Volume 573, January 2015
|Number of page(s)||10|
|Section||Interstellar and circumstellar matter|
|Published online||10 December 2014|
Absorption of crystalline water ice in the far infrared at different temperatures
Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany
Received: 26 May 2014
Accepted: 16 September 2014
The optical properties of ice in the far infrared are important for models of protoplanetary and debris disks. In this report, we derive a new set of data for the absorption (represented by the imaginary part of the refractive index κ) of crystalline water ice in this spectral range. The study includes a detailed inspection of the temperature dependence, which has not been conducted in such detail before. We measured the transmission of three ice layers with different thicknesses at temperatures ϑ = 10...250 K and present data at wavelengths λ = 80...625 μm. We found a change in the spectral dependence of κ at a wavelength of 175 ± 6 μm. At shorter wavelengths, κ exhibits a constant flat slope and no significant temperature dependence. Long-ward of that wavelength, the slope gets steeper and has a clear, approximately linear temperature dependence. This change in behaviour is probably caused by a characteristic absorption band of water ice. The measured data were fitted by a power-law model that analytically describes the absorption behaviour at an arbitrary temperature. This model can readily be applied to any object of interest, for instance a protoplanetary or debris disk. To illustrate how the model works, we simulated the spectral energy distribution (SED) of the resolved, large debris disk around the nearby solar-type star HD 207129. Replacing our ice model by another, commonly used data set for water ice results in a different SED slope at longer wavelengths. This leads to changes in the characteristic model parameters of the disk, such as the inferred particle size distribution, and affects the interpretation of the underlying collisional physics of the disk.
Key words: methods: laboratory: solid state / techniques: spectroscopic / circumstellar matter / stars: individual: HD 207129
© ESO, 2014
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