults. Limitations including decorrelation and atmospheric effects are also summarized.
The document discusses the induced polarization (IP) method, including its origins, mechanisms, and measurement techniques. Specifically, it describes how:
1) IP effects arise from either grain (electrode) polarization at mineral grain surfaces or membrane (electrolytic) polarization caused by pore constrictions or clays.
2) IP is measured using time-domain, frequency-domain, phase-domain, or spectral techniques to analyze the decay of voltage after an applied current is switched off.
3) Time-domain techniques measure the decay curve of overvoltage over time after current switch-off to calculate chargeability and apparent chargeability.
This document analyzes the relationship between solar activity and weather/climate in Indonesia from 1948-2003. It finds:
1) Tight correlations exist between solar activity (sunspot number), geophysical variables like cloud cover, sea surface temperature, and rainfall throughout Indonesia.
2) Correlations between sunspot number and rainfall increase with higher geomagnetic latitudes of stations, suggesting solar activity has a stronger influence on areas with less shielded cosmic rays.
3) Eastern Indonesia sees above/below normal rainfall corresponding to sunspot maxima/minima after 1976, linked to El Nino/La Nina. Western Indonesia sees rainfall peaks tied to sunspot maxima.
This document describes a Bayesian inversion approach to jointly interpret multiple seismic data types that provide information about anisotropic layering in the upper mantle. Surface wave dispersion curves, SKS splitting measurements, and receiver functions are traditionally interpreted separately, but sample different volumes of the Earth and have different sensitivities and uncertainties. The proposed method directly inverts seismograms for SKS and P phases using a cross-convolution approach, avoiding intermediate processing steps. A transdimensional Markov chain Monte Carlo scheme obtains probabilistic 1-D seismic velocity profiles down to 350 km depth beneath two stations, treating the number of layers and presence of anisotropy as unknown parameters. For both stations, the lithosphere-asthenosphere boundary is clearly visible and marked by
The document presents work on the MIDAS project which aims to identify particle masses using multiple sampling. It outlines results from initial MATLAB simulations showing electrons can be distinguished from muons and protons below 500 MeV. A Geant4 simulation using the SETA environment was also developed to model the TRASGO detector in more detail. Further simulations are needed but combining velocity, chi-squared values with additional information like timing may allow ambiguous particles to be discriminated.
The document discusses calibration of the tanks at the Pierre Auger Observatory. It describes a three step calibration process: 1) adjusting PMT voltages to obtain the same signal for a vertical muon, 2) setting the trigger threshold to obtain a 100Hz single particle rate at 150 channels, and 3) using charge histograms to determine the signal produced by a vertical muon. Calibration information like histograms of baseline, pulse height, and charge are provided with event data. Analysis of inclined showers is also discussed, noting they are important for composition studies and increasing statistics. Understanding the tank response to inclined muons is crucial, but has not been directly measured.
The document provides an overview of the HADES RPC ToF Wall cosmic ray commissioning project. It discusses (1) the instrumentation of the 6 RPC sectors and initial cosmic ray testing, (2) the collection of approximately 50 days of cosmic ray data totaling 895 GB, and (3) preliminary analysis of cosmic ray tracks using the TimTrack algorithm, including reconstructed position and time results. The aim is to validate the RPC detector performance before data taking with particle beams begins.
TimTrack is an algorithm for tracking charged particles using data from detectors. It estimates the parameters of a "SAETA", which defines a particle track using 6 parameters. TimTrack uses a least squares method to minimize the differences between measured and predicted values from a model. It can handle data from various detector geometries by defining appropriate configuration and data matrices. The method provides a matrix solution that is fast to compute and easy to implement.
The document summarizes a simulation of extensive air showers (EAS) using the AIRES code. Key results include:
1) Simulations of EAS were conducted for primaries of protons, carbon, iron, and gamma rays with energies of 1015 eV in the "knee" region.
2) Observables like particle type, arrival time, zenith angle, and azimuthal angle were recorded for electrons and muons at varying distances from the shower core.
3) Preliminary analysis of arrival times and angular distributions shows differences between primaries that could help identify the primary particle.
4) Further multivariate analysis of correlations between observables may provide hidden insights into the primary cosmic ray
The document discusses estimating a saeta (trajectory) using a linear model, where available data Y is modeled as a function of known quantities X and unknown parameters that determine the saeta plus some errors. It describes how to obtain the estimator for the parameters and its properties. It then poses three questions about estimating a saeta under different references, imposing restrictions like going through the origin, and combining information from multiple estimated saetas.
Este documento describe los rayos cósmicos, incluyendo su interacción con la atmósfera terrestre, su composición y espectro de energía, y los métodos para estudiarlos. También presenta el proyecto Trasgo, el cual propone desarrollar un detector de rastreo de partículas basado en cámaras de placas resistivas para proporcionar información adicional sobre las partículas de alta energía.
