Can planet formation resolve the dust budget crisis in high redshift galaxies?
arXiv:1708.07053 · doi:10.1093/mnras/stx2162
Abstract
The process of planet formation offers a rich source of dust production via grain growth in protostellar discs, and via grinding of larger bodies in debris disc systems. Chemical evolution models, designed to follow the build up of metals and dust in galaxies, do not currently account for planet formation. We consider the possibility that the apparent under-prediction of dust mass in high redshift galaxies by chemical evolution models could be in part, due to these models neglecting this process, specifically due to their assumption that a large fraction of the dust mass is removed from the interstellar medium during star formation (so-called astration). By adding a planet formation phase into galaxy chemical evolution, we demonstrate that the dust budget crisis can be partially ameliorated by a factor of 1.3-1.5 only if a) circumstellar discs prevent a large fraction of the dust mass entering the star during its birth, and b) that dust mass is preferentially liberated via jets, winds and outflows rather than accreted into planetary-mass bodies.
9 pages, 11 figures, accepted for publication in MNRAS
References in corpus (23)
- The NumPy array: a structure for efficient numerical computation
- A Dust-Obscured Massive Maximum-Starburst Galaxy at a Redshift of 6.34
- One or more bound planets per Milky Way star from microlensing observations
- Dust Formation and Survival in Supernova Ejecta
- A dusty, normal galaxy in the epoch of reionization
- Freshly Formed Dust in the Cassiopeia A Supernova Remnant as Revealed by the Spitzer Space Telescope
- A stubbornly large mass of cold dust in the ejecta of Supernova 1987A
- Star formation and the interstellar medium in z>6 UV-luminous Lyman-break galaxies
- The dust mass in Cassiopeia A from a spatially resolved Herschel analysis
- The dust budget crisis in high-redshift submillimetre galaxies
- Dust production 680-850 million years after the Big Bang
- G11.92-0.61 MM1: A Keplerian disc around a massive young proto-O star
- The dust production rate of AGB stars in the Magellanic Clouds
- Dust origin in late-type dwarf galaxies: ISM growth vs. type II supernovae
- Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments
- Herschel-ATLAS: Properties of dusty massive galaxies at low and high redshifts
- Interstellar Dust Models and Evolutionary Implications
- The Herschel exploitation of local galaxy Andromeda (HELGA) V: Strengthening the case for substantial interstellar grain growth
- Grand challenges in protoplanetary disc modelling
- A "Rosetta Stone" for protoplanetary disks: The synergy of multi-wavelength observations
- From flux to dust mass: Does the grain-temperature distribution matter for estimates of cold dust masses in supernova remnants?
- Constraint on dust evolution processes in normal galaxies at detected by ALMA
- The sudden appearance of dust in the early Universe