Black holes
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This document discusses black holes, including their formation from collapsed stars, composition of an event horizon and singularity, and properties like rotating black holes dragging space-time and Hawking radiation causing black holes to evaporate. It also briefly mentions worm holes and what would happen if one were to fall into a black hole.
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Black hole ppt
The document introduces black holes by discussing their origins from proposals in the 18th century and definitions put forth by Einstein. It describes black holes as regions of space where gravity is so strong that not even light can escape, and that are created when large stars collapse at the end of their life cycles. The document outlines three main types of black holes and describes the key parts of black holes, including their event horizons, singularities, accretion disks, and ergospheres. Hawking radiation, in which black holes are predicted to emit and evaporate over time via quantum effects, is also summarized.
Black Holes
This document discusses black holes, including their types, formation, and properties. It describes how black holes form from the gravitational collapse of massive stars or the concentration of mass in galactic centers. There are three main types - miniature, stellar, and supermassive black holes. Stellar black holes form from collapsed stars, while supermassive black holes exist at the center of most galaxies including the Milky Way. Black holes have strong gravitational pulls that distort spacetime and prevent anything from escaping, making them act like ideal blackbodies.
Black Hole
The basic information about Black Hole. What is Black Hole? How to detect Black Hole? The creation of Black Hole. The founder of Black Hole.
The blackhole origins........
This document discusses the history and properties of black holes. It explains that black holes were first proposed in the 18th century and describes how Einstein's general relativity theory led to the modern understanding of them. The key aspects covered include: the formation of black holes via gravitational collapse; the defining presence of an event horizon and singularity at the center; Hawking's prediction that black holes emit thermal radiation and eventually evaporate; and ongoing questions around merging black holes and resolving information paradoxes.
Black Holes
This document provides information about black holes, including their structure, theories about their formation and properties, and how they are detected. It discusses that a black hole has a singularity at its center with infinite density, is surrounded by an event horizon beyond which nothing can escape, and may be accompanied by an accretion disk and jets. It also describes Sagittarius A*, the supermassive black hole at the center of the Milky Way, and Cygnus X-1, the first identified black hole.
Black Holes
This document discusses black holes, including their definition, structure, theories of formation, methods of detection, and two specific black holes - Sagittarius A* and Cygnus X-1. It defines a black hole as a region with gravitational fields too strong for light or matter to escape, and describes their key structures like the singularity, event horizon, and accretion disk. It also outlines some theoretical explanations for black holes and how astronomers detect their effects through light deflection and influences on nearby objects.
Black holes
1) Black holes are formed when massive stars over 10 times the mass of the Sun collapse in on themselves due to nuclear fusion and strong gravitational forces.
2) We can detect the presence of black holes through the X-rays emitted when matter around the black hole is heated and through gravitational lensing effects on light passing by.
3) If you fell into a black hole, the extreme tidal forces would spaghettify and kill you before you reached the central singularity, and from your perspective you would see the universe compressed into a brief flash of light before destruction.
Black Hole By Pranita & Priyanka
Black holes are objects with such strong gravity that not even light can escape. They form when massive stars collapse at the end of their life cycles. Black holes come in different sizes, from stellar-mass black holes formed by collapsed stars to supermassive black holes millions of times the sun's mass found at the centers of galaxies. Though we cannot see a black hole directly, astronomers can detect them through their effects on nearby objects like gases and stars.
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Black hole ppt
The document introduces black holes by discussing their origins from proposals in the 18th century and definitions put forth by Einstein. It describes black holes as regions of space where gravity is so strong that not even light can escape, and that are created when large stars collapse at the end of their life cycles. The document outlines three main types of black holes and describes the key parts of black holes, including their event horizons, singularities, accretion disks, and ergospheres. Hawking radiation, in which black holes are predicted to emit and evaporate over time via quantum effects, is also summarized.
Black Holes
This document discusses black holes, including their types, formation, and properties. It describes how black holes form from the gravitational collapse of massive stars or the concentration of mass in galactic centers. There are three main types - miniature, stellar, and supermassive black holes. Stellar black holes form from collapsed stars, while supermassive black holes exist at the center of most galaxies including the Milky Way. Black holes have strong gravitational pulls that distort spacetime and prevent anything from escaping, making them act like ideal blackbodies.
Black Hole
The basic information about Black Hole. What is Black Hole? How to detect Black Hole? The creation of Black Hole. The founder of Black Hole.
The blackhole origins........
This document discusses the history and properties of black holes. It explains that black holes were first proposed in the 18th century and describes how Einstein's general relativity theory led to the modern understanding of them. The key aspects covered include: the formation of black holes via gravitational collapse; the defining presence of an event horizon and singularity at the center; Hawking's prediction that black holes emit thermal radiation and eventually evaporate; and ongoing questions around merging black holes and resolving information paradoxes.
Black Holes
This document provides information about black holes, including their structure, theories about their formation and properties, and how they are detected. It discusses that a black hole has a singularity at its center with infinite density, is surrounded by an event horizon beyond which nothing can escape, and may be accompanied by an accretion disk and jets. It also describes Sagittarius A*, the supermassive black hole at the center of the Milky Way, and Cygnus X-1, the first identified black hole.
Black Holes
This document discusses black holes, including their definition, structure, theories of formation, methods of detection, and two specific black holes - Sagittarius A* and Cygnus X-1. It defines a black hole as a region with gravitational fields too strong for light or matter to escape, and describes their key structures like the singularity, event horizon, and accretion disk. It also outlines some theoretical explanations for black holes and how astronomers detect their effects through light deflection and influences on nearby objects.