Este documento describe los rayos cósmicos y su estudio mediante cascadas atmosféricas. Detalla la historia del descubrimiento de los rayos cósmicos, su composición y espectro energético. Explica cómo se forman y desarrollan las cascadas atmosféricas y cómo se pueden medir para caracterizar las partículas primarias. Finalmente, menciona algunos experimentos históricos y actuales y las técnicas que utilizan para estudiar las cascadas y los rayos cósmicos.
The TRASGO project aims to develop an innovative cosmic ray detector based on timing RPCs. The detector, called TRASGO, will be able to measure particle timing, tracking, and identification. It will consist of timing RPC planes with 100ps time resolution, a fast tracking algorithm called TimTrack, and a particle identification method called MIDAS. An array of 10-50 TRASGO detectors called MEIGA will be installed to study cosmic rays around the knee and test simulation packages. The MEIGA collaboration has been formed between universities in Spain and Portugal to develop the detectors and carry out the cosmic ray measurements.
Este documento describe un proyecto llamado Trasgo que tiene como objetivo desarrollar un detector de rastreo de partículas basado en detectores RPC. El detector Trasgo utilizaría detectores RPC de alta resolución temporal junto con algoritmos de reconstrucción de trayectorias y identificación de partículas para proporcionar información sobre las partículas de alta energía que lo atraviesan. El detector Trasgo sería modular, portátil y de bajo costo, lo que lo haría útil para una variedad de aplicaciones relacionadas con el est
Este documento describe un nuevo método llamado "TimTrack" para reconstruir trayectorias de partículas cargadas en detectores que miden tiempos. TimTrack ajusta simultáneamente los parámetros de posición, pendiente, tiempo inicial y velocidad de la partícula utilizando mediciones de tiempo de todos los detectores. Esto proporciona una reconstrucción más precisa que los métodos tradicionales. El documento también describe simulaciones realizadas para probar el algoritmo TimTrack en detectores con múltiples planos y diferentes configuraciones.
2. Outline of the talk
• First
part: A new arising (and controversial) paradigm:
Cosmoclimatology.
• Second part: Interactions between sun activity (that
modulates cosmic rays) and different patterns that
influences climate and meteorology:
•Modes of low-frequency variability (NAO)
•Weather types
•Artic Oscillation
•Blocking activity.
3.
4. ¿What is the link between climate/meteorology and cosmic
rays?
Solar wind modulates the flux of high energy particles coming from outside the solar system. These
particles, the cosmic rays, are the dominant source of ionization in the troposphere. A more active
sun implies lower tropospheric ionization.
5. ¿How does it work the link between clouds and cosmic
rays?
6. ¿How does it work the link between clouds and cosmic
rays?
Electrons set free in the air by cosmic rays help to assemble molecules of sulfuric acid for cloud
condensaion nuceli on which watervapour condenses to make clouds.
7. ¿Does this mechanism work in the real atmosphere?
Forbush Decreases: Sudden reduction in the influx of GCR as a result of
explosive events on the sun. These events provide a natural experiment for
testing hypothesis about solar influences on the Earth.
8. ¿Does this mechanism work in the real atmosphere?
Decrease of cloud water content over the world’s ocean as a result of the 5
strongest FD over the period 1987-2007. (From Special Sounder Microwave
Imager (SSM/I).
Svensmark H., Bondo T. and Svensmark J. Cosmic ray decreases affect atmospheric aerosols and clouds. GRL, 2009
9. ¿Does this mechanism work in the real atmosphere?
From these data it appears that the answer is yes!!! It works.
Svensmark H., Bondo T. and Svensmark J. Cosmic ray decreases affect atmospheric aerosols and clouds. GRL, 2009
10. Observations
Clouds have been observed from space since the beginning of the 1980's. Using the satellite data,
Henrik Svensmark of the Danish National Space Center in Copenhagen has shown that cloud
cover varies in sync with the variable cosmic ray flux reaching the Earth. More cosmic rays
mean more low level clouds.
12. ¿Is this modulation important for climate? Concept of
radiative forcing
Great uncertainty on the effects of clouds on
climate
13. Cosmoclimatology: Reconstruction of past climate
changes
The solar system periodically crosses the spiral arms of the Milky Way. Each time it does so, it
should witness an elevated level of cosmic rays. In fact, the cosmic ray flux variations arising from
our galactic journey are ten times larger than the cosmic ray flux variations due to solar activity
modulations, at the energies responsible for the tropospheric ionization (of order 10 GeV).
Shaviv & J. Veizer, "A Celestial driver of Phanerozoic Climate?", GSA Today 13, No. 7, 4, 2003.
N. Shaviv, "Cosmic Ray Diffusion from the Galactic Spiral Arms, Iron Meteorites, and a Possible Climatic Connection", Physical Review Letters 89,
051102, (2002).
