Stars - Liling
•
1 like•371 views
I
ihslStars are collections of dust and gas held together by gravity. They can be classified based on characteristics like temperature, luminosity, type, spectral class, and size. The main types of stars are main sequence, dwarf, giant, and supergiant stars. Nuclear fusion is the process by which stars generate energy by fusing hydrogen into helium. A star typically begins as a stellar nebula, collapses under gravity, and progresses through stages as a red giant or supergiant before exploding as a planetary nebula or supernova, eventually becoming a white dwarf, neutron star, or black hole.
Report
Share
Report
Share
Recommended
Interactive PowerPoint: Classifying Stars
Stars form from clouds of dust and gas called nebulae. Gravity causes the gas and dust to collapse into a dense protostar at the center. When the protostar becomes hot and dense enough, nuclear fusion occurs, releasing energy and causing the star to shine. A star's lifespan depends on its mass - lower mass stars last for billions of years, while higher mass stars only last millions of years before ending their lives in supernova explosions. Scientists classify stars based on their temperature and the elements they absorb, with classifications ranging from hottest O-type stars to coolest M-type stars.
Hertzsprung Russell Diagram
The document summarizes the Hertzsprung–Russell diagram, which plots stars based on their color, temperature, and brightness over their life cycles. It explains that the diagram shows how stars change from blue and hot as O class stars to red and cool as M class stars. The document uses our sun as an example, showing where it is now on the main sequence and where it will be as a red giant and white dwarf. It notes that black dwarfs would not be shown on the diagram since they emit no light or heat.
Stars
A star is a huge ball of gas held together by gravity that produces energy through nuclear fusion in its core. This energy radiates out from the star as light, making it glow and shine. Stars come in different sizes, colors, and temperatures, like our Sun which is a yellow star of average size and heat. A star shines through nuclear fusion in its core converting hydrogen to helium and releasing huge amounts of energy. This energy radiates out from the star, making it shine.
Stars
Stars originate from swirling clouds of gas and dust that condense under gravity to form dense spheres called protostars. As protostars gain mass through accretion, the internal pressure and temperature rises until nuclear fusion of hydrogen begins, forming a main sequence star. Over its lifetime, a main sequence star fuses hydrogen into helium in its core. More massive stars end as supernovae, leaving behind neutron stars or black holes, while less massive stars expand into red giants and later shed their outer layers, leaving behind a fading white dwarf.
Stars concept map_notes2_2
The document discusses the classification of stars based on size, temperature, brightness, and lifespan. It describes how stars are born from nebulae and how their lifespan and death depends on their mass. Smaller stars have less violent deaths, becoming white dwarfs, while larger stars die in supernova explosions, potentially leaving behind neutron stars or black holes. It also provides an overview of the different types of galaxies including spiral, elliptical, and irregular galaxies.
Stars
A star is a ball of plasma held together by gravity that undergoes nuclear fusion at its core, releasing electromagnetic radiation. Stars exist along a spectrum from hot, blue stars to cooler, red stars and can be classified based on their temperature, luminosity, and color. A star's life cycle begins as a contracting nebula and progresses through stages such as the main sequence, red giant, planetary nebula, and white dwarf before ending as a neutron star or black hole.
7.2 characteristics and evolution of stars
1) Stars begin as clouds of dust and gases called nebulae. Under gravity, the gases condense to form protostars and begin nuclear fusion, becoming main sequence stars like our Sun.
2) As stars age, they expand and become red giants or supergiants after exhausting hydrogen fusion. Further fusion of helium produces carbon.
3) When further fusion is no longer possible, the star collapses into a white dwarf, neutron star, or black hole in a supernova explosion, depending on the star's original mass.
The Star
This document provides an overview of the characteristics, classifications, motions, and significance of stars. It discusses their sizes, colors, temperatures, compositions, and magnitudes. Stars are classified based on their spectral types, which relate to their surface temperatures. The Hertzsprung-Russell diagram plots stars' luminosities and temperatures. Stars exhibit both apparent and actual motions, including proper motion across the sky. Studying stars helps us understand how elements are formed, how our solar system evolved, and the dynamics influencing galaxies.
Recommended
Interactive PowerPoint: Classifying Stars
Stars form from clouds of dust and gas called nebulae. Gravity causes the gas and dust to collapse into a dense protostar at the center. When the protostar becomes hot and dense enough, nuclear fusion occurs, releasing energy and causing the star to shine. A star's lifespan depends on its mass - lower mass stars last for billions of years, while higher mass stars only last millions of years before ending their lives in supernova explosions. Scientists classify stars based on their temperature and the elements they absorb, with classifications ranging from hottest O-type stars to coolest M-type stars.
Hertzsprung Russell Diagram
The document summarizes the Hertzsprung–Russell diagram, which plots stars based on their color, temperature, and brightness over their life cycles. It explains that the diagram shows how stars change from blue and hot as O class stars to red and cool as M class stars. The document uses our sun as an example, showing where it is now on the main sequence and where it will be as a red giant and white dwarf. It notes that black dwarfs would not be shown on the diagram since they emit no light or heat.
Stars
A star is a huge ball of gas held together by gravity that produces energy through nuclear fusion in its core. This energy radiates out from the star as light, making it glow and shine. Stars come in different sizes, colors, and temperatures, like our Sun which is a yellow star of average size and heat. A star shines through nuclear fusion in its core converting hydrogen to helium and releasing huge amounts of energy. This energy radiates out from the star, making it shine.
Stars
Stars originate from swirling clouds of gas and dust that condense under gravity to form dense spheres called protostars. As protostars gain mass through accretion, the internal pressure and temperature rises until nuclear fusion of hydrogen begins, forming a main sequence star. Over its lifetime, a main sequence star fuses hydrogen into helium in its core. More massive stars end as supernovae, leaving behind neutron stars or black holes, while less massive stars expand into red giants and later shed their outer layers, leaving behind a fading white dwarf.
Stars concept map_notes2_2
The document discusses the classification of stars based on size, temperature, brightness, and lifespan. It describes how stars are born from nebulae and how their lifespan and death depends on their mass. Smaller stars have less violent deaths, becoming white dwarfs, while larger stars die in supernova explosions, potentially leaving behind neutron stars or black holes. It also provides an overview of the different types of galaxies including spiral, elliptical, and irregular galaxies.
Stars
A star is a ball of plasma held together by gravity that undergoes nuclear fusion at its core, releasing electromagnetic radiation. Stars exist along a spectrum from hot, blue stars to cooler, red stars and can be classified based on their temperature, luminosity, and color. A star's life cycle begins as a contracting nebula and progresses through stages such as the main sequence, red giant, planetary nebula, and white dwarf before ending as a neutron star or black hole.
7.2 characteristics and evolution of stars
1) Stars begin as clouds of dust and gases called nebulae. Under gravity, the gases condense to form protostars and begin nuclear fusion, becoming main sequence stars like our Sun.
2) As stars age, they expand and become red giants or supergiants after exhausting hydrogen fusion. Further fusion of helium produces carbon.
3) When further fusion is no longer possible, the star collapses into a white dwarf, neutron star, or black hole in a supernova explosion, depending on the star's original mass.