Black holes
1) Black holes are formed when massive stars over 10 times the mass of the Sun collapse in on themselves due to nuclear fusion and strong gravitational forces.
2) We can detect the presence of black holes through the X-rays emitted when matter around the black hole is heated and through gravitational lensing effects on light passing by.
3) If you fell into a black hole, the extreme tidal forces would spaghettify and kill you before you reached the central singularity, and from your perspective you would see the universe compressed into a brief flash of light before destruction.
Black Hole By Pranita & Priyanka
Black holes are objects with such strong gravity that not even light can escape. They form when massive stars collapse at the end of their life cycles. Black holes come in different sizes, from stellar-mass black holes formed by collapsed stars to supermassive black holes millions of times the sun's mass found at the centers of galaxies. Though we cannot see a black hole directly, astronomers can detect them through their effects on nearby objects like gases and stars.
Black hole
This document discusses black holes and some of the key contributors to the field of black hole research. It provides information on what a black hole is, defines key terms like the event horizon, and discusses the goal of understanding the term "black hole" and learning about important contributors and discoveries. Three contributors are highlighted: John Michell who first proposed the idea of a body so massive that light could not escape in 1783; Albert Einstein whose theory of general relativity helped establish the modern concept of black holes; and Stephen Hawking who showed in 1974 that black holes emit thermal radiation known as Hawking radiation.
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The document provides information about black holes from a physics group at Jahangirnagar University. It discusses the history of black hole theory, what a black hole is, how they form from massive stars, their properties including singularities and event horizons, evidence of their existence, Stephen Hawking's contributions, and some facts about black holes. The document contains sections on the history, formation, properties, detection, Hawking's work, and interesting facts about black holes. It aims to explain black holes and solve the mystery of these astronomical objects.
Black holes (2)
Black holes are formed when giant stars collapse under their own gravity. If the star's mass is large enough, its gravitational pull becomes so strong that not even light can escape, forming an event horizon around the black hole. Anything that crosses this boundary, including light, cannot escape the black hole. Black holes can also rotate, forming an ergosphere outside the event horizon where the rotation of the black hole drags spacetime itself along. While black holes themselves are invisible, astronomers can detect them through their interaction with nearby matter and the strong gravitational lensing they produce.
Black holes
The document discusses black holes, including their definition, structure, properties, classifications, and how astronomers detect them. Black holes are very dense objects with gravity so strong that not even light can escape. They are categorized into stellar, supermassive, and primordial black holes. Astronomers find evidence for black holes' existence by observing their effects on nearby matter like heating dust that emits x-rays, or by measuring the mass of an unseen object that is gravitationally influencing a companion star. Black holes are theorized to exist at the centers of most galaxies.
Black holes
Black holes are celestial objects with immense gravitational pull that not even light can escape. They are classified by size into primordial, stellar, and supermassive black holes. Black holes form through supernovae or the gravitational collapse of matter in the early universe. Key components include the singularity at the center, the event horizon boundary, and accretion disks of orbiting material. Theories explore phenomena like wormholes, the grandfather paradox in time travel, and the Novikov self-consistency principle governing causality near black holes. Astronomers detect black holes indirectly through their effects on nearby objects.
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This presentation describes little introduction about the Black holes and also explains some points about the Hawking radiation.
Year 4 Space by Jordan V
1) Black holes are regions where gravity is so strong that nothing, not even light, can escape and they are formed by the collapse of massive stars at the end of their life cycles.
2) Very massive stars end their lives in huge explosions that blow away the outer parts of the star, leaving behind a very dense core that collapses into a black hole.
3) At the center of a black hole is a singularity, a point where all the dust and gases from the collapsed star swirl around at near light speed due to the extreme gravitational pull.
Black holes powerpoint
This document provides a history and overview of black holes. It discusses that the idea of black holes was first proposed by John Mitchell in the 18th century. Key developments include Einstein's theory of relativity in 1915 and the work of Israel, Carter and Robinson establishing the no-hair theorem in the 1970s. The term "black hole" was first publicly used by John Wheeler and first recorded in an article by Ann Ewing. The document then covers the classification, features and examples of different types of black holes such as their event horizons, singularities, photon spheres, and ergospheres. Black holes can be supermassive, stellar-mass or hypothetical micro black holes. They are also classified based on their properties as
BLACK HOLE-THE OTHER DIMENSION
"Black holes are where God divided by zero" - Albert Einstein
Black hole – A region in the space where the gravitational pull is so strong that neither substance nor light can leave this area.
An Introduction about The Black Hole and its types
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They form when massive stars over 8 times the sun's mass die in supernova explosions. Billions of black holes exist between galaxies and millions exist within our own Milky Way galaxy. Black holes can be detected by their gravitational effects on nearby stars and the intense light produced from material falling into supermassive black holes at galaxy cores. Orbiting black holes is possible only at precise speeds - too slow will lead to spiraling in, too fast will escape, and intermediate speeds result in complex rosetta orbits.
Black hole
Black holes are regions of spacetime where gravity is so strong that nothing, not even light, can escape. They form when massive stars collapse at the end of their life cycle. Black holes absorb surrounding matter and other objects, growing increasingly massive over time. Scientists have discovered that black holes may affect the passage of time and have links to accretion disks and plasma jets. Different types of black holes are defined based on their rotation and electric charge.
Black holes presentation
Black holes are objects with extremely strong gravitational fields that do not allow anything, including light, to escape once it passes the event horizon. They are formed when very massive stars collapse at the end of their life cycles. Black holes are small but incredibly dense, with all their mass concentrated at a central singularity. If material such as gas from a nearby star falls into a black hole, it becomes heated and glows, making the black hole visible with telescopes.
