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How can you tell if a star has a protoplanetary disc around it, when the disc is too small to image directly? Using the technique of spectroscopy, scientists can deduce the temperature and chemical composition of material around a star, even if they cannot see the disc itself. Spectroscopy involves spreading the light from a star into a spectrum (in visible light, we are familiar with white light being spread out into a rainbow when it passes through a prism), and then measuring exactly how much light is present in each wavelength. The top illustration represents the spectrum of a star with no circumstellar disc or other surrounding material. The distribution of light at any given wavelength follows a specific and well-known line, determined by the laws of physics and the temperature of the star. In the case of a star, most of the light is produced at shorter wavelengths (the left side of the diagram), due to the high temperature of the star's surface. Moving to the right-hand side of the diagram, the wavelengths increase to lower energies (indicating lower temperatures) and, the starlight drops off.
In the second diagram, we see the spectrum of a star with a disc of dust and gas around it. The warm dust and gas disc around the star produces its own infrared light, which changes the shape of the spectrum. The circumstellar material is cooler than the surface of the star, so it emits most of its light at longer infrared wavelengths, closer to the right-hand side of the diagram. Now, there is an excess of infrared emission, which can not be coming from the star itself. The disc is revealed.
Going a step further, in the third diagram we see the spectrum of a star with a circumstellar disc around it, but in this case, the inner part of the disc has been swept away, perhaps by the formation of a planet. The dust closest to the star was also the hottest, so its absence means that there is less emission from the disc at higher temperatures. The only dust producing infrared light is much cooler than the star, and radiates only at long wavelengths. This low temperature "bump" on the spectrum indicates a disc with a missing center, and may be the first clue that planets have formed inside the disc.
|Description||Spectra Show Protoplanetary Disc Structures|
|Date||27 May 2004|
|Author||NASA/JPL-Caltech/D. Watson (University of Rochester)|
(Reusing this file)
see http://gallery.spitzer.caltech.edu/Imagegallery/image.php?image_name=ssc2004-08c High quality tif files also avaliable.
|This file is in the public domain because it was created by NASA. NASA copyright policy states that "NASA material is not protected by copyright unless noted". (See Template:PD-USGov, NASA copyright policy page or JPL Image Use Policy.)
|Size, bytes||0.041275390625 мб|
|Orientation of image||1|
|Image resolution in width direction||300|
|Image resolution in height direction||300|
|Unit of X and Y resolution||2|
|Color space information||65535|
|Exif image width||1200|
|Exif image length||1200|
|Software used||Adobe Photoshop 7.0|
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