2002MNRAS.331L...1B

A band of pure crystalline forsterite (100 per cent Mg₂ SiO₄) occurs at 69.67µm at room temperature (295K); for olivines with ≳10 per cent Fe the corresponding feature is at ≳73µm. The Mg-rich forsterite feature is observed in a variety of ISO LWS spectra, but the corresponding Fe-rich olivine feature is not. For the 10 astronomical sources in our sample, the forsterite band peaks in the 68.9-69.3µm range and narrows with decreasing peak wavelength. This is consistent with the shortwards shifting of the peak observed when laboratory samples are cooled to 77K (69.07µm) and 3.5K (68.84µm). The shifted peak is produced by lattice contraction and the sharpening is due to a decrease in phonon density at lower temperatures. However, the astronomical bands are narrower than those of the laboratory samples. By comparing the laboratory and astronomical peak wavelengths, we deduce characteristic forsterite 69-µm band temperatures that are in the 27-84K range for the eight post-main-sequence objects in our sample. These values are shown to be consistent with the local continuum temperatures derived using a β =1.5 dust emissivity index, similar to derived interstellar values of the opacity index. For the pre-main sequence-objects HD 100546 and MWC 922, the characteristic 69-µm forsterite band temperatures (127±18 and 139±10K, respectively) are significantly higher than those of the post-main-sequence objects and are more than twice as high as their local continuum temperatures deduced using β =1.5. The assumption of large grains (β =0) can produce agreement between the derived 69-µm and continuum temperatures for one of these objects but not for the other - a spatial separation between the forsterite and continuum-emitting grains may therefore be implied for it. We conclude that observations of the peak wavelength and FWHM of the 69-µm forsterite band show great promise as a new diagnostic of characteristic grain temperatures.