Star's Life Cycle
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Stars go through life cycles like humans, being born from collapsing gas clouds, burning hydrogen through nuclear fusion on the main sequence, and eventually dying. Medium and low mass stars end as white dwarfs after shedding their outer layers, while high mass stars explode as supernovae, leaving behind neutron stars or black holes. Neutron stars are incredibly dense, rotating rapidly, while black holes have event horizons beyond which nothing, not even light, can escape.
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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.
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.
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.
Stars
Stars are giant balls of gas that produce light and heat through nuclear fusion at their cores. They vary greatly in size, from dwarf stars like our Sun to massive supergiant stars over 200 times the Sun's diameter. Stars end their lives in different ways depending on their mass - smaller stars become white dwarfs, while larger stars explode as supernovae or collapse into neutron stars and other compact objects.
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.
Life Cycle Of Stars
All stars begin as nebulae of dust and gas that collapse under gravity into protostars. They fuse hydrogen into helium during the main sequence stage, which is the longest phase in a star's life. A star's ultimate fate depends on its mass. Small mass stars become white dwarfs after the main sequence, while medium mass stars become red giants then white dwarfs. Large mass stars over 15 solar masses may 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.
Types of galaxies
Types of galaxies
You can edit this powerpoint for your own presentation but don't re-upload.
I used hyperlink(especially on images) and alot of animation.
Recommended
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.
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.
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.
Stars
Stars are giant balls of gas that produce light and heat through nuclear fusion at their cores. They vary greatly in size, from dwarf stars like our Sun to massive supergiant stars over 200 times the Sun's diameter. Stars end their lives in different ways depending on their mass - smaller stars become white dwarfs, while larger stars explode as supernovae or collapse into neutron stars and other compact objects.
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.
Life Cycle Of Stars
All stars begin as nebulae of dust and gas that collapse under gravity into protostars. They fuse hydrogen into helium during the main sequence stage, which is the longest phase in a star's life. A star's ultimate fate depends on its mass. Small mass stars become white dwarfs after the main sequence, while medium mass stars become red giants then white dwarfs. Large mass stars over 15 solar masses may 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.
Types of galaxies
Types of galaxies
You can edit this powerpoint for your own presentation but don't re-upload.
I used hyperlink(especially on images) and alot of animation.
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.
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.
Size and Scale of the Universe
The document discusses the immense size and scale of the universe. It provides sizes and comparisons for objects from Earth to the observable universe. Earth is compared to a salt grain, while the Sun is like a gumball. The solar system spans a football stadium and galaxies are like orbits of outer planets. The observable universe extends as far as the Oort cloud at the edge of our solar system. Precise measurement techniques are needed to determine astronomical distances.
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.
Birth of a star
Stars are born in vast nebulae clouds of dust and gas scattered throughout space. Gravity gathers hydrogen in these clouds, causing them to grow denser and hotter over time. Eventually, the hydrogen heats up to 18 million degrees Fahrenheit, igniting nuclear fusion reactions that turn the hydrogen into helium - this is the moment a star is born. The color of stars depends on their temperature, ranging from hot blue-white to cooler and dimmer red. The largest known star is VY Canis Majoris, which could fit the sun inside it over 2,000 times.
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.
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.
Life cycle of stars
There are different life cycle stages for stars depending on their original mass. Low mass stars progress through the stages of nebula, main sequence, red giant, planetary nebula, white dwarf, and black dwarf. High mass stars go through nebula, main sequence, red supergiant, supernova, and either become a neutron star or black hole. The main sequence stage can last billions of years for low mass stars but only millions for high mass stars.
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.
Types of stars
This document describes different stages and types of stars:
- Main sequence stars like our Sun spend most of their lives fusing hydrogen into helium in their cores.
- Red giants are large, reddish stars that have exhausted hydrogen fusion and begun fusing helium.
- Planetary nebulae form when average-sized stars eject their outer layers after becoming red giants, leaving behind dense, hot cores called white dwarfs.
- Brown dwarfs are failed stars too small to sustain nuclear fusion.
- Variable stars change in brightness over timescales from seconds to years as they evolve.
- Binary stars are two gravitationally bound stars that orbit a common center of mass.
The Life Cycle of a Star
Stars are formed from clouds of gas and dust called nebulae. As stars age and evolve, they progress through different stages - from stars to red giants or dwarfs to supernovae. The most massive stars may collapse into neutron stars or black holes. Black holes are objects so dense that not even light can escape their powerful gravitational pull. Material near a black hole forms a swirling accretion disk and is ejected at nearly light speed in powerful jets. Advancing technology is improving our understanding of stellar evolution and black hole formation.
