Life of Stars
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This talks about stars- from how they are formed to the death of a star, from the nebula to the black hole.
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Conley cis100 ppt_assignment
This document provides an overview of star formation, evolution, and death. It discusses how stars form from clouds of hydrogen and helium in nebulas. Once stars accumulate enough mass, nuclear fusion begins in their cores. The document outlines the life cycles of stars of different masses, from red giants to supernovae and the formation of neutron stars or black holes. Key stages in a massive star's death are described, such as the core collapse that causes type II supernovae and the ejection of heavier elements into space.
Life cycle of stars
The document summarizes the typical lifecycle of a star in 8 stages:
1. Nebula - a cloud of dust and gas that contracts under gravity to form a protostar.
2. Protostar - the interior heats up to over 10,000K and nuclear fusion begins.
3. Main sequence - nuclear fusion of hydrogen occurs steadily for billions of years.
4. Red giant - the star expands greatly after exhausting hydrogen and fuses helium.
5. Planetary nebula - low mass stars eject their outer layers, forming a glowing shell.
6. Supernova - massive stars explode in a gigantic blast, distributing elements into space.
7. White dwarf - the remaining
Stellar Evolution by Raveendra Bagade
Stellar evolution refers to the process by which stars change over their lifetime. As stars age, they undergo nuclear fusion in their cores which fuses lighter elements into heavier ones. Eventually the fuel is depleted, forcing the star to evolve into different phases. Stars begin as hot balls of hydrogen gas and spend most of their lives on the main sequence fusing hydrogen into helium. Later, they expand into red giants or supergiants as heavier elements are fused, and ultimately end their lives as white dwarfs, neutron stars, or black holes depending on their mass.
Stellar evolution
1. Stellar evolution begins with the fragmentation of massive molecular clouds into smaller masses, each initiating their own star formation process.
2. As clouds collapse under gravity, the gravitational energy is transformed to radiation through molecular hydrogen and dust grains, causing an isothermal collapse. Further collapse becomes adiabatic as stars become opaque.
3. Stars sustain themselves through nuclear fusion, with more massive stars having shorter lifespans than less massive stars due to the greater energy requirements.
4. Stellar remnants include white dwarfs, neutron stars, pulsars, and black holes, depending on the star's original mass.
Adolfo
1) The document discusses the lifecycle of stars, from their birth in nebulae made of hydrogen and helium gas, to their evolution through different stages as they fuse hydrogen and helium into heavier elements.
2) It describes how massive stars may end as red supergiants or supernovae, and how the material from dying stars can form nebulae and be incorporated into new stars and planets.
3) It also discusses the formation of planets from protoplanetary disks around new stars, and the different classes of objects in our solar system like planets, asteroids, comets, and meteorites.
Supernovae & the First Stars in the Universe
A presentation on the first cosmic explosions and how the Universe started to make heavy elements, by Monash University's Professor Alexander Heger from the Faculty of Science, School of Mathematical Science.
Ch 17 -our dynamic sun
The Sun is a dynamic object with complex internal structure and outer atmosphere. It has a core reaching temperatures over 27 million degrees Fahrenheit where nuclear fusion occurs. Energy radiates outward through the radiative zone and flows in convection currents in the convection zone before emerging in the photosphere. Above the photosphere lies the chromosphere and transition region where temperatures rise into the million degrees before reaching the super-hot corona extending far into space. The solar wind and coronal mass ejections influence space weather throughout the solar system.
Naturalists at Large - Nebula
A nebula is an interstellar cloud of dust, gas, and plasma that is the first stage of star formation. Nebulae form from the gravitational collapse of gas clouds in space. As gas and dust clump together in nebulae, it can form stars and planetary systems. Some nebulae are formed from stellar explosions like supernovae, which throw off ionized material that glows.
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Conley cis100 ppt_assignment
This document provides an overview of star formation, evolution, and death. It discusses how stars form from clouds of hydrogen and helium in nebulas. Once stars accumulate enough mass, nuclear fusion begins in their cores. The document outlines the life cycles of stars of different masses, from red giants to supernovae and the formation of neutron stars or black holes. Key stages in a massive star's death are described, such as the core collapse that causes type II supernovae and the ejection of heavier elements into space.
