The Crab’s Heart

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Wow!!  This is the Crab Nebula?  It is indeed, and what a difference looking at it with the Chandra X-ray Telescope makes!!  Check it out, we are looking right into the heart of the Nebula and we can see the remnant from the supernova that blew the original star apart and it even shows the jets coming off from it.

The Crab Nebula is also known as M1 because it was first catalog listing for Charles Messier.  When star that created it blew up on July 4^th, 1054, the supernova was visible here on Earth even during the day for over three weeks.

I am amazed because this is such a different view than I am used to seeing.  This object is viewable from Earth with even a small backyard telescope, I’ve seen it again and again, but without X-ray vision, nothing remotely like this.  Now I got to go dig up the images I took about a month ago.  Way to go Chandra!

The Crab Nebula is a magnitude 8.4 and, if you have dark skies you might even be able to see it with binoculars although I’ve never tried.  To find the Crab Nebula  look over the top of the constellation of Orion about 10 degrees,  (about a fists width at arms length).

Here are the coordinates:
RA:  5h 53m 54s
Dec: +07^o 31’ 48”
Or
Az: 220^o 25’ 28”
Altitude: +46^o 16’ 36”

Here’s the Chandra press release:

This image gives the first clear view of the faint boundary of the Crab Nebula’s X-ray-emitting pulsar wind nebula. The nebula is powered by a rapidly rotating, highly magnetized neutron star, or pulsar (white dot near the center). The combination of rapid rotating and strong magnetic field generates an intense electromagnetic field that creates jets of matter and anti-matter moving away from the north and south poles of the pulsar, and an intense wind flowing out in the equatorial direction.

The inner X-ray ring is thought to be a shock wave that marks the boundary between the surrounding nebula and the flow of matter and antimatter particles from the pulsar. Energetic electrons and positrons (antielectrons) move outward from this ring to brighten the outer ring and produce an extended X-ray glow.

The fingers, loops, and bays in the image all indicate that the magnetic field of the nebula and filaments of cooler matter are controlling the motion of the electrons and positrons. The particles can move rapidly along the magnetic field and travel several light years before radiating away their energy. In contrast, they move much more slowly perpendicular to the magnetic field, and travel only a short distance before losing their energy.

This effect can explain the long, thin, fingers and loops, as well as the sharp boundaries of the bays. The conspicuous dark bays on the lower right and left are likely due to the effects of a toroidal magnetic field that is a relic of the progenitor star.