Come on over to the other side...of the Bermuda Triangle!
When you visit the coastal region of Western Australia you are standing on the Antipode (opposite side) of the Bermuda Triangle!
If the earth were a glass ball and you were able to see through it to the other side what would you find directly beneath your feet? The Island of Bermuda is almost directly opposite Fremantle, Rottnest Island (Perth Metro Area).
The Triangle includes the greater part of the West Australian coastline. When visiting this region of Western Australia you are literally on the 'Other Side' of the infamous Bermuda Triangle!
About the geography of Antipodal positions on a spherical planet
From Wikipedia, the free encyclopedia
The antipodes of any place on the Earth is the place which is diametrically opposite it — so situated that a line drawn from the one to the other passes through the centre of the Earth and forms a true diameter. For example, the antipodes of New Zealand's North Island lies in Spain. Most of the earth's land surfaces have ocean at its antipodes, this being a consequence of most land being in the northern hemisphere.
An antipodal point is sometimes called an antipode, a back-formation from the Greek plural antipodes, whose singular in Greek is antipous.
The antipodes of any place on Earth must be distant from it by 180° of longitude, and must be as many degrees to the north of the equator as the original is to the south; in other words, the latitudes are numerically equal, but one is north and the other south. The map shown above is based on this relationship; it shows a Lambert azimuthal equal-area projection map of the Earth, in pink, overlaid on which is another map, in blue, shifted horizontally by 180° of longitude and inverted about the equator with respect to latitude. This map allows the antipodes of any point on the Earth to be easily located.
Noon at the one place is midnight at the other (although daylight saving and irregularly-shaped time zones affect this in most places); seasonally, the longest day at one point corresponds to the shortest day at the other, and midwinter at one point is contemporaneous with midsummer at the other.
In the calculation of days and nights, midnight on the one side may be regarded as corresponding to the noon either of the previous or of the following day. If a voyager sails eastward, and thus anticipates the sun, his dating will be twelve hours in advance, while the reckoning of another who has been sailing westward will be as much in arrears.
There will thus be a difference of twenty-four hours between the two when they meet. To avoid the confusion of dates which would thus arise, it is necessary to determine a meridian at which dates should be brought into agreement, known as the International Date Line.
The infamous Bermuda Triangle, known for macabre events and unexplainaed disappearances, encompasses a region of the west Atlantic ocean of the coast of the United States.
The triangle is roughly defined by three points: Miami, Florida, Puerto Rico and the island of Bermuda (the northern apex).
This region of claims some of the deepest water in the world's oceans. While many of the mysterious events have had explaination, some have not.
The antipodal postion (opposite side) of the Bermuda Triangle is located in the Indian Ocean and includes a majority of the Western Australian coastline from approximately.
Thank you:Bermuda South - The other side of the Bermuda Triangle - Perth, Fremantle and Rottnest Island Western Australia
What u think about Bermuda triangle, it's the biggest dimension of time in this world, isn't it? wanna share all your opinion...
If i compare Black hole in galaxy and Triangle on our world has affect dimension of time in universe or just fortuity...
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 deformation of spacetime caused by a very compact mass. Around a black hole there is an undetectable surface which marks the point of no return, called an event horizon. It is called "black" because it absorbs all the light that hits 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 the Milky Way galaxy.
In 1915, Albert Einstein developed his general theory of relativity, having earlier shown that gravity does influence light's motion. A few months later, Karl Schwarzschild gave the solution for the gravitational field of a point mass and a spherical mass, showing that a black hole could theoretically exist. The Schwarzschild radius is now known to be the radius of the event horizon of a non-rotating black hole, but this was not well understood then and Schwarzschild himself thought it was not physical. Johannes Droste, a student of Hendrik Lorentz, independently gave the same solution for the point mass a few months after Schwarzschild and wrote more extensively about its properties.
In 1930, astrophysicist Subrahmanyan Chandrasekhar calculated, using general relativity, that a non-rotating body of electron-degenerate matter above 1.44 solar masses (the Chandrasekhar limit) would collapse. His arguments were opposed by Arthur Eddington, who believed that something would inevitably stop the collapse.
Eddington was partly correct: a white dwarf slightly more massive than the Chandrasekhar limit will collapse into a neutron star, which is itself stable because of the Pauli exclusion principle. But in 1939, Robert Oppenheimer and others predicted that stars above approximately three solar masses (the Tolman-Oppenheimer-Volkoff limit) would collapse into black holes for the reasons presented by Chandrasekhar.
Oppenheimer and his co-authors used Schwarzschild's system of coordinates (the only coordinates available in 1939), which produced mathematical singularities at the Schwarzschild radius, in other words some of the terms in the equations became infinite at the Schwarzschild radius. This was interpreted as indicating that the Schwarzschild radius was the boundary of a bubble in which time stopped.
This is a valid point of view for external observers, but not for infalling observers. Because of this property, the collapsed stars were called "frozen stars," because an outside observer would see the surface of the star frozen in time at the instant where its collapse takes it inside the Schwarzschild radius.
This is a known property of modern black holes, but it must be emphasized that the light from the surface of the frozen star becomes redshifted very fast, turning the black hole black very quickly.
Many physicists could not accept the idea of time standing still at the Schwarzschild radius, and there was little interest in the subject for over 20 years.
The no hair theorem states that, once it achieves a stable condition after formation, a black hole has only three independent physical properties: mass, charge, and angular momentum. Any two black holes that share the same values for these properties, or parameters, are classically indistinguishable.
These properties are special because they are visible from outside the black hole. For example, a charged black hole repels other like charges just like any other charged object. Similarly, the total mass inside a sphere containing a black hole can be found by using the gravitational analog of Gauss's law, the ADM mass, far away from the black hole.
Likewise, the angular momentum can be measured from far away using frame dragging by the gravitomagnetic field.
When a black hole swallows any form of matter, its horizon oscillates like a stretchy membrane with friction, a dissipative system, until it reaches a simple final state (see membrane paradigm).
Similarly, any information about the charge distribution of the matter is lost as the field is evenly distributed along the event horizon as if the black hole was acting like a conducting sphere with a definite resistivity. This is different from other field theories like electromagnetism, which does not have any friction or resistivity at the microscopic level, because they are time reversible.
Because the black hole eventually achieves a stable state with only three parameters, there is no way to avoid losing information about the initial conditions: The gravitational and electric fields of the black hole give very little information about what went in.
The information that is lost includes every quantity that cannot be measured far away from the black hole horizon, including the total baryon number, lepton number, and all the other nearly conserved pseudo-charges of particle physics. This behavior is so puzzling, that it has been called the black hole information loss paradox