"as a lifeboat. He is attacked by manifestations of Corrick and a resurrected Weir. Miller fights them off and detonates the explosives, sacrificing himself. The gravity drive activates, pulling the ship's rear section into a black hole. Starck and Cooper enter stasis, beside a comatose Justin, and wait to be rescued. Seventy-two days later, the forward section of the ""Event Horizon"" is boarded by a rescue party, who discover the remaining crew still in stasis. A newly awakened Starck sees Weir posing as one of the rescuers, then wakes up screaming and is comforted by Cooper. As Cooper restrains the"
"to cover the horizon and thermalize into a Planck length-thick membrane. A complete description of event horizons is expected to, at minimum, require a theory of quantum gravity. One such candidate theory is M-theory. Another such candidate theory is loop quantum gravity. Event horizon In general relativity, an event horizon (EH) is a region in spacetime beyond which events cannot affect an outside observer. In layman's terms, it is defined as the shell of ""points of no return"", i.e., the boundary at which the gravitational pull of a massive object becomes so great as to make escape impossible. An event"
"horizon but there is an additional surface outside the event horizon named the ""ergosurface"" given by formula_11 in Boyer–Lindquist coordinates, which can be intuitively characterized as the sphere where ""the rotational velocity of the surrounding space"" is dragged along with the velocity of light. Within this sphere the dragging is greater than the speed of light, and any observer/particle is forced to co-rotate. The region outside the event horizon but inside the surface where the rotational velocity is the speed of light, is called the ""ergosphere"" (from Greek ""ergon"" meaning ""work""). Particles falling within the ergosphere are forced to rotate"
"a wide geographical extent that are used in stratigraphic correlation. Layers of tuff (lithified volcanic ash) are often used for this purpose. An event horizon is a bed that marks a geological event, such as an earthquake or a meteorite impact. It is the basic unit used in event stratigraphy. Horizon (geology) In geology, a horizon refers to either a bedding surface where there is marked change in the lithology within a sequence of sedimentary or volcanic rocks, or a distinctive layer or thin bed with a characteristic lithology or fossil content within a sequence. In the interpretation of seismic"
"object is most likely a black hole—a region of space with a gravitational field that is strong enough to prevent the escape of electromagnetic radiation from the interior. The boundary of this region is called the event horizon and has an effective radius called the Schwarzschild radius, which is about for Cygnus X-1. Anything (including matter and photons) that passes through this boundary is unable to escape. Evidence of just such an event horizon may have been detected in 1992 using ultraviolet (UV) observations with the High Speed Photometer on the Hubble Space Telescope. As self-luminous clumps of matter spiral"
"astrophysicists searching for black holes must generally rely on indirect observations. For example, a black hole's existence can sometimes be inferred by observing its gravitational interactions with its surroundings. The Event Horizon Telescope (EHT), however, run by MIT's Haystack Observatory, is an attempt to directly observe the immediate environment of the event horizon of Sagittarius A*, the black hole at the centre of the Milky Way, and to produce a silhouetted image of it. The first such image may appear as early as 2018. In 2015, the EHT managed to detect magnetic fields just outside the event horizon of Sagittarius"
"spin and/or electric charge, the radius is smaller, until an extremal black hole could have an event horizon close to The defining feature of a black hole is the appearance of an event horizon—a boundary in spacetime through which matter and light can only pass inward towards the mass of the black hole. Nothing, not even light, can escape from inside the event horizon. The event horizon is referred to as such because if an event occurs within the boundary, information from that event cannot reach an outside observer, making it impossible to determine if such an event occurred. As"
