A supernova is the biggest explosion that humans have ever seen. The brightest recorded supernova was SN 1006, which occurred in 1006 AD in the constellation of Lupus, and was described by observers across China, Japan, Iraq, Egypt, and Europe. The highlighted passages refer to the Chinese observation of SN 1054. ", "Astronomers Just Narrowed Down The Source of Those Powerful Radio Signals From Space", Nuclear Physics B: Proceedings Supplements, "The hot white-dwarf companions of HR 1608, HR 8210, and HD 15638", Publications of the Astronomical Society of the Pacific, "Sternberg Astronomical Institute Supernova Catalogue", "List of Supernovae with IAU Designations", IAU: Central Bureau for Astronomical Telegrams, Monte Agliale Supernovae and Asteroid Survey, Magnetospheric eternally collapsing object, ʿAjā'ib al-makhlūqāt wa gharā'ib al-mawjūdāt, https://en.wikipedia.org/w/index.php?title=Supernova&oldid=980949463, Short description is different from Wikidata, Articles containing potentially dated statements from 2010, All articles containing potentially dated statements, Creative Commons Attribution-ShareAlike License, Electron capture in a degenerate O+Ne+Mg core, Black hole after fallback of material onto an initial neutron star, II-P, sometimes a hypernova, possible GRB, None (or luminous supernova? If a supernova's spectrum contains lines of hydrogen (known as the Balmer series in the visual portion of the spectrum) it is classified Type II; otherwise it is Type I. Type Ib/c and II-L, and possibly most Type IIn, supernovae are only thought to be produced from stars having near-solar metallicity levels that result in high mass loss from massive stars, hence they are less common in older, more-distant galaxies. It was used, as "super-Novae", in a journal paper published by Knut Lundmark in 1933,[25] and in a 1934 paper by Baade and Zwicky. [124][132], In the modern universe, old asymptotic giant branch (AGB) stars are the dominant source of dust from s-process elements, oxides, and carbon. Around 1% of these neutrinos are thought to deposit sufficient energy into the outer layers of the star to drive the resulting catastrophe, but again the details cannot be reproduced exactly in current models. [118], The progenitors of Type Ib/c supernovae are not observed at all, and constraints on their possible luminosity are often lower than those of known WC stars. Please continue to respect all commenters and create constructive debates. The most recent directly observed supernova in the Milky Way was Kepler's Supernova in 1604, but the remnants of more recent supernovae have been found. [38][39], Supernova discoveries are reported to the International Astronomical Union's Central Bureau for Astronomical Telegrams, which sends out a circular with the name it assigns to that supernova. [74][75] When a massive star develops an iron core larger than the Chandrasekhar mass it will no longer be able to support itself by electron degeneracy pressure and will collapse further to a neutron star or black hole. For example, the sub-luminous SN 2008ha is often referred to as SN 2002cx-like or class Ia-2002cx. For cores of around 60–130 M☉, the fusion of oxygen and heavier elements is so energetic that the entire star is disrupted, causing a supernova. This is one scenario for producing high luminosity supernovae and is thought to be the cause of Type Ic hypernovae and long duration gamma-ray bursts. The expanding shock waves of supernovae can trigger the formation of new stars.
Blue supergiants form an unexpectedly high proportion of confirmed supernova progenitors, partly due to their high luminosity and easy detection, while not a single Wolf–Rayet progenitor has yet been clearly identified. The peak luminosity varies considerably and there are even occasional Type Ib/c supernovae orders of magnitude more and less luminous than the norm. Our journalists will try to respond by joining the threads when they can to create a true meeting of independent Premium. Today, amateur and professional astronomers are finding several hundred every year, some when near maximum brightness, others on old astronomical photographs or plates. Are you sure you want to delete this comment? A white dwarf is a degenerating star that is reaching the end of its life cycle. For core masses of 40–60 M☉, the collapse halts and the star remains intact, but collapse will occur again when a larger core has formed. Very luminous progenitors have not been securely identified, despite numerous supernovae being observed near enough that such progenitors would have been clearly imaged. ), Initial asymmetries have also been confirmed in Type Ia supernovae through observation. Supernovae are more energetic than novae.
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