SIMBAD references

2013ApJ...762..128O - Astrophys. J., 762, 128 (2013/January-2)

The physical structure of protoplanetary disks: the Serpens cluster compared with other regions.

OLIVEIRA I., MERIN B., PONTOPPIDAN K.M. and VAN DISHOECK E.F.

Abstract (from CDS):

Spectral energy distributions are presented for 94 young stars surrounded by disks in the Serpens Molecular Cloud, based on photometry and Spitzer/IRS spectra. Most of the stars have spectroscopically determined spectral types. Taking a distance to the cloud of 415 pc rather than 259 pc, the distribution of ages is shifted to lower values, in the 1-3 Myr range, with a tail up to 10 Myr. The mass distribution spans 0.2-1.2 M, with median mass of 0.7 M. The distribution of fractional disk luminosities in Serpens resembles that of the young Taurus Molecular Cloud, with most disks consistent with optically thick, passively irradiated disks in a variety of disk geometries (Ldisk/Lstar∼ 0.1). In contrast, the distributions for the older Upper Scorpius and η Chamaeleontis clusters are dominated by optically thin lower luminosity disks (Ldisk/Lstar∼ 0.02). This evolution in fractional disk luminosities is concurrent with that of disk fractions: with time disks become fainter and the disk fractions decrease. The actively accreting and non-accreting stars (based on Hα data) in Serpens show very similar distributions in fractional disk luminosities, differing only in the brighter tail dominated by strongly accreting stars. In contrast with a sample of Herbig Ae/Be stars, the T Tauri stars in Serpens do not have a clear separation in fractional disk luminosities for different disk geometries: both flared and flat disks present wider, overlapping distributions. This result is consistent with previous suggestions of a faster evolution for disks around Herbig Ae/Be stars. Furthermore, the results for the mineralogy of the dust in the disk surface (grain sizes, temperatures and crystallinity fractions, as derived from Spitzer/IRS spectra) do not show any correlation to either stellar and disk characteristics or mean cluster age in the 1-10 Myr range probed here. A possible explanation for the lack of correlation is that the processes affecting the dust within disks have short timescales, happening repeatedly, making it difficult to distinguish long-lasting evolutionary effects.

Abstract Copyright:

Journal keyword(s): circumstellar matter - methods: statistical - planetary systems - protoplanetary disks - stars: pre-main sequence

VizieR on-line data: <Available at CDS (J/ApJ/762/128): table1.dat>

Simbad objects: 106

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2021.09.27-20:37:57

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