Processing of silicate dust grains in Herbig Ae/Be systems

Abstract

Abstract. We have analysed the 10 µm spectral region of a sample of Herbig Ae/Be (HAEBE) stars. The spectra are dominated by a broad emission feature caused by warm amorphous silicates, and by polycyclic aromatic hydrocarbons. In HD 163296 we find aliphatic carbonaceous dust, the first detection of this material in a HAEBE star. The silicate band shows a large variation in shape, due to variable contributions of three components: (i) a broad shoulder at 8.6 µm; (ii) a broad maximum at 9.8 µm; and (iii) a narrow feature with a broad underlying continuum at 11.3 µm. From detailed modeling these features can be identified with silica (SiO2), sub-micrometer sized amorphous olivine grains and micrometer sized amorphous olivine grains in combination with forsterite (Mg2SiO4), respectively. Typical mass fractions are 5 to 10 per cent of crystalline over amorphous olivine, and a few per cent of silica compared to the olivines. The detection of silica in emission implies that this material is heated by thermal contact with other solids that have a high absorptivity at optical to near-IR wavelengths. The observed change in peak position of the silicate band in HAEBE stars from 9.7 µm to 11.3 µm is dominated by an increase in average grain size, while changes in composition play only a minor rôle. The HAEBE stars, β Pic and the solar system comet Halley form a sequence of increasing crystallinity. We find that the abundance of SiO2 tends to increase with increasing crystallinity. This is consistent with the compositional changes expected from thermal annealing of amorphous grains in the inner regions of the disk. We confirm earlier studies that the timescale for crystallisation of silicates in disks is longer than that of coagulation. Our results indicate that the processes that governed grain processing in the proto-solar nebula, are also at work in HAEBE stars.

Episodic formation of cometary material in the outburst of a young Sun-like star

“…Longward of this peak no other crystalline features are present in the spectrum. The observed crystalline features are similar to those present in comet spectra 3,14 (panel d) and in a number of protoplanetary disks 15,16 . The remaining differences between EX Lupi and Since the quiescent spectrum exhibits no crystalline silicate features, the appearance of crystalline features in the EX Lupi outburst strongly suggests that we witness on-going crystal formation; to our knowledge for the first time in a celestial object.…”

Dust amorphization in protoplanetary disks

“…Therefore, this model is more realistic than previous methods using polynomials (Bouwman et al 2001), single temperature We conclude from the spectral fits that the continuous temperature distribution of the disk is a robust model to approximate the continuum emission. We are able to adjust the background by just one geometrical parameter, i.e.…”

A new analysis of the nucleus of NGC 1068 with MIDI observations

“…In addition to grain sizes, such a difference in extinction laws of the Galactic ISM and Seyfert II AGNs can also result from a temperature gradient in the obscuring dust (Imanishi 2000). Evidence of the flattening of the silicates optical depth with the growth of grain size is presented by Bouwman et al (2001) and Kemper et al (2004).…”