Studying the complex aftermath of a supernova

Two new Chandra images reveal the titanic shock waves and pulsars that result from stellar explosions.
By and | Published: November 25, 2014 | Last updated on May 18, 2023

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Key Takeaways:

  • Two new images from NASA’s Chandra X-ray Observatory of supernova remnants MSH 11-62 and G327.1-1.1 reveal complex post-explosion structures of massive stars.
  • Supernovae result in the formation of ultra-dense neutron stars (pulsars) that generate powerful winds of high-energy particles, leading to the creation of glowing pulsar wind nebulae (PWNe).
  • The PWN within MSH 11-62 is characterized by an irregular shell of hot gas surrounding an extended X-ray nebula, with its elongated shape potentially influenced by reverse and secondary shock waves.
  • G327.1-1.1 features a distorted, comet or lobster-like PWN, likely reshaped by a reverse shock and the rapid motion of its pulsar, possibly a consequence of an asymmetric supernova recoil kick, with the origin of its "lobster claw" features yet undetermined.
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Supernovae remnants
Two new Chandra images of supernova remnants reveal intricate structures left behind after massive stars exploded. Powerful winds of high-energy particles are released from the dense core of the dead star to create so-called pulsar wind nebulas. MSH 11-62 and G327.1-1.1 are examples of how complex the aftermath of stellar explosions can be.

MSH 11-62: NASA/CXC/SAO/P.Slane et al; G327.1-1.1: NASA/CXC/GSFC/T.Temim et al.
A supernova that signals the death of a massive star sends titanic shock waves rumbling through interstellar space. An ultra-dense neutron star is usually left behind, which is far from dead, as it spews out a blizzard of high-energy particles. Two new images from NASA’s Chandra X-ray Observatory provide fascinating views, including an enigmatic lobster-like feature, of the complex aftermath of a supernova.

When a massive star runs out of fuel, the central regions usually collapse to form a neutron star. The energy generated by the formation of the neutron star triggers a supernova. As the outward-moving shock wave sweeps up interstellar gas, a reverse shock wave is driven inward, heating the material ejected by the star.

Meanwhile, the rapid rotation and intense magnetic field of the neutron star, also known as a pulsar, combine to generate a powerful wind of high-energy particles. This so-called pulsar wind nebula can glow brightly in X-rays and radio waves.

A long observation with Chandra of the supernova remnant MSH 11-62 reveals an irregular shell of hot gas, shown in red, surrounding an extended nebula of high-energy X-rays, shown in blue. Even though scientists have yet to detect any pulsations from the central object within MSH 11-62, the structure around it has many of the same characteristics as other pulsar wind nebulae. The reverse shock and other secondary shocks within MSH 11-62 appear to have begun to crush the pulsar wind nebula, possibly contributing to its elongated shape.

MSH 11-62 is located about 16,000 light-years from Earth. The foreground of MSH 11-62 is speckled with hundreds of sources associated with the open stellar cluster Trumpler 18, located at a distance of about 5,000 light years, revealing a vast collection of stars.

The supernova remnant G327.1-1.1, located about 29,000 light years from Earth, is another spectacular debris field left behind when a massive star exploded. The Chandra image of G327.1-1.1 shows the outward-moving or forward shock wave (seen as the faint red color) and a bright pulsar wind nebula (blue). The pulsar wind nebula appears to have been distorted by the combined action of the reverse shock wave that may have flattened it and by the motion of the pulsar, which created a comet or lobster-like tail. An asymmetric supernova explosion may have given a recoil kick to the pulsar, causing it to move rapidly and drag the pulsar wind nebula along with it.

Two structures resembling lobster claws protrude from near the head of the pulsar wind nebula. The origin of these features, which may be produced by the interaction of the pulsar wind with the reverse shock, is unknown.

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