Mike Micallef Black Holes
Black holes are formed when massive stars collapse in on themselves after exhausting their nuclear fuel. The collapsed star's immense gravity causes even light to be unable to escape, creating an event horizon around the black hole. There is strong evidence that supermassive black holes exist at the centers of galaxies, helping to shape their structure and hold stars in orbit. Black holes can continue growing by absorbing nearby matter and other objects that come too close and cross the event horizon.
Black Hole
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They can form when large stars collapse at the end of their life cycles, compressing their mass into a tiny space. Black holes warp spacetime so severely that they can pull objects inward and may potentially serve as portals to other universes or allow for time travel according to some theories. Scientists study black holes by observing the effects of their strong gravitational forces, such as emitting x-rays and warping of light.
The black hole theory
This document discusses black holes and their properties. It begins with an introduction to black holes and their structure, including their singularity, event horizon, and accretion disks. It then covers different types of black holes like stellar-mass and supermassive black holes. The document discusses how light behaves near black holes and facts about them. Specific black holes like Sagittarius A* and Cygnus X-1 are mentioned. The formation and growth of black holes over time is summarized. Stephen Hawking's theory about black hole radiation is briefly outlined. The document concludes by discussing how astronomers locate black holes and the ongoing controversy around whether information can escape from black holes.
Black holes
Black holes are regions of spacetime where gravity is so strong that nothing, not even light, can escape. They form when massive stars collapse at the end of their life cycles. There are two main types - stellar black holes, which are relatively small and formed by collapsing stars, and supermassive black holes, which are much larger and found at the center of galaxies. Black holes are invisible but can be detected through their interaction with nearby stars and gas.
BLACK HOLES
This document discusses black holes, beginning with a definition - a region of space-time where gravity prevents anything, even light, from escaping. It describes how black holes are formed from massive stars collapsing at the end of their life. Key terms are explained, like the event horizon boundary and gravitational singularity at the center. Black holes can be stellar (4-15 solar masses), intermediate (100-10,000 solar masses), or supermassive (millions to billions of solar masses, found at galaxy centers). The document concludes with how stars can be consumed by black holes after exceeding the Chandrasekhar limit.
BLACK HOLES
1) Black holes were first theorized in 1783 and were described by Einstein's theory of general relativity in 1916. The term "black hole" was coined in 1967.
2) Black holes are regions of space where gravity is so strong that not even light can escape. They form when massive stars collapse at the end of their life cycles.
3) There are three main types of black holes - stellar black holes resulting from collapsed stars, supermassive black holes at the centers of galaxies, and theoretical micro black holes. Black holes cannot be seen directly but their effects on nearby stars and gas provide evidence of their existence.
Blackholes
The document summarizes what is known about black holes, including:
- Einstein's theory of general relativity predicted black holes could exist, though they were not believed to be real until convincing evidence in the 1970s.
- Black holes are extremely dense regions with gravity so strong that not even light can escape, where the escape velocity exceeds the speed of light.
- Observational evidence like hot material falling into black holes and jets of glowing gas have shown that while invisible, black holes' effects can be observed and they are widespread throughout the universe.
Make your own nebulae
This document outlines a lesson plan to teach students about nebulae through hands-on activities. The plan includes having students act out the formation of nebulae by getting smaller and hotter, then throwing off gas and becoming stars. Students will then make their own nebulae by painting papers with gouache paints and glitter to represent different nebula types. Safety materials like freezer bags are provided for the painting to prevent messy hands. The lesson aims to make abstract space topics more concrete for students through embodied drama and art activities.
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This document discusses black holes and some of the key contributors to the field of black hole research. It provides information on what a black hole is, defines key terms like the event horizon, and discusses the goal of understanding the term "black hole" and learning about important contributors and discoveries. Three contributors are highlighted: John Michell who first proposed the idea of a body so massive that light could not escape in 1783; Albert Einstein whose theory of general relativity helped establish the modern concept of black holes; and Stephen Hawking who showed in 1974 that black holes emit thermal radiation known as Hawking radiation.
Black Holes [Krunal Saija]
Detail about Black holes. It's definition, components and then history of black hole and General theory of relativity.
Life cycle of a star and formation of black hole in space.
Different types of choice after star's life end.
Different types of Black hole on basis on mass of Parent star. and classification of black holes on basis of charge and rotational motion of black holes. Quantum theory of physics.
Study of Black holes using Quantum mechanics by Steaphen Hawking.
Current research on black holes.
Black holes, from birth to now.
The document provides information about black holes from a physics group at Jahangirnagar University. It discusses the history of black hole theory, what a black hole is, how they form from massive stars, their properties including singularities and event horizons, evidence of their existence, Stephen Hawking's contributions, and some facts about black holes. The document contains sections on the history, formation, properties, detection, Hawking's work, and interesting facts about black holes. It aims to explain black holes and solve the mystery of these astronomical objects.
Black holes (2)
Black holes are formed when giant stars collapse under their own gravity. If the star's mass is large enough, its gravitational pull becomes so strong that not even light can escape, forming an event horizon around the black hole. Anything that crosses this boundary, including light, cannot escape the black hole. Black holes can also rotate, forming an ergosphere outside the event horizon where the rotation of the black hole drags spacetime itself along. While black holes themselves are invisible, astronomers can detect them through their interaction with nearby matter and the strong gravitational lensing they produce.
Black holes
The document discusses black holes, including their definition, structure, properties, classifications, and how astronomers detect them. Black holes are very dense objects with gravity so strong that not even light can escape. They are categorized into stellar, supermassive, and primordial black holes. Astronomers find evidence for black holes' existence by observing their effects on nearby matter like heating dust that emits x-rays, or by measuring the mass of an unseen object that is gravitationally influencing a companion star. Black holes are theorized to exist at the centers of most galaxies.
