Our journey towards the stars
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This document discusses humanity's journey to the stars and the future of civilization. It examines questions around whether we are alone in the universe and Fermi's paradox of why we haven't encountered other civilizations. Various models of civilization development and collapse are presented, as well as ideas around ensuring the long term survival of civilization through backups of genomes and the biosphere. The future of space exploration through technologies like 3D printing and self-replicating robots is also considered.
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Black holes are formed when a large star dies and collapses in on itself, compressing its matter into an incredibly small space with powerful gravity. Black holes can vary greatly in size, from being as small as a single atom to having a mass over a million times that of our Sun. Once matter crosses the event horizon of a black hole, it can never escape and is pulled inward towards the black hole's singularity at its center.
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This document provides an overview of black holes, including what they are, how they form, different classifications, and some key facts:
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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. Black holes can be stellar-mass, weighing around 10 times the mass of our Sun, or supermassive - containing millions to billions of solar masses at the centers of galaxies. Although black holes themselves are invisible, astronomers can detect them through their interaction with nearby stars and gas.
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A presentation I gave to the Brighton Astronomy Society in Jan 2016 - http://brightonastro.com/ , https://www.facebook.com/brightonastro/
Annoyingly that's removed the videos from the slides, so here are links to those:
https://www.youtube.com/watch?v=e-P5IFTqB98&t=18s
(This Youtube channel "In a nutshell" is absolutely fantastic by the way and I highly recommend a look through their other videos!)
https://www.youtube.com/watch?v=duoHtJpo4GY
https://vimeo.com/8723702
I've also made my notes from preparing the slides available here as well:
https://docs.google.com/document/d/1gqgsAbvoCB_7-_gPToqOuSixc02YnU-ajf-uT60R1vc/edit?usp=sharing
-- there are LOTS of further links to interesting videos in there as well, that I didn't use on the night so worth a scan through.
Any further questions, feel free to ask in comments on here
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There are three main types of black holes: primordial, stellar, and supermassive. Primordial black holes are the smallest and have a mass of a single atom. Stellar black holes are medium-sized with a mass up to 20 times the sun and fit within 10 miles. Supermassive black holes are the largest, with masses over a million suns, located at the center of galaxies. Black holes form when massive stars collapse and the gravity is too strong for anything to escape. We can observe black holes indirectly by detecting the radiation given off by nearby matter being pulled in.
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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. Black holes can be stellar-mass, weighing around 10 times the mass of our Sun, or supermassive - containing millions to billions of solar masses at the centers of galaxies. Although black holes themselves are invisible, astronomers can detect them through their interaction with nearby stars and gas.
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This is a presentation on Black Holes.
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>>What is Black Hole.
>>History.
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>>Classification.
>>Closest Black Hole.
>>Largest Black Hole.
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.
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.
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This document provides an overview of black holes including their history, formation, characteristics, growth, size, gravitational pull, and impact of falling into one. It discusses how black holes were first conceptualized in the 18th century and ideas developed over time from Einstein to Hawking. Black holes form during supernova from collapsed stars, have intense gravity preventing escape, and can feed off other matter making them grow enormously over time. Falling into a black hole results in time dilation effects and eventual death once passing the event horizon.
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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 Holes
Black holes are areas of extremely dense mass that have such strong gravitational pull that not even light can escape. They are formed when giant stars collapse at the end of their life cycles. Black holes can range significantly in size, from around 6 miles across to larger than our entire solar system. Scientists identify black holes by observing the orbits and emissions of objects near them, like stars and gas, using instruments that detect x-rays, radio waves, and other forms of light.
Black hole presentation
A presentation I gave to the Brighton Astronomy Society in Jan 2016 - http://brightonastro.com/ , https://www.facebook.com/brightonastro/
Annoyingly that's removed the videos from the slides, so here are links to those:
https://www.youtube.com/watch?v=e-P5IFTqB98&t=18s
(This Youtube channel "In a nutshell" is absolutely fantastic by the way and I highly recommend a look through their other videos!)
https://www.youtube.com/watch?v=duoHtJpo4GY
https://vimeo.com/8723702
I've also made my notes from preparing the slides available here as well:
https://docs.google.com/document/d/1gqgsAbvoCB_7-_gPToqOuSixc02YnU-ajf-uT60R1vc/edit?usp=sharing
-- there are LOTS of further links to interesting videos in there as well, that I didn't use on the night so worth a scan through.
Any further questions, feel free to ask in comments on here
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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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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.
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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 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.
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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 Holes and its Effects
1. 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.
2. There are two main types of black holes - static and rotating. The rotating type, known as Kerr black holes, form when collapsed stars have angular momentum.
