In astrophysics, an extreme mass ratio inspiral (EMRI) is the orbit of a relatively light object around a much heavier (by a factor 10,000 or more) object, that gradually decays due the emission of gravitational waves.
 Such systems are likely to be found in the centers of galaxies, where stellar mass compact objects, such as stellar black holes and neutron stars, may be found orbiting a supermassive black hole.
 In the case of a black hole in orbit around another black hole this is an extreme mass ratio binary black hole.
 The term EMRI is sometimes used as a shorthand to denote the emitted gravitational waveform as well as the orbit itself.
The Penrose process (also called Penrose mechanism) is a process theorised by Roger Penrose wherein energy can be extracted from a rotating black hole.
 That extraction is made possible because the rotational energy of the black hole is located not inside the event horizon of the black hole, but on the outside of it in a region of the Kerr spacetime called the ergosphere, a region in which a particle is necessarily propelled in locomotive concurrence with the rotating spacetime.
 All objects in the ergosphere become dragged by a rotating spacetime.
 In the process, a lump of matter enters into the ergosphere of the black hole, and once it enters the ergosphere, it is forcibly split into two parts.
 For example, the matter might be made of two parts that separate by firing an explosive or rocket which pushes its halves apart.
 The momentum of the two pieces of matter when they separate can be arranged so that one piece escapes from the black hole (it "escapes to infinity"), whilst the other falls past the event horizon into the black hole.
 With careful arrangement, the escaping piece of matter can be made to have greater mass-energy than the original piece of matter, and the infalling piece has negative mass-energy.
 Although momentum is conserved the effect is that more energy can be extracted than was originally provided, the difference being provided by the black hole itself.
 In summary, the process results in a slight decrease in the angular momentum of the black hole, which corresponds to a transference of energy to the matter.
 The momentum lost is converted to energy extracted.
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 by an oblated spheroid, while with higher spins it resembles a pumpkin-shape.
 The equatorial (maximum) radius of an ergosphere corresponds to the Schwarzschild radius of a non-rotating black hole; the polar (minimum) radius can be as little as half the Schwarzschild radius (the radius of a non-rotating black hole) in the case that the black hole is rotating maximally (at higher rotation rates the black hole could not have formed).
In general relativity, the de Sitter–Schwarzschild solution describes a black hole in a causal patch of de Sitter space.
 Unlike a flat-space black hole, there is a largest possible de Sitter black hole, which is the Nariai spacetime.
 The Nariai limit has no singularities, the cosmological and black hole horizons have the same area, and they can be mapped to each other by a discrete reflection symmetry in any causal patch.
In black hole theory, the black hole membrane paradigm is a simplified model, useful for visualising and calculating the effects predicted by quantum mechanics for the exterior physics of black holes, without using quantum-mechanical principles or calculations.
 It models a black hole as a thin, classically radiating surface (or membrane) at or vanishingly close to the black hole's event horizon.
 This approach to the theory of black holes was created by Kip S. Thorne, R. H. Price and D. A. Macdonald.
"The Wonderful Thing About Tiggers" is the theme song and personal anthem of Tigger, a fictional tiger from the children's book series Winnie-the-Pooh.
 Although Tigger's birthday is believed to be in October 1928, the year that "The House at Pooh Corner" was first published, on Tigger-related merchandise, Disney often indicates Tigger's birth year as 1968, a reference to the first year that Tigger appeared in a Disney production, "Winnie the Pooh and the Blustery Day".
 That was also the same instance when Tigger first sang this song.
 The song is repeated in Disney's 1974 release "Winnie the Pooh and Tigger Too!
", The Many Adventures of Winnie the Pooh ride and then again in the 1977 release "The Many Adventures of Winnie the Pooh".
 "The Wonderful Thing About Tiggers" opens up the 2000 release of "The Tigger Movie".
 In 1974, Paul Winchell earned a Grammy for his rendition of the song.
The Black Hole is a 1979 American science fiction film directed by Gary Nelson and produced by Walt Disney Productions.
 The film stars Maximilian Schell, Robert Forster, Joseph Bottoms, Yvette Mimieux, Anthony Perkins, and Ernest Borgnine, while the voices of the main robot characters are provided by Roddy McDowall and Slim Pickens (both unbilled).
 The music for the film was composed by John Barry.
 It was the first film from Walt Disney Productions to receive a PG rating.
 The film was released on December 18, 1979 in the United Kingdom and on December 21, 1979 in the United States.
M33 X-7 is a black hole binary system in the galaxy M33.
 The system is made up of a stellar mass black hole and a companion star.
 M33 X-7 is the largest known stellar black hole with an estimated mass of 15.65 times that of the Sun (M ).
 The total mass of the system is estimated to be around 85.7 M , which would make it the most massive black hole binary system.
The Tigger Movie is a 2000 American animated musical comedy-drama film written and directed by Jun Falkenstein from a story by Eddie Guzelian.
 Part of the "Winnie-the-Pooh" series, this film features Pooh's friend Tigger searching for his family tree and other Tiggers like himself.
V404 Cygni is a microquasar and a binary system consisting of a black hole with a mass of about and an early K companion star of mass slightly smaller than the Sun in the constellation of Cygnus.
 The star and the black hole orbit each other every at fairly close range.
 Due to their proximity and the intense gravity of the black hole, the companion star loses mass to an accretion disk around the black hole and ultimately to the black hole itself.

Question: The Black Hole and The Tigger Movie are both what type of media?
Answer: film