Black holes
Black holes are celestial objects with immense gravitational pull that not even light can escape. They are classified by size into primordial, stellar, and supermassive black holes. Black holes form through supernovae or the gravitational collapse of matter in the early universe. Key components include the singularity at the center, the event horizon boundary, and accretion disks of orbiting material. Theories explore phenomena like wormholes, the grandfather paradox in time travel, and the Novikov self-consistency principle governing causality near black holes. Astronomers detect black holes indirectly through their effects on nearby objects.
Hawking radiation
This presentation describes little introduction about the Black holes and also explains some points about the Hawking radiation.
Year 4 Space by Jordan V
1) Black holes are regions where gravity is so strong that nothing, not even light, can escape and they are formed by the collapse of massive stars at the end of their life cycles.
2) Very massive stars end their lives in huge explosions that blow away the outer parts of the star, leaving behind a very dense core that collapses into a black hole.
3) At the center of a black hole is a singularity, a point where all the dust and gases from the collapsed star swirl around at near light speed due to the extreme gravitational pull.
Black holes powerpoint
This document provides a history and overview of black holes. It discusses that the idea of black holes was first proposed by John Mitchell in the 18th century. Key developments include Einstein's theory of relativity in 1915 and the work of Israel, Carter and Robinson establishing the no-hair theorem in the 1970s. The term "black hole" was first publicly used by John Wheeler and first recorded in an article by Ann Ewing. The document then covers the classification, features and examples of different types of black holes such as their event horizons, singularities, photon spheres, and ergospheres. Black holes can be supermassive, stellar-mass or hypothetical micro black holes. They are also classified based on their properties as
BLACK HOLE-THE OTHER DIMENSION
"Black holes are where God divided by zero" - Albert Einstein
Black hole – A region in the space where the gravitational pull is so strong that neither substance nor light can leave this area.
An Introduction about The Black Hole and its types
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They form when massive stars over 8 times the sun's mass die in supernova explosions. Billions of black holes exist between galaxies and millions exist within our own Milky Way galaxy. Black holes can be detected by their gravitational effects on nearby stars and the intense light produced from material falling into supermassive black holes at galaxy cores. Orbiting black holes is possible only at precise speeds - too slow will lead to spiraling in, too fast will escape, and intermediate speeds result in complex rosetta orbits.
Black hole
Black holes are regions of spacetime where gravity is so strong that nothing, not even light, can escape. They form when massive stars collapse at the end of their life cycle. Black holes absorb surrounding matter and other objects, growing increasingly massive over time. Scientists have discovered that black holes may affect the passage of time and have links to accretion disks and plasma jets. Different types of black holes are defined based on their rotation and electric charge.
Black holes presentation
Black holes are objects with extremely strong gravitational fields that do not allow anything, including light, to escape once it passes the event horizon. They are formed when very massive stars collapse at the end of their life cycles. Black holes are small but incredibly dense, with all their mass concentrated at a central singularity. If material such as gas from a nearby star falls into a black hole, it becomes heated and glows, making the black hole visible with telescopes.
Mike Micallef Black Holes
Black holes are formed when massive stars collapse in on themselves after exhausting their nuclear fuel. The collapsed star's immense gravity causes even light to be unable to escape, creating an event horizon around the black hole. There is strong evidence that supermassive black holes exist at the centers of galaxies, helping to shape their structure and hold stars in orbit. Black holes can continue growing by absorbing nearby matter and other objects that come too close and cross the event horizon.
Black Hole
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They can form when large stars collapse at the end of their life cycles, compressing their mass into a tiny space. Black holes warp spacetime so severely that they can pull objects inward and may potentially serve as portals to other universes or allow for time travel according to some theories. Scientists study black holes by observing the effects of their strong gravitational forces, such as emitting x-rays and warping of light.
The black hole theory
This document discusses black holes and their properties. It begins with an introduction to black holes and their structure, including their singularity, event horizon, and accretion disks. It then covers different types of black holes like stellar-mass and supermassive black holes. The document discusses how light behaves near black holes and facts about them. Specific black holes like Sagittarius A* and Cygnus X-1 are mentioned. The formation and growth of black holes over time is summarized. Stephen Hawking's theory about black hole radiation is briefly outlined. The document concludes by discussing how astronomers locate black holes and the ongoing controversy around whether information can escape from black holes.
Black holes
Black holes are regions of spacetime where gravity is so strong that nothing, not even light, can escape. They form when massive stars collapse at the end of their life cycles. There are two main types - stellar black holes, which are relatively small and formed by collapsing stars, and supermassive black holes, which are much larger and found at the center of galaxies. Black holes are invisible but can be detected through their interaction with nearby stars and gas.
BLACK HOLES
This document discusses black holes, beginning with a definition - a region of space-time where gravity prevents anything, even light, from escaping. It describes how black holes are formed from massive stars collapsing at the end of their life. Key terms are explained, like the event horizon boundary and gravitational singularity at the center. Black holes can be stellar (4-15 solar masses), intermediate (100-10,000 solar masses), or supermassive (millions to billions of solar masses, found at galaxy centers). The document concludes with how stars can be consumed by black holes after exceeding the Chandrasekhar limit.
BLACK HOLES
1) Black holes were first theorized in 1783 and were described by Einstein's theory of general relativity in 1916. The term "black hole" was coined in 1967.
2) Black holes are regions of space where gravity is so strong that not even light can escape. They form when massive stars collapse at the end of their life cycles.
