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Stars are massive self-luminous celestial objects composed of gaseous matter held together by gravity. The nearest star to Earth is the Sun. Stellar evolution is the process by which a star is born, lives, and dies, beginning with the gravitational contraction of hydrogen gas into a protostar. As the protostar's density and temperature increase at its core, nuclear fusion of hydrogen into helium begins, releasing energy and establishing a steady state balance between gravitational contraction and radiation pressure.
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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.
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 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
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.
Stars, Star Life Cycle, Constellations
Stars begin as clouds of gas and dust called nebulae. When the cloud contracts under gravity, it heats up and forms a protostar at the center. Once the protostar reaches critical mass, nuclear fusion begins and the star enters the main sequence phase. During the main sequence, stars fuse hydrogen into helium. Eventually the star runs out of fuel and its life cycle depends on its size - smaller stars become white dwarfs while very massive stars explode as supernovae.
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 Cycle of Stars
A nebula of dust and gas contracts over 10 million years to form a protostar and eventually a star through nuclear fusion. Stars exist in a main sequence phase fusing hydrogen for billions of years depending on their mass. As hydrogen fusion slows, gravity causes smaller stars to expand into red giants and later white dwarfs, while larger stars become supergiants and eventually explode as supernovae, 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.
Recommended
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.
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 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
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.
Stars, Star Life Cycle, Constellations
Stars begin as clouds of gas and dust called nebulae. When the cloud contracts under gravity, it heats up and forms a protostar at the center. Once the protostar reaches critical mass, nuclear fusion begins and the star enters the main sequence phase. During the main sequence, stars fuse hydrogen into helium. Eventually the star runs out of fuel and its life cycle depends on its size - smaller stars become white dwarfs while very massive stars explode as supernovae.
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 Cycle of Stars
A nebula of dust and gas contracts over 10 million years to form a protostar and eventually a star through nuclear fusion. Stars exist in a main sequence phase fusing hydrogen for billions of years depending on their mass. As hydrogen fusion slows, gravity causes smaller stars to expand into red giants and later white dwarfs, while larger stars become supergiants and eventually explode as supernovae, 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.
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's Life Cycle
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.
Kinds of stars according to color- Grade Six Science
The document discusses different types of stars categorized by their color, from coolest red stars like Betelguese and Antares at around 3000 degrees Celsius, to hotter orange, yellow like our sun, and white stars like Sirius and Vega around 11,000 degrees Celsius, with the hottest being bluish-white stars like Rigel at 20,000 degrees Celsius. Examples are provided for each color category along with their surface temperatures. The document also covers star magnitudes, twinkling, measuring distance in light years, and identifying star types based on descriptions of their size.
E2 - Types of Star & HR Diagram
The document describes different types of stars:
1) Red giants are very large, cool stars that all main sequence stars evolve into. Nuclear fusion occurs in red giants, fusing helium into heavier elements.
2) White dwarfs are very small and dense remnants of red giants. They have high temperatures but low luminosities due to their small size.
3) Neutron stars form from massive stars and are very hot and dense, composed mostly of neutrons. Pulsars are rotating, magnetized neutron stars that emit beams of electromagnetic radiation.
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.
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.
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.
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.
Galaxies nebulae stars notes
Within galaxies, star forming regions called nebulae contain clouds of dust, hydrogen and helium gases. Stars sometimes form within these nebulae as the gases and dust collapse under their own gravity. A nebula with protostars, or young stars that are still forming, is shown in the diagram. The document then goes on to describe the life cycle of stars like our Sun and the changes it will undergo as it evolves and eventually dies in approximately 5 billion years.
Stars & Galaxies
The document summarizes the life cycle of stars and galaxies in the universe. It begins with the Big Bang 13 billion years ago which formed the first quarks, electrons, protons and neutrons. Over billions of years, hydrogen and helium atoms were pulled together by gravity to form the first stars and galaxies. The document then describes the typical life cycle of stars from their birth as protostars to their death as white dwarfs, neutron stars, or black holes depending on their mass.
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.
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.
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.
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.
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
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.