3. As a star collapses, it passes through stages as a red giant, white dwarf, and neutron star until its mass exceeds around 3 solar masses, causing it to collapse entirely into a black hole with a singularity at its center.
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Black holes are regions of space with immense gravitational pull that not even light can escape. They have a boundary called an event horizon inside of which matter becomes infinitely dense. Stephen Hawking theorized that black holes transform what enters them and eject it when they evaporate, while a 2012 doomsday theory claimed a black hole would destroy Earth. Scientists search for black holes by looking for areas with large concentrated mass that emit no light.
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This document discusses black holes, including their introduction, historical background, parts, types, formation, detection, and the first picture of the M87 black hole. A black hole is a region of space with such strong gravity that nothing, not even light, can escape. They are detected through their effects on nearby matter like emitting x-rays and distorting spacetime to act as a gravitational lens.
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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.
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When certain chemicals combine, they can form a solid or jelly-like substance called a precipitate. A video link shows precipitate forming in a test tube, with some sinking to the bottom and some forming at the top. Combining chemicals can also cause a temperature change if they create a new substance, like magnesium and hydrochloric acid producing heat. Other changes include a color change, like combining clear chemicals to make blue, and the release of energy in the form of gas, light or heat. A chemical change is irreversible and can involve temperature change, energy release or a permanent color change like a precipitate.
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Kia New SORENTO 2014: Công nghệ mới - Đẳng cấp mới (Hotline: 0909016946)
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The Milan model in psychotherapy: evolution of a practice
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Our journey towards the stars
- 1. OUR JOURNEY TOWARDS THE STARS: THE FUTURE OF THE CIVILIZATION And the part astronomy plays in the chaos that will occur
- 2. ARE WE ALONE? • Radiotelescopy– Frank Drake • SETI - Search for extraterrestrial intelligence • Quantum astronomy
- 3. FERMI’S PARADOX • Why haven’t we heard anybody? (60’s) • Civilizations? • Inteligence? • Technological civilizations
- 4. HOW TO FIND US?
- 5. THE DREAM SOCIETY • Optimism Rolfa Jensena • Gradual stupidification of the civilization • Less investment in education • Social collapse – Western Roman empire • Without foundations for further progress
- 6. DEVELOPMENT SCHEME OF THE CIVILIZATION • Technological civilization • Dream society Today’s • Empathical civilization situation • ? • Cataclism Decided in the next 15 years!
- 7. IDEAS • Slavoj Žižak: shooting the antipatical ones • Jared Diamond: organisation with nature or collaps – eating up the foundations • Dimitrij Orlov: pesimism • Digital immortality • Earth is our spaceship
- 8. KARADAŠEV’S TYPES OF CIVILIZATIONS • Division according to the civilization’s energy consumption 1) Civilization type 1 – home planet 2) Civilization type 2 – home star 3) Civilization type 3 – home galaxy
- 9. HR DIAGRAM
- 10. DYSON SPHERE • Freeman Dyson (previously worked on space stations)
- 12. A NEW HOPE • Roberto Vacca • Transformation • Cycles from 300 to 1000 years
- 13. CRYPTS OF TIME • Svalbard • Ozymandias project
- 14. UNDERSTANDING OF THE BIOSPHERE • Homo sapiens as an appendix of the evolution
- 15. HOW TO DESTROY A CIVILIZATION FROM THE OUTSIDE? • Celestial body impact
- 16. • Gamma ray outburst
- 17. • Death of the Sun
- 18. BACKUP OF THE CIVILIZATION • Copies of genoms and the biosphere in independent systems
- 19. TERRAFORMING OF MARS • 2.5 – 3 million years
- 20. THE FUTURE • Technology of 3D printing • Modeling out of asteroids • Self-replicating robots
- 21. WAY TOWARDS THE STARS • τ Ceti, ε Eridani – 50 light years away
- 23. =
- 24. TELESCOPE KEPLER
- 25. MODELS OF STAR SHIPS • Dedalus – fusion of helium 3 – 5,6 tons to Alpha Centauri
- 26. • Orion – fission
- 27. • Bussard – space dust vacuum cleaner
- 28. STARGATE • Perhaps possible – quantum astronomy
- 29. VOYAGER 1 AND 2
- 30. IN IDEAL CONDITIONS • After 500 years – two stars • After 2000 years – ten stars • After 3 750 000 years – the entire galaxy
- 31. WHY HAVEN’T WE SEEN ANYTHING?
- 32. THANK YOU FOR YOUR ATTENTION! Konstantin Eduardovich Tsiolkovski: „The Earth is the craddle of mankind, but one cannot live in the craddle forever.” Anton Perkov