15. Modes of low frequecy variability
NAO EA
EA/WR SCA
15
16. Correlations of different patterns with rainfall (DJF) in Galicia (1980-2006)
Lorenzo and Taboada, JAOS, 2005 16
17. Correlation of different modes of low frequecy variability
with rain
Peinador (1960-2005)
NAO EA EA/WR SCA
DJF -0.45 0.42 -0.51 0.46
MAM -0.30 0.17 0.08 0.13
JJA -0.18 0.02 0.17 0.10
SON -0.22 0.23 0.04 0.66
Coruña – Completa (1960-2005)
NAO EA EA/WR SCA
DJF -0.36 0.39 -0.52 0.36
MAM -0.36 0.15 0.16 0.20
JJA -0.35 0.03 0.05 0.11
SON -0.24 0.35 -0.09 0.66
17
18. Variariability of the correlation over time: Influence of
solar activity
High correlation between the
interaction of NAO with
climate variability in Galicia
and solar activity
Estación Peinador (Vigo)
¿Change of circulation
0.4
regime in North Hemisphere 0.3
at mid 70´s? 0.2
0.1
0
1955
-0.1 1960 1965 1970 1975 1980 1985 1990
-0.2
-0.3
-0.4
-0.5
-0.6
-0.7
18
Media SS 20 años corr. NAO-Lluvia (20 años)
19. Correlation of different modes of low frequecy variability
with temperature
Peinador (1960-2005)
NAO EA EA/WR SCA
DJF 0.15 0.70 0.10 -0.24
MAM 0.17 0.15 0.16 -0.57
JJA 0.04 0.13 -0.37 -0.46
SON -0.08 0.20 0.16 -0.61
Coruña – Completa (1960-2005)
NAO EA EA/WR SCA
DJF 0.25 0.73 0.08 -0.24
MAM 0.12 0.29 0.26 -0.50
JJA 0.03 0.15 -0.27 -0.33
SON -0.31 0.35 0.08 -0.51
19
20. Weather types
• Automatic clasification of weather types
1. Direction of flow was given by tan-1(WF/SF),
180° being added if WF is positive. The
appropriate direction was computed using an
eight-point compass, allowing 45° per sector.
2. If |Z|<F, flow is essentially straight and
considered to be of a pure directional type (eight
different cases, according to the directions of the
compass).
3. If |Z|>2F, the pattern was considered to be of
a pure cyclonic type if Z>0, or of a pure
anticyclonic type if Z<0.
4. If F<|Z|<2F, flow was considered to be of a
hybrid type and is therefore characterized by
SF = 1.350[0.25( p5 + 2 p9 + p13 ) − 0.25( p4 + 2 p8 + p12 )] both direction and circulation (8 x 2 different
WF = [0.5( p12 + p13 ) − 0.5( p4 + p5 )] types).
ZS = 0.85[0.25( p6 + 2 p10 + p14 ) − 0.25( p5 + 2 p9 + p13 ) − 0.25( p4 + 2 p8 + p12 )
+ 0.25( p3 + 2 p 7 + p11 )]
ZW = 1.12[0.5( p15 + p16 ) − 0.5( p8 + p9 )] − 0.91[0.5( p8 + p9 ) − 0.5( p1 + p2 )]
F = ( SF 2 + WF 2 )1 2 20
Z = ZS + ZW
21. 100%
N
80%
NW
W
60% SW
S
SE
40% E
NE
A
20%
C
0%
1 2 3 4 5 6 7 8 9 10 11 12
Frequency of appearance of different weather types in Galicia in different
months.
M.N. Lorenzo, J.J. Taboada and L. Gimeno. “Links between circulation weather types and teleconnection patterns and their
influence on precipitation patterns in Galicia (NW Spain)”. International Journal of Climatology 2008.
21
22. Each weather type explains different quantities of rain
Tipo Annual Winter Spring Summer Autumn
NE 0.91 1.22 0.77 0.87 1.06
E 1.86 3.18 1.94 0.74 1.69
SE 2.36 2.94 1.82 0.33 2.45
S 3.02 5.00 2.70 0.43 2.61
SW 10.31 13.64 9.26 3.48 9.61
W 11.80 14.63 9.79 4.35 14.05
NW 5.37 8.99 4.86 2.43 5.86
N 1.70 3.47 1.57 1.05 2.01
C 13.41 15.34 13.57 6.63 17.22
A 0.21 0.31 0.28 0.08 0.21
22
23. Outlook
•¿Does sun activity correlate with frequency of appearance of different Weather
Types?. Work in progress – Diego Ramos
Preliminary results for other areas of Europe (Huth et al. 2002) shows interesting
results.
• ¿Does the effects on blocking activity (BarrioPedro et al., 2008) has an
influence on Galician climate variability?
• ¿Does the effects on modes of oscillation has an influence on Galician climate
variability?
The whole picture until now shows an enhanced zonality
under solar maxima