The Star
This document provides an overview of the characteristics, classifications, motions, and significance of stars. It discusses their sizes, colors, temperatures, compositions, and magnitudes. Stars are classified based on their spectral types, which relate to their surface temperatures. The Hertzsprung-Russell diagram plots stars' luminosities and temperatures. Stars exhibit both apparent and actual motions, including proper motion across the sky. Studying stars helps us understand how elements are formed, how our solar system evolved, and the dynamics influencing galaxies.
life cycle of a star
The life cycle of stars depends on their mass. Lower mass stars like our Sun will eventually become red giants then white dwarfs. Higher mass stars live shorter lives and end as supernovas, leaving behind neutron stars or black holes. All stars begin as nebulae of dust and gas that collapse under gravity into protostars and main sequence stars fueled by nuclear fusion.
H-R Diagram
This document discusses the Hertzsprung-Russell diagram (H-R diagram), which plots stars' brightness against their surface temperatures. It shows that 90% of stars are average "main sequence" stars that are not too bright, hot, or large. The remaining 10% are "giants", "supergiants", and "white dwarfs". The H-R diagram demonstrates that hotter stars are usually brighter, while cooler stars appear dimmer.
Spectral classification of stars
This document discusses how the spectral classification of stars can reveal information about their composition and temperature. It explains that stars are classified into seven main categories (O, B, A, F, G, K, M) based on their absorption spectra, with O being the hottest and M being the coolest. Each class is associated with a range of surface temperatures and colors. By analyzing a star's spectrum, astronomers can determine what chemical elements are present in its atmosphere and measure its temperature, allowing insights into its composition and properties.
Stars and Galaxies Notes PowerPoint
This document discusses stars, galaxies, and the universe. It covers topics like constellations, star properties, the sun's layers and features, stellar evolution, types of galaxies, the Milky Way galaxy, and theories of the universe's origin and expansion. Key points include how stars evolve from nebulae to white dwarfs or other remnants, the classification of galaxies as spiral, elliptical, or irregular, and the Big Bang theory that the universe began in an enormous explosion over 12 billion years ago.
Stars
I. Interstellar Medium refers to the gas and dust between stars.
II. A nebula is a dense cloud of dust and gases that begins to contract due to gravity, increasing pressure and temperature to form a protostar.
III. When the protostar gets hot enough, fusion begins and a main sequence star is born.
The life cycle of a star
The document outlines the life cycle of stars from birth in nebulae of gas and dust through their main sequence phase, later evolution into red giants, and final stages as white dwarfs, neutron stars, or black holes. It describes how gravity pulls gas together in nebulae to form protostars, which become main sequence stars fueling nuclear fusion for millions of years. As hydrogen runs out in their cores, more massive stars explode as supernovae while lower mass stars expand into red giants then contract into white dwarfs.
Birth of the star
Stars are formed in nebulae, clouds of dust and gas found in spiral galaxies. Dense parts of these clouds undergo gravitational collapse, compressing to form a rotating gas globule. As the globule collapses over thousands to millions of years due to gravity and pressure, the increasing temperature and rotation cause it to form a central core and surrounding protoplanetary disk. Once the core reaches temperatures over 27 million degrees and nuclear fusion begins, it becomes a stable main sequence star.
Life Cycle Of A Star
The document discusses the life cycle of stars from their birth in nebulae to their death. Stars are born when gas and dust clouds collapse under gravity and heat up. During their main sequence phase, stars fuse hydrogen into helium in their cores. Later, larger stars become red giants or supergiants as their cores shrink and outer layers expand. Eventually, stars die and eject their outer layers, leaving behind dense remnants like white dwarfs, neutron stars, or black holes.
THE LIFE CYCLE OF A STAR!
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.
Constellations-EV etc.
This document discusses various celestial objects and concepts related to observing the night sky, including:
- The celestial sphere, an imaginary sphere surrounding Earth on which stars and other celestial objects appear to be located. Important circles on the celestial sphere include the celestial equator and the ecliptic.
- Constellations, patterns of stars grouped together, of which there are 88 officially recognized. Asterisms are smaller distinctive star groups within constellations.
- The zodiac, a band of 13 constellations along the ecliptic through which the sun passes each year.
- How the night sky appearance changes based on one's latitude on Earth. Tools for observing and measuring positions of celestial objects
The Life Cycle of a Star PowerPoint
Stars are born from clouds of gas and dust called nebulae. Over billions of years, stars progress through various stages as they age. Lower mass stars begin as protostars and become main sequence stars fueled by nuclear fusion. As their hydrogen runs out, they become red giants and eventually white dwarfs. Higher mass stars explode as supernovae at the end of their lives, leaving behind neutron stars or black holes.
25 1
This document discusses properties of stars including constellations, binary stars, light-years, apparent and absolute magnitude, main sequence stars, red giants, supergiants, Cepheid variables, novas, and nebulae. Key concepts covered are that a star's color is related to its temperature, binary stars help determine a star's mass, parallax angles are largest for nearby stars and too small to measure for distant stars, and apparent brightness depends on a star's size, temperature, and distance from Earth. A Hertzsprung-Russell diagram shows the relationship between absolute magnitude and temperature for stars.
Life cycle of stars
The document summarizes the life cycle of stars from their birth in nebulae to their death as either white dwarfs, neutron stars, or black holes. It describes how stars are born from dense clouds of gas and dust called nebulae. As stars age, they evolve from the main sequence to red giants fueled by nuclear fusion. Small stars eventually die as white dwarfs, while massive stars die spectacularly in supernovae, leaving behind neutron stars or black holes.
Star Classification
Stars are large balls of ionized gas held together by gravity that emit energy through nuclear reactions. They are classified based on size, temperature, and brightness. Size categories include super giants, red giants, main sequence, white dwarfs, and neutron stars. Temperature determines color, from red (coolest) to blue (hottest). Brightness depends on both a star's intrinsic luminosity and its distance from Earth. Spectrographs are used to analyze starlight and determine properties like chemical composition, temperature, and distance.
L Ife Of A Star
The life cycle of a star begins as a nebula of gas and dust that collapses under gravity into a protostar. Once dense and hot enough, nuclear fusion begins, creating the energy output of a star. Most stars, including our sun, spend the longest part of their life on the main sequence. Eventually stars grow into red giants and later white dwarfs as they run out of fuel. More massive stars may explode as supernovae, leaving behind neutron stars or black holes.
Star formation
The document discusses the lifecycle of stars from their formation to death. It begins by defining what stars and constellations are. It then focuses on our sun as a medium-sized, yellow star at the center of our solar system. Stars are classified based on temperature and brightness as young dwarf stars or older, larger supergiant stars. The document outlines the typical stages a star like the sun will progress through over billions of years from birth from clouds of dust and gas, burning hydrogen through nuclear fusion as a main sequence star, and eventual death through expansion and explosion at the end of its life. Various nebulae and supernova remnants are used as examples of star birth and death.
Life Cycle Ppt.
