On planet formation in HL Tau
By Giovanni Dipierro, Daniel J. Price, Guillaume Laibe, Kieran Hirsh, Alice Cerioli, G. Lodato. 2015
202 citations recorded by the source corpus.
We explain the axisymmetric gaps seen in recent long-baseline observations of the HL Tau protoplanetary disc with the Atacama Large Millimetre/Submillimetre Array (ALMA) as being due to the different response of gas and dust to embedded planets in protoplanetary discs. We perform global, three dimensional dusty smoothed particle hydrodynamics calculations of multiple planets embedded in dust/gas discs which successfully reproduce most of the structures seen in the ALMA image. We find a best match to the observations using three embedded planets with masses of 0.2, 0.27 and 0.55 MJ in the three main gaps observed by ALMA, though there remain uncertainties in the exact planet masses from the disc model.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/7a27136d336696368a63b9ab5e554703240e1466
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In Astronomy and Astrophysics
- Christoph Federrath
- S. Glover
- Ralf Klessen
- Daniel J. Price
- C. Dobbs
- S. Okuzumi
- Hidekazu Tanaka
- A. Morbidelli
Citations in the corpus
- Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics (2017, methodology): “For recent applications of Phantom to more realistic problems involving dust/gas mixtures see Dipierro et al. (2015, 2016), Ragusa et al. (2017) and Tricco et al. (2017).”
- DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, background): “Dedicated HL Tau simulations by Dipierro et al. (2015) indicate planet masses between 60 and 175 M⊕, which is, depending on the ring, of the same order or up to a factor ∼ 10 larger than our mass estimate.”
- SINTERING-INDUCED DUST RING FORMATION IN PROTOPLANETARY DISKS: APPLICATION TO THE HL TAU DISK (2015, background): “…interaction (Paardekooper & Mellema 2004, 2006; Fouchet et al. 2010; Zhu et al. 2012; Pinilla et al. 2012; Gonzalez et al. 2012; Dong et al. 2015; Dipierro et al. 2015), magnetorotational instability (Johansen et al. 2009; Uribe et al. 2011), and/or steep radial variation of the disk viscosity…”
- Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, background): “Also, the rings observed in the disk around the still embedded <1 Myr old HL Tau protostar (ALMA Partnership et al. 2015) may be carved by the presence of planets (e.g., Dipierro et al. 2015) suggesting, again, early planet formation.”