Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.astro.spbu.ru/staff/ilin2/INTAS2/PAP/P2_3.pdf Äàòà èçìåíåíèÿ: Fri Nov 19 16:18:19 2010 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 02:59:58 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: massive stars

Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

www.elsevier.com/locate/jqsrt

A database of optical constants of cosmic dust analogs
Cornelia Jagera ; , Vladimir B. Il'inb , Thomas Henningc; a , Harald Mutschkea , Dirk Fabiana , Dmitry A. Semenova; b , Nikolai V. Voshchinnikovb
a

Astrophysical Institute and University Observatory, Friedrich Schiller University, Max-Wien-Platz 1, D-07745 Jena, Germany b Astronomical Institute of St. Petersburg State University, 198504 St. Petersburg, Russia c Max Planck Institute for Astronomy, D-69117 Heidelberg, Germany Received 31 May 2002; accepted 13 August 2002

Abstract We describe the current state and future of the WWW Jena-Petersburg database of optical constants (JPDOC) that also contains references to papers and links to internet resources related to measurements or calculations of the optical constants of materials of astronomical interest. The most important part of the JPDOC are data measured in broad wavelength ranges and partly at low temperatures in the Jena Laboratory. To demonstrate the use of these data, we show as examples infrared refractive indices of crystalline and amorphous magnesium silicates, spinel, and hydrogenated amorphous carbon and calculate the absorption cross-sections of small particles composed of these materials. ? 2003 Elsevier Science Ltd. All rights reserved.
Keywords: Spectroscopy; Optical constants; Databases; Light scattering

1. Introduction Nanometer- and micrometer-sized solid particles are distributed in the interstellar medium and play an important role for astrophysical processes such as star and planet formation. These particles show a rich chemistry and mineralogy as has been revealed by spectroscopic astronomical observations in the last decades. Many new observational data have been measured in the last years, e.g. by the Infrared Space Observatory in 1995 ­1998, and the interpretation of these spectroscopic data is still in progress. This requires the comparison with data of "analog materials" delivered by spectroscopical laboratories.


Corresponding author. Tel.: +49-3641-947-535; fax: +49-3641-947-532. E-mail address: conny@astro.uni-jena.de (C. Jager).

0022-4073/03/$ - see front matter ? 2003 Elsevier Science Ltd. All rights reserved. PII: S0022-4073(02)00301-1


766

C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

Various terrestrial analogs of cosmic solids have been studied in chemical and physical laboratories. However, many of these experiments neither took into account the speciÚcs of cosmic dust materials (composition, lattice structure, processing, etc.), nor covered the wavelength intervals of the current astrophysical interests. Note also that these data are mainly in the form of graphics in papers, and free world wide web (WWW) resources on the optical constants are generally limited by several collections of refractive indices for a few materials. Since 1992, the Astrophysical Institute and University Observatory (AIU) Jena operates a Chemical and Spectroscopical Laboratory with the goal to study optical properties of analog materials of cosmic dust in the wavelength range from the ultraviolet to the far infrared. During this period, a compilation of optical constants (i.e. the complex refractive index m = n + ik or the complex dielectric function = m2 ) of such materials has been created. In collaboration with the Astronomical Institute of St. Petersburg University, this collection was expanded into an internet database that has been made available for the public in 1998 at http://www.astro.uni-jena.de/Users/database/entry.html or http://www.astro.spbu.ru/JPDOC/entry.html. In this paper, we describe the current state and future of the database and give several examples of the data it contains and their possible applications. 2. Electronic database 2.1. Current state The Jena-Petersburg database of optical constants (JPDOC) provides access to references to the papers, data Úles and links to the internet resources related to measurements and calculations of optical constants in the wavelength interval from X-rays to the radio domain. The materials being considered are: · · · · · · · amorphous/glassy/crystalline silicates of di erent kinds, silicon, SiO, crystalline/fused SiO2 , metals: Fe, Mg and others, oxides: FeO, Fe2 O3 ; Fe3 O4 , MgO, Al2 O3 ; MgAl2 O4 , sulÚdes: FeS, MgS, SiS2 , carbides: SiC, FeC, TiC, carbonaceous species: diamonds, graphite, coals, kerogens, HAC, glassy/amorphous carbon, PAHs and so on, · organics: tholin, "organic refractory", etc., · ices: H2 O, CO, CO2 ; NH3 , HCN, etc., and their mixtures, · FeSi, CaCO3 and others.