3) There are three main types of black holes - stellar black holes resulting from collapsed stars, supermassive black holes at the centers of galaxies, and theoretical micro black holes. Black holes cannot be seen directly but their effects on nearby stars and gas provide evidence of their existence.
Blackholes
The document summarizes what is known about black holes, including:
- Einstein's theory of general relativity predicted black holes could exist, though they were not believed to be real until convincing evidence in the 1970s.
- Black holes are extremely dense regions with gravity so strong that not even light can escape, where the escape velocity exceeds the speed of light.
- Observational evidence like hot material falling into black holes and jets of glowing gas have shown that while invisible, black holes' effects can be observed and they are widespread throughout the universe.
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An Introduction about The Black Hole and its types
An Introduction about The Black Hole and its types
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The document lists several websites that contain information about the Polaris star including its color, distance from Earth and the sun, and temperature. The websites include wiki.answers.com, answers.yahoo.com, universetoday.com, and constellationsofwords.com and provide facts about the prominent northern star that helps with navigation.
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Polaris is a yellow-white supergiant star located in the Ursa Minor constellation about 434 light years from Earth. It is notable for being very close to Earth's north celestial pole, making it an important navigational reference point. Polaris is over 7 times more massive and 2,200 times brighter than our Sun. It is part of a multiple star system containing two smaller companion stars, Polaris AB and Polaris B. Polaris has been used for centuries by navigators and continues to be studied by astronomers today.
Quasa rs
Quasars are the most luminous and energetic objects in the universe. They are formed when matter falls into supermassive black holes at the centers of galaxies, releasing enormous amounts of energy. Quasars can outshine entire galaxies and their luminosity can vary over time. They serve as reference points for establishing the international celestial reference system due to their brightness, small size, and distant locations throughout the universe.
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This document discusses the field of astroinformatics, which uses machine learning algorithms and computational tools to analyze large astronomy datasets. It summarizes that quasars are extremely luminous celestial objects located far from Earth that emit unusually large amounts of energy. The document also notes that analyzing detailed spectra of thousands of quasars using machine learning could help identify anomalous emission patterns. Finally, it predicts that astroinformatics will be crucial for making sense of the huge volumes of data that will be produced by next-generation telescopes.
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Black holes anabelcarlosandres_1eso
This document provides an overview of black holes, including what they are, how they form, different classifications, and some key facts:
- Black holes are areas in space where gravity is so strong that not even light can escape. They form when massive stars collapse in on themselves at the end of their life cycles.
- There are three main classifications of black holes: primordial, stellar, and supermassive. Supermassive black holes exist at the center of galaxies and are millions of times the mass of our sun.
- Although powerful, black holes far away like the one at the center of our Milky Way galaxy do not pose a threat to Earth. A black hole would need to be very close to
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.
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.
Cuásar o quasar
Los cuásares son objetos extremadamente brillantes ubicados a grandes distancias que emiten grandes cantidades de energía de manera similar a las estrellas pero con un desplazamiento al rojo mayor debido al efecto Doppler, indicando que se están alejando a velocidades extremadamente altas. Se cree que los cuásares contienen agujeros negros supermasivos en sus centros que atraen grandes cantidades de materia a través de discos de acreción.
Black holes ITAES
Black holes are regions of space with immense gravitational pull that not even light can escape. There are two main types - stellar-mass black holes formed by supernovae of massive stars, and supermassive black holes likely formed as galaxies formed at their centers, containing millions to billions of solar masses. While black holes cannot be seen directly, astronomers use instruments detecting X-ray emissions and effects on nearby matter to study them. X-rays provide insights into extreme conditions near black holes like accretion disks heating matter to millions of degrees.
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.
Cuasares
Los cuásares son agujeros negros extremadamente brillantes que se alimentan de gases galácticos, expulsando grandes cantidades de energía. Se forman a partir de supernovas o la colisión de galaxias, dejando polvo y gas para que el agujero negro se alimente. Brillan tanto debido a que la fuerte gravedad del agujero negro hace que los gases se friccionen a altas velocidades y se calienten a millones de grados.
Quasar 3 c_273
Quasars are extremely bright objects located at the core of active galaxies. Quasar 3C 273 was discovered in 1963 by Marten Schmidt and is located over 2 billion light years away. Pictures taken by the Hubble Space Telescope show 3C 273 emitting two jets of ionized gas. It has a redshift of 0.157, indicating it is moving away from Earth at over 655,000 miles per second.
Blackholes 2
The document discusses black holes, beginning with how blue giant stars can go supernova and collapse into black holes due to intense gravity compressing the remains. It then mentions how the Hubble Space Telescope took the first picture of a black hole and how white holes are theorized to work in the opposite way of black holes by pushing objects out rather than pulling them in. The document concludes by stating there is still more to learn about mysterious black holes and thanks the viewer for learning some facts.
Stars Of The North
A short presentation on stars which can be easily seen from Alabama in the north part of the sky. Intended for use with grades 6-8, but good for anyone interested in naked-eye astronomy.
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.
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New Microsoft Office PowerPoint Presentation
A black hole is formed when a massive star collapses under its own gravity at the end of its life. It creates a region of space where the gravitational pull is so strong that nothing, not even light, can escape. Black holes were first theorized in the 18th century and their existence was predicted by Einstein's theory of general relativity. They have been observed through their effects on nearby stars and gas and the emission of x-rays. Black holes come in different sizes from stellar black holes formed by collapsed stars to supermassive black holes millions of times the sun's mass at the center of galaxies.
