Space weather refers to changes in the space environment near Earth that are driven by solar activity like solar flares and coronal mass ejections. There are three main types of space weather storms: radio blackouts caused by solar flares that arrive in 8 minutes, radiation storms from energetic particles that arrive within 15 minutes to 24 hours, and geomagnetic storms from coronal mass ejections that arrive within 1 to 4 days. Each type of storm has different effects, affecting systems like radio communications, satellites, power grids, and navigation.
The document discusses upcoming NASA space shuttle missions, an asteroid passing close to Earth, and provides an introduction to astronomy topics including the Big Bang theory, formation of stars and galaxies, light years, types of galaxies, solar systems, and milestones in space exploration. Key information includes the launch dates and durations of the final two space shuttle missions, an asteroid passing within 45,000 km of Earth on October 5, and an overview of how the universe formed and evolved according to the current scientific understanding.
This document provides an overview of the internal structure of the Earth. It describes the three main layers - crust, mantle, and core. The crust is the outermost layer and is divided into continental and oceanic crust. Beneath the crust is the mantle, which makes up most of the Earth's volume. The core is at the center and has a solid inner core and liquid outer core. Seismic waves and magnetic reversals provide evidence about the composition and movement of materials in the Earth's interior.
The Earth has a magnetic field that extends into space and protects the planet. The magnetic field is generated by Earth's core and behaves like a giant bar magnet. It has a north and south magnetic pole that are located near the geographic poles but can wander over time. The magnetic field deflects solar winds and cosmic rays, protecting the atmosphere. It can be mapped and measured at different locations on Earth. Animals like birds are able to detect the magnetic field to aid navigation.
Atmospheric refraction is the bending of light as it passes through the atmosphere due to changes in air density with altitude. This causes distant objects to appear elevated, lowered, or shimmering. It also causes advanced sunrise and delayed sunset, the apparent elevation of stars, and the lack of twinkling in planets. Refraction makes the sun appear larger and flattened at sunrise/sunset but circular at noon. It can also create mirages by refracting light to appear as reflected sky.
Solar wind consists of charged particles released from the sun's corona that bombard the Earth at high speeds. While solar wind prevents harmful cosmic rays, it can also disrupt Earth's magnetic field and potentially damage the atmosphere. In the past, solar wind was even more dangerous when the sun was younger and hotter. Mars lacked a strong magnetic field to protect it from solar wind, which led to the loss of its atmosphere and climate. To strengthen Earth's protection, we must reduce pollution that damages the ozone layer and weakens the magnetic field.
This document discusses deep sky objects such as asteroids, meteorites, and comets. It provides information on what asteroids are made of and where they are located in the asteroid belt between Mars and Jupiter. Meteorites are pieces of asteroids or comets that have fallen to Earth. Comets are described as "dirty snowballs" made of dust, ice, and rock that originate from the Oort cloud or Kuiper belt and have tails pointing away from the Sun. Examples of famous comets like Halley and comets that have impacted planets like Jupiter are mentioned. The differences between asteroids, meteorites, and comets are summarized.
The document summarizes key information about the interior structure and composition of the Earth. It is divided into three main layers:
1) The crust is the outermost solid layer and thinnest, varying between 5-50 km thick. It is broken into tectonic plates that move over time.
2) The mantle, the largest layer, makes up over 80% of the Earth's volume. It is divided into the upper and lower mantle.
3) The core is the innermost layer and has a solid inner core and liquid outer core, composed primarily of iron and nickel.
1. The document provides information about the planet Jupiter and its moons. Jupiter is the largest planet in the solar system and has many moons, including the four largest Galilean moons - Io, Europa, Ganymede, and Callisto.
2. The Cassini spacecraft obtained images of Saturn and its rings and moons. Saturn has a vast ring system made of small particles of ice and rock. It has several large moons such as Titan, which has a thick atmosphere.
3. The document discusses the gas giant planets Jupiter and Saturn, their compositions, atmospheric features, rotations, magnetic fields, rings and moons as observed by spacecraft such as Galileo, Cassini, and Voyager.
There are four main types of galaxies: spiral, elliptical, lenticular, and irregular. Spiral galaxies have a central bulge and rotating spiral arms containing young stars. Elliptical galaxies are spherical and contain mostly older, redder stars. Lenticular galaxies resemble ellipticals but have a disk of gas and dust. Irregular galaxies do not fit into the other categories and often have regions of intense star formation. The Milky Way is classified as a barred spiral galaxy while Andromeda is a spiral galaxy as well.
This is an introduction to stars, including the basics of observing and classifying stars as well as their evolution and life cycle. This is a modification of a presentation I found online.
The document discusses evidence that supports the collision theory of lunar formation, in which an object the size of Mars collided with Earth, ejecting material that formed the moon. Key evidence includes the moon's similar surface composition to Earth's crust and mantle, the lack of an atmosphere due to the force of the impact, and similar oxygen atoms between Earth and the moon that are different from other celestial objects. The document also provides an overview of Apollo missions to the moon and features observed like maria, highlands, and craters.
The document summarizes the layers that make up the Earth. It is divided into four main layers from outer to inner: the crust, mantle, outer core, and inner core. The crust is the topmost layer and thinnest, varying in thickness from 5-100km. Below is the mantle, the largest layer making up 80% of the Earth's volume. Within the mantle are the lithosphere and asthenosphere. The outer core is liquid, while the inner core is solid iron and nickel, and is the source of Earth's magnetic field. Scientists study seismic waves to determine the composition of each layer without being able to directly observe or drill to the deep interior.
The document summarizes key aspects of Earth's structure and composition. It describes Earth's distinct atmospheric layers and how pressure decreases with altitude. It also outlines Earth's internal layering, including the crust, mantle, and core. The crust is divided into continental and oceanic types based on differences in density and thickness. The mantle conveys heat via convection currents. The liquid outer core generates Earth's magnetic field through the geodynamo process.