The database contains more than 1000 references to the papers, reports, dissertations where the refractive index, re ectivity, transmittance, etc., were derived. It also gives references to useful books and reviews on the subject. Data accessible via the JPDOC are mainly those measured in the laboratory of the AIU Jena supplemented with data freely available in the internet. The database also provides links to internet collections of optical data Úles and personal WWW pages with relevant software. The Úrst version of the JPDOC was described in [1]. In the following years (1999 ­2001) only minor improvements were made. All the time the site was rather well visited--on average about Úve


C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

767

visitors a day and all together over 5000 visits for 3 years--and many visitors found the database helpful. That encouraged us to make essential updates in 2002. We increased by about 25% the number of references to papers (not only to the recent ones) in physical and astronomical journals as well as to books and reviews. Further, we opened access to more data from the Jena Laboratory, connected new pages presenting recently calculated low-temperature Rosseland and Planck mean opacities, included new materials (FeSi, CaCO3 , etc.), gave more links to other internet resources (incl. Io e Institute site, database of optical properties (DOP), etc.), and presented some more graphical illustrations and information about the physical properties of the materials. 2.2. Future plans We intend to continue including new data and collecting references and links to resources on the subject. Collaboration is planned with the Physical Institute of the St. Petersburg University, Io e Physical Institute and the St. Petersburg Institute of Precise Mechanics and Optics. If it is successful, original data and bibliography for the materials--interesting not only for astronomical but some other applications--will be involved as well. Some changes of the general design of the database are planned too, but main e orts will be directed at extension of the JPDOC. The next step will be the creation of the DOP of scatterer models which will include the JPDOC as a part. 2.3. Database of optical properties In astrophysics, the optical constants are mainly used to calculate the optical properties of scatterers, i.e. cross-sections, scattering matrix, etc. For many applications, it is necessary to understand general trends in the data. This understanding can often be gained from consideration of results obtained by simpliÚed scattering models. Optical properties derived from such models have been discussed in some books (see, e.g. [2,3]). In principle they can be calculated by using various light-scattering tools which are freely available via the internet [4]. Nevertheless, there is a deÚnite necessity of a WWW database devoted to systematic consideration of the optical properties of various model scatterers and related topics. As of this writing, our database will include: · original codes realizing various methods to calculate the optical properties of homogeneous and inhomogeneous, spherical and nonspherical particles; · review(s) of exact and approximate methods of light scattering theory (including discussion of their applicability ranges); · a review on the e ective medium theory (EMT) and computer programs to mix the optical constants for composite particles according to di erent EMT rules; · a database of several thousands references to papers on various aspects of light scattering theory and its applications; · a graphics library illustrating light scattering by particles of di erent size/shape/structure (a part of the data will be in tabular form to serve as benchmarks); · a special tool to calculate on-line selected optical characteristics of di erent scatterers (homogeneous and core-mantle spheres, inÚnite cylinders, spheroids, etc.);