Shadow of rotating Hayward blackhole bounded by Perfect Fluid Dark Matter
I do not have any questions. The document appears to be a research proposal on various topics related to black holes, including their formation, properties of rotating and charged black holes, geodesic motion, dark matter, Hawking radiation, and the shadow they cast.
Black Holes
Black holes are regions of space with immense gravity formed after giant stars collapse. Anything that crosses the event horizon of a black hole cannot escape its gravitational pull and would appear to an outside observer to freeze at the horizon. At the center of a black hole is a singularity, a point of infinitely dense mass. The Milky Way galaxy likely contains a supermassive black hole at its center called Sagittarius A*, which has a mass over 2.5 million times that of the Sun.
The black hole theory
This document discusses black holes and provides information on their structure, types, behavior, and formation. It describes how black holes have intense gravity that prevents even light from escaping once it passes the event horizon. The document also discusses famous black holes like Cygnus X-1 and Sagittarius A*, the supermassive black hole at the center of the Milky Way galaxy. Stephen Hawking's theory that black holes emit radiation and glow is also summarized.
New microsoft office power point presentation
A black hole is formed when a massive star collapses under its own gravity at the end of its life. It creates a region of space where the gravitational pull is so strong that nothing, not even light, can escape. Black holes were first theorized in the 18th century and their existence was predicted by Einstein's theory of general relativity. They have been observed through their effects on nearby stars and gas and the emission of x-rays. Black holes come in different sizes, from stellar black holes formed by collapsed stars to supermassive black holes millions of times the sun's mass at the center of galaxies.
The black hole
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They form when large stars collapse at the end of their life cycles, squeezing matter into an infinitely small space where density and gravity become infinite. Albert Einstein first predicted black holes in 1916, and the term was coined by John Wheeler in 1967. At the center of a black hole is a gravitational singularity, and its powerful gravity is why black holes were long thought to be completely dark, though Hawking radiation shows they may emit some light.
Black hol es
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They form when massive stars collapse at the end of their life cycles. Scientists detect black holes by observing their effects on nearby stars and gas, like orbiting and high-energy light emissions. Though invisible, black holes reveal their presence through radiation and gravitational interactions with their environment. There are still many open questions around these enigmatic celestial objects.
Black Holes - Luka
Black holes are massive cosmic objects created when large stars collapse in on themselves. They have immense gravity that sucks in everything around them, even light. While invisible, scientists believe black holes exist at the center of most galaxies based on their gravitational effects. They were first proposed by Einstein's theory of general relativity in 1915 as points in spacetime where gravity becomes infinite.
Black holes
Black holes are regions of space where gravity is so strong that nothing, not even light, can escape. They form when large stars collapse at the end of their life cycles, compressing their mass into a tiny space. There are several types of black holes including stellar black holes formed by collapsed stars and supermassive black holes found at the center of galaxies containing billions of solar masses. If matter enters a black hole's event horizon, it becomes "spaghettified" as tidal forces stretch and compress it due to the extreme warping of spacetime.
Black holes
It is said that fact is sometimes stranger than fiction, and nowhere is this more true than in the case of black holes. Black holes are stranger than anything dreamt up by science fiction writers, but they are firmly matters of science ~fact.
Black hole ppt
Black holes are formed from the remnants of massive stars over 10 times the mass of the Sun that collapse at the end of their life. They are incredibly dense objects with such strong gravity that nothing, not even light, can escape from them. Theories suggest black holes could be tunnels to parallel universes or collapsed stars. At the center of a black hole is a singularity of infinite density where the laws of physics break down.
Black hole
Black holes are predicted by Einstein's theory of general relativity and are formed when massive stars collapse at the end of their life cycle. They have immense gravitational pull such that not even light can escape, creating a region of space-time known as the event horizon. Beyond this point, time stops and space ceases to exist, forming a gravitational singularity. Though small, black holes have such intense gravity that they can affect objects orbiting much larger stars and galaxies.
Black holes definitivo
Black holes form from dying massive stars and are regions of space where gravity is so strong that nothing, not even light, can escape. They have an event horizon boundary and extreme density at the singularity at the center. Small stellar black holes form from supernovae, while supermassive black holes with masses of billions of suns are found at the centers of galaxies. Matter falling into a black hole's intense gravity is stretched or "spaghettified" as it crosses the event horizon.
Journey Through the Cosmos: Exploring Black Holes & Dr. Stephen Hawking's Leg...
Title: Journey Through the Cosmos: Exploring Black Holes & Dr. Stephen Hawking's Legacy
Embark on a captivating journey through the depths of space and the brilliant mind of one of history's most renowned scientists, Dr. Stephen Hawking. In this enlightening presentation, we delve into the enigmatic phenomenon of Black Holes, their mysterious nature, and the groundbreaking discoveries that have shaped our understanding of the universe.
Unlock the secrets of these celestial wonders as we explore topics such as the fundamental question: What is a Black Hole? Delve into the gripping tale of their discovery and unravel the intricate process of their formation. From the mind-bending structure of Black Holes to the various types that exist across the cosmos, each slide unveils a new layer of cosmic intrigue.
But what happens if someone were to venture too close, falling into the gravitational abyss of a Black Hole? Discover the scientific speculation and theories that surround this captivating scenario, offering insight into the ultimate fate of such an intrepid explorer.
Moreover, journey through the extraordinary life and groundbreaking research of Dr. Stephen Hawking, a visionary whose contributions to theoretical physics revolutionized our understanding of the cosmos. Explore the trials and triumphs of his remarkable journey, from his early years to his groundbreaking work on Black Holes and beyond.