Life cycle of stars
The document summarizes the typical lifecycle of a star in 8 stages:
1. Nebula - a cloud of dust and gas that contracts under gravity to form a protostar.
2. Protostar - the interior heats up to over 10,000K and nuclear fusion begins.
3. Main sequence - nuclear fusion of hydrogen occurs steadily for billions of years.
4. Red giant - the star expands greatly after exhausting hydrogen and fuses helium.
5. Planetary nebula - low mass stars eject their outer layers, forming a glowing shell.
6. Supernova - massive stars explode in a gigantic blast, distributing elements into space.
7. White dwarf - the remaining
Stellar Evolution by Raveendra Bagade
Stellar evolution refers to the process by which stars change over their lifetime. As stars age, they undergo nuclear fusion in their cores which fuses lighter elements into heavier ones. Eventually the fuel is depleted, forcing the star to evolve into different phases. Stars begin as hot balls of hydrogen gas and spend most of their lives on the main sequence fusing hydrogen into helium. Later, they expand into red giants or supergiants as heavier elements are fused, and ultimately end their lives as white dwarfs, neutron stars, or black holes depending on their mass.
Stellar evolution
1. Stellar evolution begins with the fragmentation of massive molecular clouds into smaller masses, each initiating their own star formation process.
2. As clouds collapse under gravity, the gravitational energy is transformed to radiation through molecular hydrogen and dust grains, causing an isothermal collapse. Further collapse becomes adiabatic as stars become opaque.
3. Stars sustain themselves through nuclear fusion, with more massive stars having shorter lifespans than less massive stars due to the greater energy requirements.
4. Stellar remnants include white dwarfs, neutron stars, pulsars, and black holes, depending on the star's original mass.
Adolfo
1) The document discusses the lifecycle of stars, from their birth in nebulae made of hydrogen and helium gas, to their evolution through different stages as they fuse hydrogen and helium into heavier elements.
2) It describes how massive stars may end as red supergiants or supernovae, and how the material from dying stars can form nebulae and be incorporated into new stars and planets.
3) It also discusses the formation of planets from protoplanetary disks around new stars, and the different classes of objects in our solar system like planets, asteroids, comets, and meteorites.
Supernovae & the First Stars in the Universe
A presentation on the first cosmic explosions and how the Universe started to make heavy elements, by Monash University's Professor Alexander Heger from the Faculty of Science, School of Mathematical Science.
Ch 17 -our dynamic sun
The Sun is a dynamic object with complex internal structure and outer atmosphere. It has a core reaching temperatures over 27 million degrees Fahrenheit where nuclear fusion occurs. Energy radiates outward through the radiative zone and flows in convection currents in the convection zone before emerging in the photosphere. Above the photosphere lies the chromosphere and transition region where temperatures rise into the million degrees before reaching the super-hot corona extending far into space. The solar wind and coronal mass ejections influence space weather throughout the solar system.
Naturalists at Large - Nebula
A nebula is an interstellar cloud of dust, gas, and plasma that is the first stage of star formation. Nebulae form from the gravitational collapse of gas clouds in space. As gas and dust clump together in nebulae, it can form stars and planetary systems. Some nebulae are formed from stellar explosions like supernovae, which throw off ionized material that glows.
The sun
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.
Ch 19 -life and death of stars
1. Stars are born through nuclear fusion and spend most of their life fusing hydrogen into helium as a main sequence star.
2. When stars exhaust their hydrogen fuel, low mass stars become red giants and high mass stars explode as supernovae.
3. The remnants of dead stars are white dwarfs, neutron stars, or black holes depending on the original star's mass.
The sun
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 Our Star Lecture Presentation
The document discusses the physical structure and properties of the Sun. It describes how the Sun generates energy through nuclear fusion reactions in its core, where hydrogen is fused into helium. This releases energy according to Einstein's equation. It also summarizes the Sun's interior structure, atmosphere, activity cycles, and how observations of neutrinos and vibrations have informed our understanding.