Life Cycle of Stars - Revision
A nebula begins as a dense cloud of gas and dust that contracts due to gravity. As pressure and temperature increase, it forms a protostar. When hot enough, fusion reactions begin and a main sequence star is born. Over time, a star will expand into a red giant as fusion outweighs gravity. After swelling to many times its size, a red giant cools and its outer layers form a planetary nebula surrounding the core which shrinks into a white dwarf. For very massive stars, a supernova explosion marks the end, briefly outshining the galaxy before leaving behind a crushed core such as a neutron star or black hole.
Stars
It is a slide showing the general information as well as some interesting information about stars that a student needs for his school.
Death of a star
Stars eventually die when they exhaust their nuclear fuel. Small stars cool and shrink into white dwarfs, while larger stars that become red giants either shed their outer layers leaving behind dense neutron stars or explode in gigantic supernovae. The oldest stars are around 13.7 billion years old, formed shortly after the Big Bang, while big bright stars only live for around 10 million years and stars like the Sun will live for approximately 10 billion years.
Space science ( stars and galaxy)
The document summarizes key concepts in space science, including the life cycles of stars and galaxies. It describes how stars are formed from contracting gas clouds, progressing through steady state burning of hydrogen to helium, then expanding as red giants before ending as white dwarfs, neutron stars, or black holes depending on their mass. It also explains that galaxies are groups of millions of stars held together by gravity, and summarizes the types of galaxies including spiral, elliptical, and irregular. Finally, it provides an overview of the leading cosmological model of the Big Bang theory which proposes the expansion of the universe from an initial hot, dense state approximately 13.8 billion years ago.
Evolution of universe
The document discusses the evolution of the universe from the Big Bang theory to present day. It covers:
1) The Big Bang theory which proposes the universe began as a hot, dense point around 14 billion years ago and has been expanding and cooling ever since.
2) The formation of stars, galaxies, and planets as the universe evolved, with our solar system forming around 5 billion years ago.
3) Two other theories - the Steady State theory which proposes the universe has always existed in a constant state, and the Pulsating universe theory.
1. universe, planets and solar system.pptx
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What's hot
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's Life Cycle
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.
Kinds of stars according to color- Grade Six Science
The document discusses different types of stars categorized by their color, from coolest red stars like Betelguese and Antares at around 3000 degrees Celsius, to hotter orange, yellow like our sun, and white stars like Sirius and Vega around 11,000 degrees Celsius, with the hottest being bluish-white stars like Rigel at 20,000 degrees Celsius. Examples are provided for each color category along with their surface temperatures. The document also covers star magnitudes, twinkling, measuring distance in light years, and identifying star types based on descriptions of their size.
E2 - Types of Star & HR Diagram
The document describes different types of stars:
1) Red giants are very large, cool stars that all main sequence stars evolve into. Nuclear fusion occurs in red giants, fusing helium into heavier elements.
2) White dwarfs are very small and dense remnants of red giants. They have high temperatures but low luminosities due to their small size.
3) Neutron stars form from massive stars and are very hot and dense, composed mostly of neutrons. Pulsars are rotating, magnetized neutron stars that emit beams of electromagnetic radiation.
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.
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.
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.
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.
Galaxies nebulae stars notes
Within galaxies, star forming regions called nebulae contain clouds of dust, hydrogen and helium gases. Stars sometimes form within these nebulae as the gases and dust collapse under their own gravity. A nebula with protostars, or young stars that are still forming, is shown in the diagram. The document then goes on to describe the life cycle of stars like our Sun and the changes it will undergo as it evolves and eventually dies in approximately 5 billion years.
Stars & Galaxies
The document summarizes the life cycle of stars and galaxies in the universe. It begins with the Big Bang 13 billion years ago which formed the first quarks, electrons, protons and neutrons. Over billions of years, hydrogen and helium atoms were pulled together by gravity to form the first stars and galaxies. The document then describes the typical life cycle of stars from their birth as protostars to their death as white dwarfs, neutron stars, or black holes depending on their mass.
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.
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.
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.
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.
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
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.
