X-Shooter study of accretion in Chamaeleon I

By C. Manara, L. Testi, G. Herczeg, Ilaria Pascucci, J. Alcalá, A. Natta, S. Antoniucci, D. Fedele, G. Mulders, T. Henning and 3 more. 2015

148 citations recorded by the source corpus.

We present the analysis of 34 new VLT/X-Shooter spectra of young stellar objects in the Chamaeleon I star forming region, together with four more spectra of stars in Taurus and two in Chamaeleon II. The broad wavelength coverage and accurate flux calibration of our spectra allow us to estimate stellar and accretion parameters for our targets by fitting the photospheric and accretion continuum emission from the Balmer continuum down to 700 nm. The dependence of accretion with stellar properties for this sample is consistent with previous results from the literature. The accretion rates for transitional disks are consistent with those of full disks in the same region. The spread of mass accretion rates at any given stellar mass is found to be smaller than in many studies, but is larger than that derived in the Lupus clouds using similar data and techniques. Differences in the stellar mass range and in the environmental conditions between our sample and that of Lupus may account for the discrepancy in scatter between Chamaeleon I and Lupus. Complete samples in Chamaeleon I and Lupus are needed to determine whether the difference in scatter of accretion rates and the lack of evolutionary trends are robust to sample selection.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/6c53310f67d92f14cc040b7f56556f4088a09422

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Citations in the corpus

Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “The accretion luminosity is usually 1%–10% of the photospheric luminosity and can therefore be ignored, though in rare cases the accretion luminosity may dominate (e.g., Manara et al. 2017).”
Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud (2019, background): “Disk size–luminosity relationship Disk population studies reveal scaling relations in multiple dimensions (e.g., M∗,Mdisk, Ṁ∗, Rdisk), linking disk evolution with the bulk properties of disks (e.g., Manara et al. 2016, Ansdell et al. 2016, Pascucci et al. 2016, Mulders et al. 2017).”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, methodology): “As discussed in Manara et al. (2016a) and C. Manara et al. (2016, in preparation), the difference between the new and literature spectral type is in most cases less than a spectral subclass.”
Formation of planetary systems by pebble accretion and migration (2018, background): “If one were to only consider viscously driven gas accretion, the initial accretion rate would be Ṁgas = 7 × 10−10 M yr−1, which would be in a lower range of observed gas accretion rates around young stars (Manara et al. 2016).”
Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, background): “Furthermore, significantly underestimated disk dust masses would conflict with the observed general agreement of the measured disk masses and mass accretion rates with expectations from viscous evolution theory (e.g., Manara et al. 2016; Rosotti et al. 2017; Lodato et al. 2017).”