Black Holes
Black holes are formed when large stars collapse at the end of their life cycle. The gravity becomes so strong that nothing, not even light, can escape. At the center is a singularity, surrounded by an event horizon from which matter is pulled back into the black hole. Black holes rotate rapidly and are invisible due to the lack of light, with the nearest being several light-years away.
period 7 Sheharyar Sohail Black Holes
Black holes are regions of space where the gravitational pull is so strong that nothing, not even light, can escape. Surrounding the black hole is an event horizon, which marks the point of no return beyond which the gravitational forces are inescapable. Albert Einstein's theory of general relativity first theorized black holes by explaining how gravity can bend space and time. Black holes have immense gravitational forces that can feed on and destroy stars that come too close, collapsing them into the black hole. The largest known black holes are supermassive black holes that can be millions of times the size of our sun.
Black hole
A black hole is a region of space where gravity is so strong that nothing, not even light, can escape. They form when massive stars collapse at the end of their life cycles. There are several types of black holes including stellar black holes formed by collapsed stars and supermassive black holes millions to billions times the mass of our sun. As objects fall into a black hole's event horizon, they become "spaghettified" as the black hole's immense gravity stretches and pulls them apart.
Black hole
1) A black hole is an object with such strong gravity that not even light can escape, forming at the collapse of a massive star.
2) It has an "event horizon", the point of no return beyond which nothing, not even light, can escape the black hole.
3) Black holes were first theorized by geologist John Michell in 1783, and the modern theory was proposed by physicist Stephen Hawking.
Black hole
Recent advances in the study of black holes include:
1. The first image of a black hole was captured in 2019 using the Event Horizon Telescope, showing the shadow of the supermassive black hole at the center of the Messier 87 galaxy.
2. Gravitational waves detected in 2015 by the LIGO observatory provided direct evidence of black holes from the merger of two stellar-mass black holes.
3. Observations of stars orbiting Sagittarius A* provided evidence of a supermassive black hole at the center of the Milky Way galaxy.
4. X-ray binaries, where matter falls from a donor star onto a compact object like a neutron star or black hole
Black hole
Black holes are objects of extreme density that have such strong gravitational attraction that even light cannot escape once it passes the event horizon. The event horizon marks the boundary of a black hole beyond which anything passing is trapped forever. At the center is a singularity of infinite density where gravitational forces become infinite. The distance from the singularity to the event horizon is called the Schwarzschild radius. If one were to fall into a black hole, powerful tidal forces would stretch and compress their body as they crossed the event horizon and approached the singularity.
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Shadow of rotating Hayward blackhole bounded by Perfect Fluid Dark Matter
Shadow of rotating Hayward blackhole bounded by Perfect Fluid Dark Matter
Journey Through the Cosmos: Exploring Black Holes & Dr. Stephen Hawking's Leg...
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CLASS 12th CHEMISTRY SOLID STATE ppt (Animated)
Description:
Dive into the fascinating realm of solid-state physics with our meticulously crafted online PowerPoint presentation. This immersive educational resource offers a comprehensive exploration of the fundamental concepts, theories, and applications within the realm of solid-state physics.
From crystalline structures to semiconductor devices, this presentation delves into the intricate principles governing the behavior of solids, providing clear explanations and illustrative examples to enhance understanding. Whether you're a student delving into the subject for the first time or a seasoned researcher seeking to deepen your knowledge, our presentation offers valuable insights and in-depth analyses to cater to various levels of expertise.
Key topics covered include:
Crystal Structures: Unravel the mysteries of crystalline arrangements and their significance in determining material properties.
Band Theory: Explore the electronic band structure of solids and understand how it influences their conductive properties.
Semiconductor Physics: Delve into the behavior of semiconductors, including doping, carrier transport, and device applications.
Magnetic Properties: Investigate the magnetic behavior of solids, including ferromagnetism, antiferromagnetism, and ferrimagnetism.
Optical Properties: Examine the interaction of light with solids, including absorption, reflection, and transmission phenomena.
With visually engaging slides, informative content, and interactive elements, our online PowerPoint presentation serves as a valuable resource for students, educators, and enthusiasts alike, facilitating a deeper understanding of the captivating world of solid-state physics. Explore the intricacies of solid-state materials and unlock the secrets behind their remarkable properties with our comprehensive presentation.
Alternate Wetting and Drying - Climate Smart Agriculture
Alternate Wetting and Drying - Climate Smart AgricultureInternational Food Policy Research Institute- South Asia Office
PPT on Alternate Wetting and Drying presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024. Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
Direct Seeded Rice - Climate Smart Agriculture
Direct Seeded Rice - Climate Smart AgricultureInternational Food Policy Research Institute- South Asia Office
PPT on Direct Seeded Rice presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024.
(June 12, 2024) Webinar: Development of PET theranostics targeting the molecu...
(June 12, 2024) Webinar: Development of PET theranostics targeting the molecu...Scintica Instrumentation
Targeting Hsp90 and its pathogen Orthologs with Tethered Inhibitors as a Diagnostic and Therapeutic Strategy for cancer and infectious diseases with Dr. Timothy Haystead.在线办理(salfor毕业证书)索尔福德大学毕业证毕业完成信一模一样
学校原件一模一样【微信：741003700 】《(salfor毕业证书)索尔福德大学毕业证》【微信：741003700 】学位证，留信认证（真实可查，永久存档）原件一模一样纸张工艺/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。
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Describing and Interpreting an Immersive Learning Case with the Immersion Cub...
