X-ray, optical, IR and radio image of SNR  G352.7-0.1
Credit: X-ray: NASA/CXC/Morehead State Univ/T.Pannuti et al.; Optical: DSS; Infrared: NASA/JPL-Caltech; Radio: NRAO/VLA/Argentinian Institute of Radioastronomy/G.Dubner


Moving around large pieces of a galaxy is no easy feat. It requires an engine of enormous power, such as a supernova explosion. In a core-collapse supernova, a massive star runs out of nuclear fuel and falls inwards. Energy generated in this collapse results in the destruction of the star and the expulsion of the outer stellar layers at high velocities, producing as much power as generated by all the rest of the stars in the galaxy combined. The ejected material smashes into its surroundings and sweeps them up into a roughly spherical ball. The image above shows an interesting example of this process at work. This image of a supernova remnant in the Milky Way called G352.7-0.1, is a composite of an X-ray image from the Chandra X-ray Observatory (in blue), an optical image (in white), an infrared image (in gold, from the Spitzer Space Telescope) and a radio image in purple (from the Jansky VLA). This multi-wavelength image shows extraordinary details of the interaction of the supernova's powerful shock wave and the surrounding gas and dust in the Galaxy. Observations with Chandra and XMM-Newton show the hottest gas is dominated by the ejecta from the supernova explosion bounded by cooler swept-up material seen in the radio and infrared. Studies show that the amount of swept-up material is enormous, about 45 times the mass of the Sun, and the amount of hot X-ray emitting gas in the interior is about twice the Sun's mass. Given the age of the remnant (about 2200 years), it's a puzzle why the X-ray emission is dominated by the interior ejecta; in other remnants of similar age, X-ray emission is usually dominated by the outer swept-up material. Astronomers are still searching for the remnant of the exploded star's core, which may be a young neutron star or baby black hole.
Published: April 21, 2014

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Page Author: Dr. Michael F. Corcoran
Last modified Monday, 28-Apr-2014 07:38:38 EDT