768

C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

· a self-training algorithm of determination of the optical properties of randomly oriented fractal-like clusters of spherical particles based on an artiÚcial neural network (perceptron) (see [5] for more details); · a collection of links to related internet resources. The work on all the parts of the DOP is either in progress or has been Únished. It is undertaken by several persons from di erent institutes of former Soviet Union countries under support of an INTAS grant. The DOP will be (partly) available via the Internet [6] upon its completion scheduled at the end of 2002. Because of the large volume due to the graphics library, the whole database may be available only on CDs. 3. Examples of data contained in the JPDOC Most of the materials studied in Jena are synthetic compounds prepared especially for the purpose of spectroscopic investigation. They include silicates in both amorphous and crystalline state, oxides of magnesium, iron, and aluminum, sulÚdes, and carbon in di erent forms. Chemical and physical analytical methods were generally applied to conÚrm the homogeneity, composition, and crystal structure of the products prior to the spectroscopic measurements. Further, some natural crystals (oxides and silicates) have been included in the studies. If necessary, data have been determined for the di erent crystallographic axes. For part of the compounds, data are available at cryogenic temperatures. A summary of the data currently available is given in Table 1. In the following we give some examples of the data and their possible applications. 3.1. Crystalline silicates Silicate minerals of the olivine and pyroxene classes have been shown to be present in out ows of evolved stars as well as in comets and protoplanetary disks. The positions of the infrared emission
Table 1 Summary of data measured in the Jena laboratory, which are currently available from the JPDOC Compound Silicates Composition (Mg; Fe)SiO3 , (Mg; Fe)2 SiO4 MgSiO3 , (Mg; Fe)2 SiO4 MgSix Oy (Ca; Al; Mg; Fe)Six O (Mg,Fe)S SiS2 (Mg,Fe)O Al2 O3 (Mg; Al)Ox a-C:H Cryst. state Glassy Cryst. Amorph. Amorph. Cryst. Cryst. Cryst. Amorph. Cryst. Amorph. Spectral range UV/VIS/IR IR UV/VIS/IR IR IR IR UV/VIS/IR IR IR UV/VIS/IR Data sets 10 2 5 13 5 1 6 2 8 6 At 10 K 1 1 1 1 1

SulÚdes Oxides Carbon

y


C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

769

bands produced by these minerals are diagnostic for the crystal structure as well as for the chemical composition, especially the iron content. Comparison of the laboratory data with observed features can constrain the conditions in these environments which have led to the formation or processing of the dust grains. We have used the infrared optical constants of forsterite contained in the database for calculating the absorption cross sections of spherical and nonspherical particles with sizes small compared to the wavelength (see Fig. 1). The calculations have been performed for prolate spheroidal shapes with the long spheroid axis corresponding to the crystallographic c direction. The spectra show resonances due to surface modes which shift very strongly as a function of the aspect ratio of the particles. This e ect is probably very important for the identiÚcation of emission features in astronomical spectra [8,9]. Interstellar polarization measurements and laboratory experiments on the growth of silicate particles [10] support the presence of elongated grains in astrophysical environments. Information about the grain shape may provide constraints for the formation mechanism of crystalline silicate grains, i.e. the role of direct condensation vs. processing of previously amorphous material. 3.2. Amorphous magnesium silicate About 85 ­90% of the dust condensing in the envelopes of oxygen-rich evolved stars consist of amorphous magnesium or magnesium­iron silicates [7]. Therefore, special attention is paid to the production and spectroscopic characterization of analog materials for this dust component. The comparison between di erently produced magnesium silicates demonstrates that the amorphous state of any magnesium silicate is not unique. There exist di erent possibilities for the structural arrangement of subunits in the amorphous silicate network, similar to the varying structures of amorphous carbon. Optical constants (n; k ) of stoichiometric and nonstoichiometric magnesium silicates with Mg/Si ratios from 0.7 to 2.4 produced by the sol­gel method have been derived from re ection measurements by a combination of Kramers­Kronig analysis and Lorentz-oscillator Út method (see Fig. 2). The absorption cross sections calculated for particles small compared to the wavelength show that the Mg/Si ratio in uences the position and the width of the 10 and 20 m bands. With increasing MgO content the 10 m band shifts to longer wavelengths whereas the 20 m band becomes broadened and centered at shorter wavelengths. The astrophysical relevance of these sol­gel silicates was tested by comparison of optically thin model spectra based on the new optical data with the dust emissivity derived from ISO-SWS spectra of AGB stars in the range between 8 and 30 m. The emission spectrum of TY Dra, an evolved dust-forming star, can excellently be reproduced by the models, suggesting that the dust grains may indeed consist of pure amorphous Mg silicate [11]. 3.3. Magnesium­aluminium oxide (spinel) Magnesium­aluminium spinel (MgAl2 O4 ) has been considered as a primary condensate in the out ows of oxygen-rich AGB stars and as a potential carrier of the 13 m emission band observed in the spectra of these stars [12]. Therefore, in the Jena laboratory, a systematic study of the infrared properties of Mg­Al oxides of both synthetic and natural origin was performed in order to derive the