Stars
It is a slide showing the general information as well as some interesting information about stars that a student needs for his school.
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.
Galaxies
Galaxies come in different shapes and sizes. The largest are spiral galaxies which have a flattened disk with spiral arms and a bulge in the center. Elliptical galaxies have no definite shape and little gas or dust. Irregular galaxies have an irregular shape and active star formation. Well-known galaxies include the Andromeda Galaxy, Whirlpool Galaxy, Sombrero Galaxy, and Sunflower Galaxy.
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.
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.
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.
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.
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.
The Outer Planets
The outer planets are Jupiter, Saturn, Uranus, and Neptune. They are the largest planets in our solar system and are mainly composed of gases like hydrogen and helium, giving them low density. Most have a similar structure with an atmosphere of gases, a liquid hydrogen mantle, and a small molten rock core. Jupiter is the largest and has a prominent Great Red Spot storm and over 60 moons. Saturn is notable for its extensive ring system. Uranus and Neptune are both blue-green due to methane in their atmospheres.
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.
Doppler Effect - Red Shift
The document discusses the Doppler effect and how it provides evidence for the Big Bang theory. It explains that the Doppler effect is when the frequency of a wave changes depending on whether the source of the wave is moving towards or away from an observer. It then asks what would happen to sound waves in front of and behind a moving object compared to a stationary object. Finally, it notes that the Doppler effect can cause absorption lines in spectra to shift towards the red or blue side when observing celestial objects, providing evidence that the universe is expanding.
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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.
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.
Size and Scale of the Universe
The document discusses the immense size and scale of the universe. It provides sizes and comparisons for objects from Earth to the observable universe. Earth is compared to a salt grain, while the Sun is like a gumball. The solar system spans a football stadium and galaxies are like orbits of outer planets. The observable universe extends as far as the Oort cloud at the edge of our solar system. Precise measurement techniques are needed to determine astronomical distances.
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.
Birth of a star
Stars are born in vast nebulae clouds of dust and gas scattered throughout space. Gravity gathers hydrogen in these clouds, causing them to grow denser and hotter over time. Eventually, the hydrogen heats up to 18 million degrees Fahrenheit, igniting nuclear fusion reactions that turn the hydrogen into helium - this is the moment a star is born. The color of stars depends on their temperature, ranging from hot blue-white to cooler and dimmer red. The largest known star is VY Canis Majoris, which could fit the sun inside it over 2,000 times.
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.
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.
Life cycle of stars
There are different life cycle stages for stars depending on their original mass. Low mass stars progress through the stages of nebula, main sequence, red giant, planetary nebula, white dwarf, and black dwarf. High mass stars go through nebula, main sequence, red supergiant, supernova, and either become a neutron star or black hole. The main sequence stage can last billions of years for low mass stars but only millions for high mass stars.
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.
Types of stars
This document describes different stages and types of stars:
- Main sequence stars like our Sun spend most of their lives fusing hydrogen into helium in their cores.
- Red giants are large, reddish stars that have exhausted hydrogen fusion and begun fusing helium.
- Planetary nebulae form when average-sized stars eject their outer layers after becoming red giants, leaving behind dense, hot cores called white dwarfs.
- Brown dwarfs are failed stars too small to sustain nuclear fusion.
- Variable stars change in brightness over timescales from seconds to years as they evolve.
- Binary stars are two gravitationally bound stars that orbit a common center of mass.
The Life Cycle of a Star
Stars are formed from clouds of gas and dust called nebulae. As stars age and evolve, they progress through different stages - from stars to red giants or dwarfs to supernovae. The most massive stars may collapse into neutron stars or black holes. Black holes are objects so dense that not even light can escape their powerful gravitational pull. Material near a black hole forms a swirling accretion disk and is ejected at nearly light speed in powerful jets. Advancing technology is improving our understanding of stellar evolution and black hole formation.
Stars
It is a slide showing the general information as well as some interesting information about stars that a student needs for his school.
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.
Galaxies
Galaxies come in different shapes and sizes. The largest are spiral galaxies which have a flattened disk with spiral arms and a bulge in the center. Elliptical galaxies have no definite shape and little gas or dust. Irregular galaxies have an irregular shape and active star formation. Well-known galaxies include the Andromeda Galaxy, Whirlpool Galaxy, Sombrero Galaxy, and Sunflower Galaxy.
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.
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.
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.
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.
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.
The Outer Planets
The outer planets are Jupiter, Saturn, Uranus, and Neptune. They are the largest planets in our solar system and are mainly composed of gases like hydrogen and helium, giving them low density. Most have a similar structure with an atmosphere of gases, a liquid hydrogen mantle, and a small molten rock core. Jupiter is the largest and has a prominent Great Red Spot storm and over 60 moons. Saturn is notable for its extensive ring system. Uranus and Neptune are both blue-green due to methane in their atmospheres.