Life Cycle of Stars - Revision
A nebula begins as a dense cloud of gas and dust that contracts due to gravity. As pressure and temperature increase, it forms a protostar. When hot enough, fusion reactions begin and a main sequence star is born. Over time, a star will expand into a red giant as fusion outweighs gravity. After swelling to many times its size, a red giant cools and its outer layers form a planetary nebula surrounding the core which shrinks into a white dwarf. For very massive stars, a supernova explosion marks the end, briefly outshining the galaxy before leaving behind a crushed core such as a neutron star or black hole.
Stars
It is a slide showing the general information as well as some interesting information about stars that a student needs for his school.
Death of a star
Stars eventually die when they exhaust their nuclear fuel. Small stars cool and shrink into white dwarfs, while larger stars that become red giants either shed their outer layers leaving behind dense neutron stars or explode in gigantic supernovae. The oldest stars are around 13.7 billion years old, formed shortly after the Big Bang, while big bright stars only live for around 10 million years and stars like the Sun will live for approximately 10 billion years.
What's hot (19)
Kinds of stars according to color- Grade Six Science
Kinds of stars according to color- Grade Six Science
Similar to Smitha g s
Space science ( stars and galaxy)
The document summarizes key concepts in space science, including the life cycles of stars and galaxies. It describes how stars are formed from contracting gas clouds, progressing through steady state burning of hydrogen to helium, then expanding as red giants before ending as white dwarfs, neutron stars, or black holes depending on their mass. It also explains that galaxies are groups of millions of stars held together by gravity, and summarizes the types of galaxies including spiral, elliptical, and irregular. Finally, it provides an overview of the leading cosmological model of the Big Bang theory which proposes the expansion of the universe from an initial hot, dense state approximately 13.8 billion years ago.
Evolution of universe
The document discusses the evolution of the universe from the Big Bang theory to present day. It covers:
1) The Big Bang theory which proposes the universe began as a hot, dense point around 14 billion years ago and has been expanding and cooling ever since.
2) The formation of stars, galaxies, and planets as the universe evolved, with our solar system forming around 5 billion years ago.
3) Two other theories - the Steady State theory which proposes the universe has always existed in a constant state, and the Pulsating universe theory.
1. universe, planets and solar system.pptx
hghdcigsdiucsdiucsdcijsdbcksjcnsdkjcbsdkbxsjkbsdjcbsdjcbdcbdcjsdbcjdbcdcbkjcbsdkcbdkjcdkjcdcjkdnjkcdncdjkcndkjcndkjcnsdlclnsdlcsdncsdnckdncdcndjkcndkjcndkjcnsdkjcnsdkcnskcnskjcdsjkcdjkcdkjcdkjcdjkcdjkjcdkjcfjkjcfkjcfkcdfbjkcbnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuuunnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnnn
Ns1 origin of universe
The document discusses the origin and evolution of the universe, Earth, and life over billions of years according to scientific theories. It describes how the universe began with the Big Bang around 14 billion years ago, then galaxies, stars, and planetary systems formed. Around 4.5 billion years ago, Earth formed from accretion in our solar system. Early life emerged around 3.8 billion years ago, evolving into complex organisms over time. The document provides timelines of these cosmic and biological events from the birth of the universe to the present.
1universe hp
The document provides information about the universe and solar system. It discusses:
- The universe is approximately 13.8 billion years old and consists of dark energy, dark matter, and normal matter.
- The solar system formed from a collapsing cloud of gas and dust around the sun approximately 4.6 billion years ago. Planetesimals collided and accreted to form the planets.
- The current model is that the sun and planets formed from a protoplanetary disk, with collisions forming the terrestrial planets close to the sun and condensation forming the gas giants further out.
The Beginning of the Universe
The document provides information about several theories of the origin and evolution of the universe and solar system. It discusses the Big Bang theory, which proposes that the universe began in an extremely hot and dense state and has been expanding ever since. It also describes theories for how the sun, planets, and natural satellites formed, such as the nebular hypothesis which suggests they formed from a rotating cloud of gas and dust. The document then gives details about the properties of planets in our solar system as well as dwarf planets like Pluto.