Stars are formed from dense clouds of gas and dust called nebulas. Over millions of years, the nebula collapses under gravity to form a protostar. Once the protostar's core reaches 10 million K, nuclear fusion begins and the star enters the main sequence stage. During the main sequence, internal pressure balances gravitational forces. Low and medium mass stars end as white dwarfs, then eventually black dwarfs. Massive stars may explode as supernovae, leaving behind neutron stars or black holes.
Life cycle of a star
Stars are born from contracting nebulae of gas and dust. They spend most of their lives on the main sequence, fusing hydrogen into helium in their cores. Eventually they run out of fuel in their cores and their outer layers expand, forming red giants or supergiants. From there, smaller stars shed their outer layers to form planetary nebulae and white dwarfs, while larger stars explode as supernovae, leaving behind neutron stars or black holes.
Star Life Cycle
Stars are born from clouds of gas and dust called nebulas. As the gas spins faster under gravity, it heats up and forms a protostar. Nuclear fusion then occurs, turning the protostar into a main sequence star that shines for millions of years by fusing hydrogen into helium. Eventually the hydrogen runs out, causing the star to expand into a red giant. From there, less massive stars will blow off their outer layers and collapse into white dwarfs, while more massive stars will explode in supernovas and collapse into neutron stars or black holes.
Stars And Galaxies
1. Stars form from nebulae, which are dusty clouds in space. They begin as protostars and then become main sequence stars like our sun or massive stars.
2. After billions of years, main sequence stars become red giants as they run out of hydrogen fuel. Massive stars become red supergiants.
3. When stars die, red giants form planetary nebulae and red supergiants explode as supernovae. The remains of stars form neutron stars, black holes, white dwarfs or black dwarfs.
METEOR - Liling
Meteors are space rocks that enter Earth's atmosphere. They form outside of Earth and produce light when they rub against the air. Meteors range in size from a grain of sand to a baseball and the fastest ones travel at 26 miles per second. A million meteors reach the atmosphere every day and there are about 9 annual meteor showers.
More Related Content
What's hot
life cycle of a star
The life cycle of stars depends on their mass. Lower mass stars like our Sun will eventually become red giants then white dwarfs. Higher mass stars live shorter lives and end as supernovas, leaving behind neutron stars or black holes. All stars begin as nebulae of dust and gas that collapse under gravity into protostars and main sequence stars fueled by nuclear fusion.
H-R Diagram
This document discusses the Hertzsprung-Russell diagram (H-R diagram), which plots stars' brightness against their surface temperatures. It shows that 90% of stars are average "main sequence" stars that are not too bright, hot, or large. The remaining 10% are "giants", "supergiants", and "white dwarfs". The H-R diagram demonstrates that hotter stars are usually brighter, while cooler stars appear dimmer.
Spectral classification of stars
This document discusses how the spectral classification of stars can reveal information about their composition and temperature. It explains that stars are classified into seven main categories (O, B, A, F, G, K, M) based on their absorption spectra, with O being the hottest and M being the coolest. Each class is associated with a range of surface temperatures and colors. By analyzing a star's spectrum, astronomers can determine what chemical elements are present in its atmosphere and measure its temperature, allowing insights into its composition and properties.
Stars and Galaxies Notes PowerPoint
This document discusses stars, galaxies, and the universe. It covers topics like constellations, star properties, the sun's layers and features, stellar evolution, types of galaxies, the Milky Way galaxy, and theories of the universe's origin and expansion. Key points include how stars evolve from nebulae to white dwarfs or other remnants, the classification of galaxies as spiral, elliptical, or irregular, and the Big Bang theory that the universe began in an enormous explosion over 12 billion years ago.
Stars
I. Interstellar Medium refers to the gas and dust between stars.
II. A nebula is a dense cloud of dust and gases that begins to contract due to gravity, increasing pressure and temperature to form a protostar.
III. When the protostar gets hot enough, fusion begins and a main sequence star is born.
The life cycle of a star
The document outlines the life cycle of stars from birth in nebulae of gas and dust through their main sequence phase, later evolution into red giants, and final stages as white dwarfs, neutron stars, or black holes. It describes how gravity pulls gas together in nebulae to form protostars, which become main sequence stars fueling nuclear fusion for millions of years. As hydrogen runs out in their cores, more massive stars explode as supernovae while lower mass stars expand into red giants then contract into white dwarfs.
Birth of the star
Stars are formed in nebulae, clouds of dust and gas found in spiral galaxies. Dense parts of these clouds undergo gravitational collapse, compressing to form a rotating gas globule. As the globule collapses over thousands to millions of years due to gravity and pressure, the increasing temperature and rotation cause it to form a central core and surrounding protoplanetary disk. Once the core reaches temperatures over 27 million degrees and nuclear fusion begins, it becomes a stable main sequence star.
Life Cycle Of A Star
The document discusses the life cycle of stars from their birth in nebulae to their death. Stars are born when gas and dust clouds collapse under gravity and heat up. During their main sequence phase, stars fuse hydrogen into helium in their cores. Later, larger stars become red giants or supergiants as their cores shrink and outer layers expand. Eventually, stars die and eject their outer layers, leaving behind dense remnants like white dwarfs, neutron stars, or black holes.
THE LIFE CYCLE OF A STAR!
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.
Constellations-EV etc.
This document discusses various celestial objects and concepts related to observing the night sky, including:
- The celestial sphere, an imaginary sphere surrounding Earth on which stars and other celestial objects appear to be located. Important circles on the celestial sphere include the celestial equator and the ecliptic.
- Constellations, patterns of stars grouped together, of which there are 88 officially recognized. Asterisms are smaller distinctive star groups within constellations.
- The zodiac, a band of 13 constellations along the ecliptic through which the sun passes each year.
- How the night sky appearance changes based on one's latitude on Earth. Tools for observing and measuring positions of celestial objects
The Life Cycle of a Star PowerPoint
Stars are born from clouds of gas and dust called nebulae. Over billions of years, stars progress through various stages as they age. Lower mass stars begin as protostars and become main sequence stars fueled by nuclear fusion. As their hydrogen runs out, they become red giants and eventually white dwarfs. Higher mass stars explode as supernovae at the end of their lives, leaving behind neutron stars or black holes.
25 1
This document discusses properties of stars including constellations, binary stars, light-years, apparent and absolute magnitude, main sequence stars, red giants, supergiants, Cepheid variables, novas, and nebulae. Key concepts covered are that a star's color is related to its temperature, binary stars help determine a star's mass, parallax angles are largest for nearby stars and too small to measure for distant stars, and apparent brightness depends on a star's size, temperature, and distance from Earth. A Hertzsprung-Russell diagram shows the relationship between absolute magnitude and temperature for stars.
Life cycle of stars
The document summarizes the life cycle of stars from their birth in nebulae to their death as either white dwarfs, neutron stars, or black holes. It describes how stars are born from dense clouds of gas and dust called nebulae. As stars age, they evolve from the main sequence to red giants fueled by nuclear fusion. Small stars eventually die as white dwarfs, while massive stars die spectacularly in supernovae, leaving behind neutron stars or black holes.