"own clocks, which appear to them to tick normally, they cross the event horizon after a finite time without noting any singular behaviour; in classical General Relativity, it is impossible to determine the location of the event horizon from local observations, due to Einstein's equivalence principle. The shape of the event horizon of a black hole is always approximately spherical. For non-rotating (static) black holes the geometry of the event horizon is precisely spherical, while for rotating black holes the event horizon is oblate. At the center of a black hole, as described by general relativity, lies a gravitational singularity,"
"Circumhorizontal arc A circumhorizontal arc is an optical phenomenon that belongs to the family of ice halos formed by the refraction of sun- or moonlight in plate-shaped ice crystals suspended in the atmosphere, typically in cirrus or cirrostratus clouds. In its full form, the arc has the appearance of a large, brightly spectrum-coloured band (red being the topmost colour) running parallel to the horizon, located far below the Sun or Moon. The distance between the arc and the Sun or Moon is twice as far as the common 22-degree halo. Often, when the halo-forming cloud is small or patchy, only"
"The boundary past which events cannot ever be observed is an event horizon, and it represents the maximum extent of the particle horizon. The criterion for determining whether a particle horizon for the universe exists is as follows. Define a comoving distance ""d"" as In this equation, ""a"" is the scale factor, ""c"" is the speed of light, and ""t"" is the age of the Universe. If (i.e., points arbitrarily as far away as can be observed), then no event horizon exists. If , a horizon is present. Examples of cosmological models without an event horizon are universes dominated by"
"matter or by radiation. An example of a cosmological model with an event horizon is a universe dominated by the cosmological constant (a de Sitter universe). A calculation of the speeds of the cosmological event and particle horizons was given in a paper on the FLRW cosmological model, approximating the Universe as composed of non-interacting constituents, each one being a perfect fluid. If a particle is moving at a constant velocity in a non-expanding universe free of gravitational fields, any event that occurs in that Universe will eventually be observable by the particle, because the forward light cones from these"
"the cosmological horizon in an Accelerating universe never reaches the observer, because the space in between the observer and the object is expanding too rapidly. The observable universe is one ""causal patch"" of a much larger unobservable universe; other parts of the Universe cannot communicate with Earth yet. These parts of the Universe are outside our current cosmological horizon. In the standard hot big bang model, without inflation, the cosmological horizon moves out, bringing new regions into view. Yet as a local observer sees such a region for the first time, it looks no different from any other region of"
"an event horizon. Event horizon: An awareness of plans and events in time and space. It includes an awareness of what has happened (useful for diagnosis, to achieve SA, to frame situations). It also includes prognosis, an awareness of what might happen next. That includes on the one hand an awareness both of what might occur based on diagnosis and the current situation, and on the other hand on an awareness of current plans and intentions. All four aspects may drive SA processes. Being aware of the status of particular objects (cues), one might infer that particular situations are on-going,"
"event horizon, that they start off as modes with a wavelength much shorter than the Planck length. Since the laws of physics at such short distances are unknown, some find Hawking's original calculation unconvincing. The trans-Planckian problem is nowadays mostly considered a mathematical artifact of horizon calculations. The same effect occurs for regular matter falling onto a white hole solution. Matter which falls on the white hole accumulates on it, but has no future region into which it can go. Tracing the future of this matter, it is compressed onto the final singular endpoint of the white hole evolution, into"
"and angular momentum. The outer surface encloses the ergosphere and has a shape similar to a flattened sphere. The inner surface marks the ""radius of no return"" also called the ""event horizon""; objects passing through this radius can never again communicate with the world outside that radius. However, neither surface is a true singularity, since their apparent singularity can be eliminated in a different coordinate system. Objects between these two horizons must co-rotate with the rotating body, as noted above; this feature can be used to extract energy from a rotating black hole, up to its invariant mass energy, ""Mc""."