Chapter 1 origin of the universe
This document provides an overview of theories on the origin of the universe and the solar system. It begins by defining important terms like dark matter, dark energy, and theories. It then discusses creation myths from different cultures and the biblical creation story in Genesis. The majority of the document focuses on explaining the Big Bang Theory, including the inflation epoch, events after the Big Bang like formation of the basic elements, and evidence that supports it like galaxy redshifts and the cosmic microwave background. It also briefly outlines other theories like the steady state theory, string theory, and M-theory. The second half summarizes theories of solar system formation like the nebula hypothesis and compares terrestrial and Jovian planets.
David y carlos s.
The document summarizes information about the universe and the formation of planets. It describes early models of the universe centered around Earth and later recognizing other galaxies. The Big Bang theory established that the universe rapidly expanded from an initial hot, dense state. Dark matter and an accelerating expansion suggest unknown forces at work. Space exploration helps observe the universe by overcoming Earth's atmosphere. Galaxies, nebulae, and stars are described along with the stages of star formation. Planets form from disks around new stars, and our solar system contains rocky inner and gaseous outer planets along with satellites, asteroids, comets, and planetary debris.
Stellar life cycle section 3
Stellar Life Cycle
1. Stars are born from dense clouds of gas and dust called nebulae.
2. Most stars, including our Sun, spend the majority of their lifespan fusing hydrogen into helium as main sequence stars.
3. Towards the end of their life, stars expand into red giants or supergiants and begin fusing heavier elements, before shrinking into white dwarfs, neutron stars, or black holes.
Astonishing Astronomy 101 - Chapter 6
This document summarizes key components and concepts about the structure of the solar system:
- The solar system consists of the Sun, eight planets, dwarf planets, asteroids, comets, and other small bodies. The Sun contains over 99% of the solar system's mass.
- The inner terrestrial planets are rocky, while the outer gas giants are large planets composed primarily of hydrogen and helium. An asteroid belt exists between Mars and Jupiter.
- Factors like a planet's mass, distance from the Sun, composition, and atmospheric properties help determine its environment and surface conditions. Larger planets retain heat and atmospheres better than smaller ones.
- Techniques like radioactive dating indicate the solar system formed
Into the Edge of the Stars Humanity’s changing vision of the cosmos Presenter...
Into the Edge of the Stars Humanity’s changing vision of the cosmos Presenter...Haileyesus Wondwossen
Into the Edge of the Stars Humanity’s changing vision of the cosmos
Presenter: Haileyesus Wondwossen
Basic measurement.
How old our universe is?
Evidence that the universe had a beginning.
Size comparison.
The universe-Earth
Faster travel.
Search for life-bearing planets
Mystery question
oriaethiopia1@gmail.com
+251920720556Unit8astronomy09 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.
Physical Science Module 1.pptx
The document discusses how elements are formed in the universe through three main nuclear reactions: nucleosynthesis during the Big Bang formed light elements like hydrogen and helium, nuclear fusion in stars forms heavier elements up to iron, and neutron capture reactions during supernovae explosions produce elements heavier than iron. These nuclear reactions require extremely high temperatures and pressures to fuse atomic nuclei together or allow neutron capture, conditions only found in the early universe, inside stars and supernovae. Element formation relies on balancing the number of protons and neutrons in atomic nuclei to achieve stable configurations through fusion, fission, radioactive decay, or transmutation into other elements.
Other Theories on the Origin of the Universe.pptx
The document discusses several theories on the origin of the universe:
- The Steady State Theory proposed the universe has always and will always remain the same.
- The Oscillating Universe Theory proposed the universe exists in a cycle of big bangs and big crunches.
- The Eternal Inflation Theory proposes inflation never stops after the big bang.
- For the formation of the solar system, theories included the Nebular Hypothesis of a collapsing cloud forming the sun and planets, and the Condensation Theory of dust accumulating in the solar nebula.
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.
Apes earth systems
The document summarizes the origins and evolution of the universe, galaxy, solar system, and Earth. It begins by explaining how the Big Bang occurred approximately 13.7 billion years ago, marking the expansion of the early universe. It then describes how the universe cooled and formed elemental structures, galaxies, stars, and planets over billions of years. Specific details are provided about the formation of the Milky Way galaxy and solar system, including Earth. The geological history of Earth is outlined, dividing time into eons, eras, periods, and epochs marked by significant evolutionary changes and extinctions.
