Black Holes

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Black Holes

Black holes and astronomy, galaxies, cosmic strings, science, mysteries, the unknown, atom smasher, the large hadron collider, LHC, time travel, space and secrets of the universe. Featuring news, pictures, books, videos, RSS feeds, information and much more.

 

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Introduction To Black Holes 

According to the general theory of relativity, a black hole is a region of space from which nothing, including light, can escape. It is the result of the defomation of spacetime caused by a very compact mass. Around a black hole there is an undetecable surface which marks the point of no return, called an event horizon. It is called "black" because it absorbs all the light that comes towards it, reflecting nothing, just like a perfect black body in thermodynamics. Under the theory of quantum mechanics black holes possess a temperature and emit Hawking radiation.

Despite its invisible interior, a black hole can be observed through its interaction with other matter. A black hole can be inferred by tracking the movement of a group of stars that orbit a region in space. Alternatively, when gas falls into a stellar black hole from a companion star, the gas spirals inward, heating to very high temperatures and emitting large amounts of radiation that can be detected from earthbound and earth-orbiting telescopes.

Astronomers have identified numerous stellar black hole candidates, and have also found evidence of supermassive black holes at the center of galaxies. After observing the motion of nearby stars for 16 years, in 2008 astronomers found compelling evidence that a supermassive black hole of more than 4 million solar masses is located near the Sagittarius A* region in the center of our own Milky Way galaxy.

Introduction To Event Horizon 

In general relativity, an event horizon is a boundary in spacetime, most often an area surrounding a black hole, beyond which events cannot affect an outside observer. Light emitted from beyond the horizon can never reach the observer, and any object that approaches the horizon from the observer's side appears to slow down and never quite pass through the horizon, with its image becoming more and more redshifted as time elapses. The traveling object, however, experiences no strange effects and does, in fact, pass through the horizon in a finite amount of proper time.

More specific types of horizon include the related but distinct absolute and apparent horizons found around a black hole. Still other distinct notions include the Cauchy and Killing horizon; the photon spheres and ergospheres of the Reissner-Nordström solution; particle and cosmological horizons relevant to cosmology; and isolated and dynamical horizons important in current black hole research.

Introduction To Ergosphere 

The ergosphere is a region located outside a rotating black hole. Its name is derived from the Greek word ergon, which means ?work?. It received this name because it is theoretically possible to extract energy and mass from the black hole in this region.

The ergosphere is ellipsoidal in shape and is situated so that at the poles of a rotating black hole it touches the event horizon and stretches out to a distance that is equal to the radius of the event horizon. Within the ergosphere, spacetime is dragged along in the direction of the rotation of the black hole at a speed greater than the speed of light in relation to the rest of the universe. This process is known as the Lense-Thirring effect or frame-dragging.[http://www.daviddarling.info/encyclopedia/L/Lense-Thiring_effect.html] Because of this dragging effect, objects within the ergosphere are not stationary with respect to the rest of the universe unless they travel faster than the speed of light, which is impossible based on the laws of physics. But in truth, particles are not moving with that speed, it is the spacetime of the ergosphere that moves with a speed higher than the speed of light. Another result of this dragging of space is the existence of negative energies within the ergosphere.

The outer limit of the ergosphere is the stationary limit. At the stationary limit, objects moving at the speed of light are stationary with respect to the rest of the universe. [http://www.daviddarling.info/encyclopedia/E/ergosphere.html] This is because the space here is being dragged at exactly the speed of light relative to the rest of space. Outside this limit space is still dragged, but at a rate less than the speed of light.

Since the ergosphere is outside the event horizon, it is still possible for objects to escape from the gravitational pull of the black hole. An object can gain energy by entering the black hole's rotation and then escaping from it, thus taking some of the black hole's energy with it. This process of removing energy from a rotating black hole was proposed by the mathematician Roger Penrose in 1969, and is called the Penrose process.[http://www.ias.ac.in/jarch/jaa/6/85-100.pdf] The theoretical maximum of possible energy extraction is 29% of the total energy of a rotating black hole. When this energy is removed, the black hole loses its spin and the ergosphere no longer exists. This process is considered a possible explanation for a source of energy of such energetic phenomena as gamma ray bursts. Results from computer models show that the Penrose process is capable of producing the high energy particles that are observed being emitted from quasars and other active galactic nuclei.