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Life cycle of a star
This document summarizes the life cycle of stars from birth to death. Stars are born in stellar nurseries as gas and dust condense under gravity. Once the temperature is high enough, nuclear fusion begins and the star enters the main sequence phase. Eventually, the star will run out of fuel for fusion and expand into a red giant. The star will then collapse into a white dwarf, neutron star, or black hole depending on its original mass. Gravity ultimately wins out over fusion as the star dies once it can no longer sustain nuclear reactions in its core.
Life cycle of a star
This document summarizes the life cycle of stars from birth to death. Stars are born in stellar nurseries as gas and dust condense under gravity. Once the temperature is high enough, nuclear fusion begins and the star enters the main sequence phase. Eventually, the star will run out of fuel for fusion and expand as a red giant. The star will then collapse into a white dwarf, neutron star, or black hole depending on its original mass. Gravity ultimately wins out over fusion as the star dies once it can no longer sustain nuclear reactions in its core.
Stellar evolution
Stellar evolution begins with nebulae, large clouds of gas and dust where stars form under the influence of gravity. As nebulae contract under their own gravity, the pressure and temperature increases, forming glowing protostars at the centers of contracting gas clumps. Once the core is dense and hot enough, nuclear fusion of hydrogen to helium begins, releasing energy and marking the birth of a star. The size of a star is determined by the balance between gravitational collapse and pressure from nuclear fusion. Over their lifetimes, stars evolve from the main sequence through red giant phases as their cores shrink and outer layers expand and cool. The final fate of a star depends on its original mass, becoming a white dwarf, neutron star, or black
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.
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.
LIFE OF A STAR
Stars are luminous balls of gas held together by gravity. They are formed within dense clouds of dust and gas when disturbances cause fragments to form, with the largest fragments collapsing under their own gravity into protostars. As protostars grow denser and hotter through accretion, nuclear fusion begins, creating a stable star. Stars end their lives differently depending on their size - smaller stars become white dwarfs, medium stars become red giants then white dwarfs, while massive stars undergo violent supernovae, leaving behind neutron stars or black holes.
09 uni 07
Stars form from dense clouds of gas and dust called nebulae. As gravity pulls the particles together, nuclear fusion begins in the core, converting hydrogen to helium and releasing energy. Over billions of years, a star will burn through its hydrogen fuel. Less massive stars will expand into red giants then shed their outer layers, leaving behind a dense white dwarf core. More massive stars explode as supernovae, leaving behind neutron stars or black holes depending on their original mass.
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 star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, the brightest of which gained proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardised stellar designations. However, most of the stars in the Universe, including all stars outside our galaxy, the Milky Way, are invisible to the naked eye from Earth. Indeed, most are invisible from Earth even through the most powerful telescopes.'
07 stars, constellations, and asterisms
Stars form from clouds of gas and dust through gravitational collapse. They spend most of their existence fusing hydrogen into helium in their cores, until they run out of hydrogen fuel and their life cycles end. Smaller stars like our Sun will become red giants and white dwarfs, while larger stars over 10 solar masses will explode as supernovae, leaving behind neutron stars or black holes. Constellations are patterns of stars in the sky, while asterisms are smaller patterns within constellations like the Big Dipper in Ursa Major.
STAR AND GALAXIES IN THE UNIVERSE - NUR AIN BALQIS.pptx
Galaxies consist of millions of stars, gas and dust. Our galaxy, the Milky Way, is a medium-sized spiral galaxy located in the universe. It contains approximately 200 billion stars, and our solar system is situated in one of its spiral arms. Stars are formed from the gravitational collapse of large clouds of dust and gas called nebulae. As the core of the forming star grows denser through gravitational compression, the rising temperature and pressure triggers nuclear fusion, releasing energy and forming a star.
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.
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.
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.
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.
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.
Birth to blackhole life of a star.pptx
All stars begin as clouds of dust and gas that collapse under gravity. As the cloud collapses it spins and chunks break off, each becoming a star. Smaller stars like the sun become red giants then white dwarfs, while larger stars explode as supernovae, leaving behind neutron stars or black holes. Black holes form when massive stars collapse at the end of their life, their immense gravity crushing matter into an inescapable singularity.
