The Dark Sector of the Cosmos
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Jesus Martinez-Manso from the NSB-Spark Pay team is going to talk to us about infinity and beyond! Most of the Universe is made of dark and scary stuff that is going into our mouths every second (no kidding), yet we know very little about it. In this talk, Jesus will give an overview of cosmic dark sector and explain the basics of how we know about its existence. We will cover topics like dark energy, dark matter, black holes and galaxy evolution.
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Life of stars
Giant molecular clouds collapse under gravity to form protostars that grow into main sequence stars through nuclear fusion. As stars age, they expand into red giants and shed their outer layers, leaving behind white dwarfs that slowly cool over billions of years. More massive stars have shorter lifespans and die in spectacular supernovae, potentially leaving behind neutron stars or black holes.
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.
4.2 Stars have Life Cycles
Stars change over their life cycles depending on their mass. Low-mass stars like our Sun remain on the main sequence for billions of years, slowly fusing hydrogen into helium. Eventually they expand into red giants and later cool into white dwarfs. High-mass stars burn through their fuel quickly and explode as supernovae after millions of years, leaving behind neutron stars or black holes. All stars form from contracting nebulae of gas and dust.
Life Cycle Of A Star
The document discusses the life cycle of stars from their birth in nebulae to their death. Stars are born when gas and dust clouds collapse under gravity and heat up. During their main sequence phase, stars fuse hydrogen into helium in their cores. Later, larger stars become red giants or supergiants as their cores shrink and outer layers expand. Eventually, stars die and eject their outer layers, leaving behind dense remnants like white dwarfs, neutron stars, or black holes.
Black holes
Einstein's theory of general relativity from 1915 predicted the possibility of black holes, but they were not believed to exist until convincing evidence was found in the 1970s. Black holes are incredibly dense regions formed after massive stars collapse, where gravity is so strong that not even light can escape. They can be stellar-mass, supermassive, or mid-mass depending on their origin and size, with supermassive black holes found at the centers of many galaxies including the Milky Way.
Life cycle of a star
Stars are born from contracting nebulae of gas and dust. They spend most of their lives on the main sequence, fusing hydrogen into helium in their cores. Eventually they run out of fuel in their cores and their outer layers expand, forming red giants or supergiants. From there, smaller stars shed their outer layers to form planetary nebulae and white dwarfs, while larger stars explode as supernovae, leaving behind neutron stars or black holes.
Life Cycle of Stars Stations
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Life of stars
Giant molecular clouds collapse under gravity to form protostars that grow into main sequence stars through nuclear fusion. As stars age, they expand into red giants and shed their outer layers, leaving behind white dwarfs that slowly cool over billions of years. More massive stars have shorter lifespans and die in spectacular supernovae, potentially leaving behind neutron stars or black holes.
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.
4.2 Stars have Life Cycles
Stars change over their life cycles depending on their mass. Low-mass stars like our Sun remain on the main sequence for billions of years, slowly fusing hydrogen into helium. Eventually they expand into red giants and later cool into white dwarfs. High-mass stars burn through their fuel quickly and explode as supernovae after millions of years, leaving behind neutron stars or black holes. All stars form from contracting nebulae of gas and dust.
Life Cycle Of A Star
The document discusses the life cycle of stars from their birth in nebulae to their death. Stars are born when gas and dust clouds collapse under gravity and heat up. During their main sequence phase, stars fuse hydrogen into helium in their cores. Later, larger stars become red giants or supergiants as their cores shrink and outer layers expand. Eventually, stars die and eject their outer layers, leaving behind dense remnants like white dwarfs, neutron stars, or black holes.
Black holes
Einstein's theory of general relativity from 1915 predicted the possibility of black holes, but they were not believed to exist until convincing evidence was found in the 1970s. Black holes are incredibly dense regions formed after massive stars collapse, where gravity is so strong that not even light can escape. They can be stellar-mass, supermassive, or mid-mass depending on their origin and size, with supermassive black holes found at the centers of many galaxies including the Milky Way.
