Top Document: [sci.astro] Stars (Astronomy Frequently Asked Questions) (7/9) Previous Document: G.01.2 What are all those different kinds of stars? White Dwarfs How are white dwarfs classified? What Next Document: G.01.4 What are all those different kinds of stars? Black Holes See reader questions & answers on this topic! - Help others by sharing your knowledge Author: Joseph Lazio <jlazio@patriot.net> Neutron stars are the remnants of massive stars. Sufficiently massive stars form iron in their cores during the process of nuclear fusion. Iron proves problematic for the star, though, as iron is among the most tightly bound nuclei. Nuclear fusion involving iron actually requires energy to occur, as opposed to nuclear fusion involving lighter nuclei in which the fusion produces energy. At some point so much iron accumulates in the core of the star that its nuclear reactions do not produce enough heat (i.e., pressure) to counter-balance the force of gravity due to the star's mass. The star implodes in a supernova, blowing off much of its outer layers and leaving an NS as a remnant. A star has to be (roughly) at least 8 times as massive as the Sun and not more than 25--50 times as massive as the Sun to form an NS. (The upper limit is quite uncertain.) (There has been a second mechanism postulated as a way to form neutron stars. There is an upper limit to the mass of a white dwarf, 1.4 times the mass of the Sun, called the Chandrasekhar limit after Subrahmanyan Chandrasekhar who first described it. Above this mass the force of gravity overwhelms the internal pressure provided by the electrons in the WD. If one had a WD that was quite close to the Chandrasekhar limit and a small amount of mass was added to it, it might collapse to form an NS. This process is called "accretion-induced collapse." It is not clear if this mechanism actually occurs, however.) NSs can be divided into three broad classes, rotation-powered pulsars, accretion-powered pulsars, and magnetars. Rotation-powered pulsars are the kind of pulsars most commonly described and were the first kind of NSs observed. These NSs have powerful magnetic fields and rotate. If the axes of the star's rotation and magnetic field are not aligned, this rotating magnetic field produces an electric field; in the case of NSs, the electric fields are strong enough to rip particles from the crust of the NS and accelerate them. The accelerated particles radiate. The magnetic field collimates the accelerated particles, so the radiation from the NS is emitted in two narrow beams. If one of the beams sweeps across the Earth, we observe a pulsating source---a pulsar. Most of the known rotation-powered pulsars are observed in the radio (though the radio emission itself is a usually just a tiny fraction of the rotation energy of the NS). Rotation-powered pulsars are often further sub-divided into strong-field and recycled pulsars. Strong-field pulsars have magnetic fields of about 10^8 Tesla and observed pulse periods about 1 second. As the pulsars lose energy, their rates of spin slow down. At some point, the rotating magnetic field is no longer produces electric fields strong enough to power the pulsar mechanism, and the pulsar "shuts off." However, if the NS is a member of a binary system, its companion star, during the course of its own evolution, increase in size and start spilling matter onto the NS. As the matter spills onto the NS, if it hits the NS in the same direction that the NS is rotating, it can increase the rate at which the NS is spinning or "spin-up" the NS. If this spin-up process goes on for a long enough period of time, the NS may "turn on" as a pulsar again. The process of matter spilling onto the pulsar tends to suppress the magnetic field, though. With a weaker magnetic field, the spun-up pulsar doesn't spin down as fast as before. So, these recycled pulsars are distinguished by having very slow spin-down rates. As it turns out, they also tend to have very short pulse periods, typically less than 0.1 seconds, with the shortest being 0.00156 seconds. Accretion-powered pulsars are NSs onto which matter is spilling. The gravity well around an NS is so deep, it is actually fairly difficult for matter to fall onto the NS. Only matter that starts at rest with respect to the NS can fall directly onto its surface. If the matter has any velocity relative to the NS, as it falls toward the NS, it will begin to orbit the NS. (This is the same principle that causes a skater to spin faster as she pulls in her arms.) If a lot of matter is falling toward the NS, a disk is formed around the NS. Due to "frictional" forces within the disk, matter slowly works its way closer to the NS until finally falling a short distance onto its surface. The process of the matter falling onto the NS' surface is known as accretion, so the disk is called an accretion disk. The gravitational potential of a NS is so deep that a lot of energy can be released as the matter forms an accretion disk and spills onto the NS' surface. Consequently, accretion-powered NSs are typically seen as X-ray sources. Magnetars are a recently recognized class of NSs. It is thought that rotation-powered pulsars only work if the magnetic field is not too strong. If the magnetic field is too strong, it can effectively shut down the process by which the particles are produced. The critical field seems to be about 10^10 Tesla. Only a few examples of magnetars are known. These generally appear as fairly constant X-ray sources, though magnetars have also been suggested to be responsible for sources known as soft-gamma ray repeaters. User Contributions:Top Document: [sci.astro] Stars (Astronomy Frequently Asked Questions) (7/9) Previous Document: G.01.2 What are all those different kinds of stars? White Dwarfs How are white dwarfs classified? What Next Document: G.01.4 What are all those different kinds of stars? Black Holes Part0 - Part1 - Part2 - Part3 - Part4 - Part5 - Part6 - Part7 - Part8 - Single Page [ Usenet FAQs | Web FAQs | Documents | RFC Index ] Send corrections/additions to the FAQ Maintainer: jlazio@patriot.net
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