Star Classification
Stars are large balls of ionized gas held together by gravity that emit energy through nuclear reactions. They are classified based on size, temperature, and brightness. Size categories include super giants, red giants, main sequence, white dwarfs, and neutron stars. Temperature determines color, from red (coolest) to blue (hottest). Brightness depends on both a star's intrinsic luminosity and its distance from Earth. Spectrographs are used to analyze starlight and determine properties like chemical composition, temperature, and distance.
L Ife Of A Star
The life cycle of a star begins as a nebula of gas and dust that collapses under gravity into a protostar. Once dense and hot enough, nuclear fusion begins, creating the energy output of a star. Most stars, including our sun, spend the longest part of their life on the main sequence. Eventually stars grow into red giants and later white dwarfs as they run out of fuel. More massive stars may explode as supernovae, leaving behind neutron stars or black holes.
Star formation
The document discusses the lifecycle of stars from their formation to death. It begins by defining what stars and constellations are. It then focuses on our sun as a medium-sized, yellow star at the center of our solar system. Stars are classified based on temperature and brightness as young dwarf stars or older, larger supergiant stars. The document outlines the typical stages a star like the sun will progress through over billions of years from birth from clouds of dust and gas, burning hydrogen through nuclear fusion as a main sequence star, and eventual death through expansion and explosion at the end of its life. Various nebulae and supernova remnants are used as examples of star birth and death.
Life Cycle Ppt.
Stars are formed from dense clouds of gas and dust called nebulas. Over millions of years, the nebula collapses under gravity to form a protostar. Once the protostar's core reaches 10 million K, nuclear fusion begins and the star enters the main sequence stage. During the main sequence, internal pressure balances gravitational forces. Low and medium mass stars end as white dwarfs, then eventually black dwarfs. Massive stars may explode as supernovae, leaving behind neutron stars or black holes.
Life cycle of a star
Stars are born from contracting nebulae of gas and dust. They spend most of their lives on the main sequence, fusing hydrogen into helium in their cores. Eventually they run out of fuel in their cores and their outer layers expand, forming red giants or supergiants. From there, smaller stars shed their outer layers to form planetary nebulae and white dwarfs, while larger stars explode as supernovae, leaving behind neutron stars or black holes.
Star Life Cycle
Stars are born from clouds of gas and dust called nebulas. As the gas spins faster under gravity, it heats up and forms a protostar. Nuclear fusion then occurs, turning the protostar into a main sequence star that shines for millions of years by fusing hydrogen into helium. Eventually the hydrogen runs out, causing the star to expand into a red giant. From there, less massive stars will blow off their outer layers and collapse into white dwarfs, while more massive stars will explode in supernovas and collapse into neutron stars or black holes.
Stars And Galaxies
1. Stars form from nebulae, which are dusty clouds in space. They begin as protostars and then become main sequence stars like our sun or massive stars.
2. After billions of years, main sequence stars become red giants as they run out of hydrogen fuel. Massive stars become red supergiants.
3. When stars die, red giants form planetary nebulae and red supergiants explode as supernovae. The remains of stars form neutron stars, black holes, white dwarfs or black dwarfs.
What's hot (20)
Viewers also liked
METEOR - Liling
Meteors are space rocks that enter Earth's atmosphere. They form outside of Earth and produce light when they rub against the air. Meteors range in size from a grain of sand to a baseball and the fastest ones travel at 26 miles per second. A million meteors reach the atmosphere every day and there are about 9 annual meteor showers.
Fault - Ping Tian
The document defines three types of faults: normal faults where one land moves down, reverse faults where one land moves up, and strike-slip faults where lands move sideways relative to each other. It also asks and answers three questions: there are three kinds of faults, they are named normal, reverse, and strike-slip faults, and a fault is a break in the ground where land moves.
management areas
Managers have key functional areas of management that include production, marketing, personnel management, and financial management. Financial management is closely related to other functional areas. Production determines requirements for fixed and working capital. Changes in production, like expansion or new products, impact financial requirements.
Critical angle and total internal reflection by muhammad ahad butt
This document discusses the concepts of critical angle and total internal reflection. It defines total internal reflection as the complete reflection of a light ray when the angle of incidence exceeds the critical angle at the interface between two mediums where the lower medium has a higher density. Diagrams and references are provided to illustrate the refraction of light rays at boundaries between different optical densities, and definitions are given for related terms like incident ray, refracted ray, angle of incidence, angle of refraction, normal, and medium.
Areas of management
The document discusses several areas of management including financial management, production management, personnel management, purchasing management, marketing management, research and development management, and maintenance management. For each area, it provides definitions, objectives, functions, and the typical duties and responsibilities of the associated manager.
Areas of management
This document summarizes five key areas of management: marketing management, financial management, production management, human resource management, and office management. For each area, it provides a brief overview of the functions and sub-areas. Marketing management involves activities like sales, advertising, and market research. Financial management includes accounting, costing, and taxation. Production management covers planning, quality control, and monitoring production progress. Human resource management focuses on recruitment, training, and employee benefits. Finally, office management organizes office activities and personnel.
opticle fiber
An optical fiber is a flexible transparent fiber made of glass or plastic, slightly thicker than a human hair, that carries light between its ends. Optical fibers transmit data over longer distances and at higher speeds than metal wires, with less signal loss and immunity to electromagnetic interference. Total internal reflection guides light through the fiber's core by trapping it inside when the light strikes the core-cladding boundary at an angle greater than the critical angle. Optical fibers come in single mode and multi-mode types and are used widely in fiber optic communication systems due to their high bandwidth and ability to transmit signals over long distances.
3 Total Internal Reflection
Total internal reflection of light occurs when light travels from a denser medium to a less dense medium and the angle of incidence is greater than the critical angle. The critical angle is the angle of incidence in the denser medium when the angle of refraction in the less dense medium is 90 degrees.
Fault Management System (OSS)
an overview of Fault Management System in the telco network environment.
One piece of OSS transformation puzzle.
introducing PING comand
Introducing the ping command and its parameters with example –in Persian
how to read syntax of cmd commands and use ping command in windows OS.
ping video on youtube:
https://youtu.be/DIE2Qa0pF5A
https://youtu.be/cuvTAHnuStU
Role of OpManager in event and fault management
Managing Event and Fault are not new to any IT managers. However if not implemented properly, this could be the most daunting of network monitoring and network management tasks.
Check out this presentation, to understand
# The basics of Event and Fault Management &
# How ManageEngine OpManager helps in effective Fault Management
Linear differential equation with constant coefficient
The document discusses linear differential equations with constant coefficients. It defines the order, auxiliary equation, complementary function, particular integral and general solution. It provides examples of determining the complementary function and particular integral for different types of linear differential equations. It also discusses Legendre's linear equations, Cauchy-Euler equations, and solving simultaneous linear differential equations.
LINEAR ACCELERATOR
The document discusses the components and operation of a linear accelerator used for radiation therapy. It describes the key parts of a linear accelerator including the electron gun, accelerator structure, treatment head and how they work together to generate photon or electron beams for radiation treatment. The linear accelerator uses microwave technology to accelerate electrons which are then converted into x-ray or electron beams that can be aimed at a tumor from multiple angles using the rotating gantry.