Life cycle of a star
Stars are born from contracting nebulae of gas and dust. They spend most of their lives on the main sequence, fusing hydrogen into helium in their cores. Eventually they run out of fuel in their cores and their outer layers expand, forming red giants or supergiants. From there, smaller stars shed their outer layers to form planetary nebulae and white dwarfs, while larger stars explode as supernovae, leaving behind neutron stars or black holes.
Life Cycle of Stars Stations
The document provides background information on stars' life cycles and how they are determined by mass. It states that stars with greater mass will have shorter life cycles as they must burn hot and fast to maintain equilibrium, using up fuel quickly and dying young in traumatic explosions. Average stars will live longer, peaceful deaths. It then lists directions for an activity involving classifying stars on the Hertzsprung-Russell diagram and answering conclusion questions.
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The document discusses the properties of stars based on their spectra and position on the Hertzsprung-Russell diagram. It describes how stellar spectra can reveal a star's chemical composition and temperature, with Annie Jump Cannon developing the stellar classification system. The Hertzsprung-Russell diagram plots stars based on luminosity and temperature, separating them into main sequence, red giant, supergiant, and white dwarf categories. Relationships between a star's mass, luminosity, radius, and temperature are also explained.
THE LIFE CYCLE OF A STAR!
All stars begin as clouds of dust and gas called nebulae. When gravity causes the nebula to collapse, a protostar forms at the center. The protostar grows in size and temperature through nuclear fusion reactions until it becomes a stable main sequence star. Small stars like our Sun will eventually expand into red giants and shed their outer layers, leaving behind dense white dwarf cores. Larger stars may explode as supernovae, collapsing into neutron stars or black holes. The life cycle of a star depends on its initial mass, with smaller stars ending as white dwarfs and more massive stars ending as black holes or neutron stars.
Life Cycle Of A Star
The life cycle of a star consists of 5 main stages:
1. Protostars form from huge clouds of gas that collapse under gravity.
2. Main sequence stars like our Sun fuse hydrogen for billions of years.
3. Red giants expand and their outer layers cool as hydrogen runs out.
4. White dwarfs form as red giants collapse under gravity into dense remnants.
5. Black dwarfs are the final remains that cool for eternity, emitting no light.
The Life Cycle of a Star PowerPoint
Stars are born from clouds of gas and dust called nebulae. Over billions of years, stars progress through various stages as they age. Lower mass stars begin as protostars and become main sequence stars fueled by nuclear fusion. As their hydrogen runs out, they become red giants and eventually white dwarfs. Higher mass stars explode as supernovae at the end of their lives, leaving behind neutron stars or black holes.
life cycle of a star
The 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.
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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.
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Stars are born from clouds of gas and dust called nebulas. As the gas spins faster under gravity, it heats up and forms a protostar. Nuclear fusion then occurs, turning the protostar into a main sequence star that shines for millions of years by fusing hydrogen into helium. Eventually the hydrogen runs out, causing the star to expand into a red giant. From there, less massive stars will blow off their outer layers and collapse into white dwarfs, while more massive stars will explode in supernovas and collapse into neutron stars or black holes.
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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.
Planetary nebulae formation
Planetary nebulae form during the late stages of evolution for low-to-medium mass stars. As a star expands into a red giant, it ejects its outer layers through pulsations and stellar winds. The hot core ionizes the ejected gas, causing it to glow brightly. This energized shell of nebulous gas appears as a planetary nebula. Examples are the Helix Nebula and Ring Nebula. More massive stars may explode as supernovae, leaving behind neutron stars or black holes, depending on the star's original mass. The document discusses these stages of stellar evolution and death that give rise to different astronomical phenomena like planetary nebulae and neutron stars.
