A supernova (English: Supernova) is a type of stellar explosion that results in the destruction of the star and remains as a neutron star or black hole. Inside stars 8-15 times more massive than the Sun, hydrogen fusion reactions form helium, helium fusion forms carbon, and that carbon fusion forms iron.
Iron formation completes the series of central reactions, as the next reaction is endothermic. At such a time, as the external pressure inside the star decreases significantly, it can no longer resist the gravitational attraction force, resulting in a massive implosion in the star. Most of the star's mass is compressed at its center, And the gaseous atmosphere is torn apart and spread around with great velocity. This event is known as a supernova explosion.
Such explosions release huge amounts of energy and the associated star temporarily becomes brighter than the entire galaxy. Supernova explosions are divided into two categories based on the amount of hydrogen present in the ejected gaseous material --- type 2 if the ejected material is hydrogen-rich and type 1 if the ejected material is hydrogen-poor. People have known about supernovas since long time ago. Chinese astronomers are reported to have seen a supernova in 1054 AD.
The recent supernova explosion SN1987A in the Large Magellanic Cloud (LMC) was seen almost exclusively with the naked eye. The explosion of a supernova can create a lot of heavy elemental matter and scatter it throughout the galaxy. Kepler's Supernova Remnant, A multi-wavelength X-ray image (from the Lunar X-Ray Observatory) Nomenclature Edit Supernova Name origin Edit The Latin word nova means new. A nova refers to stars located in the b-sphere that appear very bright.
The nominative prefix super is added to nova to become supernova, simultaneously marking the difference between nova and supernova. A supernova also refers to a star that is getting brighter. But in this case the cause and mechanism of star brightness is quite different. According to Merriam-Webster's Collegiate Dictionary, the term supernova was first used in 1926.
Supernovas have been dubbed supernovas. It is evident that navtara is associated with ultra-symptoms. Navtara means nova. When new supernovae are discovered, information is sent to the International Astronomical Union's Central Bureau for Astronomical Telegrams. The department publishes the name of supernova along with its description through a circular. Supernovae are named by the year of discovery followed by a one or two letter indicator. The first 26 supernovae discovered in a year are named using the uppercase letters of the English alphabet from A to Z. Then pairs of lowercase letters are used, eg: AA, AB etc. Professional and amateur astronomers find up to several hundred supernovae each year.
For example, 367 supernovae were discovered in 2005 and 551 in 2006. For example, the last supernova discovered in 2005 was named SN 2005NC, meaning it was the 367th supernova discovered in 2005. Historical supernovae are named using only the year of their discovery, eg: SN 185, SN 1006, SN 1054 (Tycho's nova) and SN 1604 (Kepler's star). No year before 1885 had more than one supernova been discovered. That year, however, a supernova was discovered. But since 1885, alphabetic designations have been used with supernova names. eg SN 1885A, SN 1907A etc. In fact, it was not until 1947 that more than one supernova was discovered.
Therefore, the last occurrence of using an alphabetic indicator with a name occurred in the case of the supernova called SN 1947A. "SN" used at the beginning of the name is an optional prefix. — Inventions are a rare phenomenon, This happens at most once every 50 years in galaxies like the Milky Way. Therefore, studying supernovae requires observing many galaxies together in very fine detail. It is not possible to accurately predict the occurrence of supernovae in distant galaxies. When they are discovered, the explosive process begins.
Therefore, in order to pass this observation in the judgment of scientific truth, it is necessary to observe the maximum brightness of each supernova. That's why it's so important to discover every supernova before it reaches peak brightness. Amateur astronomers outnumber professional astronomers. Hobbyists have therefore contributed more to the discovery of supernovas. They made this discovery possible by regularly observing relatively nearby galaxies with optical telescopes. This is done by comparing the new images with the previous ones can be observed. In the late 20th century, the use of computer-controlled telescopes and charge-coupled devices, or CCDs, for ultranova hunting increased dramatically.
They are very popular with amateur astronomers. In addition, large facilities like the Katzman Automatic Imaging Telescope have been built for professional observation of supernovae. In addition, through the current Supernova Early Warning System (SNEWS), neutrinos have been detected to provide advance news of galactic supernova explosions. A large number of neutrinos are produced during supernova explosions and these neutrinos are not scattered or absorbed by interstellar dust, gas and cosmic dust.
Research on supernova explosions can be divided into two categories: Observing relatively nearby events and observing distant explosions. If the Doppler emission (redshift, redshift) and emission spectrum of a distant star are known due to the expansion of the universe, its distance can be measured. On average, the expansion velocity of distant objects is greater than that of nearby objects, and therefore the redshifts of distant objects are higher. So ultimately the search for supernovae splits into two parts, high redshift and low redshift. In this case the condition range is z = 0.1 - 0.3. where Z denotes a dimensionless quantity measuring the frequency shift of the spectrum. Supernova light curves are observed in cases of high redshift observations of supernovae. This observation has the function, Using this, Hubble diagrams can be drawn using standard or specially modified candles. Cosmic predictions are possible through this diagram.
Ultranova spectroscopy is very useful in low-redshift studies. This observation method is used to study the physics and environment of supernovae. Low Raul observations contain the short-distance end of the Hubble curve. This part of the curve again produces a plot of distance versus redshift for visible galaxies. ***Collected*** Creates a graph of distance versus red gradient in case. ***Collected*** Creates a graph of distance vs red gradient in case