Origin of the Universe and the Solar System
The most widely accepted theory of planetary formation, known as the nebular hypothesis, maintains that 4.6 billion years ago, the Solar System formed from the gravitational collapse of a giant molecular cloud which was light years across.
Universe and the Solar System (Lesson 1).pptx
SHS Earth and Life Grade 11 Lesson 1. This lesson discusses the compos of the universe, the origin of the universe, different hypotheses of the origin of the universe
grade 6 Gravity and the solar system.ppt grade 6
Gravity is a force that attracts all objects with mass. It causes planets, stars, and galaxies to form and keeps smaller bodies in orbit around larger ones. Kepler discovered that planets follow elliptical orbits around the sun, with the sun at one focus, and that their orbital periods and distances from the sun are mathematically related. Newton later formulated the law of universal gravitation, stating that all objects attract each other through a gravitational force proportional to their masses and inversely proportional to the square of the distance between them. Gravity provides the centripetal force needed to keep planets in circular orbits around the sun.
Alex y juan carlos
The universe consists of all space, time, matter and energy according to the document. It began expanding after the Big Bang, and astronomers believe the expansion will continue indefinitely due to the presence of dark matter and an unknown accelerating force. The universe contains galaxies which are grouped into larger structures called clusters. Galaxies themselves contain stars, nebulae, black holes and other astronomical objects. Stars are born in nebulae and pass through various life stages involving nuclear fusion until ending as white dwarfs or exploding as supernovae.
Similar to Smitha g s (20)
Into the Edge of the Stars Humanity’s changing vision of the cosmos Presenter...
Into the Edge of the Stars Humanity’s changing vision of the cosmos Presenter...
Recently uploaded
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...University of Maribor
Slides from talk:
Aleš Zamuda: Remote Sensing and Computational, Evolutionary, Supercomputing, and Intelligent Systems.
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Inter-Society Networking Panel GRSS/MTT-S/CIS Panel Session: Promoting Connection and Cooperation
https://www.etran.rs/2024/en/home-english/The binding of cosmological structures by massless topological defects
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
Thornton ESPP slides UK WW Network 4_6_24.pdf
ESPP presentation to EU Waste Water Network, 4th June 2024 “EU policies driving nutrient removal and recycling
and the revised UWWTD (Urban Waste Water Treatment Directive)”
原版制作(carleton毕业证书)卡尔顿大学毕业证硕士文凭原版一模一样
原版纸张【微信：741003700 】【(carleton毕业证书)卡尔顿大学毕业证】【微信：741003700 】学位证，留信认证（真实可查，永久存档）offer、雅思、外壳等材料/诚信可靠,可直接看成品样本，帮您解决无法毕业带来的各种难题！外壳，原版制作，诚信可靠，可直接看成品样本。行业标杆！精益求精，诚心合作，真诚制作！多年品质 ,按需精细制作，24小时接单,全套进口原装设备。十五年致力于帮助留学生解决难题，包您满意。
本公司拥有海外各大学样板无数，能完美还原海外各大学 Bachelor Diploma degree, Master Degree Diploma
1:1完美还原海外各大学毕业材料上的工艺：水印，阴影底纹，钢印LOGO烫金烫银，LOGO烫金烫银复合重叠。文字图案浮雕、激光镭射、紫外荧光、温感、复印防伪等防伪工艺。材料咨询办理、认证咨询办理请加学历顾问Q/微741003700
留信网认证的作用:
1:该专业认证可证明留学生真实身份
2:同时对留学生所学专业登记给予评定
3:国家专业人才认证中心颁发入库证书
4:这个认证书并且可以归档倒地方
5:凡事获得留信网入网的信息将会逐步更新到个人身份内，将在公安局网内查询个人身份证信息后，同步读取人才网入库信息
6:个人职称评审加20分
7:个人信誉贷款加10分
8:在国家人才网主办的国家网络招聘大会中纳入资料，供国家高端企业选择人才
Deep Software Variability and Frictionless Reproducibility
Deep Software Variability and Frictionless ReproducibilityUniversity of Rennes, INSA Rennes, Inria/IRISA, CNRS
The ability to recreate computational results with minimal effort and actionable metrics provides a solid foundation for scientific research and software development. When people can replicate an analysis at the touch of a button using open-source software, open data, and methods to assess and compare proposals, it significantly eases verification of results, engagement with a diverse range of contributors, and progress. However, we have yet to fully achieve this; there are still many sociotechnical frictions.