The document discusses various types of weathering that break down rock into sediment. It describes mechanical (physical) weathering which cracks rocks without changing their chemical composition through processes like abrasion, frost wedging, and plant growth. It also describes chemical weathering which involves chemical changes through processes like carbonation, oxidation, hydrolysis, and acid rain dissolving rocks. The rate of weathering depends on climate, rock type, particle size, and depth of burial - with smaller, more exposed particles weathering faster. Weathering produces sediments, colloids, and dissolved minerals, and is an important part of soil formation.
This document discusses various units used to measure astronomical distances, including the astronomical unit (AU), light year, and parsec. It describes how trigonometric parallax can be used to determine the distance to stars by measuring their change in position over half a year. Standard candles, like Cepheid variables and Type Ia supernovae, which have known intrinsic luminosities, allow distances to be calculated using the inverse square law. The Hubble law relates a galaxy's redshift to its distance from Earth, showing the expansion of the universe.
GEOGRAPHY IGCSE: PLATE TECTONICS. Earth's layers. Inner core, outer core, mantle, crust, the structure of Earth, plate boundaries and interactions, magma and igneous rocks, forming a volcano, compressional boundaries, folding.
A supernova is a massive stellar explosion that occurs at the end of a large star's life. There are two main types of supernovae that can form - Type I occurs when a white dwarf star accumulates too much matter from a nearby star, and Type II occurs when a massive star runs out of nuclear fuel and collapses under its own gravity. During its explosion, a supernova can outshine its entire host galaxy and radiate more energy than our Sun will over its entire lifetime, making them the primary source of heavy elements in the universe.
The document discusses evidence for the Coriolis effect and the Earth's rotation. It explains that the Coriolis effect causes objects moving over the Earth's surface, like winds or projectiles, to be deflected from a straight path. This deflection is to the right in the Northern Hemisphere and to the left in the Southern Hemisphere. It provides an example of a hockey puck launched from the North Pole appearing to deflect to the west as viewed by an observer on the rotating Earth. Additionally, it discusses hurricanes, tornadoes, and thunderstorms, including their formation and impacts.
All stars begin as clouds of dust and gas called nebulae. When gravity causes the nebula to collapse, a protostar forms at the center. The protostar grows in size and temperature through nuclear fusion reactions until it becomes a stable main sequence star. Small stars like our Sun will eventually expand into red giants and shed their outer layers, leaving behind dense white dwarf cores. Larger stars may explode as supernovae, collapsing into neutron stars or black holes. The life cycle of a star depends on its initial mass, with smaller stars ending as white dwarfs and more massive stars ending as black holes or neutron stars.
The document discusses the structure and composition of the Sun. It has 6 layers: the core, where fusion occurs at 15 million degrees Celsius; the radiative zone, where energy moves by radiation; the convection zone, where hot gas currents transfer energy; the photosphere, the visible surface; the chromosphere, a thin pinkish layer; and the corona, the outermost low density layer. The Sun is mostly made of hydrogen and helium and produces energy through the fusion of hydrogen into helium. It contains over 99% of the mass in the solar system and has prominent features like sunspots and solar winds.
This document discusses implementing blended learning at Heart of Worcestershire College. It recommends including a 10-50% online component in all publicly funded learning programs. The college implemented a blended learning program called SOLA which includes 30-60 hours of online learning per year for vocational courses. Key aspects of SOLA include Moodle courses, online content and activities, and assessments. Challenges discussed include engaging learners and staff. Support needed includes training, resources, and monitoring. Benefits seen include improved success rates and cost savings. The college is available for consultation, training, and content to support other organizations with blended learning.
Sunspots are dark, cooler areas on the sun's surface caused by strong magnetic fields that inhibit hot gases from rising. They typically last several days but some can persist for weeks. Solar flares are powerful explosions that heat material to millions of degrees and release energy equivalent to billions of tons of TNT in just minutes. They occur near sunspots along dividing lines of opposing magnetic fields. Solar prominences are dense loops of gases suspended above the sun for days or weeks by magnetic fields but can erupt, releasing a huge sheet of gases into space over hours.
The Sun is our closest star, with a diameter of 1.4 million km and a mass 330,000 times that of Earth. Its surface temperature is around 5,800 K and it is expected to exist for another 10 billion years. The Sun is composed of three main layers - the core, radiative zone, and convective zone - as well as an atmosphere with the photosphere, chromosphere, and corona. Features on the Sun like sunspots and solar flares are produced by its magnetic field.
The Sun is a G2V type star made of gas and dust from other stars. It is approximately 4.65 billion years old and has a lifetime of another 5.5 billion years. The Sun has different inner layers including a core with a temperature of 15 million Kelvin, a radiative zone, and a convective zone that moves the Sun's mass. The Sun's surface, called the photosphere, is about 5,800 Kelvin and features solar spots. The Sun's outer atmosphere, the corona, reaches temperatures over 20 million Kelvin and features magnetic coronal loops.
The Sun formed around 5 billion years ago from a cloud of gas and dust. Through the process of nuclear fusion at its core, the Sun generates immense heat and light by converting hydrogen into helium. It is a common yellow star that is part of a cycle that creates convection currents within its surface and sunspots that follow an 11-year cycle. The Sun provides the energy necessary to sustain life on Earth but will eventually exhaust its hydrogen fuel in around 5 billion years.
The sun is vital for life on Earth, providing light, heat, and energy. It is approximately 92 million miles from Earth, though it appears close due to its immense size—its diameter is 1.3 million kilometers and 333 Earths could fit inside it. The sun has six layers from its core to corona, and features dark sunspots on its surface that occur every 11 years and can be over 50,000 kilometers wide. Scientists have learned the sun rotates by observing the movement of sunspots.