"Black hole A black hole is a region of spacetime exhibiting such strong gravitational effects that nothing—not even particles and electromagnetic radiation such as light—can escape from inside it. The theory of general relativity predicts that a sufficiently compact mass can deform spacetime to form a black hole. The boundary of the region from which no escape is possible is called the event horizon. Although the event horizon has an enormous effect on the fate and circumstances of an object crossing it, no locally detectable features appear to be observed. In many ways a black hole acts like an ideal"
"Ergosphere The ergosphere is a region located outside a rotating black hole's outer event horizon. Its name was proposed by Remo Ruffini and John Archibald Wheeler during the Les Houches lectures in 1971 and 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 this region. The ergosphere touches the event horizon at the poles of a rotating black hole and extends to a greater radius at the equator. With a low spin of the central mass the shape of the ergosphere can be approximated"
"Oort cloud The Oort cloud (), named after the Dutch astronomer Jan Oort, sometimes called the Öpik–Oort cloud, is a theoretical cloud of predominantly icy planetesimals proposed to surround the Sun at distances ranging from 2,000 to 200,000 AU (0.03 to 3.2 light-years). It is divided into two regions: a disc-shaped inner Oort cloud (or Hills cloud) and a spherical outer Oort cloud. Both regions lie beyond the heliosphere and in interstellar space. The Kuiper belt and the scattered disc, the other two reservoirs of trans-Neptunian objects, are less than one thousandth as far from the Sun as the Oort"
"from the photon sphere, any light that crosses the photon sphere on an inbound trajectory will be captured by the black hole. Hence any light that reaches an outside observer from the photon sphere must have been emitted by objects between the photon sphere and the event horizon. Rotating black holes are surrounded by a region of spacetime in which it is impossible to stand still, called the ergosphere. This is the result of a process known as frame-dragging; general relativity predicts that any rotating mass will tend to slightly ""drag"" along the spacetime immediately surrounding it. Any object near"
"event horizons towards the other one. This protrusion extends longer and narrower until it meets the protrusion from the other black hole. At this point in time the event horizon has a very narrow X-shape at the meeting point. The protrusions are drawn out into a thin thread. The meeting point expands to a roughly cylindrical connection called a ""bridge"". Simulations had not produced any event horizons with toroidal topology (ring-shaped). Some researchers suggested that it would be possible if, for example, several black holes in the same nearly-circular orbit coalesce. An unexpected result can occur with binary black holes"
"been discovered. The proposed field and its ""quanta"" (the subatomic particles related to it) have been named the inflaton. If this field did not exist, scientists would have to propose a different explanation for all the observations that strongly suggest a metric expansion of space has occurred, and is still occurring (much more slowly) today. An expanding universe generally has a cosmological horizon, which, by analogy with the more familiar horizon caused by the curvature of Earth's surface, marks the boundary of the part of the Universe that an observer can see. Light (or other radiation) emitted by objects beyond"
"general, the conformal time at a certain time is given in terms of the scale factor formula_1 by, or The particle horizon is the boundary between two regions at a point at a given time: one region defined by events that have already been observed by an observer, and the other by events which cannot be observed ""at that time"". It represents the furthest distance from which we can retrieve information from the past, and so defines the observable universe. Hubble radius, Hubble sphere, Hubble volume, or Hubble horizon is a conceptual horizon defining the boundary between particles that are"
"experiments to falsify quantized inertia were funded by DARPA with a grant of 1.3 million dollars over a four-year study. There is an event horizon in the universe where light (and therefore any information) cannot and will never be able to reach an object, because the cosmic acceleration outpaces the speed of light: the cosmological comoving horizon. If the object accelerates in one direction, a similar event horizon is produced: the Rindler horizon. Anything beyond these horizons is outside the observable universe, and therefore can't affect the object at the center of the Rindler space. The Rindler event horizon is"
"Cosmologists often work with a given space-like slice of spacetime called the comoving coordinates. The section of spacetime which can be observed is the backward light cone, which delimits the cosmological horizon. The cosmological horizon (also called the particle horizon or the light horizon) is the maximum distance from which particles can have traveled to the observer in the age of the Universe. This horizon represents the boundary between the observable and the unobservable regions of the Universe. The existence, properties, and significance of a cosmological horizon depend on the particular cosmological model. An important parameter determining the future evolution"
