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SN 2006gy was an extremely energetic supernova, also referred to as a hypernova, [4] that was discovered on September 18, 2006. It was first observed by Robert Quimby and P. Mondol, [2] [5] and then studied by several teams of astronomers using facilities that included the Chandra, Lick, and Keck Observatories.
The estimated mass-loss rates are typically higher than 10 −3 M ☉ per year. There are indications that they originate as stars similar to luminous blue variables with large mass losses before exploding. [34] SN 1998S and SN 2005gl are examples of Type IIn supernovae; SN 2006gy, an extremely energetic supernova, may be another example. [35]
SN 2005ap was an extremely energetic type II supernova. It is reported to be the brightest supernova yet recorded, twice as bright as the previous record holder, SN 2006gy. [ 2 ] Although SN 2005ap was twice as bright at its peak than SN 2006gy it was not as energetic overall as the former brightened and dimmed in a typical period of a few days ...
It is thought that SN 2006gy is a likely candidate for a pair-instability supernova. SN 2005ap, which was discovered by Robert Quimby who also discovered SN 2006gy, was about twice as bright as SN 2006gy and about 300 times as bright as a normal type II supernova. [62] Host Galaxies of Calcium-Rich Supernovae. [63]
SN 1054 remnant (Crab Nebula)A supernova is an event in which a star destroys itself in an explosion which can briefly become as luminous as an entire galaxy.This list of supernovae of historical significance includes events that were observed prior to the development of photography, and individual events that have been the subject of a scientific paper that contributed to supernova theory.
Cash App-owner Block must offer up to $120 million in refunds to consumers who federal regulators say were exposed to potential fraud.
NAD+ supplements, IV drips, and injections have gained a lot of traction on social media due to their supposed anti-aging benefits. Here, doctors reveals the truth behind the trend.
Cobalt-56 has a half-life of 77 days and then further decays to the stable isotope iron-56 (see Supernova nucleosynthesis). For the hypernova SN 2006gy, studies indicate that perhaps 40 solar masses of the original star were released as Ni-56, almost the entire mass of the star's core regions. [4]