Images by Date
Images by Category
Solar System
White Dwarfs
Neutron Stars
Black Holes
Milky Way Galaxy
Normal Galaxies
Galaxy Clusters
Cosmology/Deep Field
Images by Interest
Space Scoop for Kids
Sky Map
Photo Blog
Top Rated Images
Image Handouts
Fits Files
Image Tutorials
Photo Album Tutorial
False Color
Cosmic Distance
Look-Back Time
Scale & Distance
Angular Measurement
Images & Processing
Image Use Policy
Web Shortcuts
Chandra Blog
RSS Feed
Email Newsletter
News & Noteworthy
Image Use Policy
Questions & Answers
Glossary of Terms
Download Guide
Get Adobe Reader
A Closer Look at Pulsar B1957+20
Click for large jpg (Credit: NASA/CXC/M.Weiss)
Jpeg, Tiff, PS

An artist's impression of the optical and X-ray emission surrounding the "Black Widow" pulsar B1957+20 is shown at left. The rapidly spinning pulsar, marked by the white star in this figure, is moving from left to right generating a "bow shock" (a sonic boom traveling ahead of the pulsar into surrounding interstellar gas.) When hydrogen atoms in this surrounding gas are overrun by this bow shock, they are hit by rapidly moving protons and electrons behind the shock. This causes them to emit "H-alpha" light, seen by optical telescopes and corresponding to the yellow rim extending in a curved arc around the pulsar.

Inside the bow shock, the pulsar generates a wind of high-energy matter and anti-matter particles, which move outwards in all directions at close to the speed of light (marked by the white rays extending out from the pulsar). This particle wind carves out an oval-shaped cavity around the pulsar, stretched out along the direction of motion. At some distance from the pulsar, this wind must suddenly slow down to match the speed of surrounding gas. This slow-down process creates "synchrotron radiation", detectable in X-rays and denoted in this figure by the red "skin" of emission which encloses the cavity hollowed out by the pulsar. In three dimensions this skin forms a cylinder enclosing the tube-like cavity, and produces the "tail-like" appearance of the X-rays seen in the actual data.

Click for large jpg (Close-Up)
(Credit: NASA/CXC/M.Weiss)

Jpeg, Tiff, PS

On a scale about a million times smaller than the main figure, the pulsar's high-energy wind also has a dramatic effect on its companion star, which orbits the pulsar every 9.2 hours. The pulsar is shown as a white dot, with its wind flowing out at high speeds in all directions. On these scales this wind is generally unimpeded, except in the directions in which it flows towards the companion star. The companion star produces its own wind, but a much weaker and slower version. The two winds collide not far above the companion star's surface, the resulting collision generating more X-rays, marked by the curved red arc in this figure. The pulsar's powerful wind and the resulting X-rays are blasting the companion, stripping it of gas and steadily evaporating it, as can be seen by the purple trail of material streaming away from the companion star. Eventually, this effect might completely destroy the companion, which is why this pulsar is known as the "Black Widow". The companion star is orbiting clockwise, causing the trail behind it to curve around in the beginnings of a spiral pattern.

Back to More Images

Return to B1957+20 (27 Feb 03)