The Sun is made up of hot plasma and provides heat and light to our solar system. It is over 1000 times more massive than all the planets combined. The Sun has an interior of a core, radiation zone and convection zone where nuclear fusion occurs. It also has an atmosphere of a photosphere, chromosphere and corona. The different layers have varying temperatures, from over 15 million Kelvin in the core to around 6,000 Kelvin in the photosphere. The Sun also produces solar wind, prominences and flares.
Space Environment & It's Effects On Space Systems course samplerJim Jenkins
This class on the space environment and its effects on space systems is for technical and management personnel who wish to gain an understanding of the important issues that must be addressed in the development of space instrumentation, subsystems, and systems. The goal is to assist students to achieve their professional potential by endowing them with an understanding of the fundamentals of the space environment and its effects. The class is designed for participants who expect to either, plan, design, build, integrate, test, launch, operate or manage payloads, subsystems, launch vehicles, spacecraft, or ground systems.
Each participant will receive a copy of the reference textbook: Pisacane, VL. The Space Environment and its Effects on Space Systems. AIAA Education Series, 2008.
This two-day professional development course taught by Dr. Alan Tribble focuses on the space environment and its implications for spacecraft design. The course provides an introduction to the space environment, including the vacuum, neutral gases, plasma, radiation, and micrometeoroids. It emphasizes techniques for minimizing environmental effects through proactive design. Participants receive course materials and can apply the concepts to engineering systems with adequate performance margins and spacecraft survivability. The instructor has extensive experience in space environments and effects analysis for NASA and DoD programs.
The document summarizes key aspects of the sun's structure and activity. It describes the sun's three layers - the core, radiative layer, and convective layer. It also outlines the three atmospheric layers of the photosphere, chromosphere, and corona. Additional sections cover sunspots, solar prominences, solar flares, and spicules. Fun facts provided include details on the sun's rotation, gravity, lifespan, and Americans' understanding of it being a star. The final section describes how scientists used observations of a solar tsunami to measure the sun's magnetic field for the first time.
Solar energy, Uneven Heating of Earth, Wind, and Ocean Currentsjdlowe78
The document discusses sea breezes and land breezes caused by uneven heating of land and water surfaces. During the day, the land heats up more quickly than the ocean, causing warm air over the land to rise and cooler air over the water to move inland, creating a sea breeze. At night, the pattern reverses as the land cools more quickly, resulting in a land breeze with warm air moving from the ocean to the land. Diagrams show this cycle of convection currents and the directional shift of winds between day and night.
The document summarizes key information about the sun. It begins by stating that the sun is an average sized star, located at the center of the solar system, composed primarily of hydrogen and helium. It then describes the various layers of the sun, including the core, radiation layer, convection layer, photosphere, chromosphere, and corona. It explains that nuclear fusion in the core converts hydrogen into helium, releasing energy in the process. This energy eventually makes its way to the surface of the sun and radiates out into space.
Computer hardware devices include webcams, scanners, mice, speakers, trackballs, and light pens. Webcams connect via USB or network and are used for video calls and conferencing. Scanners optically scan images and documents into digital formats. Mice are pointing devices that detect motion to move a cursor. Speakers have internal amplifiers and audio jacks. Trackballs contain ball and sensors to detect rotation for cursor movement. Light pens allow pointing directly on CRT displays.
Space weather refers to changes in the space environment near Earth that are driven by solar activity like solar flares and coronal mass ejections. It can affect technologies like power grids, satellites, and radio communications. Space weather begins with eruptions on the sun that emit radiation, particles, and magnetic fields. It travels through space and interacts with Earth's magnetic field, ionosphere, and atmosphere. This can cause effects like geomagnetic storms, radiation storms, and radio blackouts. The impacts depend on the size and direction of the solar events as well as Earth's location in its orbit around the sun during its 11-year solar cycle.
This document provides an overview of the space environment and its effects on satellites. It discusses several factors in space including solar activity and radiation, the solar wind, solar flares, cosmic rays, and Earth's magnetic fields. It describes how these factors can cause satellite charging through plasma bombardment and the photoelectric effect. If a charge builds up, it can lead to sudden electrostatic discharges that damage satellite hardware and cause electrical problems. The space environment is complex and dynamic, and understanding its effects is important for satellite design and operation.
This document summarizes space weather and its effects. It discusses how solar activity like sunspots, solar flares, and coronal mass ejections can cause geomagnetic storms by disturbing Earth's magnetosphere. These storms increase energetic particles in the atmosphere and cause bright auroras near the poles, in addition to potentially disrupting technologies like communications systems.
Space weather refers to changing environmental conditions in near-Earth space that can influence technology systems and human life. The three main components that drive space weather are solar flares, solar energetic particles, and coronal mass ejections from the Sun. Various scales are used to categorize space weather events based on their potential impacts, which can include power outages, communication disruptions, radiation storms, and orientation problems or increased drag on satellites. The lecture concludes by reviewing current space weather forecasts.
The document summarizes information about NASA's Solar Dynamics Observatory (SDO) satellite mission to study the sun. SDO was launched in 2010 and uses high-resolution instruments to observe the sun's atmosphere, magnetic field, and irradiance. It aims to improve understanding of the sun's influence on space weather and the solar cycle. SDO provides images every minute that are 10 times clearer than previous satellites and help scientists monitor solar activity and eruptions.
“Cis-lunar” space including lunar orbit and the lunar surface is once again a strong focus
as a destination for both robotic and human space exploration
• Multiple nations are now pursuing both robotic exploration programs with spacecraft in
lunar orbit and landers on the lunar surface.