Unit vi chapter 24 (stars, space and galaxies)
1) Stars originate from nebulae of dust and gas. They spend most of their life fusing hydrogen into helium through nuclear fusion in their cores as main sequence stars.
2) When stars have exhausted their hydrogen, their cores collapse and outer layers expand, forming red giants. More massive stars explode as supernovae, leaving behind neutron stars or black holes.
3) The sun is classified as a yellow dwarf star. Its atmosphere consists of the photosphere, chromosphere, and corona. Nuclear fusion in its core provides its energy.
The sun (more advanced)
Maybe too in-depth for most elementary students, but very good broad coverage for teacher background or more advanced students in elementary or middle school.
A1 18 Stellar Evolution
Typical stellar evolution proceeds through several stages:
1. Red Giant Branch: Stars expand and cool as hydrogen fuses to helium in a shell around the core.
2. Horizontal Giant Branch: A helium flash occurs, followed by helium fusing to carbon in the core while hydrogen fuses in a shell.
3. Asymptotic Giant Branch: Helium and hydrogen shells alternately fuse heavier elements, causing the star to further expand and cool before ejecting its outer layers as a planetary nebula.
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.
Star formation
1. Stars form from dense clouds of gas and dust in interstellar space.
2. Gravity causes the cloud to contract over many stages until fusion begins in the core and a new star is born on the main sequence.
3. The size and mass of a star determines its position on the HR diagram, with more massive stars being larger and hotter.
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.
The Sun: Not Just Our Star
The sun is a huge glowing ball of gas at the center of our solar system that provides light, heat, and energy to Earth. It is made up primarily of hydrogen and helium and has a radius about 109 times that of Earth. The sun was formed around 4.6 billion years ago and will remain stable for another 5 billion years before expanding into a red giant. It emits electromagnetic radiation across the spectrum, including visible light and infrared that we experience as heat and light. Nuclear fusion in the sun's core converts hydrogen to helium and releases enormous amounts of energy.
Parts of the sun (demo)
Here are the answers to your questions:
1. The different parts of the Sun from inner to outer are:
- Core
- Radiative Zone
- Convective Zone
- Photosphere
- Chromosphere
- Corona
2. The Sun is important because it is the center of our solar system and the sole source of light and heat for Earth. It allows life to exist on Earth.
3. Sunspots are darker regions on the Sun's surface that are cooler than surrounding areas. They can cause disruptions to radio communications and power grids on Earth. Large solar flares from sunspots can also create displays of the Northern and Southern Lights.
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.
activities of the sun
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 Our Star
The Sun is by far the largest object in the solar system, containing over 99% of the mass. It has a diameter over 100 times larger than Earth and generates energy through nuclear fusion of hydrogen into helium. Light from the Sun takes approximately 8 minutes to reach Earth. While the visible surface of the Sun appears solid, it actually consists of several layers including the core, radiative zone, convective zone, photosphere, chromosphere, and corona. Solar activity like sunspots, solar flares, and coronal mass ejections can impact power grids and communication systems on Earth. Astronomers study the Sun to better understand stars and how changes in solar output impact Earth's climate and atmosphere.
The Sun powerpoint
This PowerPoint discusses the Sun at a high school level. It talks about characteristics, solar activities/events, how energy is created, and many more.
Properties of the sun
The document provides an introduction to stars, focusing on the sun. It discusses the layers of the sun's atmosphere and interior. The sun's core generates its enormous energy output through nuclear fusion. The solar wind consists of high-energy particles escaping the sun's gravity. The sun emits across the electromagnetic spectrum, including x-rays studied by orbital telescopes. The sun's total luminosity is calculated based on the energy received by a detector at Earth's distance. Sunspots occur in pairs of opposite magnetic fields and vary in a roughly 11-year solar cycle.
Life of stars
Giant molecular clouds collapse under gravity to form protostars that grow into main sequence stars through nuclear fusion. As stars age, they expand into red giants and shed their outer layers, leaving behind white dwarfs that slowly cool over billions of years. More massive stars have shorter lifespans and die in spectacular supernovae, potentially leaving behind neutron stars or black holes.