"like an inside-out Schwarzschild black hole—each object is surrounded by a spherical event horizon. Once the other object has fallen through this horizon it can never return, and even light signals it sends will never reach the first object (at least so long as the space continues to expand exponentially). In the approximation that the expansion is exactly exponential, the horizon is static and remains a fixed physical distance away. This patch of an inflating universe can be described by the following metric: This exponentially expanding spacetime is called a de Sitter space, and to sustain it there must be"
"the black hole interior region will have a future light cone that remains in this region (such that any world line within the event's future light cone will eventually hit the black hole singularity, which appears as a hyperbola bounded by the two black hole horizons), and any event inside the white hole interior region will have a past light cone that remains in this region (such that any world line within this past light cone must have originated in the white hole singularity, a hyperbola bounded by the two white hole horizons). Note that although the horizon looks as"
"orbit of Neptune lies the area of the ""trans-Neptunian region"", with the doughnut-shaped Kuiper belt, home of Pluto and several other dwarf planets, and an overlapping disc of scattered objects, which is tilted toward the plane of the Solar System and reaches much further out than the Kuiper belt. The entire region is still largely unexplored. It appears to consist overwhelmingly of many thousands of small worlds—the largest having a diameter only a fifth that of Earth and a mass far smaller than that of the Moon—composed mainly of rock and ice. This region is sometimes described as the ""third"
"white hole interior regions are also a pair of straight lines at 45 degrees, reflecting the fact that a light ray emitted at the horizon in a radial direction (aimed outward in the case of the black hole, inward in the case of the white hole) would remain on the horizon forever. Thus the two black hole horizons coincide with the boundaries of the future light cone of an event at the center of the diagram (at ""T""=""X""=0), while the two white hole horizons coincide with the boundaries of the past light cone of this same event. Any event inside"
"a point where its ""peculiar velocity"" towards us exceeds the expansion velocity away from us (these two notions of velocity are also discussed in Comoving distance#Uses of the proper distance). The current distance to this cosmological event horizon is about 16 billion light-years, meaning that a signal from an event happening at present would eventually be able to reach us in the future if the event was less than 16 billion light-years away, but the signal would never reach us if the event was more than 16 billion light-years away. Apparent superluminal motion is observed in many radio galaxies, blazars,"
"which a particle passes through the event horizon and dwells inside it forever. Intermediate between the case of Mercury and the case of an object falling past the event horizon, there are exotic possibilities such as knife-edge orbits, in which the satellite can be made to execute an arbitrarily large number of nearly circular orbits, after which it flies back outward. The group of isometries of the Schwarzschild metric is the subgroup of the ten-dimensional Poincaré group which takes the time axis (trajectory of the star) to itself. It omits the spatial translations (three dimensions) and boosts (three dimensions). It"
"the resulting shadow will sweep through a region of space, only passing through any particular location in the region for a fixed interval of time. As viewed from such a location, this shadowing event is known as an eclipse. Typically the cross-section of the objects involved in an astronomical eclipse are roughly disk shaped. The region of an object's shadow during an eclipse is divided into three parts: A total eclipse occurs when the observer is within the umbra, an annular eclipse when the observer is within the antumbra, and a partial eclipse when the observer is within the penumbra."
"Hubble volume In cosmology, a Hubble volume or Hubble sphere is a spherical region of the observable universe surrounding an observer beyond which objects recede from that observer at a rate greater than the speed of light due to the expansion of the Universe. The Hubble volume is approximately equal to 10 cubic light years. The proper radius of a Hubble sphere (known as the Hubble radius or the Hubble length) is formula_1, where formula_2 is the speed of light and formula_3 is the Hubble constant. The surface of a Hubble sphere is called the ""microphysical horizon"", the ""Hubble surface"","
"A second example is de Sitter space which contains an event horizon. In this case the temperature formula_1 is proportional to the Hubble parameter formula_5, i.e. formula_6. Gibbons–Hawking effect The Gibbons–Hawking effect is the statement that a temperature can be associated to each solution of the Einstein field equations that contains a causal horizon. It is named after Gary Gibbons and Stephen Hawking. The term ""causal horizon"" does not necessarily refer to event horizons only, but could also stand for the horizon of the visible universe, for instance. For example, Schwarzschild spacetime contains an event horizon and so can be"