• In addition to these purely robotic exploration programs, NASA has started construction
of the Gateway space station for operations in lunar orbit and development work has
begun on the Human Landing System infrastructure which promises to return humans to
the lunar surface for the first time since the last Apollo missions in the 1970’s.
• Because the Moon has very little atmosphere and no strong intrinsic magnetic field to
protect the surface from meteoroid impacts and charge particles, respectively, the space
environments that need to be considered when designing and operating lunar
exploration missions are essentially the free-field environments used in design of
interplanetary missions
Outline
• Atmosphere
• Lunar regolith and dust
• Illumination and thermal
• Solar UV/EUV
• Ionizing radiation
o GCR
o SPE
o Albedo neutrons
• Space plasma and charging
• Meteoroid environments
o Primary impacts
o Ejecta
• DSNE Lunar Environments
The Sun is by far the largest object in the solar system, containing over 99% of its total mass. Its diameter is about 110 times that of Earth. The Sun has three interior layers - a core, radiative zone, and convective zone - and three atmospheric layers - the photosphere, chromosphere, and corona. Sunspots and 11-year solar cycles are caused by the Sun's magnetic field. Powerful solar flares and coronal mass ejections sometimes emit charged particles toward Earth but are deflected by our planet's protective magnetosphere, generated by Earth's interior movement. The northern lights occur when these particles interact with atmospheric gases.
Stars are classified using the Hertzsprung-Russell diagram, which plots stars' luminosity against their surface temperature. Most stars lie on the main sequence, including our Sun. Stars produce energy through nuclear fusion, with hydrogen fusing to form helium in their cores. This process powers stars for billions of years until they run out of hydrogen fuel and evolve into other stages like red giants or white dwarfs. The Sun has various internal layers and an atmosphere, and features like sunspots and solar flares occasionally appear on its surface.
This document provides an overview of ionizing radiation and radiation monitoring in low Earth orbit. It discusses the various sources of radiation in space, including galactic cosmic rays, solar particle events, and trapped radiation belts. It also covers the biological effects of radiation, dose terminology, radiation monitoring devices used on spacecraft, and regulations for astronaut radiation exposure limits. The goal of radiation monitoring is to ensure crew radiation exposures are as low as reasonably achievable and within safety standards to prevent both acute and long-term health effects from space radiation.
This talk was given to Airdrie Astronomy Association on 22 March 2013. Some of the material was borrowed from Daniel Mueller (ESA) and the Solar Orbiter team. More information on Solar Orbiter can be found at http://sci.esa.int/solarorbiter
This document presents an overview of space plasma physics, specifically magnetic storms and substorms. It provides basic definitions and examples to educate those unfamiliar or rusty with the science. The outline includes sections on storm and substorm basics, examples with analysis, and data collected from satellites. Magnetic storms occur over weeks/months when particles enhance the ring current. Substorms happen over hours in growth, onset/expansion, and recovery phases, seen through auroral observations and particle densities. Examples of data include images, magnetic and electric fields, and particle fluxes.
The solar wind is composed of charged particles released from the sun's corona that are accelerated along the sun's magnetic field lines. The solar wind consists mainly of electrons and protons but also contains some heavier ions. It travels through the solar system at speeds from 150-750 km/s. The solar wind interacts with Earth's magnetic field, protecting us from some cosmic rays but also posing risks during geomagnetic storms caused by coronal mass ejections. Spacecraft such as DSCOVR and SOHO monitor the solar wind and its effects.
- The lecture covered the solar activity cycle in terms of sunspots and the Sun's magnetic field, including observations of sunspots, proxies for solar activity, and the behavior of the solar magnetic field over time as seen in magnetograms and butterfly diagrams.
- A new view of the solar cycle was presented, involving "terminator events" where oppositely charged magnetic bands meet at the equator and annihilate, marking the end of a cycle. This new model allows prediction of cycle 25's maximum sunspot number to be 233, higher than other current predictions.
The Sun is a glowing ball of gas held together by gravity that is powered by nuclear fusion. It has a diameter of 1.392 million km and is made up primarily of hydrogen and helium. Nuclear fusion in the core converts hydrogen to helium, releasing enormous amounts of energy over billions of years. Features on the Sun include sunspots, solar flares, and prominences, which can impact Earth.
The Sun is a star composed of hot gas that powers itself through nuclear fusion in its core. It has several layers including the photosphere, chromosphere, and corona. The Sun's interior is divided into a radiative zone where heat transfers by radiation and a convection zone where heat rises and falls. Nuclear fusion in the core converts hydrogen to helium, releasing energy over billions of years. Magnetic activity on the surface includes sunspots, solar flares, and prominences. The solar wind carries the Sun's magnetic fields and particles into space.
- The document discusses the heliocentric model of the solar system proposed by Copernicus and refined by Kepler, including Kepler's three laws of planetary motion. It then provides an overview of the formation of the solar system according to the nebular hypothesis and describes the key characteristics of planets Mercury through Saturn, including their orbits, compositions, atmospheres, moons, and surfaces. The solar system is understood to have formed from a large nebula that collapsed under gravity to form the Sun and planets approximately 4.6 billion years ago.
This document provides an overview of solar exploration. It summarizes that the sun is a normal star that is made up mostly of hydrogen and helium. It discusses the sun's structure, temperature, magnetic field, and 11-year solar cycle. The document also describes various solar phenomena observed at different wavelengths, such as sunspots, flares, prominences, and coronal mass ejections, as well as their potential effects on Earth. It briefly mentions some open questions in the field and lists some past and present space missions that observe the sun.
The Sun is a giant ball of burning gas composed primarily of hydrogen and helium. It generates energy through the process of nuclear fusion, where hydrogen atoms fuse into helium atoms. This releases a tremendous amount of energy. The Sun supplies Earth with energy in the form of electromagnetic radiation, including visible light, infrared and ultraviolet rays. Variations in Earth's orbit and axis affect the distribution of solar energy received on Earth through Milankovitch cycles. The Sun's energy drives photosynthesis and powers natural processes on Earth.
