Planet migration in protoplanetary discs plays an important role in the longer term evolution of planetary systems, yet we currently have no direct observational test to determine if a planet is migrating in its gaseous disc. We explore the formation and evolution of dust rings - now commonly observed in protoplanetary discs by the Atacama Large Millimeter/submillimeter Array - in the presence of relatively low-mass (12-60 M) migrating planets. Through 2D hydrodynamical simulations using gas and dust we find that the importance of perturbations in the pressure profile interior and exterior to the planet varies for different particle sizes. For small sizes, a dust enhancement occurs interior to the planet, whereas it is exterior to it for large particles. The transition between these two behaviours happens when the dust drift velocity is comparable to the planet migration velocity. We predict that an observational signature of a migrating planet consists of a significant outwards shift of an observed mid-plane dust ring as the wavelength is increased.
Is the ring inside or outside the planet?: the effect of planet migration on dust rings / F. Meru, G. Rosotti, R. A Booth, P. Nazari, C. J Clarke. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 482:3(2019 Jan 21), pp. 3678-3695. [10.1093/mnras/sty2847]
Is the ring inside or outside the planet?: the effect of planet migration on dust rings
G. RosottiSecondo
;
2019
Abstract
Planet migration in protoplanetary discs plays an important role in the longer term evolution of planetary systems, yet we currently have no direct observational test to determine if a planet is migrating in its gaseous disc. We explore the formation and evolution of dust rings - now commonly observed in protoplanetary discs by the Atacama Large Millimeter/submillimeter Array - in the presence of relatively low-mass (12-60 M) migrating planets. Through 2D hydrodynamical simulations using gas and dust we find that the importance of perturbations in the pressure profile interior and exterior to the planet varies for different particle sizes. For small sizes, a dust enhancement occurs interior to the planet, whereas it is exterior to it for large particles. The transition between these two behaviours happens when the dust drift velocity is comparable to the planet migration velocity. We predict that an observational signature of a migrating planet consists of a significant outwards shift of an observed mid-plane dust ring as the wavelength is increased.File | Dimensione | Formato | |
---|---|---|---|
sty2847.pdf
accesso riservato
Tipologia:
Publisher's version/PDF
Dimensione
2.04 MB
Formato
Adobe PDF
|
2.04 MB | Adobe PDF | Visualizza/Apri Richiedi una copia |
1810.06573.pdf
accesso aperto
Tipologia:
Post-print, accepted manuscript ecc. (versione accettata dall'editore)
Dimensione
1.5 MB
Formato
Adobe PDF
|
1.5 MB | Adobe PDF | Visualizza/Apri |
Pubblicazioni consigliate
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.