Introduction To Photon Sphere 

A photon sphere is a spherical region of space where gravity is strong enough that photons are forced to travel in orbits. The formula to find the radius for a circular photon orbit is: r=3GM/c2. Because of this equation photon spheres can only exist in the space surrounding an extremely compact object, such as a black hole.

As photons travel near the event horizon of a black hole they can escape being pulled in by the gravity of a black hole by traveling at a nearly vertical direction known as an exit cone. A photon on the boundary of this cone will not completely escape the gravity of the black hole. Instead it orbits the black hole. These orbits are not stable.

The photon sphere is located further from the center of a black hole than the event horizon and ergosphere. Within a photon sphere it is possible to imagine a photon that starts at the back of your head and orbits around a black hole only then be seen by your eyes.

For non-rotating black holes, the photon sphere is a sphere of radius 3/2 Rs, where Rs denotes the Schwarzschild radius (the radius of the event horizon) - see below for a derivation of this result. No unaccelerated orbit with a semi-major axis less than this distance is possible, but within the photon sphere, a constant acceleration will allow a spacecraft or probe to hover above the event horizon.

A rotating black hole has two photon spheres. As a black hole rotates it drags space with it. The photon sphere that is closer to the black hole is moving in the same direction as the rotation, whereas the photon sphere further away is moving against it. The greater the angular velocity of the rotation of a black hole the greater distance between the two photon spheres. Because the black hole has an axis of rotation this only holds true if approaching the black hole in the direction of the equator. If approaching at a different angle, such as one from the poles of the black hole to the equator, there is only one photon sphere. This is because approaching at this angle the possibility of traveling with or against the rotation does not exist.

 

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Photos 

How a black hole would lens the Milky Way by Ethan Hein

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Videos 


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Books 

A Brief History of Time: From the Big Bang to Black Holes

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Black Holes and Time Warps: Einstein's Outrageous Legacy (Commonwealth Fund Book Program)

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Death by Black Hole: And Other Cosmic Quandaries

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Radical Amazement: Contemplative Lessons from Black Holes, Supernovas, And Other Wonders of the Universe

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Geons, Black Holes, and Quantum Foam: A Life in Physics

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Decoding the Universe: How the New Science of Information Is Explaining Everything in the Cosmos, from Our Brains to Black Holes

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Cosmic Catastrophes: Exploding Stars, Black Holes, and Mapping the Universe

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Mysterious Universe: Supernovae, Dark Energy, and Black Holes (Scientists in the Field Series)

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An Introduction To Black Holes, Information And The String Theory Revolution: The Holographic Universe

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Einstein's General Theory of Relativity: With Modern Applications in Cosmology

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The Black Hole War: My Battle with Stephen Hawking to Make the World Safe for Quantum Mechanics

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Exploring Black Holes: Introduction to General Relativity

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Galaxies in Turmoil: The Active and Starburst Galaxies and the Black Holes That Drive Them (Astronomers' Universe)

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Black Holes, Wormholes & Time Machines

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Space, Time, and Gravity: The Theory of the Big Bang and Black Holes

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Black Holes and Baby Universes and Other Essays

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The Collapsing Universe: The Story of the Black Holes

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State of the Universe 2007: New Images, Discoveries, and Events (Springer Praxis Books / Popular Astronomy)

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Black Holes: An Introduction

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Black Holes, White Dwarfs and Neutron Stars: The Physics of Compact Objects

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Quantum Field Theory in Curved Spacetime and Black Hole Thermodynamics (Chicago Lectures in Physics)

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Introducing Einstein's Relativity

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Hawking on the Big Bang and Black Holes (Advanced Series in Astrophysics and Cosmology, Vol 8)

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Gravity's Fatal Attraction: Black Holes in the Universe (Scientific American Library Series)

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A Relativist's Toolkit: The Mathematics of Black-Hole Mechanics

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