The document discusses frameworks for data mining (DM) research and argues that the field could benefit from adopting an information systems (IS) perspective. It summarizes existing theory-oriented frameworks from databases, statistics, machine learning, and data compression. It also outlines process-oriented frameworks like Fayyad's and CRISP-DM. However, it notes that most DM research focuses on technical rigor over practical relevance. The document proposes a new framework that views DM systems as IS artifacts and DM research as an IS development process, in order to increase real-world impact and organizational considerations.
Indonesia perlu memprioritaskan pendidikan IPTEK dan karakter bangsa, serta mengembangkan energi alternatif untuk menjadi negara maju. Indonesia memiliki sumber daya alam yang memadai untuk mandiri, namun perlu pemimpin yang visiioner dan tegas memerangi korupsi.
CANFIS is a generalized form of ANFIS that allows for both multiple inputs and outputs by extending the single-output framework of ANFIS. In CANFIS, the antecedents are the same for each output but the consequents differ according to the number of required outputs. Fuzzy rules are constructed with shared membership values to express correlations between outputs. This approach differs from placing independent ANFIS models side-by-side, as in MANFIS, which does not allow for modifiable parameters to be shared between models and makes realizing correlations between outputs more difficult.
This document discusses climate change in Indonesia and efforts to tackle it. It covers impacts of climate change like floods and droughts in Indonesia. It then discusses Indonesia's National Council on Climate Change, their goals of mainstreaming climate policies and strategies. This includes renewable energy development, forestry programs, and analyzing ocean carbon fluxes. The document ends by outlining Indonesia's submissions to the UNFCCC regarding adaptation, technology transfer and capacity building priorities like monitoring climate impacts on oceans.
This document discusses climate modeling and weather modification in Indonesia. It outlines computing intensive climate models and introduces soft computing approaches like adaptive neuro-fuzzy inference systems (ANFIS) and fuzzy clustering for climate forecasting. It analyzes the relationship between sunspot numbers and rainfall in several Indonesian regions and finds correlations. The document concludes that numerical climate models need modifications for Indonesian regions and that solar activity is the main factor determining Indonesia's climate.
This document discusses social networks and social network analysis. It defines social networks as connections between individuals or organizations, and social network analysis as mapping and measuring relationships between connected entities. The document outlines how social network analysis is used to measure networks in terms of degree centrality, betweenness centrality, and closeness centrality. It provides examples of how social network analysis has been applied and discusses how technologies like LinkedIn and blogs help create social networks. The future of social networks and social network analysis is discussed in terms of reducing complexity through simulation analysis and geographic information modeling.
Introduction to-graph-theory-1204617648178088-2Houw Liong The
This document provides definitions and theorems related to graph theory. It begins by defining simple graphs, degrees of vertices, and the handshaking lemma. It then discusses paths and cycles in graphs, connectedness, Euler and Hamiltonian paths/circuits. Specific graph types are introduced like trees, planar graphs, and regular graphs. Euler's formula is presented for planar graphs. Definitions of isomorphism and subgraphs are also provided. Theorems regarding trees state that a tree with more than one vertex has at least one vertex of degree one, and that a tree with n vertices has exactly n-1 edges.
The document discusses trends and research areas in data mining, including mining complex data types like sequences, graphs, and streams; various data mining methodologies like statistical, visual, and audio approaches; applications of data mining in domains like finance, retail, science, and intrusion detection; and emerging issues at the intersection of data mining and society.
The document describes different types of clustering algorithms, including partitioning, hierarchical, density-based, and grid-based methods. Partitioning methods like k-means and k-medoids aim to partition objects into k clusters by optimizing an objective function. Hierarchical clustering builds a hierarchy of clusters based on distance, either through an agglomerative (bottom-up) or divisive (top-down) approach. Density-based methods identify clusters based on density rather than distance. Grid-based methods quantize the space into a finite number of cells that form a grid structure.
This document summarizes various clustering algorithms including:
- K-means clustering which partitions objects into k groups by iteratively updating cluster centroids.
- Hierarchical clustering which uses distance metrics to iteratively merge or split clusters in a dendrogram without needing k as input.
- Density-based methods like DBSCAN which group together densely clustered points.
- Probabilistic and model-based clustering which represent clusters as probability distributions like Gaussian mixtures fitted using EM.
This document discusses text mining and lexicon construction. It introduces text mining and describes how lexicons are important for tasks like question answering and information extraction. It then discusses different approaches for constructing lexicons, including iterative expansion of phrase lists, multilevel bootstrapping, and co-training algorithms using internal word features.
This document provides an overview of graph mining techniques. It discusses the motivation and applications of graph mining, including that graphs are useful for modeling many real-world domains. It also outlines different approaches for frequent subgraph mining, including the Apriori-based FSG algorithm and the DFS-based gSpan algorithm. FSG uses canonical labeling and other heuristics to efficiently find frequent subgraphs in a transactional graph database. gSpan represents graphs as DFS codes to explore the search space in a systematic way to discover all frequent subgraphs.
Chapter 11 cluster advanced : web and text miningHouw Liong The
This document provides an overview of advanced clustering analysis techniques discussed in Chapter 11 of the textbook "Data Mining: Concepts and Techniques". It begins with an introduction to probability model-based clustering and fuzzy clustering. It then discusses using the EM algorithm for fuzzy clustering and fitting univariate Gaussian mixture models. Next, it covers challenges with clustering high-dimensional data and methods for subspace clustering. It also briefly introduces clustering graphs and network data as well as clustering with constraints. The document concludes with an outline of the chapter.
