Neutron Stars, The Extremes of Attention Tweet
Of the many stars in the sky, there is one star who attracted the attention of scientists until now. Neutron star, so namnya, attracting the attention of scientists because the condition is very extreme.
Imagine. The star that has a diameter of only about 25 km has a mass about 1.4 solar masses, equivalent to half a million times the mass of the earth. Thus the gravitational field at the surface of these stars range from 200 billion times stronger than Earth's gravitational field at the surface.
The gravitational field of this magnitude would be able to crush objects that exist on the surface and the atoms making up the object. As an illustration, a person who falls into the surface of neutron stars will hit the surface with a speed of 150,000 km per second, or energy generated by the collision is equivalent to 100 megatons of nuclear explosions. Not stop there. A neutron star magnetic field can have up to 100 gigatesla. The magnetic field of that size could destroy all the information in all existing credit card over the surface of the earth, if the neutron star is placed in lunar orbit. For comparison, Earth's magnetic field strength only about 60 mikrotesla.
The process of star formation Neutrons
neutron stars originated from ordinary stars that have run out of nuclear fuel. The stars are visible at night have equilibrium between gravity trying to wrinkling and styles of star due to nuclear explosions are trying to break the stellar matter.
When the fuel runs out, the force of gravity began to work and pass a series of nuclear fission and fusion reactions followed by the supernova, a tremendous explosion that emits bright light to beat all the light in galaxies where stars live.
The light comes from the energy release due to a drastic decrease in mass of the star (hukun conservation of energy, E = mc2). Believed that neutron stars originating from the star 15 to 30 times the size of the sun (however, this figure is constantly changing with the increasing accuracy of supernova simulation). Heavier stars will become black holes (black hole) while the lighter star will end up as white dwarfs (white dwarf) if they experienced a similar process. In addition, the law of conservation of momentum would drastically increase the star's rotation, an explanation of why the neutron star can rotate up to 600 revolutions per second.
From the information is known that the binding energy of nuclear fusion reactions that occur will be stopped if the material has become iron star. Thus there is accumulation of iron until the mass of the neutron star to 1.4 solar masses. Having reached this phase of the electron degeneracy style that has been able to resist the contraction forces of gravity begin to give up. Very strong gravity of pressure will trigger the URCA process, namely the process of combining protons and electrons into neutrons and neutrinos. Because neutrinos are very subtle, it is believed he interacts very little with the material and the star, after helping the process of supernovae, neutrinos will go. Tinggalah neutrons which in turn form a neutron star.
Structure Nuetron Stars
The force of gravity on the surface of neutron stars is very large, 200 billion times stronger than Earth's gravity. Together with the magnetic field of 100 gigatesla arising from neutron star rotation, this force could destroy the entire structure of the atom at the surface. Thus, only the neutron star surface is dominated by the nucleus (nuclei) of iron. If we get a little inside, we will find a great deal of pressure, so its density can reach 1 ton / cc. Nuclei heavier inhabit this area. In deeper water density to 400,000 tonnes / cc, a state which allows neutrons to move freely flowing out of the nucleus.
Deeper, we will discover what the researchers as a sequence of "paste-antipasta". This row starts on the density of about 1 million tons / cc, a place where the nucleons join like "meat-meatballs". More into the longer we'll see a form of "lasagna-antilasagna", "spaghetti-antispageti", as well as the so-called "Swiss cheese". In place of a density exceeding 280 million tons / cc may appear exotic particles such as condensate-pawn, hiperon-lambda, Isobars delta, as well as quark-gluon plasma. Despite these theoretical estimates are staggering, direct observations of neutron stars have not been fully able to provide support.
Research Guide
Relatively not too difficult to calculate the pressure, tightly-mass and radius of neutron stars, provided that the mass-meeting in central neutron star and neutron star equation of state of matter is known. The calculation is done using one solution to Einstein's equations of general relativity called the equation of Tolman-Oppenheimer-Volkoff. From here the moment of inertia of neutron stars can also be calculated. Currently, experimental observations began geared to measure the moment of inertia of neutron stars. The problem is: equation of state of matter that extreme-meeting is not known with certainty and the scientists can only rely on mathematical models.
Fortunately, experimental super-meeting materials can be done on the earth's surface through ion-heavy ion collisions, such as those conducted by physicists at the GSI Darmstadt, Germany, and at RHIC Brookhaven, USA. The results of this experiment can be used to improve models of equation of state before, so the observation of neutron stars can give accurate information about the mass density at the center of neutron stars. Eventually scientists will be able to predict accurately what is happening there and in the neutron star.
