life cycle of stars Essay -- essays research papers

LIFE CYCLE OF A STARStars atomic number 18 formed in nebulae, interstellar clouds of dust and gas (mostly total heat). These stellar nurseries are abundant in the arms of spiral galaxies. In these stellar nurseries, dense parts of these clouds submit to gravitational collapse and compress to form a rotating gas globule. The globule is cooled by emitting radio waves and infrared radiation. It is compressed by gravitational forces and also by shock waves of pressure from supernova or the hot gas released from nearby happy stars. These forces cause the roughly-spherical globule to collapse and rotate. The process of collapse takes from between 10,000 to 1,000,000 years. A primaeval Core and a Protoplanetary DiskAs the collapse proceeds, the temperature and pressure deep down the globule increases, as the atoms are in closer proximity. Also, the globule rotates faster and faster. This reel work causes an increase in centrifugal forces (a radial force on spinning objects) that ca uses the globule to have a commutation core and a environ form disk of dust (called a protoplanetary disk or accretion disk). The central core becomes the star the protoplanetary disk may eventually coalesce into orbiting planets, asteroids, etc. ProtostarThe contracting cloud heats up due to friction and forms a radiance protostar this stage lasts for roughly 50 million years. If there is equal veridical in the protostar, the gravitational collapse and the heating continue. If there is not enough material in the protostar, one possible outcome is a chocolate-brown dwarf (a large, not-very-luminous celestial body having a mass between 1028 kg and 84 x 1028 kg). A Newborn StarWhen a temperature of or so 27,000,000F is reached, nuclear fusion begins. This is the nuclear reaction in which hydrogen atoms are converted to helium atoms plus energy. This energy (radiation) production prevents come along contraction of the star. Young stars emit jets of intense radiation that heat the surrounding matter to the point at which it glows brightly. These narrowly-focused jets tin support be trillions of miles long and can travel at 500,000 miles per hour. These jets may be focused by the stars magnetic field. The protostar is now a stable main place star which will remain in this state for about 10 billion years. afterward that, the hydrogen fuel is depleted and the star begins to die. Life spanThe... ...densities are shown as numbers on the the central line that defines the Main episode (M.S.) of stars. Most known stars lie along this line they describe a stage in which a star reaches both(prenominal) fixed coat and mass and commences burning of most of its hydrogen before changing to some other star type off the sequence. Star types, which are outlined on the basis of stellar surface temperatures (page 20-7), are shown by the garner (O, B,...etc.) assigned to each group and evolutionary pathways for some are indicated. This particular(prenominal) plot also shows along the right ordinate the total season that Main Sequence stars of different masses spend on that sequence before evolving along the several principal pathways (see below) as far as we now know, stars do not completely vanish, but survive as dwarfs or Black Holes ( but the latter in principle can disappear by evaporation as Hawking radiation). Temperatures were obtained using Chandra roentgen ray data.BILBLIOGRAPHYwww.enchantedlearning.com/subjects/astronomy/stars/lifecycle/imagine.gsfc.nasa.gov/docs/teachers/lifecycles/LC_main_p1.htmlhubblesite.org/newscenter/newsdesk/archive/releases/1999/20/map.gsfc.nasa.gov/m_uni/uni_101stars.htm