Chapter 9 of the document discusses advanced classification methods including Bayesian belief networks, classification using backpropagation neural networks, support vector machines, classification with frequent patterns, lazy learning, and other techniques. It describes how these methods work, including how Bayesian networks are constructed, how backpropagation trains neural networks, how support vector machines find optimal separating hyperplanes, and considerations around efficiency and interpretability. The chapter also covers mathematical mappings of classification problems and discriminative versus generative classifiers.
This document summarizes a presentation about social networks and supernetworks. It discusses the history of social network theory and applications. It also describes how supernetworks integrate social networks with economic networks to model how relationship levels and flows are codependent and coevolve over time. Computational tools are used to study supply chains, financial networks, and how social relationships impact transactions. The research aims to better understand complex network dynamics and behaviors.
The document discusses how to mathematically represent system dynamics models using differential equations. It explains that system dynamics describe systems using state variables (stocks) and their rates of change (flows), which can be expressed as differential equations. These equations can be linear or nonlinear. The document provides several examples of system dynamics models translated into systems of differential equations. It also discusses how to interpret graphical functions and their derivatives to determine behaviors.
Integrated Marketing Communications (IMC)- Concept, Features, Elements, Role of advertising in IMC
Advertising: Concept, Features, Evolution of Advertising, Active Participants, Benefits of advertising to Business firms and consumers.
Classification of advertising: Geographic, Media, Target audience and Functions.
Views in Odoo - Advanced Views - Pivot View in Odoo 17Celine George
In Odoo, the pivot view is a graphical representation of data that allows users to analyze and summarize large datasets quickly. It's a powerful tool for generating insights from your business data.
The pivot view in Odoo is a valuable tool for analyzing and summarizing large datasets, helping you gain insights into your business operations.
Principles of Roods Approach!!!!!!!.pptxibtesaam huma
Principles of Rood’s Approach
Treatment technique used in physiotherapy for neurological patients which aids them to recover and improve quality of life
Facilitatory techniques
Inhibitory techniques
How to Add Colour Kanban Records in Odoo 17 NotebookCeline George
In Odoo 17, you can enhance the visual appearance of your Kanban view by adding color-coded records using the Notebook feature. This allows you to categorize and distinguish between different types of records based on specific criteria. By adding colors, you can quickly identify and prioritize tasks or items, improving organization and efficiency within your workflow.
How to Store Data on the Odoo 17 WebsiteCeline George
Here we are going to discuss how to store data in Odoo 17 Website.
It includes defining a model with few fields in it. Add demo data into the model using data directory. Also using a controller, pass the values into the template while rendering it and display the values in the website.
Split Shifts From Gantt View in the Odoo 17Celine George
Odoo allows users to split long shifts into multiple segments directly from the Gantt view.Each segment retains details of the original shift, such as employee assignment, start time, end time, and specific tasks or descriptions.
The membership Module in the Odoo 17 ERPCeline George
Some business organizations give membership to their customers to ensure the long term relationship with those customers. If the customer is a member of the business then they get special offers and other benefits. The membership module in odoo 17 is helpful to manage everything related to the membership of multiple customers.
Lecture_Notes_Unit4_Chapter_8_9_10_RDBMS for the students affiliated by alaga...Murugan Solaiyappan
Title: Relational Database Management System Concepts(RDBMS)
Description:
Welcome to the comprehensive guide on Relational Database Management System (RDBMS) concepts, tailored for final year B.Sc. Computer Science students affiliated with Alagappa University. This document covers fundamental principles and advanced topics in RDBMS, offering a structured approach to understanding databases in the context of modern computing. PDF content is prepared from the text book Learn Oracle 8I by JOSE A RAMALHO.
Key Topics Covered:
Main Topic : DATA INTEGRITY, CREATING AND MAINTAINING A TABLE AND INDEX
Sub-Topic :
Data Integrity,Types of Integrity, Integrity Constraints, Primary Key, Foreign key, unique key, self referential integrity,
creating and maintain a table, Modifying a table, alter a table, Deleting a table
Create an Index, Alter Index, Drop Index, Function based index, obtaining information about index, Difference between ROWID and ROWNUM
Target Audience:
Final year B.Sc. Computer Science students at Alagappa University seeking a solid foundation in RDBMS principles for academic and practical applications.
About the Author:
Dr. S. Murugan is Associate Professor at Alagappa Government Arts College, Karaikudi. With 23 years of teaching experience in the field of Computer Science, Dr. S. Murugan has a passion for simplifying complex concepts in database management.
Disclaimer:
This document is intended for educational purposes only. The content presented here reflects the author’s understanding in the field of RDBMS as of 2024.
Feedback and Contact Information:
Your feedback is valuable! For any queries or suggestions, please contact muruganjit@agacollege.in
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1. Space Weather:
What is it?
How Will it Affect You?
An introduction to Space Weather
• What is it?
• Where does it come from?
• What does it do?
Rodney Viereck
NOAA Space Environment Center
Boulder Colorado
2. Space Weather:
What is it?
Space Weather refers
to changes in the space
environment near Earth
Earth
Sun
Sun:
• Energy (386 Billion Billion MegaWatts) released in
the form of…
• Light
• Particles (electrons and protons)
• Magnetic Field
• Activity Cycles
• 27 Days (solar rotation)
• ~100 Days Active Region Development
• 11 years
• 22 years
• 88 years
3. GOES Solar X-Rays
Space weather events
are usually initiated
by a solar flare or a
coronal mass
ejection
During a solar flare,
the x-ray irradiance
can increase by
several orders of
magnitude in just a
few minutes
4. Space Weather refers
to changes in the space
environment near Earth
Sun
Interplanetary Space:
• Solar Wind
•Constant outflow from the sun
•Electrons and protons
• Disturbances from the sun produce
waves and shocks in the solar wind
Interplanetary Space
Space Weather:
What is it?
