A 10 μm spectroscopic survey of Herbig Ae star disks: Grain growth and crystallization

By R. van Boekel, M. Min, L. Waters, A. D. Koter, C. Dominik, M. V. D. Ancker, J. Bouwman. 2005

256 citations recorded by the source corpus.

We present spectroscopic observations of a large sample of Herbig Ae stars in the 10 µm spectral region. We perform compositional fits of the spectra based on properties of homogeneous as well as inhomogeneous spherical particles, and derive the mineralogy and typical grain sizes of the dust responsible for the 10 µm emission. Several trends are reported that can constrain theoretical models of dust processing in these systems: i) none of the sources consists of fully pristine dust comparable to that found in the interstellar medium; ii) all sources with a high fraction of crystalline silicates are dominated by large grains; iii) the disks around more massive stars (M > 2.5 M� , L > 60 L� ) have a higher fraction of crystalline silicates than those around lower mass stars, iv) in the subset of lower mass stars (M < 2.5 M� ) there is no correlation between stellar parameters and the derived crystallinity of the dust. The correlation between the shape and strength of the 10 micron silicate feature reported by van Boekel et al. (2003) is reconfirmed with this larger sample. The evidence presented in this paper is combined with that of other studies to present a likely scenario of dust processing in Herbig Ae systems. We conclude that the present data favour a scenario in which the crystalline silicates are produced in the innermost regions of the disk, close to the star, and transported outward to the regions where they can be detected by means of 10 micron spectroscopy. Additionally, we conclude that the final crystallinity of these disks is reached very soon after active accretion has stopped.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/a2afacbbc2f5f20617b30898693450246ebda9f1

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Citations in the corpus

CRYSTALLINE SILICATES AND DUST PROCESSING IN THE PROTOPLANETARY DISKS OF THE TAURUS YOUNG CLUSTER (2007, methodology): “With various simplifying assumptions, this technique has been applied to silicate emission in the spectra of Class II objects and Herbig Ae/Be stars by many previous workers (e.g., Przygodda et al. 2003; Meeus et al. 2003; van Boekel et al. 2005; Kessler-Silacci et al. 2005; Bouwman et al. 2008).”
PHOTOEVAPORATION OF CIRCUMSTELLAR DISKS BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET AND X-RAY RADIATION FROM THE CENTRAL STAR (2008, background): “As disks evolve, dust grains are believed to coagulate and grow, and perhaps settle (e.g., van Boekel et al. 2005; Natta et al. 2000), reducing the opacity per H nucleus in the disk.”
Probing dust grain evolution in IM Lupi's circumstellar disc. Multi-wavelength observations and mo (2008, methodology): “In this paper,we adopt the spectrum obtained with the full aperture extraction method because of its better stability. grain growth in discs (e.g. van Boekel et al. 2005 and Kessler-Silacci et al. 2006).”
STRUCTURES IN THE PROTOPLANETARY DISK OF HD142527 SEEN IN POLARIZED SCATTERED LIGHT (2013, background): “The inner disk is highly crystalline and is responsible for the mid-infrared emission (Leinert et al. 2004; van Boekel et al. 2005).”
Dust Evolution and the Formation of Planetesimals (2016, background): “While the (sub-)millimeter wavelengths reveal dust growth in the disk interior, dust growth in the disk atmosphere is also evidenced by the broad and weak silicate 10µm emission features which are expected from silicates with larger sizes than those in ISM (van Boekel et al. 2005).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, methodology): “We adopt the distance estimate of van Boekel et al. (2005), d = 140pc, and the F4 spectral type determined by Dunkin et al. (1997).”
Size-sorting dust grains in the surface layers of protoplanetary disks (2008, unknown): “This solid state infrared emission feature, seen in the majority of protoplanetary disks, has often been used as a probe of grain size (e.g. van Boekel et al. 2005; Schegerer et al. 2006).”
Accretion Rates in Herbig Ae stars (2006, background): “It is worth to remind, in this context, the well known bias due to the spectral type selection, which introduces an age-mass correla- tion in the sample (e.g., van Boekel et al. 2005) and automatically excludes young, relatively low mass (<∼ 2.5 M⊙) objects.”