Inspired by David Donoho's vision, this talk aims to revisit the three crucial pillars of frictionless reproducibility (data sharing, code sharing, and competitive challenges) with the perspective of deep software variability.
Our observation is that multiple layers — hardware, operating systems, third-party libraries, software versions, input data, compile-time options, and parameters — are subject to variability that exacerbates frictions but is also essential for achieving robust, generalizable results and fostering innovation. I will first review the literature, providing evidence of how the complex variability interactions across these layers affect qualitative and quantitative software properties, thereby complicating the reproduction and replication of scientific studies in various fields.
I will then present some software engineering and AI techniques that can support the strategic exploration of variability spaces. These include the use of abstractions and models (e.g., feature models), sampling strategies (e.g., uniform, random), cost-effective measurements (e.g., incremental build of software configurations), and dimensionality reduction methods (e.g., transfer learning, feature selection, software debloating).
I will finally argue that deep variability is both the problem and solution of frictionless reproducibility, calling the software science community to develop new methods and tools to manage variability and foster reproducibility in software systems.
Exposé invité Journées Nationales du GDR GPL 2024
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...
Functional Magnetic Resonance Imaging (fMRI) provides means to characterize brain activations in response to behavior. However, cognitive neuroscience has been limited to group-level effects referring to the performance of specific tasks. To obtain the functional profile of elementary cognitive mechanisms, the combination of brain responses to many tasks is required. Yet, to date, both structural atlases and parcellation-based activations do not fully account for cognitive function and still present several limitations. Further, they do not adapt overall to individual characteristics. In this talk, I will give an account of deep-behavioral phenotyping strategies, namely data-driven methods in large task-fMRI datasets, to optimize functional brain-data collection and improve inference of effects-of-interest related to mental processes. Key to this approach is the employment of fast multi-functional paradigms rich on features that can be well parametrized and, consequently, facilitate the creation of psycho-physiological constructs to be modelled with imaging data. Particular emphasis will be given to music stimuli when studying high-order cognitive mechanisms, due to their ecological nature and quality to enable complex behavior compounded by discrete entities. I will also discuss how deep-behavioral phenotyping and individualized models applied to neuroimaging data can better account for the subject-specific organization of domain-general cognitive systems in the human brain. Finally, the accumulation of functional brain signatures brings the possibility to clarify relationships among tasks and create a univocal link between brain systems and mental functions through: (1) the development of ontologies proposing an organization of cognitive processes; and (2) brain-network taxonomies describing functional specialization. To this end, tools to improve commensurability in cognitive science are necessary, such as public repositories, ontology-based platforms and automated meta-analysis tools. I will thus discuss some brain-atlasing resources currently under development, and their applicability in cognitive as well as clinical neuroscience.
8.Isolation of pure cultures and preservation of cultures.pdf
Isolation of pure culture, its various method.
ESR spectroscopy in liquid food and beverages.pptx
With increasing population, people need to rely on packaged food stuffs. Packaging of food materials requires the preservation of food. There are various methods for the treatment of food to preserve them and irradiation treatment of food is one of them. It is the most common and the most harmless method for the food preservation as it does not alter the necessary micronutrients of food materials. Although irradiated food doesn’t cause any harm to the human health but still the quality assessment of food is required to provide consumers with necessary information about the food. ESR spectroscopy is the most sophisticated way to investigate the quality of the food and the free radicals induced during the processing of the food. ESR spin trapping technique is useful for the detection of highly unstable radicals in the food. The antioxidant capability of liquid food and beverages in mainly performed by spin trapping technique.
Unlocking the mysteries of reproduction: Exploring fecundity and gonadosomati...