Earth
5. ACE Solar Wind
• Solar Wind
– Density
• 1 to 100 particles per cm3
– Speed
• 200 to 800 km/sec
6. Space Weather refers
to changes in the space
environment near Earth
Magnetosphere
Magnetosphere:
• Created by Earth’s magnetic field
• Deformed by the Solar Wind
• Particles (electrons and protons) trapped
on magnetic field lines
Sun
Interplanetary Space
Space Weather:
What is it?
Earth
8. Space Weather refers
to changes in the space
environment near Earth
Magnetosphere
Sun
Interplanetary Space
Ionosphere
Ionosphere:
• Layer of electrons at the top of the
atmosphere (100 – 300 km up)
• Formed when extreme ultraviolet light
from the sun hits Earth’s Atmosphere
• Strongly affected by changes in the
magnetosphere
• Critical in the reflection and
transmission of radio waves
Space Weather:
What is it?
Earth
9. POES Ionospheric Particles
• Auroral Oval
– Electrons and
Protons collide with
the atmosphere
– The collisions excite
atoms and molecules
to produce the
aurora
10. Other Space Weather Terms
• Solar Flare: An eruption on the sun that emits light (UV and
x-rays) and often particles (electrons and protons).
• CME (Coronal Mass Ejection): A disturbance in the solar wind
caused by an eruption on the sun.
• Solar Wind: The outward flow of electrons, protons, and
magnetic field from the sun.
• Energetic Particles: electrons and protons that have been
accelerated to high speeds.
• Geomagnetic Storm: The disturbance in the near-Earth
particles and magnetic fields that can upset technological
systems and creates aurora.
• Radiation Storm: A large flux of solar energetic protons as
measured near Earth.
• Radio Blackout: An enhancement in the lower ionosphere as a
result of large x-ray flares.
11. Sequence Of Events
• Active Region on the Sun Erupts
1. Solar Flare (x-ray)
2. Shock (energetic particles)
3. Corornal Mass Ejection (particles and fields)
• X-rays reach Earth in 8 minutes (speed of light)
• Energetic Particles reach Earth in 15 min to 24
hours
• Coronal Mass Ejection reaches Earth in 1-4 Days
12. Three Types of Space Weather
Storms
1.Radio Blackouts
– Solar Flares send out x-
rays
– Arrive at Earth in 8
minutes
– Modify the ionosphere
– Disrupt HF radio
communication
– Impacts:
• Airline communication
• HF radio operators
• DoD Communications
• Satellite Communications
2.Radiation Storms
– Solar Flares and Coronal
Mass Ejections (CMEs)
send out Energetic
Particles
– Arrive at Earth in 15
minutes to 24 hours
– Modify the high latitude
ionosphere
– Disrupt HF radio
communication
– Impacts:
• Airline communication
• HF radio operators
• DoD Communications
– Ionizing radiation
penetrates into the
atmosphere
– Impacts:
• Astronauts (radiation)
• Satellite failures
3.Geomagnetic Storms
– Coronal Mass Ejections
(CMEs) send out Magnetic
Clouds
– Arrive at Earth in 1-4
days
– Accelerate particles within
the magnetosphere and
into the ionosphere
– Impacts:
• HF radio communication
• Radio Navigation (GPS)
• Electric Power Grids
• Increased Satellite Drag
• Aurora
13. The Sun
The Energy Source
The sun in X-rays
From GOES 12
•The Sun
• Rotates every 27 days
• Has an 11-year cycle of
activity
•Flares produce large
amounts of x-rays and
extreme ultraviolet light
but not much visible
light
An Erupting Prominence
A Solar Flare
Image from NASA TRACE Satellite
Image from NASA SOHO Satellite
14. Solar Photons (Light)
• Visible light (small slow changes)
– Most of the energy output
– Impacts climate
• UV light (medium slow changes)
– Affects ozone production and loss
• EUV light (large changes)
– Affects radio communication
– Affects navigation
– Affects satellite orbits
• X-ray light (Can change by a
factor of 1000 in five minutes)
– Affects radio communication
Solar spectrum
Solar variability
Atmospheric penetration
X-Ray Flare
Variability
(minutes)
Lean
15. Product for Radio Operators
Effect of Solar X-rays on D-Region and HF Propagation.
• D-Region Absorption Product based on GOES X-RayFlux (SEC Product)
– The map shows regionsaffected by the increased D-region ionization resulting
from enhanced x-ray flux during magnitude X-1 Flare
TJFR
16. CMEs (Coronal Mass Ejections)
in Interplanetary Space
• While Solar flares send out light
(mostly x-rays)
• CMEs produce…
– Energetic particles
– Magnetic structures
Propagate away from the sun
but their paths are modified
by the background solar wind
and the sun’s magnetic field.
Image from NASA SOHO Satellite
Image from NASA SOHO Satellite
17. Magnetosphere
What happens when a CME hits Earth?
1. Solar wind is deflected around Earth
2. Deflected solar wind drags Earth’s magnetic field with it
3. Magnetic field lines “reconnect” and accelerate particles
4. Accelerated particles follow field lines to Earth
Aurora is produced when particles hit Earth’s atmosphere
1. Solar wind
is deflected
around Earth
2. Deflected solar wind
drags Earth’s magnetic field
with it
3. Magnetic field lines
“reconnect” and
accelerate particles
4. Accelerated particles
follow field lines to Earth
Aurora
Outer
Radiation
Belt
Inner
Belt
18. Energetic Particle Effects
Spacecraft Systems
• Systems affected
– Spacecraft electronics
• Surface Charging and Discharge
• Single Event Upsets
• Deep Dielectric Charging
– Spacecraft imaging and attitude systems
Polar Satellite Image Degradation
SOHO Satellite Image
Degradation
Spacecraft Surface Charging (NASA animation)
19. Energetic Particles Effects
Radiation Hazard
Health Hazards from
Energetic Particles
• Humans in space
– Space Shuttle,
International Space
Station, missions to
Mars
• Crew/Passengers in high-
flying jets
– Concorde carries
radiation detectors
– Passengers and crew
may receive radiation
doses equivalent to many
chest X rays.