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All stars begin as clouds of dust and gas called nebulae. When gravity causes the nebula to collapse, a protostar forms at the center. The protostar grows in size and temperature through nuclear fusion reactions until it becomes a stable main sequence star. Small stars like our Sun will eventually expand into red giants and shed their outer layers, leaving behind dense white dwarf cores. Larger stars may explode as supernovae, collapsing into neutron stars or black holes. The life cycle of a star depends on its initial mass, with smaller stars ending as white dwarfs and more massive stars ending as black holes or neutron stars.
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The life cycle of a star consists of 5 main stages:
1. Protostars form from huge clouds of gas that collapse under gravity.
2. Main sequence stars like our Sun fuse hydrogen for billions of years.
3. Red giants expand and their outer layers cool as hydrogen runs out.
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Stars are born from clouds of gas and dust called nebulae. Over billions of years, stars progress through various stages as they age. Lower mass stars begin as protostars and become main sequence stars fueled by nuclear fusion. As their hydrogen runs out, they become red giants and eventually white dwarfs. Higher mass stars explode as supernovae at the end of their lives, leaving behind neutron stars or black holes.
life cycle of a star
The 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.
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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.
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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.
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The universe is composed of atoms that make up all matter. Atoms have a nucleus surrounded by an electron cloud. Stars are celestial bodies that shine through nuclear fusion, transforming hydrogen into helium. Stars are born in clusters like the Orion Nebula and range enormously in size, from our Sun to giants like Antares. Over their lifetimes, stars transform hydrogen into helium until they run out of fuel and die, collapsing into white dwarfs, then black dwarfs without light. The Big Bang generated the cosmos we live in, and massive concentrations of matter form black holes with gravity so strong that nothing, not even light, can escape.
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Stars are born from clouds of gas and dust called nebulas. As the gas spins faster under gravity, it heats up and forms a protostar. Nuclear fusion then occurs, turning the protostar into a main sequence star that shines for millions of years by fusing hydrogen into helium. Eventually the hydrogen runs out, causing the star to expand into a red giant. From there, less massive stars will blow off their outer layers and collapse into white dwarfs, while more massive stars will explode in supernovas and collapse into neutron stars or black holes.
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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.
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Planetary nebulae form during the late stages of evolution for low-to-medium mass stars. As a star expands into a red giant, it ejects its outer layers through pulsations and stellar winds. The hot core ionizes the ejected gas, causing it to glow brightly. This energized shell of nebulous gas appears as a planetary nebula. Examples are the Helix Nebula and Ring Nebula. More massive stars may explode as supernovae, leaving behind neutron stars or black holes, depending on the star's original mass. The document discusses these stages of stellar evolution and death that give rise to different astronomical phenomena like planetary nebulae and neutron stars.
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Modern physics grapples with some of humankind’s biggest questions: ‘Why is the universe the way it is? And why are we here, able to ask the question?’ In their search for answers, leading physicists have been considering some wild ideas, including the existence of multiple universes (the ‘multiverse’) and the possibility that we may actually be living in a black hole. I will explain the physics behind these wild ideas, describe how they might answer our biggest questions, and lay out the prospects for finding observational evidence to support or refute them.
Prof Jonathan Sievers (UKZN) NITheP Associate Workshop talk
The document discusses the cosmic microwave background (CMB) and what can be learned from precise measurements of it. The CMB provides information to answer fundamental questions about the universe, such as what it is made of, how old it is, and how fast it is expanding. Recent experiments like the Atacama Cosmology Telescope (ACT) have made accurate measurements of the CMB temperature and polarization, revealing the density of ordinary and dark matter, supporting inflation, and constraining the number of neutrino species and particle properties. Upgraded instruments like ACTpol aim to further improve measurements and help address open questions in cosmology and particle physics.