The pygmy halfbeak Dermogenys colletei, is known for its viviparous nature, this presents an intriguing case of relatively low fecundity, raising questions about potential compensatory reproductive strategies employed by this species. Our study delves into the examination of fecundity and the Gonadosomatic Index (GSI) in the Pygmy Halfbeak, D. colletei (Meisner, 2001), an intriguing viviparous fish indigenous to Sarawak, Borneo. We hypothesize that the Pygmy halfbeak, D. colletei, may exhibit unique reproductive adaptations to offset its low fecundity, thus enhancing its survival and fitness. To address this, we conducted a comprehensive study utilizing 28 mature female specimens of D. colletei, carefully measuring fecundity and GSI to shed light on the reproductive adaptations of this species. Our findings reveal that D. colletei indeed exhibits low fecundity, with a mean of 16.76 ± 2.01, and a mean GSI of 12.83 ± 1.27, providing crucial insights into the reproductive mechanisms at play in this species. These results underscore the existence of unique reproductive strategies in D. colletei, enabling its adaptation and persistence in Borneo's diverse aquatic ecosystems, and call for further ecological research to elucidate these mechanisms. This study lends to a better understanding of viviparous fish in Borneo and contributes to the broader field of aquatic ecology, enhancing our knowledge of species adaptations to unique ecological challenges.
BREEDING METHODS FOR DISEASE RESISTANCE.pptx
Plant breeding for disease resistance is a strategy to reduce crop losses caused by disease. Plants have an innate immune system that allows them to recognize pathogens and provide resistance. However, breeding for long-lasting resistance often involves combining multiple resistance genes
Nucleophilic Addition of carbonyl compounds.pptx
Nucleophilic addition is the most important reaction of carbonyls. Not just aldehydes and ketones, but also carboxylic acid derivatives in general.
Carbonyls undergo addition reactions with a large range of nucleophiles.
Comparing the relative basicity of the nucleophile and the product is extremely helpful in determining how reversible the addition reaction is. Reactions with Grignards and hydrides are irreversible. Reactions with weak bases like halides and carboxylates generally don’t happen.
Electronic effects (inductive effects, electron donation) have a large impact on reactivity.
Large groups adjacent to the carbonyl will slow the rate of reaction.
Neutral nucleophiles can also add to carbonyls, although their additions are generally slower and more reversible. Acid catalysis is sometimes employed to increase the rate of addition.
如何办理(uvic毕业证书)维多利亚大学毕业证本科学位证书原版一模一样
原版纸张【微信：741003700 】【(uvic毕业证书)维多利亚大学毕业证】【微信：741003700 】学位证，留信认证（真实可查，永久存档）offer、雅思、外壳等材料/诚信可靠,可直接看成品样本，帮您解决无法毕业带来的各种难题！外壳，原版制作，诚信可靠，可直接看成品样本。行业标杆！精益求精，诚心合作，真诚制作！多年品质 ,按需精细制作，24小时接单,全套进口原装设备。十五年致力于帮助留学生解决难题，包您满意。
本公司拥有海外各大学样板无数，能完美还原海外各大学 Bachelor Diploma degree, Master Degree Diploma
1:1完美还原海外各大学毕业材料上的工艺：水印，阴影底纹，钢印LOGO烫金烫银，LOGO烫金烫银复合重叠。文字图案浮雕、激光镭射、紫外荧光、温感、复印防伪等防伪工艺。材料咨询办理、认证咨询办理请加学历顾问Q/微741003700
留信网认证的作用:
1:该专业认证可证明留学生真实身份
2:同时对留学生所学专业登记给予评定
3:国家专业人才认证中心颁发入库证书
4:这个认证书并且可以归档倒地方
5:凡事获得留信网入网的信息将会逐步更新到个人身份内，将在公安局网内查询个人身份证信息后，同步读取人才网入库信息
6:个人职称评审加20分
7:个人信誉贷款加10分
8:在国家人才网主办的国家网络招聘大会中纳入资料，供国家高端企业选择人才
ANAMOLOUS SECONDARY GROWTH IN DICOT ROOTS.pptx
Abnormal or anomalous secondary growth in plants. It defines secondary growth as an increase in plant girth due to vascular cambium or cork cambium. Anomalous secondary growth does not follow the normal pattern of a single vascular cambium producing xylem internally and phloem externally.
