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1AKHViYgBGbmxi8qiJkNvoHNeDu9m3MfPE VerifiedWhen in a supernova, a star collapses to a neutron star, and its magnetic field increases dramatically in strength. Halving a linear dimension increases the magnetic field fourfold.
A similar magnetohydrodynamic dynamo process produces even more intense transient fields during coalescence of pairs of neutron stars.
The active life of a magnetar is short.
On 21 September 2006 the Swift satellite detected a 20ms soft Gamma-ray burst in Westerlund 1.
The magnetic field decay powers the emission of high-energy electromagnetic radiation, particularly X-rays and gamma rays.
A magnetar's magnetic field gives rise to very strong and characteristic bursts of X-rays and gamma rays.
Starquakes triggered on the surface of the magnetar disturb the magnetic field which encompasses it, often leading to extremely powerful gamma ray flare emissions which have been recorded on Earth in 1979, 1998, and 2004.
-- converting heat and rotational energy into magnetic energy and increasing the magnetic field, normally an already enormous 108 teslas, to more than 1011 teslas (or 1015 gauss).
The result is a magnetar.
-- to saturate instruments on BeppoSAX, WIND and RXTE. On May 29, 2008, NASA's Spitzer Space Telescope discovered a ring of matter around this magnetar. It is thought that this ring formed in the 1998 burst.
Magnetars are differentiated from other neutron stars by having even stronger magnetic fields, and by rotating comparatively more quickly. Most neutron stars rotate once every one to ten seconds, whereas magnetars rotate once in less than one second.
Duncan and Thompson calculated that when the spin, temperature and magnetic field of a newly formed neutron star falls into the right ranges, a dynamo mechanism could act, --
The fact that a neutron star was formed instead of a black hole implies that more than 95% of the star's original mass must have been lost before or during the supernova that produced the magnetar.
The theory regarding these objects was proposed by Robert Duncan and Christopher Thompson in 1992, but the first recorded burst of gamma rays thought to have been from a magnetar had been detected on March 5, 1979.
Fortuitously, XMM-Newton observations had been made four days earlier, and repeat observations 1.5 days after the burst revealed the magnetar to be the source of the burst, with the X-ray luminosity increasing by a factor of 100 during the outburst.
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Their strong magnetic fields decay after about 10,000 years, after which activity and strong X-ray emission cease. Given the number of magnetars observable today, one estimate puts the number of inactive magnetars in the Milky Way at 30 million or more.
During the following decade, the magnetar hypothesis became widely accepted as a likely explanation for soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs).
CXOU J164710.2−455216 is an anomalous X-ray pulsar in the massive galactic open cluster Westerlund 1. It is the brightest X-ray source in the cluster, and was discovered in 2005 in observations made by the Chandra X-ray observatory.
A magnetar is a type of neutron star believed to have an extremely powerful magnetic field (∼1013 to 1015 G, ∼109 to 1011 T).
Like other neutron stars, magnetars are around 20 kilometres (12 mi) in diameter and have a mass 2–3 times that of the Sun. The density of the interior of a magnetar is such that a tablespoon of its substance would have a mass of over 100 million tons.
The Westerlund 1 cluster is believed to have formed in a single burst of star formation, implying that the progenitor star must have had a mass in excess of 40 solar masses.
It is estimated that about one in ten supernova explosions results in a magnetar rather than a more standard neutron star or pulsar.
These fields then persist due to persistent currents in a proton-superconductor phase of matter that exists at an intermediate depth within the neutron star (where neutrons predominate by mass).
Unusually bright supernovae are thought to result from the death of very large stars as pair-instability supernovae (or pulsational pair-instability supernovae).
It has been suggested that SGR 0501+4516, together with 1E 1547.0-5408, should be considered as tools for a final unification of SGRs, AXPs and the “transient AXPs (TAXPs)” into a single class of “magnetars candidates”.
https://twetch.app/t/60f4ffc94f365d348a1aad73a8e1f4f9e6312d291ac740b3f177d66018003020
Magnetar found very close to the supermassive black hole, Sagittarius A*, at the center of the Milky Way Galaxy.
However, recent research by astronomers has postulated that energy released from newly formed magnetars into the surrounding supernova remnants may be responsible for some of the brightest supernovae, such as SN 2005ap and SN 2008es.
As of September 2008, ESO reports identification of an object which it has initially identified as a magnetar, SWIFT J195509+261406, originally identified by a gamma-ray burst (GRB 070610)
As of March 2016, 23 magnetars are known, with six more candidates awaiting confirmation. A full listing is given in the McGill SGR/AXP Online Catalog. Examples of known magnetars include:
After a long period of low emissions (significant bursts only in 1979 and 1993) it became active in May–August 1998, and a burst detected on August 27, 1998 was of sufficient power to force NEAR Shoemaker to shut down to prevent damage and --