Dark Eneary and Dark Mass
This document provides an overview of dark matter and dark energy from both observational evidence in the universe and theoretical work done at particle accelerators in laboratories. It summarizes that observational evidence shows the universe is made up of 70% dark energy, 25% dark matter, and only 5% ordinary matter. While much is known about the basic features and inventory of the universe, deep puzzles remain about reconciling gravity and quantum mechanics, the nature of dark matter and dark energy, and resolving why observations of dark energy are so much smaller than theoretical predictions. The document discusses how ideas like extra dimensions, supersymmetry, and multiple compactifications in string theory attempt to address these puzzles, but that challenges remain in fully explaining dark energy and connecting theory to
D5 further cosmology
This document summarizes the history and current understanding of cosmology and the universe. It discusses how early thinkers like Newton and Einstein contributed to models of the universe. Key developments include Alexander Friedmann showing the universe is dynamic and expanding or contracting, Edwin Hubble discovering galaxies are moving away, and Georges Lemaître proposing the Big Bang model. Later evidence supporting the Big Bang includes the cosmic microwave background radiation and supernovae observations. Dark matter and dark energy are now understood to make up most of the universe, but their nature remains mysterious. Ongoing questions concern the composition and ultimate fate of the expanding universe.
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(1) The document discusses the origins and evolution of the universe from the Big Bang to the potential future scenarios of the Big Freeze or Big Crunch, depending on whether dark energy or dark matter wins out.
(2) It also covers the life cycles of stars from birth to death, whether they are small or massive stars, and the formation of objects like neutron stars and black holes.
(3) Einstein's theories of relativity and the implications for time travel are mentioned, along with the impossibility of travelling faster than the speed of light according to known laws of physics.
To The Edge of Infinity
This is a very broad overview of cosmology. It includes an introduction to galaxies, the large scale structure of the universe, black holes, and the fate of the universe. It is intended for teenagers and up.
Seminar presentation on Hubble's Law and Expanding Universe
The document discusses Edwin Hubble and Hubble's Law, which states that the recession velocity of galaxies is proportional to their distance from Earth. It provides background on Hubble, describes how Hubble's Constant has been measured over time using different methods like gravitational lensing and Type 1a supernovae, and discusses applications of Hubble's Constant like the Hubble time. The document also covers topics like the expanding universe, dark matter, dark energy, the big bang theory, and the possible fates of the universe.
Black holes
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. There are three classifications of black holes based on their masses - stellar-mass, supermassive, and mid-mass. While black holes have immense gravitational pulls, we are relatively safe from them due to the vast distances between objects in space and the fact that stars and galaxies orbit around their centers rather than falling directly into the central black holes. Scientists can detect black holes through observing orbiting stars and gas disks and jets emitting x-rays as material is pulled into the black hole.
Accelerated expansion of universe and evolving ideas about gravity
Gravity from Newton and Einstein to the accelerated expansion of the universe; the Lambda_CDM Model.
Dark matter ~ Introduction
How the concept was introduced by the astrophycists and examples that provide the base for the existence of dark matter. Basic introduction to types of dark matter according to standard cosmological theory.
Period 7 - Gah Tang - The Invisible Dilemma
Dark matter is invisible matter that can only be detected through its gravitational effects. It makes up about 27% of the universe and helps hold galaxies together. Studying dark matter could bolster theories of gravity, revolutionize the Big Bang theory, and lead to new discoveries like dark energy. The presentation argues that pursuing dark matter research can advance human knowledge and progress society.
Big bang cosmology
The Big Bang model postulates that the universe began as a hot dense state around 13.8 billion years ago and has since expanded and cooled. It is supported by two theoretical pillars: general relativity, which describes gravity as the curvature of spacetime, and the cosmological principle that the universe is homogeneous and isotropic on large scales. The model accounts for the cosmic microwave background radiation and expansion of the universe, but is incomplete as it does not explain structure formation or the universe's uniformity on the largest scales.
IB Astrophysics - cosmology - Flippingphysics by nothingnerdy
The document summarizes key concepts in cosmology, including Olbers' paradox, the expanding universe, the Big Bang theory, and evidence like the cosmic microwave background radiation. It discusses how the universe originated approximately 13.7 billion years ago in a massive expansion from a single point. The universe is still expanding today, and its fate depends on whether it has a flat, closed, or open geometry based on its total mass density. While most mass is dark matter and dark energy, their exact nature remains unknown. International space projects seek to further understand these cosmological questions through observation and research.