What is greenhouse gasses and how many gasses are there to affect the Earth.
What are greenhouse gasses how they affect the earth and its environment what is the future of the environment and earth how the weather and the climate effects.
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
Although Artemia has been known to man for centuries, its use as a food for the culture of larval organisms apparently began only in the 1930s, when several investigators found that it made an excellent food for newly hatched fish larvae (Litvinenko et al., 2023). As aquaculture developed in the 1960s and ‘70s, the use of Artemia also became more widespread, due both to its convenience and to its nutritional value for larval organisms (Arenas-Pardo et al., 2024). The fact that Artemia dormant cysts can be stored for long periods in cans, and then used as an off-the-shelf food requiring only 24 h of incubation makes them the most convenient, least labor-intensive, live food available for aquaculture (Sorgeloos & Roubach, 2021). The nutritional value of Artemia, especially for marine organisms, is not constant, but varies both geographically and temporally. During the last decade, however, both the causes of Artemia nutritional variability and methods to improve poorquality Artemia have been identified (Loufi et al., 2024).
Brine shrimp (Artemia spp.) are used in marine aquaculture worldwide. Annually, more than 2,000 metric tons of dry cysts are used for cultivation of fish, crustacean, and shellfish larva. Brine shrimp are important to aquaculture because newly hatched brine shrimp nauplii (larvae) provide a food source for many fish fry (Mozanzadeh et al., 2021). Culture and harvesting of brine shrimp eggs represents another aspect of the aquaculture industry. Nauplii and metanauplii of Artemia, commonly known as brine shrimp, play a crucial role in aquaculture due to their nutritional value and suitability as live feed for many aquatic species, particularly in larval stages (Sorgeloos & Roubach, 2021).
Randomised Optimisation Algorithms in DAPHNE
Slides from talk:
Aleš Zamuda: Randomised Optimisation Algorithms in DAPHNE .
Austrian-Slovenian HPC Meeting 2024 – ASHPC24, Seeblickhotel Grundlsee in Austria, 10–13 June 2024
https://ashpc.eu/
Recently uploaded (20)
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...
The binding of cosmological structures by massless topological defects
The binding of cosmological structures by massless topological defects
Deep Software Variability and Frictionless Reproducibility
Deep Software Variability and Frictionless Reproducibility
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...
Deep Behavioral Phenotyping in Systems Neuroscience for Functional Atlasing a...
8.Isolation of pure cultures and preservation of cultures.pdf
8.Isolation of pure cultures and preservation of cultures.pdf
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ESR spectroscopy in liquid food and beverages.pptx
Unlocking the mysteries of reproduction: Exploring fecundity and gonadosomati...
Unlocking the mysteries of reproduction: Exploring fecundity and gonadosomati...
aziz sancar nobel prize winner: from mardin to nobel
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What is greenhouse gasses and how many gasses are there to affect the Earth.
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The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptx
Smitha g s
- 1. SPACE SCIENCE Stars and Galaxies
- 2. . Astronomy : • It is the branch of science deals with study of celestial objects, space and universe Star: • 1) It is a massive self luminous celestial object • 2)It contain lot of gaseous matter held together by gravity. • 3) It emits radiation through nuclear reactions Eg: Sun , Sirius, Polaris , Arcturus * Star nearest to earth is ------> Sun (Distance = 1.5 X 108 Km ) •.
- 4. Stellar evolution Stellar evolution is the process involved in the entire life cycle of Stars from birth to death
- 5. How a star is Born :(Sun like Star Step 1: Protostar : • Huge gaseous hydrogen contracts under its own gravity. • Density and temperature increases at center. • Formation of spherical structure at center. • This is called protostar.
- 7. Step II : Steady state ● Hydrogen nuclei fuse to form Helium nuclei ● Temperature increases and lot of energy is released. ●Due to enormous release of energy matter is expanded away from center . ● Force of gravity tries to contract matter but radiation pressure tends to expand matter. ● Two opposing forces balance each other. ● Now star attains steady state.