Event Horizon Deutsch "event horizon" auf Deutsch
Weir erläutert erst nach der Ankunft Captain Miller und dessen Mannschaft das Ziel des Unternehmens: Sie sollen die Event Horizon (deutsch: Ereignishorizont). Everything that crosses the event-horizon in direction of singularity has no chance to escape the eventhorizon and is stuck inside [ ] the black hole forever. Englisch-Deutsch-Übersetzungen für event horizon im Online-Wörterbuch science-planet.be (Deutschwörterbuch). Übersetzung im Kontext von „the event horizon“ in Englisch-Deutsch von Reverso Context: The boundary of the region from which no escape is possible is. Übersetzung im Kontext von „an event horizon“ in Englisch-Deutsch von Reverso Context: We need to establish an event horizon without the vortex.
In the case of a horizon perceived by a uniformly accelerating observer in empty space, the horizon seems to remain a fixed distance from the observer no matter how its surroundings move.
Varying the observer's acceleration may cause the horizon to appear to move over time, or may prevent an event horizon from existing, depending on the acceleration function chosen.
The observer never touches the horizon and never passes a location where it appeared to be. In the case of a horizon perceived by an occupant of a de Sitter universe , the horizon always appears to be a fixed distance away for a non-accelerating observer.
It is never contacted, even by an accelerating observer. One of the best-known examples of an event horizon derives from general relativity's description of a black hole , a celestial object so dense that no nearby matter or radiation can escape its gravitational field.
Often, this is described as the boundary within which the black hole's escape velocity is greater than the speed of light.
However, a more detailed description is that within this horizon, all lightlike paths paths that light could take and hence all paths in the forward light cones of particles within the horizon, are warped so as to fall farther into the hole.
Once a particle is inside the horizon, moving into the hole is as inevitable as moving forward in time - no matter what direction the particle is traveling, and can actually be thought of as equivalent to doing so, depending on the spacetime coordinate system used.
The surface at the Schwarzschild radius acts as an event horizon in a non-rotating body that fits inside this radius although a rotating black hole operates slightly differently.
The Schwarzschild radius of an object is proportional to its mass. Theoretically, any amount of matter will become a black hole if compressed into a space that fits within its corresponding Schwarzschild radius.
For the mass of the Sun this radius is approximately 3 kilometers and for the Earth it is about 9 millimeters.
In practice, however, neither the Earth nor the Sun have the necessary mass and therefore the necessary gravitational force, to overcome electron and neutron degeneracy pressure.
The minimal mass required for a star to be able to collapse beyond these pressures is the Tolman—Oppenheimer—Volkoff limit , which is approximately three solar masses.
According to the fundamental gravitational collapse models  , an event horizon forms before the singularity of black hole.
If all the stars in the Milky Way would gradually aggregate towards the galactic center while keeping their proportionate distances from each other, they will all fall within their joint Schwarzschild radius long before they are forced to collide.
Black hole event horizons are widely misunderstood. Common, although erroneous, is the notion that black holes "vacuum up" material in their neighborhood, where in fact they are no more capable of seeking out material to consume than any other gravitational attractor.
As with any mass in the universe, matter must come within its gravitational scope for the possibility to exist of capture or consolidation with any other mass.
Equally common is the idea that matter can be observed falling into a black hole. This is not possible. Astronomers can detect only accretion disks around black holes, where material moves with such speed that friction creates high-energy radiation which can be detected similarly, some matter from these accretion disks is forced out along the axis of spin of the black hole, creating visible jets when these streams interact with matter such as interstellar gas or when they happen to be aimed directly at Earth.
Furthermore, a distant observer will never actually see something reach the horizon. Instead, while approaching the hole, the object will seem to go ever more slowly, while any light it emits will be further and further redshifted.
The black hole event horizon is teleological in nature, meaning that we need to know the entire future space-time of the universe to determine the current location of the horizon, which is essentially impossible.
Because of the purely theoretical nature of the event horizon boundary, the traveling object does not necessarily experience strange effects and does, in fact, pass through the calculatory boundary in a finite amount of proper time.
A misconception concerning event horizons, especially black hole event horizons, is that they represent an immutable surface that destroys objects that approach them.
In practice, all event horizons appear to be some distance away from any observer, and objects sent towards an event horizon never appear to cross it from the sending observer's point of view as the horizon-crossing event's light cone never intersects the observer's world line.
Attempting to make an object near the horizon remain stationary with respect to an observer requires applying a force whose magnitude increases unboundedly becoming infinite the closer it gets.
In the case of the horizon around a black hole, observers stationary with respect to a distant object will all agree on where the horizon is.
While this seems to allow an observer lowered towards the hole on a rope or rod to contact the horizon, in practice this cannot be done.
The proper distance to the horizon is finite,  so the length of rope needed would be finite as well, but if the rope were lowered slowly so that each point on the rope was approximately at rest in Schwarzschild coordinates , the proper acceleration G-force experienced by points on the rope closer and closer to the horizon would approach infinity, so the rope would be torn apart.
If the rope is lowered quickly perhaps even in freefall , then indeed the observer at the bottom of the rope can touch and even cross the event horizon.