Life of stars
This document discusses the life cycle of stars. It explains that stars are born from nebulae of gas and dust when the temperature rises to millions of degrees. Stars are made primarily of hydrogen, which they fuse to emit light and heat. A star's lifespan depends on its mass - larger stars live faster lives because they use their fuel quickly. When stars die, their remains may expand and cool into a white dwarf or neutron star, or explode violently as a supernova, scattering dust that can form new stars and planets. The sun is around middle-aged at 4.5 billion years.
Life of stars
This document discusses the life cycle of stars. It explains that stars are born from nebulae of gas and dust when the temperature rises to millions of degrees. Stars are made primarily of hydrogen, which they fuse to emit light and heat. A star's lifespan depends on its mass - larger stars live faster lives because they use their fuel quickly. When stars die, their remains may expand and cool into a white dwarf or neutron star, or explode violently as a supernova, leaving behind dust from which new stars and planets can form. The sun is around middle-aged at 4.5 billion years.
Stars
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.
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Writing Design Decisions
1. Interns were instructed to review feedback from the project director on their outline and background research and discuss how to strengthen their design decision paragraphs with colleagues.
2. They were then directed to write the three design decision paragraphs for their proposal, using their outline, feedback, and other resources as guides.
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Considering Design Decisions
The document discusses strategies for writing a strong proposal to address the problem of drug-resistant malaria, including focusing on one section of the proposal at a time, using an outline to organize evidence supporting design claims, and reviewing examples to understand how different parts fit together. Interns are asked to gather evidence by outlining their design decisions for three criteria related to minimizing drug resistance, side effects, and cost in order to receive feedback on their evidence and arguments.
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Exploring Antimalarial Drugs
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Understanding Drug Resistance
Using a single drug treatment for malaria results in a shift in the parasite population toward increased resistance to that drug over time. Testing different single-drug treatments in the MalariaMed model showed that resistance developed quickly when only one drug was used. Combining multiple antimalarial drugs is preferable to delay the development of resistance compared to reliance on a single drug.
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Engaging In A Science Seminar
The document describes a classroom lesson where students will participate in a Science Seminar discussion to answer the question "What caused the stickleback population to have less armor and become faster?". The students will be split into two groups - one to lead the discussion in the inner semicircle and one to listen and take notes in the outer semicircle, and they will switch roles halfway through. The goal is for the students to use the evidence cards and their knowledge to build the best explanation for why the environmental change caused the stickleback population to change.
Examining Evidence About Sticklebacks
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Wrapping Up The Newt Mystery
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Mutations In a Population
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Introduction to Mutations
This document describes a lesson about how new traits can emerge in populations through mutations. Students will read an article on mutations and discuss how mutations could explain a new poison level trait appearing in newt populations over time. They will then use a simulation to explore how mutations can introduce variation that allows a population to adapt when the environment changes. By running the simulation with and without mutations turned on, students can compare the outcome for a population of ostrilopes in a cooling environment and see the impact of mutations on the population's ability to survive.
Reviewing Key Ideas About Natural Selection
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The Deadly Dare
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Reasoning About The Newt Mystery
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Survival and Reproduction
The document discusses natural selection and how traits become more or less common over generations within populations. It describes an investigation using a simulation of ostrilopes with different color traits. Data was collected on how many offspring each color trait produced. The data showed that ostrilopes with the yellow color 7 trait reproduced more on average and became more common in the population over time, while ostrilopes with traits like blue 1 and yellow 10 that did not provide camouflage reproduced less and became less common. This occurred because traits that helped ostrilopes survive longer, like yellow 7, allowed them to reproduce more and pass on their genes more frequently.
Reproduction and Traits
The document describes a simulation activity where students use a natural selection simulation to gather evidence about how traits are passed from parents to offspring during reproduction. The simulation shows that while offspring generally inherit traits from their parents, over multiple generations of reproduction the frequency of traits in a population can change as some traits become more or less common than others. The activity provides evidence to refute the claim that reproduction always produces offspring with adaptive traits, since in the simulation non-adaptive traits were still passed down from parents to offspring.
Explaining Changes in Trait Distribution
The document summarizes a lesson on explaining changes in a population of rough-skinned newts over time based on evidence. It discusses:
1) Having students review evidence that the newt population changed, with more highly poisonous individuals now than 50 generations ago.
2) Connecting this to the fact that snakes became part of the newts' environment between the first and second data samples.
3) Concluding that snakes likely caused high poison levels to become an adaptive trait, leading to more poisonous newts over time through natural selection.