Viewers also liked (14)
Critical angle and total internal reflection by muhammad ahad butt
Critical angle and total internal reflection by muhammad ahad butt
Linear differential equation with constant coefficient
Linear differential equation with constant coefficient
Similar to Stars - Liling
Stars
Stars are balls of plasma held together by gravity. Nuclear fusion reactions in their cores release electromagnetic radiation, determining their temperature, color, and luminosity. Stars are classified by temperature from hottest O-type blue stars to coolest M-type red stars. Main sequence stars like our Sun derive energy from hydrogen fusion. As stars age, they evolve through red giant, red supergiant, and white dwarf phases before becoming virtually dead brown or neutron stars. The death of massive stars occurs in supernova explosions that can trigger new star formation.
Stars print
The document summarizes key information about stars and stellar evolution:
- Proxima Centauri is the nearest star to our sun at about 270 km away, while the next closest stars are much farther.
- A star's apparent brightness depends on both its luminosity and distance from Earth. Luminosity is measured by absolute brightness or total power radiated.
- The Hertzsprung-Russell diagram plots stars' temperatures and luminosities and helped show stages of stellar evolution.
- Stars evolve through stages as giants, dwarfs, white and brown dwarfs, neutron stars, pulsars, planetary and diffuse nebulae as their cores fuse hydrogen and heavier elements.
The Evolution of a Star
Nebulae consist of gas and dust clouds where stars are born. Stars spend most of their lives on the main sequence, fusing hydrogen into helium in their cores. Eventually they run out of fuel and die, either exploding as supernovae or shedding their outer layers as planetary nebulae. What remains depends on the star's mass - it can become a neutron star, black hole, or white dwarf.
Beyond Earth
What's beyond earth in space? This presentation gives you some knowledge about the celestial objects beyond earth
Stars, Galaxies, and the Universe Notes
The document discusses the composition, temperature, size, and motion of stars. It can be determined that a star's composition and temperature by analyzing its spectrum using a spectrograph. The spectrum will show dark lines that indicate the elements present in the star. A star's motion can be apparent, due to Earth's movement, or actual through its rotation, revolution, or Doppler shift as it moves towards or away from Earth. The document also summarizes the life cycles of stars from their formation in nebulae to their evolution into objects like white dwarfs, neutron stars, or black holes.
Life cycle of a star
This document discusses the life cycle of stars from their formation to their death. It begins by explaining that stars are giant balls of exploding gas made up mainly of hydrogen and helium. The document then outlines the various stages of a star's life: nebula, protostar, main sequence star, red giant, white dwarf, supernova, neutron star, and black hole. For each stage, it provides a brief description of the physical changes occurring within the star. The document emphasizes that stars much more massive than our sun will end their lives as neutron stars or black holes through the supernova process.
05 Stellar Evolution Mc Neely
This document summarizes stellar evolution and the life cycles of stars. It describes how stars are born from nebulae and discusses the stages stars pass through, including their time as main sequence stars fueled by hydrogen fusion. As stars age and exhaust their hydrogen, they evolve into red giants and later planetary nebulae, leaving behind white dwarf cores. More massive stars explode as supernovae, forming neutron stars or black holes. Key concepts covered include nucleosynthesis, variable stars, and the end states of small and massive stars.
11.1 stars
Stars are spherical objects made of hot gases that radiate electromagnetic radiation from their hot cores. There are over 9000 billion billion stars in the universe. All stars go through similar life cycles of birth, formation from nebulae, nuclear fusion in their cores, and death depending on their mass. Low mass stars exist as red dwarfs for over 100 billion years and become white dwarfs. Intermediate mass stars like our Sun last 10 billion years and become red giants then white dwarfs. High mass stars over 12 solar masses burn quickly in 7 billion years and explode as supernovae, collapsing into neutron stars or black holes.
The Stars of the Sky and their Life Cycles (2).pptx
The document discusses the life cycles of stars from their birth in molecular clouds to their evolution on the main sequence and eventual death. It begins by explaining how stars are born from collapsing gas and dust in molecular clouds. It then describes how protostars form and evolve into pre-main sequence stars. Next, it discusses how stars exist on the main sequence fusing hydrogen until more massive stars die in supernovae while less massive stars become white dwarfs. The document also provides details on properties of stars like luminosity, temperature, and how the Hertzsprung-Russell diagram is used to study stellar evolution.
Stellar evolution by joey
Low-mass stars spend millions of years as protostars collapsing under gravity before arriving on the main sequence. Massive stars collapse more rapidly, in as little as 10,000 years. Once on the main sequence, a star's lifetime depends on its mass - low-mass stars can spend billions of years fusing hydrogen, while high-mass stars may last only a few million years. Eventually a star exhausts its hydrogen fuel and expands as a red giant, then moves to the horizontal branch fusing helium before becoming an asymptotic giant branch star and ending its life as a planetary nebula or white dwarf.
Unit 8 astronomy 09 10
The document discusses the big bang theory and recent efforts to recreate what it may have sounded like. According to physicist John Cramer, the big bang would have produced a deep hum rather than a bang. He analyzed cosmic microwave background radiation data from the Wilkinson Microwave Anisotropy Probe satellite to calculate the frequencies of sound waves in the early universe. Cramer then scaled these frequencies up enormously to make them audible. His recording suggests the sound became more of a bass tone as the universe expanded after the big bang.