Space weather
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.
Unit 3: Why Does the Sun Shine?
The sun generates about 400 billion billion
megawatts of power and it has done so for five
billion years. Nuclear fusion – combining lighter
atoms to make heavier ones – is what makes it
possible.
Register to explore the whole course here: https://school.bighistoryproject.com/bhplive?WT.mc_id=Slideshare12202017
57484884858u4995946Stellar-Evolution.docx
Stellar evolution is the process by which stars change over their lifetimes, ranging from millions of years for massive stars to trillions for the least massive. Stars are born from nebulae of hydrogen and dust and evolve through stages like red giants and supernovae. Supernovae occur when massive stars explode, leaving behind neutron stars or black holes. Neutron stars are incredibly dense, while black holes have such strong gravity that nothing can escape.
Life cycle of stars
The document summarizes the typical lifecycle of a star in 8 stages:
1. Nebula - a cloud of dust and gas that contracts under gravity to form a protostar.
2. Protostar - the interior heats up to over 10,000K and nuclear fusion begins.
3. Main sequence - nuclear fusion of hydrogen occurs steadily for billions of years.
4. Red giant - the star expands greatly after exhausting hydrogen and fuses helium.
5. Planetary nebula - low mass stars eject their outer layers, forming a glowing shell.
6. Supernova - massive stars explode in a gigantic blast, distributing elements into space.
7. White dwarf - the remaining
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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.
Ch 19 -life and death of stars
1. Stars are born through nuclear fusion and spend most of their life fusing hydrogen into helium as a main sequence star.
2. When stars exhaust their hydrogen fuel, low mass stars become red giants and high mass stars explode as supernovae.
3. The remnants of dead stars are white dwarfs, neutron stars, or black holes depending on the original star's mass.
The sun
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 Our Star Lecture Presentation
The document discusses the physical structure and properties of the Sun. It describes how the Sun generates energy through nuclear fusion reactions in its core, where hydrogen is fused into helium. This releases energy according to Einstein's equation. It also summarizes the Sun's interior structure, atmosphere, activity cycles, and how observations of neutrinos and vibrations have informed our understanding.
Unit vi chapter 24 (stars, space and galaxies)
1) Stars originate from nebulae of dust and gas. They spend most of their life fusing hydrogen into helium through nuclear fusion in their cores as main sequence stars.
2) When stars have exhausted their hydrogen, their cores collapse and outer layers expand, forming red giants. More massive stars explode as supernovae, leaving behind neutron stars or black holes.
3) The sun is classified as a yellow dwarf star. Its atmosphere consists of the photosphere, chromosphere, and corona. Nuclear fusion in its core provides its energy.
The sun (more advanced)
Maybe too in-depth for most elementary students, but very good broad coverage for teacher background or more advanced students in elementary or middle school.
A1 18 Stellar Evolution
Typical stellar evolution proceeds through several stages:
1. Red Giant Branch: Stars expand and cool as hydrogen fuses to helium in a shell around the core.
2. Horizontal Giant Branch: A helium flash occurs, followed by helium fusing to carbon in the core while hydrogen fuses in a shell.
3. Asymptotic Giant Branch: Helium and hydrogen shells alternately fuse heavier elements, causing the star to further expand and cool before ejecting its outer layers as a planetary nebula.
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.
Star formation
1. Stars form from dense clouds of gas and dust in interstellar space.
2. Gravity causes the cloud to contract over many stages until fusion begins in the core and a new star is born on the main sequence.
3. The size and mass of a star determines its position on the HR diagram, with more massive stars being larger and hotter.
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.
The Sun: Not Just Our Star
The sun is a huge glowing ball of gas at the center of our solar system that provides light, heat, and energy to Earth. It is made up primarily of hydrogen and helium and has a radius about 109 times that of Earth. The sun was formed around 4.6 billion years ago and will remain stable for another 5 billion years before expanding into a red giant. It emits electromagnetic radiation across the spectrum, including visible light and infrared that we experience as heat and light. Nuclear fusion in the sun's core converts hydrogen to helium and releases enormous amounts of energy.
