How do you know who reads what on here? Are you psychic? Are you in every body's home and mind? I don't think so. Some people who ask questions would like an answer and have the time and patience to read every answer. We don't cut and paste. I only wish I knew how to.
Carlos Irwin Estevez (born September 3, 1965), better known by his stage name Charlie Sheen, is an American film and television actor. He is the youngest son of actor Martin Sheen.
His character roles in films have included Chris Taylor in the 1986 Vietnam War drama Platoon, Jake Kesey in the 1986 film The Wraith, and Bud Fox in the 1987 film Wall Street. His career has also included more comedic films such as Major League, the Hot Shots! films, and Scary Movie 3 and Scary Movie 4. On television, Sheen is known for his roles on two sitcoms: as Charlie Crawford on Spin City and as Charlie Harper on Two and a Half Men. In 2010, Sheen was the highest paid actor on television, earning US$1.8 million per episode of Two and a Half Men.[2]
Sheen's personal life has also made headlines, including reports about alcohol and drug abuse and marital problems as well as allegations of domestic violence. He was fired from his role on Two and a Half Men by CBS and Warner Bros. on March 7, 2011. Sheen subsequently announced a nationwide tour.[3]
A neutron star is a type of stellar remnant that can result from the gravitational collapse of a massive star during a Type II, Type Ib or Type Ic supernova event. Such stars are composed almost entirely of neutrons, which are subatomic particles without electrical charge and with a slightly larger mass than protons. Neutron stars are very hot and are supported against further collapse by quantum degeneracy pressure due to the Pauli exclusion principle. This principle states that no two neutrons (or any other fermionic particles) can occupy the same place and quantum state simultaneously.
A typical neutron star has a mass between 1.35 and about 2.0 solar masses,[1] with a corresponding radius of about 12 km if the Akmal-Pandharipande-Ravenhall equation of state (APR EOS) is used.[2][3] In contrast, the Sun's radius is about 60,000 times that. Neutron stars have overall densities predicted by the APR EOS of 3.7×1017 to 5.9×1017 kg/m3 (2.6×1014 to 4.1×1014 times the density of the Sun),[4] which compares with the approximate density of an atomic nucleus of 3×1017 kg/m3.[5] The neutron star's density varies from below 1×109 kg/m3 in the crust, increasing with depth to above 6×1017 or 8×1017 kg/m3 deeper inside (denser than an atomic nucleus).[6] This density is approximately equivalent to the mass of the entire human population compressed to the size of a sugar cube.[7]
In general, compact stars of less than 1.44 solar masses – the Chandrasekhar limit – are white dwarfs, and above 2 to 3 solar masses (the Tolman–Oppenheimer–Volkoff limit), a quark star might be created; however, this is uncertain. Gravitational collapse will usually occur on any compact star between 10 and 25 solar masses and produce a black hole.
A black hole is a region of spacetime from which nothing, not even light, can escape.[1] The theory of general relativity predicts that a sufficiently compact mass will deform spacetime to form a black hole. Around a black hole there is a mathematically defined surface called an event horizon that marks the point of no return. It is called "black" because it absorbs all the light that hits the horizon, reflecting nothing, just like a perfect black body in thermodynamics.[2] Quantum mechanics predicts that black holes emit radiation like a black body with a finite temperature. This temperature is inversely proportional to the mass of the black hole, making it difficult to observe this radiation for black holes of stellar mass or greater.
Objects whose gravity field is too strong for light to escape were first considered in the 18th century by John Michell and Pierre-Simon Laplace. The first modern solution of general relativity that would characterize a black hole was found by Karl Schwarzschild in 1916, although its interpretation as a region of space from which nothing can escape was not fully appreciated for another four decades. Long considered a mathematical curiosity, it was during the 1960s that theoretical work showed black holes were a generic prediction of general relativity. The discovery of neutron stars sparked interest in gravitationally collapsed compact objects as a possible astrophysical reality.