For example, at ultraviolet wavelengths there is an early extremely luminous peak lasting only a few hours corresponding to the breakout of the shock launched by the initial event, but that breakout is hardly detectable optically.
They can be produced by various types of core collapse in different progenitor stars, possibly even by Type Ia white dwarf ignitions, although it seems that most will be from iron core collapse in luminous When a stellar core is no longer supported against gravity, it collapses in on itself with velocities reaching 70,000 km/s (0.23The initial collapse of degenerate cores is accelerated by In lower mass cores the collapse is stopped and the newly formed neutron core has an initial temperature of about 100 billion Some material from the outer envelope falls back onto the neutron star, and, for cores beyond about 8 The collapse of a massive non-degenerate core will ignite further fusion. The rate of mass loss for luminous stars depends on the metallicity and luminosity. There are a number of difficulties reconciling modelled and observed stellar evolution leading up to core collapse supernovae. These events are difficult to detect, but large surveys have detected possible candidates.A historic puzzle concerned the source of energy that can maintain the optical supernova glow for months. These radioisotopes excite the surrounding material to incandescence. All Wolf–Rayet stars end their lives from the Wolf–Rayet phase within a million years or so, but again it is difficult to identify those that are closest to core collapse.
Supernovae that do not fit into the normal classifications are designated peculiar, or 'pec'.These types would now all be treated as peculiar Type II supernovae (IIpec), of which many more examples have been discovered, although it is still debated whether SN 1961V was a true supernova following an A white dwarf star may accumulate sufficient material from a There are several means by which a supernova of this type can form, but they share a common underlying mechanism.
Only a tiny fraction of the 100 billion stars in a typical The earliest possible recorded supernova, known as HB9, could have been viewed and recorded by unknown There is some evidence that the youngest galactic supernova, Observation and discovery of extragalactic supernovae are now far more common.
The first such observation was of Among the earliest detected since time of detonation, and for which the earliest spectra have been obtained (beginning at 6 hours after the actual explosion), is the Type II On 20 September 2016, amateur astronomer Victor Buso from Early work on what was originally believed to be simply a new category of Supernovae in other galaxies cannot be predicted with any meaningful accuracy. Although the energy that disrupts each type of supernovae is delivered promptly, the light curves are dominated by subsequent radioactive heating of the rapidly expanding ejecta.
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