770

C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

Fig. 1. Upper panel: Imaginary part of the refractive index for crystalline forsterite (Mg2 SiO4 ) in the three di erent crystallographic directions. Lower panel: Mass-normalized absorption cross section of prolate spheroidal forsterite particles (averaged over all spatial orientations) with di erent axis ratios. The dots and asterisks below the spectra indicate positions of astronomically observed emission bands (after [7]).

optical constants of these materials. This led to the discovery of two accompanying features in the astronomical spectra at larger wavelengths, thereby strongly supporting the idea of spinel condensates in AGB star out ows (see Fig. 3, [13]). Recently, the experiments have been extended in the direction of Ca­Al oxide minerals [14] and condensation studies of oxide grains in low-pressure oxygen-rich atmospheres.


C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

771

Fig. 2. Left panel: Imaginary part of the refractive index for amorphous Mg0:7 SiO2:7 (dotted line) and Mg2:4 SiO4:4 (solid line). Right panel: Absorption cross section normalized to particle volume calculated for a continuous distribution of ellipsoidal grain shapes (CDE [3], grain sizes small compared to the wavelength) composed of the same materials.

Fig. 3. Left panel: Imaginary part of the refractive index for synthetic and natural magnesium­aluminium spinels. Right panel: Calculated normalized absorption spectra for spherical particles small compared to the wavelength composed of natural spinel (smooth solid line) and synthetic MgAl2 O4 (dotted line) in comparison to the band proÚle of the newly discovered 32 m feature [13]. "Read leak" denotes an instrumental artifact in the astronomical spectrum.

3.4. Hydrogenated amorphous carbon Amorphous carbonaceous materials can show a great diversity of optical properties due to the variability in their nanostructure. Especially in the infrared range, the optical constants can di er by orders of magnitude according to the conducting or insulating electrical behavior of the material. The amorphous-carbon data contained in the database cover a wide range of these properties as is illustrated by Fig. 4. The di erently pyrolized celluloses are representative for a suit of carbonaceous material ranging from strongly disordered (mainly aliphatic, lower pyrolysis temperature) to graphitized (mainly aromatic, higher pyrolysis temperature) material. Especially interesting for astronomy is the calculation of the absorption and scattering cross sections for particles small compared to the wavelength. Fig. 5 shows that particles composed of the


772

C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

Fig. 4. Complex refractive index of hydrogenated amorphous carbon prepared by pyrolysis (annealing) of cellulose at di erent temperatures.

Fig. 5. Volume-normalized absorption cross section calculated for spherical grains small compared to the wavelength (left panel) and a continuous distribution of ellipsoidal grain shapes (CDE [3], right panel) from the optical data given in Fig. 4.

strongly disordered material (400 C) produce an absorption which is smaller by up to 3 orders of magnitude compared to particles formed from the graphitized material (1000 C). The absorption cross section of carbonaceous particles in the far infrared ( ¿ 100 m) can be Útted by a power law (Cabs =V -Ú ) depending strongly on the internal structure of the carbon materials and on the particle shape. In the case of spherical grains, the spectral index Ú is considerably lower for the highly disordered material than for the carbon material pyrolized at higher temperature. With increasing graphitization due to a higher pyrolysis temperature there is a gradual increase of Ú [15]. Our calculations for di erent particle shapes show that there is no morphological e ect on the spectral index of the low-temperature samples in contrast to the more graphitic materials. For the latter materials we Únd a signiÚcantly lower index in the case of broad shape distributions (CDE) compared to spherical grain shapes. This is caused by percolation e ects, present in the more graphitized samples which contain free charge carriers. We should note that the results of the CDE


C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

773

calculations serve as an illustrative example. For a more realistic calculation, one a special aggregate structure and/or shape distribution of the individual particles [16 values of the refractive indices, however, computational methods for the calculation of by aggregates or elongated particles become numerically cumbersome and may even 4. Summary and outlook

has to assume ]. For extreme the absorption fail.