20. Ionosphere
• The particles collide with
the atmosphere and
produce the Aurora and
currents in the
ionosphere
• As geomagnetic activity
increases, the aurora
gets brighter, more
active, and moves away
from the polar regions.
– Electric Power is affected
– Navigation Systems are
affected
– Radio Communications are
affected
Image from NASA IMAGE Satellite
21. Geomagnetic Storm Effects
March 1989
Hydro Quebec Loses Electric Power for 9 Hours
Transformer Damage
Electric Power
Transformer
22. Aurora
• The particles spiral
down the magnetic
filed lines and collide
with the atmosphere
to produce the
aurora.
• Colors indicate the
atoms or molecules
that are excited by
the incoming particles
23. Geomagnetic Storm Effects
Aurora
• Intensity and location of the aurora depend on strength of storm
• Best time to view is around midnight
• No guarantee that aurora will occur
G5
G3
G1
Photo by Jan Curtis, http://www.geo.mtu.edu/weather/aurora
24. Geomagnetic Storms
• Disrupt Radio Communications • Impact Electric Power Systems
• Impact Satellites• Disrupt Radio Navigations
25. NASA Animation
Sun to Earth
• An animation of a space weather event as it
starts at the sun and end up at Earth
– Solar Flare
• Light
• Particles
• CME
– Magnetosphere
• Deflects the solar wind
• Responds to the disturbance
• Accelerates particles
– Ionosphere
• Accelerated particles collide with the atmosphere
producing the aurora
26. Space Weather Storms
Timing and Consequences
• At T = 0, A Flare and CME
Erupts on the Sun
• 8 Minutes later: First blast of
EUV and X-Ray light increases
the ionospheric density
– Radio transmissions are lost
• 30 min. to 24 hrs. later:
Energetic Particles Arrive
– Astronauts are at risk
– Satellites are at risk
– High altitude aircraft crew
are at risk
• 1 to 4 Days Later: CME Arrives
and energizes the
magnetosphere and ionosphere
– Electric Power is affected
– Navigation Systems are
affected
– Radio Communications are
affected
Movie from NASA SOHO Satellite
27. What Controls the Size a Space Weather
Storm?
• The Size of Flare or CME
– Big solar events tend to
make big storms
• The Location of the flare
site on the SUN
– If it is directed at Earth, it
is more likely to make a
storm
– If it toward the west side of
the sun, the particles will
arrive sooner
• The Direction of the
Magnetic Field in the CME
– If the interplanetary
magnetic field is southward,
then there will likely be a big
storm
Note, there does not have to be
a solar flare or CME to
create a geomagnetic storm
28. Space Weather Scales
• Three Categories
– Geomagnetic Storms
(CMEs)
– Solar Radiation Storms
(Particle Events)
– Radio Blackouts
(Solar Flares)
Combs
Rabin
29. How Often Do Space Weather Storms Occur?
• Solar Cycle is about 11 Years
Radiation Storms
1-4 per month at max
Geomagnetic Storms
3-5 per month at max
Radio Blackouts
50-100 per month at max
Sunspot Number
11-year cycle
1955 1960 1965 1970 1975 1980 1985 1990 1995 2000
Year
EventsPerMonthEventsPerMonth
EventsPerMonth
30. The Solar Cycles of the Past
• Sunspots have been recorded for the last 400 years
• Note that there were no sunspots for nearly 60
years after 1640
• During the same period, it was very cold in Europe.
This is a period called “The Little Ice Age”
• Is there a Connection?
• Recent studies say there may be
Solar Maximum
Solar
Minimum
31. Sun and Climate
• The sun is the primary engine for weather and the climate
• Very large climate changes (Ice ages) are known to be caused by
changes in insolation (amount and distribution of sunlight)
• The sun is likely responsible for some of the climate change… up to
1960s… but not the rapid increase in temperatures since then.
NCAR Climate Model
Ammann: SORCE 2003
32. NOAA POES
NOAA GOES
NASA ACE
NASA SOHO
Primary Space Weather Satellites
for SEC
• ACE
– Solar wind composition,
speed, and direction
– Magnetic field
strength and direction
• SOHO
– Solar EUV Images
– Solar Corona
(CMEs)
• STEREO
– CME Direction and
Shape
– Solar wind composition,
speed, and direction
– Magnetic field
strength and direction
• GOES
– Energetic Particles
– Magnetic Field
– Solar X-ray Flux
– Solar X-Ray Images
• POES
– High Energy
Particles
– Total Energy
Deposition
– Solar UV Flux
NASA STEREO
(Ahead)
NASA STEREO
(Behind)
• Events are observed on and near the sun
• No measurements until the Particles or CMEs
are 99% of the way to Earth
• This provides only 30 minutes lead time for
CMEs and no lead time for other events
33. Summary
Arrival 8 minutes 15 min. to 24 hrs. 1 to 4 days
Time
Radio Blackouts
Bursts of X-ray and
EUV radiation
Radiation Storms
Energetic Particles
(electrons and protons)
Geomagnetic
Storms
When the CME
reaches Earth
Systems Radio Comm. Satellites Power Companies
Affected Airlines Astronauts Radio Comm.
Radio Comm. Navigation (GPS)
Satellite Drag
• Space Weather Storms come in three main categories
• Each category originates from different physical processes
• Each category arrives at a different speed
• Each category affects different users and technologies
Space
Weather
Event