The protoplanetary disk population in the ρ-Ophiuchi region L1688 and the time evolution of Class II YSOs
| Autor: | L. Testi, A. Natta, C. F. Manara, I. de Gregorio Monsalvo, G. Lodato, C. Lopez, K. Muzic, I. Pascucci, E. Sanchis, A. Santamaria Miranda, A. Scholz, M. De Simone, J. P. Williams |
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| Přispěvatelé: | European Research Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science |
| Jazyk: | angličtina |
| Rok vydání: | 2022 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
Protoplanetary disks MCC FOS: Physical sciences Astronomy and Astrophysics 3rd-DAS QC Physics Astrophysics - Solar and Stellar Astrophysics planetary systems [Submillimeter] Space and Planetary Science QB Astronomy Solar and Stellar Astrophysics (astro-ph.SR) formation [Stars] QC Astrophysics - Earth and Planetary Astrophysics QB |
| Popis: | (Abridged) We present a study of the disk population in L1688, the densest and youngest region in Ophiuchus, and we compare it with other nearby regions of different age, namely Lupus, Chamaeleon I, Corona Australis, Taurus and Upper Scorpius. We select our L1688 sample using a combination of criteria (ALMA data, Gaia, optical/near-IR spectroscopy) and determine stellar and disk properties, specifically stellar mass (Mstar), average population age, mass accretion rate (Macc) and disk dust mass (Mdust). a) In L1688 the relations between Macc and Mstar, Mdust and Mstar, and Macc and Mdust have a roughly linear trend with slopes 1.8-1.9 for the first two relations and ~1 for the third, similarly to what found in the other regions. b) When ordered according to the characteristic age of each region, Macc decreases as 1/t, when corrected for the different stellar mass content; Mdust follows roughly the same trend between 0.5 and 5 Myr, but has an increase of a factor ~3 at ages of 2-3 Myr. We suggest that this could result from an earlier planet formation, followed by collisional fragmentation that temporarily replenishes the millimeter-size grain population. c) The dispersion of Macc and Mdust around the best-fitting relation with Mstar, as well as that of Macc versus Mdust are large: we find that the dispersions have continuous distributions with a log-normal shape and similar width (~0.8 dex). The amount of dust observed at ~1 Myr does not appear to be sufficient to assemble the majority of planetary systems, which suggests an earlier planetary cores formation. The dust mass traces to a large extent the disk gas mass evolution. Two properties remain puzzling: the steep dependence of Macc and Mdust on Mstar and the cause of the large dispersion in the three relations analyzed in this paper, in particular the one of the Macc versus Mdust relation. A&A in press |
| Databáze: | OpenAIRE |
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