But once this happens it is impossible to pull the bottom of rope back out of the event horizon, since if the rope is pulled taut, the forces along the rope increase without bound as they approach the event horizon and at some point the rope must break.
Furthermore, the break must occur not at the event horizon, but at a point where the second observer can observe it. Assuming that the possible apparent horizon is far inside the event horizon, or there is none, observers crossing a black hole event horizon would not actually see or feel anything special happen at that moment.
In terms of visual appearance, observers who fall into the hole perceive the eventual apparent horizon as a black impermeable area enclosing the singularity.
Increasing tidal forces are also locally noticeable effects, as a function of the mass of the black hole. In realistic stellar black holes , spaghettification occurs early: tidal forces tear materials apart well before the event horizon.
However, in supermassive black holes , which are found in centers of galaxies, spaghettification occurs inside the event horizon.
A human astronaut would survive the fall through an event horizon only in a black hole with a mass of approximately 10, solar masses or greater.
A cosmic event horizon is commonly accepted as a real event horizon, whereas the description of a local black hole event horizon given by general relativity is found to be incomplete and controversial.
At present, it is expected by the Hawking radiation mechanism that the primary impact of quantum effects is for event horizons to possess a temperature and so emit radiation.
For black holes , this manifests as Hawking radiation , and the larger question of how the black hole possesses a temperature is part of the topic of black hole thermodynamics.
For accelerating particles, this manifests as the Unruh effect , which causes space around the particle to appear to be filled with matter and radiation.
According to the controversial black hole firewall hypothesis, matter falling into a black hole would be burned to a crisp by a high energy "firewall" at the event horizon.
An alternative is provided by the complementarity principle , according to which, in the chart of the far observer, infalling matter is thermalized at the horizon and reemitted as Hawking radiation, while in the chart of an infalling observer matter continues undisturbed through the inner region and is destroyed at the singularity.
An der Entstehung der Bilder insgesamt entstanden vier jeweils an einem Beobachtungstag waren an vier Tagen im April acht Teleskope beteiligt.
Die effektive Auflösung des Teleskops, die sich aus der Zusammenschaltung der Einzelteleskope ergibt, entspricht dem weitesten Abstand der Beobachtungsstationen Die entspricht nur der Summe der beteiligten Teleskope.
Inzwischen ist das EHT Netzwerk noch erweitert worden. Die sehr umfangreichen Daten viele Petabytes, jedes der acht Teleskope lieferte täglich rund Terabyte ,  deren physischer Transport zum Beispiel aus der Antarktis ein besonderes Problem darstellte, mussten dann zeitlich und bezüglich der Teleskopausrichtung exakt verglichen werden.
Die Datenauswertung erfolgte am Max-Planck-Institut für Radioastronomie und am MIT-Haystack-Observatorium und zog sich zwei Jahre hin, nicht nur wegen der Zusammensetzung der Daten der verschiedenen Teleskope, sondern auch weil die beteiligten Wissenschaftler sichergehen wollten, dass sie am Ende der komplexen Prozedur der Bilderstellung wirklich eine direkte Aufnahme eines Schwarzen Lochs vor sich hatten.
Beteiligt waren über Wissenschaftler aus 20 Nationen und von 59 Institutionen. An den vier Beobachtungstagen am 5. April herrschte ein Fenster guten Wetters auf allen acht Stationen.
Cam scurt filmul, cred ca subiectul merita ceva mai mult timp. In rest, mi se pare a fi un SF cu accente de horror chiar mai bun decat unele dintre horror-urile actuale.
Acelasi lucru il pot spune si despre efectele speciale. Excelent filmul! Efectele vizuale inca sunt la zi.
Recomand filmul fanii genului. Cand am vazut acest film la cinematograf in ,am fost impresionata de efectele speciale,de tensiunea in care se desfasoara actiunea,de originalitatea ideeii.
Actorii sunt dintre cei mai buni si isi fac bine treaba,elementele horror amplifica tensiune dar echilibrat,fara exagerari. Filmul poate fi savurat si acum de iubitorii genului.
Dan Gerose pe 30 Ianuarie Mie mi-a placut. Si efectele sunt OK si actiunea. Luci'S pe 11 Martie Pai asta a fost si intentia.
Sa fie lugubru, horror. Da nu prea le-a iesit. Nu te lasa inselat de cadrul SF. Desi mie mi-a placut cat de cat tocmai pt ca e SF.
Ilila pe 30 Ianuarie Prea lugubru! Direct, fara sa uzez inutil tastele: un film SF de duzina, cu un scenariu ultra-simplist si final aproape previzibil, potrivit cu calapodul sau formula standard a filmelor horror.
Probabil tocmai acest "metisaj" e ceea ce il depuncteaza in randul specatorilor de science fiction si eventual il ridica in categoria iubitorilor de horror.
Oricum ar fi situatia, Event Horizon se prezinta intr-o nuanta de fictiune cu umbre discrete de stiinta popularizata lucru bun, de apreciat si everntual educativ.
Cu toate acestea, inspiratia scenariului vine fara urma de jena din multe alte pelicule similare, sub forma unei mutatii lipsite de pretentii dar care are totusi Matrix pe 30 Ianuarie