I need this essay checked for correctness a proofread and w.pdf
Ip noeinetedd t hoisu te isf spaoys scihbelec.k tehda nfokr ycoour.rectness. a proofread and whatever information isnt correct
SftshAplTbsgTtdeaAialaMiToSpotOsscIonttcitutooeonoygttssuuaroryrixn fhufu hh h ts u aaamupaer mss eaash a cpn it deatccacs c ee infc nbtrgttresastetsvtrtuhihmaaoe olt p e' e ns h ao-n s, e s s bu cl r si et f rp fH et et p erreorns ea e r ae eor r oi rw yaa uyp ed o 'xnr . lv a 'se,l t s ee r lc rmea lrsr o ,p,s sra rl i nl c y o f ote hap g icr e,s a al ar i e xy h z t ice u a e a a an rf upt c g v t eitr yotc,i n nt s heuses cz e ysuateo s gn l lchea coar s as osl e m b d d hhsars, t a a rueiunotedbles saas r ohttr eenop,o i o u e ta na ev sadncbor as e i e i , cenr ne .tagstaret p r e w s x icidrse r d on iioh cv u nt nlmd,aht t oncsIcr ne v t pov yt ht asetn,oaeu esn igh avcu,i io h n- e o d .n a f lr fptsg e r roi,dm n s nu g a r y rae tlosna n t d l g Tg v h iemohesh u oeh s c nett t ts - ttvm n t rtie t i uho e o e h iet rRm a a a n o i i a t nq uieeiteoteaioenao tui eae r oet l n e d p t o t gt n r g u w a d e u d nt b r np n u e t n hntohrl s e aa t e n us t o l he l m ss e m ia i h hsi ooe syb li ed g yg n t a n r t s tr yn ronetsnaovedl. e a i uws o aed e e aeei ia it t a ab uec oaa c t n o b s osie l T rg f thrr,Hgisnnfenetnt e cec lseu a tnl e t ol g fho o n l h h s evihaea,tieacrf o d ud c - n s l r l tn g soeru (fi e t fe e Rsre n e e i r ar d n o l nw ur g a H c a d f t po ie e l t e tb utr s o e snr d a a . s n ii l e mu o loa r la aihf a nn i n s - dlnefrtn a r s s fe p Thd t r R l r t rr c nit e a l is r gc l io e oit g e. ch g o o u tsh c n n a n s ia ah f he odssul ns) os o o nfh M e u men mee a u u p t t ng iaaamlg lfi ep os . o x d e ln intred m s n i c c s drk t r t a e e nt, s i e of y O u i mb t ha ae s n v at e s l l me md oaedt , rie se r tnhuogwr f s h t al emol a a o c u rg niawslestcaaeetcvieoocfaedt,cerh l t h tc r shf r rho icunoH e le y r rr a in r ve ed ve c d a e t e icalwce ao c k e ev e ft t t rl , r e u e f f, or a - e oyhimasf roetni l u u tra ot oe x e iR o i s o oem s i dai rlo t m .S n tr ar l n , o l s s s i f ha n en av tlr meu S s wre T as r ni i ubr t w i i a itnede ags e .s c .t r t oe ot sd alhexeuob p hg eia a e ne s nti sn tr Tr f a n w a n r adepaua t nlfose aeete r t n o .t s act e rhh t ic .o h f giy a lcd e iu-mn ov sgd h t f o c f .alocprdhtmeeofT f lta e r n y i al n y e i e ee si g klr ta y l oa to u fe so f s ov n h o d y eplh ro i tbo n o r x a t mlfsotnr os tin e e o hn d yehept er s aparair cps esca ns n f os m s m o egc ne r o. a r c ar la u u tifvaot s, a gc a utea vsl h t o f i b c u ten p s mt o l c eltda c wh n e gf lrtnhlerralaariteap.deeuohhleodercuntach. h u dae i hrsti sn r d r s f r eal ue s t g c ge esteu T aota osa e t ei t i di g d rtHc dlseo.in arolipn su a t i hstatoard e tb rve air uou d Weg h r i- n v u pdt i a ra o nc t v e a e s s sda Rw lssr ' h o e e . r l it c sv f i ee th su d. t a t p h l tt c re n o e n hhlf w lsTit ,a io g y de p u.
Unit8astronomy09 10-101024160150-phpapp02
The document summarizes key information about astronomy and the universe:
1) The universe started as a single extremely dense point that exploded in an enormous explosion known as the Big Bang around 12-15 billion years ago and has been expanding ever since.
2) Evidence for the expansion of the universe comes from the Doppler effect observed in the redshift of light from galaxies moving away from us as the universe expands.
3) Astronomers use large units like light years to measure the vast distances between celestial objects, where one light year is the distance light travels in one year.
Life cycle of a star
Stars are born from contracting nebulae of gas and dust. They spend most of their lives on the main sequence, fusing hydrogen into helium in their cores. Eventually they run out of fuel in their cores and their outer layers expand, forming red giants or supergiants. From there, smaller stars shed their outer layers to form planetary nebulae and white dwarfs, while larger stars explode as supernovae, leaving behind neutron stars or black holes.
unit8astronomy09-10-101024160150-phpapp02 (1).pdf
The document discusses the planet Mercury. It is the closest planet to the Sun and has little atmosphere. Its landscape is dominated by craters and cliffs, and it experiences extreme temperature variations between day and night. Mercury rotates around the Sun every 88 days and has no moons.
Life Cycle of Stars Stations
The document provides background information on stars' life cycles and how they are determined by mass. It states that stars with greater mass will have shorter life cycles as they must burn hot and fast to maintain equilibrium, using up fuel quickly and dying young in traumatic explosions. Average stars will live longer, peaceful deaths. It then lists directions for an activity involving classifying stars on the Hertzsprung-Russell diagram and answering conclusion questions.
Star Formations and Life Cycles
This document provides information about star formation and the life cycles of stars. It explains that stars form from collapsing clouds of gas and dust, and describes the protostar and T Tauri stages before stars reach the main sequence. It outlines the stages stars pass through as they age, such as becoming red giants or white dwarfs, and how some massive stars end as supernovae or neutron stars. Color and temperature correlations for different types of stars are also presented.
Stars
A barred spiral galaxy is a rotating disk of stars, gas and dust with a central bar of stars. Stars are classified based on their surface temperature, from hottest O-type blue stars to coolest M-type red stars. Stars evolve over their lifetimes, starting as protostars and becoming main sequence stars, then red giants, white dwarfs, neutron stars or black holes at the end of their lives.
Birth & death of stars (teach)
A short description, at the elementary school level, describing stars and telling how they are created and how they end.
Star (Earth Science)
Stars are the most widely recognized astronomical objects and represent the fundamental building blocks of galaxies. Stars are luminous spheres of plasma held together by gravity that produce energy through nuclear fusion of hydrogen into helium. The properties and life cycles of stars can be categorized by characteristics like temperature, size, color, luminosity, and lifetime. Common types include yellow and red dwarfs, blue giants, and red giants.
Similar to Stars - Liling (20)
The Stars of the Sky and their Life Cycles (2).pptx
The Stars of the Sky and their Life Cycles (2).pptx
I need this essay checked for correctness a proofread and w.pdf
I need this essay checked for correctness a proofread and w.pdf
More from ihsl
Science portfolio Presentation - Conductors
The document summarizes an experimental design lab report that tested how the conductivity of different materials affected the temperature of water. The experiment tested copper, aluminum, plastic and glass and measured the temperature change of water in each material over 20 minutes. The results showed that copper produced the highest temperature change and fastest heat transfer, while plastic produced almost no change, supporting the hypothesis. The conclusion was that materials with smaller specific heat capacity can transfer thermal energy faster.
Science Portfolio Presentation - Color and Temperature
This document summarizes an experimental design lab report that tested how different fabric colors are affected by temperature when exposed to heat. The experiment tested 5 different colored fabrics (dark blue, red, yellow, light blue, and green) and measured their temperature over time under a heat lamp. The results showed that dark blue absorbed the most heat, with an average temperature of 20°C, while light blue absorbed the least at 10°C. Overall, the conclusion was that darker colored fabrics absorbed more heat than lighter colored fabrics due to darker colors having a longer wavelength.
Science Portfolio Presentation - Insulation
The document describes an experimental design lab report that tested how insulators affect temperature. The experiment tested sand, cotton, and air as insulators by measuring the temperature change of each over time. The hypothesis was that sand would be the best insulator. The results showed that sand had the lowest average temperature change of 4.67°C, supporting the hypothesis that it was the best insulator compared to air and cotton.
Shaima Portfolio Presentation 2017
This experimental design lab report examines how covered and uncovered bottles affect temperature. The background discusses how greenhouse gases and the atmosphere affect energy transfer to Earth and temperature changes related to climate change. The hypothesis is that the temperature of air will be higher in covered bottles. Tables and graphs of the results from measuring bottle temperatures over time support the hypothesis, with covered bottles showing higher average temperatures and less variation than uncovered bottles. The conclusions determine the experiment was successful in validating the hypothesis.
