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G292.0+1.8 (Supernova Remnant)


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G292.0+1.8
Supernova Remnant (超新星残骸)
SNR


星座 (Constellation)
ケンタウルス座 (Cen) (Centaurus)

距離 (Distance)

20,000光年 (20,000 light-years)

G292.0+1.8 is a supernova remnant located 20,000 light years from the Earth in the constellation Centaurus.

G292.0+1.8 (Supernova Remnant) : Picture

G292.0+1.8 (Supernova Remnant)
G292.0+1.8 (Supernova Remnant)
(C) NASA/CXC/Penn State/S.Park et al.
The aftermath of the death of a massive star is shown in beautiful detail in this new composite image of G292.0+1.8. In color is the Chandra X-ray Observatory image - easily the deepest X-ray image ever obtained of this supernova remnant - and in white is optical data from the Digitized Sky Survey. Although considered a "textbook" case of a supernova remnant, the intricate structure shown here reveals a few surprises.

Near the center of G292.0+1.8 is the so-called pulsar wind nebula, most easily seen in high energy X-rays. This is the magnetized bubble of high-energy particles that surrounds the "pulsar", a rapidly rotating neutron star that remained behind after the original, massive star exploded. The narrow, jet-like feature running from north to south in the image is likely parallel to the spin axis of the pulsar.

The pulsar is located slightly below and to the left of the center of G292.0+1.8. Assuming that the pulsar was born at the center of the remnant, it is thought that recoil from the lopsided explosion may have kicked the pulsar in this direction. However, the kick direction and the pulsar spin direction do not appear to be aligned, in contrast to apparent spin-kick alignments seen in some other supernova remnants.

Another key feature of this remnant is the long white line running from left to right across the center called the equatorial belt. This structure is thought to be created when the star - before it died - expelled material from around its equator via winds. The orientation of the equatorial belt suggests the parent star maintained the same spin axis both before and after it exploded.

One puzzling aspect of the image is the lack of evidence for thin filaments of high energy X-ray emission, thought to be an important site for cosmic ray acceleration in supernova remnants. These filaments are seen in other supernova remnants such as Cassiopeia A, Tycho and Kepler. One explanation may be that efficient acceleration occurs primarily in very early stages of supernova remnant evolution, and G292.0+1.8, with an estimated age of several thousand years, is too old to show these effects. Casseiopeia A, Tycho and Kepler, with ages of several hundred years, are much younger.

Pulsar Wind Nebula in G292.0+1.8
Pulsar Wind Nebula in G292.0+1.8
(C) NASA/CXC/Penn State/S.Park et al.
Chandra's image of G292.0+1.8 shows remarkable complexity and structure in the debris field of this exploded star. Each color represents different elements such as oxygen, neon, magnesium, and silicon. The distribution of these elements gives astronomers clues about how the star exploded. The close-up zooms into the region around the dense core that remains of the star, seen in the highest-energy X-rays detected by Chandra.

Hard X-ray Image of G292.0+1.8
Hard X-ray Image of G292.0+1.8
(C) NASA/CXC/Penn State/S.Park et al.
When a massive star explodes like the one that produced G292.0+1.8, it creates a shell of hot gas that glows brightly in X-rays. Chandra is able to observe the stellar debris, revealing the dynamics of the explosion. With nearly six days of Chandra observing time devoted to studying G292.0+1.8, astronomers hope they can use this particular remnant to better understand the complicated details of such an explosion. This image shows the high-energy X-rays only (1.810-2.050 and 2.400-2.620 keV).

G292.0+1.8 with Scale Bar Hard X-ray Image of G292.0+1.8
G292.0+1.8 with Scale Bar
(C) NASA/CXC/Penn State/S.Park et al.
Hard X-ray Image of G292.0+1.8
(C) NASA/CXC/Penn State/S.Park et al.
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G292.0+1.8 (Supernova Remnant) : Movie

G292.01 8 in 60 Seconds
This image shows how complex a star's afterlife can be.
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