Current descriptions of immersive learning cases are often difficult or impossible to compare. This is due to a myriad of different options on what details to include, which aspects are relevant, and on the descriptive approaches employed. Also, these aspects often combine very specific details with more general guidelines or indicate intents and rationales without clarifying their implementation. In this paper we provide a method to describe immersive learning cases that is structured to enable comparisons, yet flexible enough to allow researchers and practitioners to decide which aspects to include. This method leverages a taxonomy that classifies educational aspects at three levels (uses, practices, and strategies) and then utilizes two frameworks, the Immersive Learning Brain and the Immersion Cube, to enable a structured description and interpretation of immersive learning cases. The method is then demonstrated on a published immersive learning case on training for wind turbine maintenance using virtual reality. Applying the method results in a structured artifact, the Immersive Learning Case Sheet, that tags the case with its proximal uses, practices, and strategies, and refines the free text case description to ensure that matching details are included. This contribution is thus a case description method in support of future comparative research of immersive learning cases. We then discuss how the resulting description and interpretation can be leveraged to change immersion learning cases, by enriching them (considering low-effort changes or additions) or innovating (exploring more challenging avenues of transformation). The method holds significant promise to support better-grounded research in immersive learning.
Summary Of transcription and Translation.pdf
Hello Everyone Here We are Sharing You with The process of protien Synthesis in very short points you will be Able to understand It Very well
Evidence of Jet Activity from the Secondary Black Hole in the OJ 287 Binary S...
Wereport the study of a huge optical intraday flare on 2021 November 12 at 2 a.m. UT in the blazar OJ287. In the binary black hole model, it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact based on a prediction made 8 yr earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R–I spectral index by 1.0 ±0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary BH. We then ask why we have not seen this phenomenon before. We show that OJ287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability using the Krakow data set of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In machine-readable Tables 1 and 2, we give the full orbit-linked historical light curve of OJ287 as well as the dense monitoring sample of Krakow.
Mending Clothing to Support Sustainable Fashion_CIMaR 2024.pdf
Ozturkcan, S., Berndt, A., & Angelakis, A. (2024). Mending clothing to support sustainable fashion. Presented at the 31st Annual Conference by the Consortium for International Marketing Research (CIMaR), 10-13 Jun 2024, University of Gävle, Sweden.
fermented food science of sauerkraut.pptx
This ppt contains the production of a fermented food name - sauerkraut
The cost of acquiring information by natural selection
This is a short talk that I gave at the Banff International Research Station workshop on Modeling and Theory in Population Biology. The idea is to try to understand how the burden of natural selection relates to the amount of information that selection puts into the genome.
It's based on the first part of this research paper:
The cost of information acquisition by natural selection
Ryan Seamus McGee, Olivia Kosterlitz, Artem Kaznatcheev, Benjamin Kerr, Carl T. Bergstrom
bioRxiv 2022.07.02.498577; doi: https://doi.org/10.1101/2022.07.02.498577
ESA/ACT Science Coffee: Diego Blas - Gravitational wave detection with orbita...
ESA/ACT Science Coffee: Diego Blas - Gravitational wave detection with orbita...Advanced-Concepts-Team
Presentation in the Science Coffee of the Advanced Concepts Team of the European Space Agency on the 07.06.2024.
Speaker: Diego Blas (IFAE/ICREA)
Title: Gravitational wave detection with orbital motion of Moon and artificial
Abstract:
In this talk I will describe some recent ideas to find gravitational waves from supermassive black holes or of primordial origin by studying their secular effect on the orbital motion of the Moon or satellites that are laser ranged.Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
Pests of Storage_Identification_Dr.UPR.pdf
InIndia-post-harvestlosses-unscientificstorage,insects,rodents,micro-organismsetc.,accountforabout10percentoftotalfoodgrains
Graininfestation
Directdamage
Indirectly
•theexuviae,skin,deadinsects
•theirexcretawhichmakefoodunfitforhumanconsumption
About600speciesofinsectshavebeenassociatedwithstoredgrainproducts
100speciesofinsectpestsofstoredproductscauseeconomiclosses
Anti-Universe And Emergent Gravity and the Dark Universe
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
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Anti-Universe And Emergent Gravity and the Dark Universe
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Black holes
- 1. BLACK HOLES K.D.SRINIVAS 15481A04A1 K.HEMANTH 15481A04A3 K.LALITH 15481A04B9 Submitted to Dr. Vijaya Lakshmi
- 2. Contents What is a black hole? Formation of a black hole Composition of black hole Rotating black holes Contribution of Stephen Hawking Relation bw Black hole & Worm hole What happens when you fall into black hole? Fascinating facts about black holes A brief Summary
- 3. A few definitions from the dictionary: Region of space resulting from the collapse of a star Region of space with strong gravitational field Dungeon or dark cell in a prison A black hole is a place in space where gravity pulls so much that even light can not get out
- 4. Formed when a star collapses Collapse of star produces Neutron star & Black Hole Compression of any object into its Schwarzschild radius gives a Black Hole
- 5. They consist of: Event horizon Singularity Event horizon Completely black and reflects nothing. Once entered no escaping back. Empty and full of gravity.
- 6. Singularity Density= ∞? Volume= 0? Surface area= 0? Gravity= ∞ Schwarzschild radius Singularity
- 7. A rotating black hole has an ergo sphere around the outside of the event horizon. In the ergo sphere, space and time themselves are dragged along with the rotation of the black hole
- 8. Contribution of Stephen Hawking Black holes evaporate eventually by phenomenon Hawking Radiation
- 9. But new research suggests that, if a speculative theory called loop quantum gravity is right, white holes could be real Worm hole warps space time Hypothesis only
- 10. What happens when you fall into Black Hole? As you fall into to a black hole, you shine a blue flashlight at a friend exterior to the hole, he sees