Star Characteristics
Stars are hot balls of gas made primarily of hydrogen and helium. Astronomers classify stars based on characteristics like their age, color, brightness, temperature, and size to better understand the different types of stars. Key characteristics include a star's luminosity or brightness, temperature which determines its color, possible sizes ranging from dwarf to supergiant, and spectral class which is determined by temperature and color.
Energy on Earth
This document provides information on topics related to the atmosphere and climate change, including:
- The composition of the atmosphere and its layers.
- The electromagnetic spectrum and visible light spectrum.
- Energy, heat transfer, and the greenhouse effect.
- How changes in Earth's energy balance can influence climate through increases in greenhouse gases and global warming.
Scientific Method - Portfolio Presentation Example
The student conducted an experiment to determine if water has the same mass in liquid and solid form. They weighed ice cubes and then melted the ice and weighed the liquid water. In two of the three trials, the masses were equal, supporting the hypothesis. However, in one trial the liquid water had a slightly higher mass, possibly due to sources of error like not fully drying the beaker. The student concluded that while the masses are nearly equal, more trials could provide more definitive evidence.
Portfolio Lab Report Presentation Example - H2O Liquid & Solid
This lab report compares the mass of water in its solid (ice) and liquid states. The hypothesis is that the mass will be equal since it is the same substance, H2O, in different states. Data from trials show the mass was equal in the solid and liquid states for two trials but different in one trial, possibly due to error. The conclusion is that the mass of H2O is nearly the same in both solid and liquid forms.
Earthquake - Wei Xun
This document discusses how to prepare for an earthquake. It recommends taking several steps before an earthquake hits, such as securing heavy furniture to walls, preparing an emergency kit with supplies like water and food, and making an evacuation plan. The summary also notes that it's important to practice drop, cover, and hold on drills so everyone knows how to stay safe during shaking.
Earth plate wei xun
The document discusses plate tectonics and describes how the Earth's lithosphere is broken into tectonic plates that move over time. It explains that there are two main types of plates - oceanic plates composed mostly of basalt beneath the oceans, and continental plates composed mostly of granite located on land. There are about 16 major tectonic plates that are in constant slow motion, generating geological events like mountain building and volcanism at their boundaries. Alfred Wegener originally proposed the theory of continental drift that recognized plates moved over time.
Nouman Ijaz Divergent Boundary Powerpoint
The document discusses tectonic plates and divergent plate boundaries. It explains that tectonic plates are large, solid pieces of Earth's lithosphere or crust. When two plates move apart at a divergent boundary, new crust is formed by magma from the mantle welling up between the separating plates. There are two main types of divergent boundaries - oceanic-oceanic boundaries which form undersea mountain ridges, and continental-continental boundaries which form rift valleys as the continents move apart.
Photographic evidence Joanne
This document provides information about different types of plate boundaries including convergent, divergent, and transform boundaries. It describes how each boundary forms different geological features like mountains, trenches, and faults. It also discusses earthquakes, seismic waves, tsunamis, volcanoes, and the structure of the Earth's interior.
Continental drift- Yalizet
The document summarizes the theory of continental drift, which was proposed by Alfred Wegener in 1912. It explains that the continents move across the ocean bed due to shifting tectonic plates at a rate of 1 to 10 cm per year. This movement of plates causes volcanic and seismic activity at plate boundaries. The document also discusses Pangaea, a supercontinent that existed 300 million years ago before breaking apart over 100 million years.
Convection currents - Yalizet
Convection currents in the Earth's interior are thought to cause folding and mountain building by dragging tectonic plates. Convection currents are driven by heat from the Earth's core and radioactive decay in the mantle and crust. Mapping of rock formations and magnetic reversals at ocean ridges provides evidence that supports plate tectonics and convection currents driving the movement of plates.
Convection currents
Convection currents in the Earth's interior are thought to cause folding and mountain building by dragging tectonic plates. Convection currents are driven by heat from the Earth's core, radioactive decay in the mantle and crust, and cooling of the mantle. Mapping of rock formations and magnetic reversals at ocean ridges provided evidence that supports plate tectonics and convection currents driving the movement of plates.
Subduction zone
Subduction zones occur at convergent plate boundaries where one tectonic plate slides under another plate. There are two types of lithosphere - oceanic and continental - and subduction zones can involve either oceanic-oceanic convergence, oceanic-continental convergence, or continental-continental convergence. Subduction zones are where one plate is pushed down into the mantle as it slides under the edge of another plate.
Photographic evidence - Plate Tectonics
The Himalaya mountain is the highest in the world and contains Mount Everest, the tallest peak. Mount Everest was first climbed in 1953 and both it and the Himalayas were formed at a convergent plate boundary when Earth plates moved toward each other, causing the land to be pushed up and creating the massive mountain range.
Tsunami - Elshaima
A tsunami is a series of huge waves caused by earthquakes or volcanic eruptions under the sea. While tsunamis appear to be only 3 feet tall in water, they can travel very quickly at over 600 mph and destroy entire coastal cities when they make landfall. The size and speed of tsunamis makes them extremely dangerous when they hit land.
Subduction zone - Elshaima
Subduction zones occur at convergent plate boundaries where one tectonic plate slides under another plate. There are two types of lithosphere - oceanic and continental - and subduction can happen between oceanic-oceanic plates, oceanic-continental plates, or continental-continental plates. When two plates converge, one plate will subduct below the other at a boundary called a subduction zone.
Seismic waves - Elshaima
There are three main types of seismic waves: P waves, S waves, and L waves. P waves are the first to arrive and move side to side, while S waves follow and move up and down. L waves, also known as surface waves, are the largest and come last, moving in a circular motion. Seismic waves are caused by the breaking of rock in earth's plates and are recorded by seismographs.
More from ihsl (20)
Science Portfolio Presentation - Color and Temperature
Science Portfolio Presentation - Color and Temperature
Scientific Method - Portfolio Presentation Example
Scientific Method - Portfolio Presentation Example
Portfolio Lab Report Presentation Example - H2O Liquid & Solid
Portfolio Lab Report Presentation Example - H2O Liquid & Solid
Recently uploaded
BÀI TẬP BỔ TRỢ TIẾNG ANH LỚP 9 CẢ NĂM - GLOBAL SUCCESS - NĂM HỌC 2024-2025 - ...
BÀI TẬP BỔ TRỢ TIẾNG ANH LỚP 9 CẢ NĂM - GLOBAL SUCCESS - NĂM HỌC 2024-2025 - ...Nguyen Thanh Tu Collection
https://app.box.com/s/tacvl9ekroe9hqupdnjruiypvm9rdaneBenner "Expanding Pathways to Publishing Careers"
This presentation was provided by Rebecca Benner, Ph.D., of the American Society of Anesthesiologists, for the second session of NISO's 2024 Training Series "DEIA in the Scholarly Landscape." Session Two: 'Expanding Pathways to Publishing Careers,' was held June 13, 2024.
Andreas Schleicher presents PISA 2022 Volume III - Creative Thinking - 18 Jun...
Andreas Schleicher, Director of Education and Skills at the OECD presents at the launch of PISA 2022 Volume III - Creative Minds, Creative Schools on 18 June 2024.