Parts of the sun (demo)
Here are the answers to your questions:
1. The different parts of the Sun from inner to outer are:
- Core
- Radiative Zone
- Convective Zone
- Photosphere
- Chromosphere
- Corona
2. The Sun is important because it is the center of our solar system and the sole source of light and heat for Earth. It allows life to exist on Earth.
3. Sunspots are darker regions on the Sun's surface that are cooler than surrounding areas. They can cause disruptions to radio communications and power grids on Earth. Large solar flares from sunspots can also create displays of the Northern and Southern Lights.
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.
activities of the sun
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 Our Star
The Sun is by far the largest object in the solar system, containing over 99% of the mass. It has a diameter over 100 times larger than Earth and generates energy through nuclear fusion of hydrogen into helium. Light from the Sun takes approximately 8 minutes to reach Earth. While the visible surface of the Sun appears solid, it actually consists of several layers including the core, radiative zone, convective zone, photosphere, chromosphere, and corona. Solar activity like sunspots, solar flares, and coronal mass ejections can impact power grids and communication systems on Earth. Astronomers study the Sun to better understand stars and how changes in solar output impact Earth's climate and atmosphere.
The Sun powerpoint
This PowerPoint discusses the Sun at a high school level. It talks about characteristics, solar activities/events, how energy is created, and many more.
Properties of the sun
The document provides an introduction to stars, focusing on the sun. It discusses the layers of the sun's atmosphere and interior. The sun's core generates its enormous energy output through nuclear fusion. The solar wind consists of high-energy particles escaping the sun's gravity. The sun emits across the electromagnetic spectrum, including x-rays studied by orbital telescopes. The sun's total luminosity is calculated based on the energy received by a detector at Earth's distance. Sunspots occur in pairs of opposite magnetic fields and vary in a roughly 11-year solar cycle.
Life of stars
Giant molecular clouds collapse under gravity to form protostars that grow into main sequence stars through nuclear fusion. As stars age, they expand into red giants and shed their outer layers, leaving behind white dwarfs that slowly cool over billions of years. More massive stars have shorter lifespans and die in spectacular supernovae, potentially leaving behind neutron stars or black holes.
Space weather
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.
Unit 3: Why Does the Sun Shine?
The sun generates about 400 billion billion
megawatts of power and it has done so for five
billion years. Nuclear fusion – combining lighter
atoms to make heavier ones – is what makes it
possible.
Register to explore the whole course here: https://school.bighistoryproject.com/bhplive?WT.mc_id=Slideshare12202017
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Stellar evolution is the process by which stars change over their lifetimes, ranging from millions of years for massive stars to trillions for the least massive. Stars are born from nebulae of hydrogen and dust and evolve through stages like red giants and supernovae. Supernovae occur when massive stars explode, leaving behind neutron stars or black holes. Neutron stars are incredibly dense, while black holes have such strong gravity that nothing can escape.
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The document summarizes the typical lifecycle of a star in 8 stages:
1. Nebula - a cloud of dust and gas that contracts under gravity to form a protostar.
2. Protostar - the interior heats up to over 10,000K and nuclear fusion begins.
3. Main sequence - nuclear fusion of hydrogen occurs steadily for billions of years.
4. Red giant - the star expands greatly after exhausting hydrogen and fuses helium.
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6. Supernova - massive stars explode in a gigantic blast, distributing elements into space.
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Stars are formed from dense clouds of gas and dust called nebulae. Once formed, stars exist in different life stages depending on their mass. The main sequence stage where nuclear fusion occurs in the core can last billions of years for smaller stars. Eventually stars run out of hydrogen fuel and expand as red giants before shedding their outer layers. The smallest stars collapse into white dwarfs, medium stars may become neutron stars via supernovae, and the largest stars form black holes.