Big Bang Theory
Big bang theory
Formation of stars
Formation of galaxies
Expansions of space
Birth of solar system
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Big Bang Theory & Other Recent Sciences || 2014 - Dr. Mahbub Khan
Big Bang Theory & Other Recent Sciences || 2014 - Dr. Mahbub Khan
Big Bang Theory & Other Recent Sciences || 2014 - Dr. Mahbub Khan
Big Bang Theory & Other Recent Sciences || 2014 - Dr. Mahbub Khan
Do We Live in a Black Hole? Modern Conceptions of the Multiverse
Do We Live in a Black Hole? Modern Conceptions of the Multiverse
Prof Jonathan Sievers (UKZN) NITheP Associate Workshop talk
Prof Jonathan Sievers (UKZN) NITheP Associate Workshop talk
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Seminar presentation on Hubble's Law and Expanding Universe
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Accelerated expansion of universe and evolving ideas about gravity
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The Dark Sector of the Cosmos
- 1. The dark sector Jesús Martínez Manso
- 2. What is the Universe made of? 68% 27% 5% Dark energy Dark matter "Normal" matter • Gas (H) • Stars • Dust
- 3. What? How? Dark matter Galaxies South Pole Telescope: microwavesSpitzer: infraredGTC: visible My research
- 4. Dark energy: the weirdo Universe is expanding, and accelerating! Mysterious effect, let’s call it DARK ENERGY
- 5. Einstein’s equations Geometry of space Energy and mass G
- 6. Einstein’s equations Gmn =8pG Tmn 3 space + 1 time components… 16 equations, ugh! Universe is isotropicAssumptions: Universe is homogeneous … at large scales Just ONE equation for the expansion of the Universe:
- 7. Observations Riess, Perlmutter & Schmidt 1998
- 8. Perlmutter, Schmidt & Riess 1998 “speed ” “distance” Universe is accelerating!! Observations
- 9. Fitting theory to observations Extra term: dark energy “speed ” “distance”
- 10. Weird properties DE density remains constant as Universe expands while matter and radiation get diluted DE will increasingly dominate the Universe, accelerating expansion even more Size of Universe time (billion years) 0 7 14 21 28 35 Big Rip You are here Where is this extra energy coming from?
- 11. But, what is it, really? Λ = vacuum energy? 10120 prediction Evacuum measured Λ > Merp.
- 13. Cool discoveries ahead Some day we might harness the power of dark energy in technology
- 14. Fritz Zwicky, 1933 Galaxy cluster “Coma” Dark matter
- 15. H. Babcock, 1939
- 18. Dark matter How does it interact? Gravitational force Electromagnetic force Weak force Strong force ?
- 19. Dark matter What can it be? We need to figure out things like: • Better measurement of its temperature • Does it annihilate with itself? Unlike with dark energy, here we have some plausible candidates, like WIMPS BUT
- 20. Black holes Come closer, I just wanna play… Hi, I’m a region where space is so warped that not even light can escape.
- 21. Formation of BH depends on density, not just on total mass. There are several ways to form one Main types Micro BH, Mass < 1 gram Stellar BH, Mass ~ 10 Msun Supermassive BH, Mass ~ 1 Billion Msun
- 22. Stellar black holes • Most common black holes • Final evolutionary stage of large stars
- 23. Stellar black holes We should not fear their fly- by’s any more than other bodies of same mass
- 24. Supermassive black holes • Almost every biggish galaxy has one at its center • They have masses around 1 BILLION times our Sun Our galaxy has one too:
- 25. Supermassive black holes From time to time, they will swallow gas clouds and light up the entire galaxy. In these stages, they are called Active Galactic Nuclei
- 26. Gultekin et al. 2009 Supermassive black holes We don’t know how they formed!! BH mass is correlated to host galaxy mass: Which formed first??
- 27. Thanks!