Mule event processing models | MuleSoft Mysore Meetup #47
Mule event processing models | MuleSoft Mysore Meetup #47
Event Link:- https://meetups.mulesoft.com/events/details/mulesoft-mysore-presents-mule-event-processing-models/
Agenda
● What is event processing in MuleSoft?
● Types of event processing models in Mule 4
● Distinction between the reactive, parallel, blocking & non-blocking processing
For Upcoming Meetups Join Mysore Meetup Group - https://meetups.mulesoft.com/mysore/YouTube:- youtube.com/@mulesoftmysore
Mysore WhatsApp group:- https://chat.whatsapp.com/EhqtHtCC75vCAX7gaO842N
Speaker:-
Shivani Yasaswi - https://www.linkedin.com/in/shivaniyasaswi/
Organizers:-
Shubham Chaurasia - https://www.linkedin.com/in/shubhamchaurasia1/
Giridhar Meka - https://www.linkedin.com/in/giridharmeka
Priya Shaw - https://www.linkedin.com/in/priya-shaw
A Visual Guide to 1 Samuel | A Tale of Two Hearts
These slides walk through the story of 1 Samuel. Samuel is the last judge of Israel. The people reject God and want a king. Saul is anointed as the first king, but he is not a good king. David, the shepherd boy is anointed and Saul is envious of him. David shows honor while Saul continues to self destruct.
BIOLOGY NATIONAL EXAMINATION COUNCIL (NECO) 2024 PRACTICAL MANUAL.pptx
Practical manual for National Examination Council, Nigeria.
Contains guides on answering questions on the specimens provided
Wound healing PPT
This document provides an overview of wound healing, its functions, stages, mechanisms, factors affecting it, and complications.
A wound is a break in the integrity of the skin or tissues, which may be associated with disruption of the structure and function.
Healing is the body’s response to injury in an attempt to restore normal structure and functions.
Healing can occur in two ways: Regeneration and Repair
There are 4 phases of wound healing: hemostasis, inflammation, proliferation, and remodeling. This document also describes the mechanism of wound healing. Factors that affect healing include infection, uncontrolled diabetes, poor nutrition, age, anemia, the presence of foreign bodies, etc.
Complications of wound healing like infection, hyperpigmentation of scar, contractures, and keloid formation.
Gender and Mental Health - Counselling and Family Therapy Applications and In...
A proprietary approach developed by bringing together the best of learning theories from Psychology, design principles from the world of visualization, and pedagogical methods from over a decade of training experience, that enables you to: Learn better, faster!
BÀI TẬP DẠY THÊM TIẾNG ANH LỚP 7 CẢ NĂM FRIENDS PLUS SÁCH CHÂN TRỜI SÁNG TẠO ...
BÀI TẬP DẠY THÊM TIẾNG ANH LỚP 7 CẢ NĂM FRIENDS PLUS SÁCH CHÂN TRỜI SÁNG TẠO ...Nguyen Thanh Tu Collection
https://app.box.com/s/qhtvq32h4ybf9t49ku85x0n3xl4jhr15Beyond Degrees - Empowering the Workforce in the Context of Skills-First.pptx
Iván Bornacelly, Policy Analyst at the OECD Centre for Skills, OECD, presents at the webinar 'Tackling job market gaps with a skills-first approach' on 12 June 2024
Temple of Asclepius in Thrace. Excavation results
The temple and the sanctuary around were dedicated to Asklepios Zmidrenus. This name has been known since 1875 when an inscription dedicated to him was discovered in Rome. The inscription is dated in 227 AD and was left by soldiers originating from the city of Philippopolis (modern Plovdiv).
Recently uploaded (20)
BÀI TẬP BỔ TRỢ TIẾNG ANH LỚP 9 CẢ NĂM - GLOBAL SUCCESS - NĂM HỌC 2024-2025 - ...
BÀI TẬP BỔ TRỢ TIẾNG ANH LỚP 9 CẢ NĂM - GLOBAL SUCCESS - NĂM HỌC 2024-2025 - ...
Andreas Schleicher presents PISA 2022 Volume III - Creative Thinking - 18 Jun...
Andreas Schleicher presents PISA 2022 Volume III - Creative Thinking - 18 Jun...
Mule event processing models | MuleSoft Mysore Meetup #47
Mule event processing models | MuleSoft Mysore Meetup #47
BIOLOGY NATIONAL EXAMINATION COUNCIL (NECO) 2024 PRACTICAL MANUAL.pptx
BIOLOGY NATIONAL EXAMINATION COUNCIL (NECO) 2024 PRACTICAL MANUAL.pptx
Gender and Mental Health - Counselling and Family Therapy Applications and In...
Gender and Mental Health - Counselling and Family Therapy Applications and In...
BÀI TẬP DẠY THÊM TIẾNG ANH LỚP 7 CẢ NĂM FRIENDS PLUS SÁCH CHÂN TRỜI SÁNG TẠO ...
BÀI TẬP DẠY THÊM TIẾNG ANH LỚP 7 CẢ NĂM FRIENDS PLUS SÁCH CHÂN TRỜI SÁNG TẠO ...
NEWSPAPERS - QUESTION 1 - REVISION POWERPOINT.pptx
NEWSPAPERS - QUESTION 1 - REVISION POWERPOINT.pptx
Beyond Degrees - Empowering the Workforce in the Context of Skills-First.pptx
Beyond Degrees - Empowering the Workforce in the Context of Skills-First.pptx
Stars - Liling
- 1. Stars Extension Project- Extra Credit By: Liling Class: L
- 2. Star and Categories What is a star? A star is a collection of duct and gas in ball form that is gathered together by gravity. What are the characteristics? The characteristics are stars are temperatures, luminosity, types of stars and spectral class and sizes which we can use to classified the stars.
- 3. Characteristics Temperature: how hot is it. Luminosity: how bright is it. Types of stars: Main Sequence, Giant, Supergiant, Dwarf Spectral class: O,B,A,F,G,K,M (from hottest to coldest) Sizes: how large is it.
- 4. Types of stars Main Sequence: A major grouping of stars that transfer hydrogen into energy, it has longest period in a stars lifetime. Dwarf: A star has low mass, small size and average or below luminosity. Giant: bigger than main sequence and hotter than main sequence but with the same surface temperature. Supergiant: most massive (big) and brightest stars
- 5. H-R Diagram & Nuclear Fusion H-R Diagram is a graph that classified the stars according to sizes, types of stars, temperature, color and luminosity. Nuclear Fusion is a process that transfer 2 hydrogen molecules into 1 helium molecule, it creates energy.
- 6. Life of a star
- 7. Stellar Nebula- a collection of dust and gas that it gathered together by gravity. Then collection of gas and dust get closer and closer formed either massive star or average star. AS it gets closer the surface gets colder that formed either red giant or red supergiant. Red giant explodes and becomes Planetary Nebula/ Red Supergiant explodes and becomes supernova. Planetary Nebula becomes White Dwarf when it gets smaller and lose it light. It becomes Black Dwarf that it’s dead. Supernova becomes either Neutron star (the star that spin) or black hole (it stuck everything in and everything inside is disappeared).