Nevertheless, astronomers believe that most stars like the Sun will eventually go through such a phase.

(Editor's Note: UniSci readers might prefer to see the images first before continuing with this story. For those who do, they can be seen at this website.)

This star, named OH231.8+4.2, is seen in these infrared pictures blowing out gas and dust in two opposite directions. So much dust has been cast off and surrounds the star that it cannot be seen directly, only its starlight that is reflected off the dust. 

The flow of gas is fast, with a velocity up to 450,000 mph (700,000 km/h). With extreme clarity, these Hubble Near Infrared Camera and Multi-Object Spectrometer (NICMOS) images reveal that the fast-moving gas and dust are being collimated into several thin streamers (on the right) and a jet-like structure (on the left), which can be seen extending away from the centers of both pictures. 

On the right, wisps of material in jet-like streamers appear to strike some dense blobs of gas. This interaction must produce strong shock waves in the gas.

The pictures represent two views of the object. The color image is a composite of four images taken with different NICMOS infrared filters on March 28, 1998. It shows that the physical properties of the material, both composition and temperature, vary significantly throughout the outflowing material. The black-and-white image was taken with one NICMOS infrared filter. That image is able to show more clearly the faint detail and structure in the nebula than can be achieved with the color composites.

Observations by radio astronomers have found many unusual molecules in the gas around this star, including many containing sulfur, such as hydrogen sulfide and sulfur dioxide. These sulfur compounds are believed to be produced in the shock waves passing through the gas. Because of the large amount of sulfur compounds, this object has earned the nickname "The Rotten Egg" Nebula. It resides in the constellation Puppis.

These NICMOS data pose a serious challenge to astrophysical theorists: How can a star generate such tightly collimated streams of gas and dust and accelerate them to such very high velocities? 

William B. Latter from the California Institute of Technology and his group are using these data to obtain a better understanding of the detailed structure in the outflowing material, look for evidence for the origin of the thin streamers and jets, and learn more about the star itself. 

This information will give astronomers a more complete understanding of the final stages in the life of stars like our Sun.

These results were presented at a conference called "Asymmetrical Planetary Nebulae II: From Origins to Microstructures," Aug. 3 to 6, 1999 at the Massachusetts Institute of Technology. The results will be published in the Astrophysical Journal.

Credit: NASA, ESA, William B. Latter (SIRTF Science Center/California Institute of Technology), John H. Bieging (University of Arizona), Casey Meakin (University of Arizona), A.G.G.M. Tielens (Kapteyn Astronomical Institute), Aditya Dayal (IPAC/NASA Jet Propulsion Laboratory), Joseph L. Hora (Center for Astrophysics), and Douglas M. Kelly (University of Arizona).

Related images:

Via links in http://oposite.stsci.edu/pubinfo/latest.html and http://oposite.stsci.edu/pubinfo/pictures.html

Higher resolution digital versions (300 dpi JPEG and TIFF) available at: http://oposite.stsci.edu/pubinfo/pr/1999/39/pr-photos.html and http://oposite.stsci.edu/pubinfo/pr/1999/39/extra-photos.html

[Contact: Ray Villard, Lars Lindberg Christensen]
 

19-Oct-1999