We have presented recent developments in the Jena-Petersburg database of optical constants (JPDOC) and have demonstrated examples for the application of optical constants contained for purposes of comparison with astronomical spectroscopic observations. The database will be continued to be improved. This will include measurements on further analog materials of cosmic dust such as oxide and carbonaceous particles from gas condensation experiments, nanodiamonds, and others. An extensive database will give better possibilities to achieve uniqueness in the identiÚcation of astronomically observed bands and provide the possibility to study grain size, shape and agglomeration e ects in a realistic way. The authors will highly acknowledge any contribution to the database such as references, data Úles and links to be included in the database. Acknowledgements We are grateful to all the people who sent us their comments and remarks on the JPDOC. We also thank the German Research Foundation for supporting our experimental work by several grants to the Research Group "Laboratory Astrophysics". The development of the WWW database was supported by the Volkswagen Foundation and the INTAS grant 99/652. V.I. acknowledges the support by the RFBR grant 00-15-96607. References
[1] Henning T, Il'in VB, Krivova NA, Michel B, Voshchinnikov NV. WWW database of optical constants for astronomy. Astron Astrophys Suppl 1999;136:405 ­ 6. [2] Wickramasinghe NC. Light scattering functions for small particles with applications in astronomy. London: Chapman & Hall, 1973. [3] Bohren CF, Hu man DR. Absorption and scattering of light by small particles. New York: Wiley, 1983. [4] Th.Wriedt web site. http://www.T-matrix.de. [5] Beletsky SA, Tishkovets VP, Waters LBFM, Dominic C, Litvinov PV. Database of the optical properties of chaotically oriented fractal-like clusters of spherical particles. In: Optics of cosmic dust. Abstracts of NATO Advanced Research Workshop, Bratislava, 2002, p. 10 ­1. [6] DOP project web site. http://www.astro.spbu.ru/sta /ilin2/DOP/. [7] Molster FJ, Waters LBFM, Tielens AGGM. Crystalline silicates around evolved stars II. The crystalline silicate complexes. Astron Astrophys 2002;382:222 ­ 40. [8] Fabian D, Henning T, Jager C, Mutschke H, Dorschner J, Werhan O. Steps toward interstellar silicate mineralogy VI. Dependence of crystalline olivine IR spectra on iron content and particle shape. Astron Astrophys 2001;378: 228 ­ 38. [9] Henning T, Mutschke H. Optical properties of cosmic dust analogs. In: Sitko ML, Sprague AL, Lynch DK, editors. Thermal emission spectroscopy and analysis of dust, disks, and regoliths. ASP Conf Ser 2000;196:253­71.


774

C. Jager et al. / Journal of Quantitative Spectroscopy & Radiative Transfer 79­80 (2003) 765 ­ 774

[10] Tsuchiyama A. Condensation experiments using a forsterite evaporation source in H2 at low pressures. Mineral J 1998;20:59 ­ 80. [11] Jager C, Dorschner J, Posch T, Henning T. Steps toward interstellar silicate mineralogy VII. Spectral properties and crystallization behaviour of magnesium silicates produced by the sol­gel method. Astron Astrophys, submitted for publication. [12] Posch T, Kerschbaum F, Mutschke H, Fabian D, Dorschner J, Hron J. On the origin of the 13 m feature. Astron Astrophys 1999;352:609 ­ 18. [13] Fabian D, Posch T, Mutschke H, Kerschbaum F, Dorschner J. Infrared optical properties of spinels. Astron Astrophys 2001;373:1125 ­ 38. [14] Mutschke H, Posch T, Fabian D, Dorschner J. On the identiÚcation of circumstellar hibonite, Astron Astrophys. 392, 1047­52. [15] Jager C, Mutschke H, Dorschner J, Henning T. Optical properties of carbonaceous dust analogues. Astron Astrophys 1998;332:291 ­ 301. [16] Quinten M, Kreibig U, Henning T, Mutschke H. Wavelength-dependent optical extinction of carbonaceous particles in atmospheric aerosols and interstellar dust. Appl Opt-LP, 41, 7102­12.