Of the many stars in the sky, there is one star who attracted the attention of scientists until now. Neutron star, so namnya, attracting the attention of scientists because the condition is very extreme.
Imagine. The star that has a diameter of only about 25 km has a mass about 1.4 solar masses, equivalent to half a million times the mass of the earth. Thus the gravitational field at the surface of these stars range from 200 billion times stronger than Earth's gravitational field at the surface.
The gravitational field of this magnitude would be able to crush objects that exist on the surface and the atoms making up the object. As an illustration, a person who falls into the surface of neutron stars will hit the surface with a speed of 150,000 km per second, or energy generated by the collision is equivalent to 100 megatons of nuclear explosions. Not stop there. A neutron star magnetic field can have up to 100 gigatesla. The magnetic field of that size could destroy all the information in all existing credit card over the surface of the earth, if the neutron star is placed in lunar orbit. For comparison, Earth's magnetic field strength only about 60 mikrotesla.
The process of star formation Neutrons
neutron stars originated from ordinary stars that have run out of nuclear fuel. The stars are visible at night have equilibrium between gravity trying to wrinkling and styles of star due to nuclear explosions are trying to break the stellar matter.
When the fuel runs out, the force of gravity began to work and pass a series of nuclear fission and fusion reactions followed by the supernova, a tremendous explosion that emits bright light to beat all the light in galaxies where stars live.
The light comes from the energy release due to a drastic decrease in mass of the star (hukun conservation of energy, E = mc2). Believed that neutron stars originating from the star 15 to 30 times the size of the sun (however, this figure is constantly changing with the increasing accuracy of supernova simulation). Heavier stars will become black holes (black hole) while the lighter star will end up as white dwarfs (white dwarf) if they experienced a similar process. In addition, the law of conservation of momentum would drastically increase the star's rotation, an explanation of why the neutron star can rotate up to 600 revolutions per second.
From the information is known that the binding energy of nuclear fusion reactions that occur will be stopped if the material has become iron star. Thus there is accumulation of iron until the mass of the neutron star to 1.4 solar masses. Having reached this phase of the electron degeneracy style that has been able to resist the contraction forces of gravity begin to give up. Very strong gravity of pressure will trigger the URCA process, namely the process of combining protons and electrons into neutrons and neutrinos. Because neutrinos are very subtle, it is believed he interacts very little with the material and the star, after helping the process of supernovae, neutrinos will go. Tinggalah neutrons which in turn form a neutron star.
Structure Nuetron Stars
The force of gravity on the surface of neutron stars is very large, 200 billion times stronger than Earth's gravity. Together with the magnetic field of 100 gigatesla arising from neutron star rotation, this force could destroy the entire structure of the atom at the surface. Thus, only the neutron star surface is dominated by the nucleus (nuclei) of iron. If we get a little inside, we will find a great deal of pressure, so its density can reach 1 ton / cc. Nuclei heavier inhabit this area. In deeper water density to 400,000 tonnes / cc, a state which allows neutrons to move freely flowing out of the nucleus.
Deeper, we will discover what the researchers as a sequence of "paste-antipasta". This row starts on the density of about 1 million tons / cc, a place where the nucleons join like "meat-meatballs". More into the longer we'll see a form of "lasagna-antilasagna", "spaghetti-antispageti", as well as the so-called "Swiss cheese". In place of a density exceeding 280 million tons / cc may appear exotic particles such as condensate-pawn, hiperon-lambda, Isobars delta, as well as quark-gluon plasma. Despite these theoretical estimates are staggering, direct observations of neutron stars have not been fully able to provide support.
Research Guide
Relatively not too difficult to calculate the pressure, tightly-mass and radius of neutron stars, provided that the mass-meeting in central neutron star and neutron star equation of state of matter is known. The calculation is done using one solution to Einstein's equations of general relativity called the equation of Tolman-Oppenheimer-Volkoff. From here the moment of inertia of neutron stars can also be calculated. Currently, experimental observations began geared to measure the moment of inertia of neutron stars. The problem is: equation of state of matter that extreme-meeting is not known with certainty and the scientists can only rely on mathematical models.
Fortunately, experimental super-meeting materials can be done on the earth's surface through ion-heavy ion collisions, such as those conducted by physicists at the GSI Darmstadt, Germany, and at RHIC Brookhaven, USA. The results of this experiment can be used to improve models of equation of state before, so the observation of neutron stars can give accurate information about the mass density at the center of neutron stars. Eventually scientists will be able to predict accurately what is happening there and in the neutron star.