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Stars are formed from the collapse of giant clouds of dust and gas in space. As the cloud collapses due to gravity, it heats up and eventually nuclear fusion begins in its core, forming a new star. Stars exist in different colors and sizes depending on their mass, with more massive stars being hotter, brighter, and having shorter lifespans than less massive stars. Eventually a star runs out of hydrogen fuel for fusion in its core, causing it to expand into a red giant and later die, leaving behind a white dwarf, neutron star, or black hole depending on its original mass.
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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.
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Stars are spheres of gas held together by gravity. A star's life cycle depends on its mass, beginning as a nebula and ending as a white dwarf, neutron star, or black hole. Small red dwarf stars can last trillions of years while massive blue giants only last 10,000-100,000 years before exploding. Our Sun is a medium yellow star that will become a red giant and eventually a white dwarf. Constellations are patterns of stars used to identify positions in the sky.
Stellar evolution ppt
This document provides a summary of stellar evolution from the birth of stars to their death. It discusses how stars are formed inside nebulae from collapsing gas clouds. As stars age, they progress through different stages such as protostars, T-Tauri stars, and red giants. More massive stars may die in supernova explosions, leaving behind neutron stars or black holes. Lower mass stars end as white dwarfs. The document also describes different types of nebulae and compact objects like neutron stars and black holes.
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.
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.
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Life of Stars
- 1. Astronomy (Life of Stars) by Merlin Raphael Page 1
- 2. The Universe Scientists believe the universe began in a “big bang”, about 13,700 million years ago. The universe continues to expand today. The evidence for the “big bang” theory includes the existence of a microwave background radiation and red shift. The universe contains extremely dense objects and may consist mostly of dark matter that cannot be seen. Stars do not remain the same- they change as they age. Page 2
- 3. The Origin of Stars Nebula: A large cloud of gas (helium and hydrogen) and dust which forms into a star. Dust and gas particles exert a gravitational force on each other which keeps pulling them closer together. As the particles pull closer together the temperature increases. At 10,000,000o C fusion takes place and energy radiates outward through the condensing ball of gas. Page 3
- 4. -Cloud Collapse - occurs deep in cloud -“EGGS” (Evaporating Gaseous Globules) : Dense regions forming new stars - surrounding gas & dust “eaten into” by strong stellar winds, UV photons & ionization fronts. Page 4
- 5. The Star A star is a luminous globe of gas producing its own heat and light by nuclear reactions. They are born from nebulae and consist mostly of hydrogen and helium gas. Surface temperatures range from 2000°C to above 30,000°C, and the corresponding colours from red to blue- white. Page 5
- 6. Red Giants After hydrogen is exhausted in core, energy released from nuclear fusion counter- acts inward force of gravity. -Core collapses, •Kinetic energy of collapse is converted into heat. •This heat expands the outer layers. -There is an increase in temperature and pressure during the collapse. Page 6
- 7. Planetary Nebula Planetary nebulae are the outer layers of the star that are lost when it changes from a red giant to a white dwarf. After helium is exhausted, the core collapses and the outer layer of the star is expelled. The outer atmosphere is ionized by the hot remaining core. Page 7
- 8. White Dwarf White dwarfs are the shrunken remains of normal stars whose nuclear supplies have been used up. They consist of degenerate matter with a very high density due to gravitational effects. A white dwarf cools and fades over several billion years. Page 8
- 9. Supernova This is the explosive death of a star. It often results in the star obtaining the brightness of 100 million suns for a short time. Type1- These occur in binary star systems in which gas from one star falls onto a white dwarf, causing it to explode. Type2- These occur in massive stars, which suffer runaway internal nuclear reactions at the end of their lives. Page 9
- 10. Neutron Stars These stars are composed mainly of neutrons and are produced when a supernova explodes, forcing the protons and electrons to combine to produce a neutron star. It is very dense. Typical stars have a mass of 3 times the sun, but a diameter of only 20km. If its mass is any greater, it will shrink further to become a black hole. Page 10
- 11. Black Holes These are believed to form from massive stars at the end of their lifetime. The gravitational pull in a black hole is so great, nothing can escape from it- not even light. The density of matter in a black hole cannot be measured. Black holes distort the space around them, and can often suck neighboring matter into them, including stars. Page 11
- 12. Page 12