Adaptive Traits
This document describes an investigation of how traits change over time in different environments using a simulation of ostrilopes. Students observe an ostrilope population in two environments - one with a predator where being yellow provides camouflage, and one without a predator. In the environment with a predator, the population shifts to being entirely yellow over time as yellow ostrilopes are more likely to survive. In the environment without a predator, the trait distribution changes little. This provides evidence that yellow color is only adaptive in an environment where it provides camouflage from predators. The document then discusses using a modeling tool to predict how traits in a thornpalm population might change over time in response to environmental factors like
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How to Manage Your Lost Opportunities in Odoo 17 CRM
How to Manage Your Lost Opportunities in Odoo 17 CRM
Star's Life Cycle
- 2. EVOLUTION AND LIFE CYCLE OF STARS
- 5. EXAMPLES LOOK ON P. 764 in TEXT Book
- 6. STARS Life Cycles: • A Star goes through a life cycle just like humans would. Birth Life Death
- 10. Birth of a star A shockwave causes nebula gas and dust to collapse due to gravity. As the cloud collapses and shrinks due to gravity, it compresses the gas and starts to heat up inside (compression creates heat). It gets so hot that nuclear fusion starts inside the center of the cloud (a protostar forms).
- 11. Birth of a Star The high heat and temperature from the fusion reaction increases the forces of outward pressure and the protostar grows and starts to expand. Eventually, a balance between gravity wanting to collapse the protostar and the heat and pressure wanting to expand the protostar is met. A star is born and burns happily.
- 12. Shockwave Gravity compresses star Heats up fusion begins, pressure balances with gravity. Hydrogen is burning and balancing out the compression from gravity. REVIEW…
- 13. This balance between gravity and heat and pressure from fusion must be kept in order for a star to live peacefully. If a star does not burn enough hydrogen, then gravity will overcome it and it will start to collapse in on itself again. If a star makes too much energy, it will expand too much, thus shutting down the fusion reactions, ultimately causing the star to collapse again until fusion starts back up A star will continue to live happily as long as it balances internal pressure and gravity. Fusion for a star is like FOOD for us, With it we are sustained and can live. Without it, we die. HAPPY LIFE – Main Sequence
- 14. Implication More Mass • The more massive a star, the harder it has to try to overcome the force of gravity working to collapse it. More Fusion • The only way a star can overcome the collapsing force of gravity, is through the expanding heat and pressure of fusion. More Hydrogen • The more massive stars, need to burn more hydrogen than less massive stars.
- 15. Star live happy until it uses up its food: Hydrogen Stars live happy until they run out of food. It can no longer overcome gravity and starts to compress again. Bigger stars need more food to overcome gravity and thus use up there food faster (die earlier). A dying star changes from a main sequence start to another type of star. Depending on the mass of the star.
- 16. What happens when a star eats all its food? When it’s hydrogen inside its core runs out? THE STAR EXPANDS And is now burning Helium BECOMES A RED GIANT or SUPER GIANT
- 17. DEATH • At this time, gravity and heat and pressure are unbalanced. • The star begins to collapse as it cannot overcome gravity without fusion. • What happens after this point depends on the MASS of the star.
- 18. Medium – Low Mass Stars (like the sun). The stars core continues to collapse The star collapses so much that the enormous amount of heat produced causes leftover hydrogen in a cloud outside the core and He in the core to burn. This burning causes the outer atmosphere of the star to be wisped off into space leaving just the stars core behind. This core is called a white dwarf. White dwarfs are the same size as earth but way more dense.
- 19. High Mass Stars Hydrogen runs out in the core much more quickly because of its high mass, collapsing the core. It collapses so much that the inside heats up much more than inside a medium mass star. High mass stars are more massive, fusion of elements heavier than H and He take place, causing the star to expand rapidly into a super giant star. Eventuall y, the star runs out of fuel in the core causing fusion to stop. The star collapses in on itself and then explodes outward forming a supernova After the explosion however, the core of the star remain and becomes either a black hole or a neutron star depending on just how massive it is.
- 20. Supernova
- 21. From a Supernova… now what? 1.4 to 3 times the mass of the sun Core will collapse to about the size of a small city. Pressure from neutrons in the core stop the core from collapsing further. Neutron Star Greater than 3.0 the mass of the sun. Core will collapse to about the size of a small city. Pressure from neutrons in the core CANNOT stop the core from collapsing. Core shrinks down to a point called a singularity. Black Hole is formed.
- 22. Neutron Stars • Small • Extremely Dense - teaspoon weighs a mountain • Stupendous surface gravity • Rotate 1000 times per second (pulsar) neutron star marshmallow 3-megaton explosion
- 23. Black Holes • Massively dense core of a dead star compressed to a speck. • There is an imaginary sphere around the black hole called an event horizon. • Anything that goes into the event horizon can not escape its stupendous gravity.
- 24. Black Holes If Sun became black hole (not possible)…orbits of planets would be engulfed. event horizon BH