Dispersal timescale of protoplanetary disks in the low-metallicity young cluster Dolidze 25
| Autor: | Nick Wright, Giuseppina Micela, Salvatore Sciortino, Katia Biazzo, Jeremy J. Drake, Ettore Flaccomio, L. Prisinzano, Coralie Neiner, F. Damiani, M. G. Guarcello |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Metallicity
Population FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Q1 01 natural sciences Planet 0103 physical sciences QB460 Cluster (physics) Astrophysics::Solar and Stellar Astrophysics QD education 010303 astronomy & astrophysics Stellar density Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics QB600 O-type star QB Earth and Planetary Astrophysics (astro-ph.EP) Physics education.field_of_study 010308 nuclear & particles physics Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Photoevaporation Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Biological dispersal Astrophysics::Earth and Planetary Astrophysics Astrophysics - Earth and Planetary Astrophysics |
| ISSN: | 0004-6361 |
| Popis: | The dispersal of protoplanetary disks sets the timescale available for planets to assemble, and thus it is one of the fundamental parameters in theories of planetary formation. Disk dispersal is determined by several properties of the central star, the disk itself, and the surrounding environment. In particular, the metallicity of disks may impact their evolution, even if to date controversial results exist: in low-metallicity clusters disks seem to rapidly disperse, while in the Magellanic Clouds some evidence supports the existence of accreting disks few tens of Myrs old. In this paper we study the dispersal timescale of disks in Dolidze~25, the young cluster in proximity of the Sun with lowest metallicity, with the aim of understanding whether disk evolution is impacted by the low-metallicity of the cluster. We have analyzed Chandra/ACIS-I observations of the cluster and combined the resulting source catalog with existing optical and infrared catalogs of the region. We selected the disk-bearing population and the disk-less population of Dolidze 25. We have derived stellar parameters from isochrones fitted to color-magnitude diagrams. We derived a disk fraction of about 34% and a median age of 1.2 Myrs. By comparing this estimate with existing estimates of the disk fraction of clusters younger than 10 Myrs, our study suggests that the disk fraction of Dolidze 25 is lower than what is expected from its age alone. Even if our results are not conclusive given the intrinsic uncertainty on stellar ages estimated from isochrones fitting to color-magnitude diagrams, we suggest that disk evolution in Dolidze 25 may be impacted by the environment. Given the poor O star population and low stellar density of the cluster, it is more likely that disks dispersal timescale is dictated more by the low metallicity of the cluster rather than external photoevaporation or dynamical encounters. Accepted for publication by Astronomy & Astrophysics |
| Databáze: | OpenAIRE |
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