dc.contributor.author
Curone, P.
dc.contributor.author
Izquierdo, A. F.
dc.contributor.author
Testi, L.
dc.contributor.author
Lodato, G.
dc.contributor.author
Facchini, S.
dc.contributor.author
Natta, A.
dc.contributor.author
Pinilla, P.
dc.contributor.author
Kurtovic, N. T.
dc.contributor.author
Toci, C.
dc.contributor.author
Sanchis, Enrique
dc.date.accessioned
2022-11-14T10:10:10Z
dc.date.available
2022-11-14T10:10:10Z
dc.identifier.uri
https://refubium.fu-berlin.de/handle/fub188/36861
dc.identifier.uri
http://dx.doi.org/10.17169/refubium-36574
dc.description.abstract
Context. Exoplanetary research has provided us with exciting discoveries of planets around very low-mass (VLM) stars (0.08 M⊙ ≲ M* ≲ 0.3 M⊙; e.g., TRAPPIST-1 and Proxima Centauri). However, current theoretical models still strive to explain planet formation in these conditions and do not predict the development of giant planets. Recent high-resolution observations from the Atacama Large Millimeter/submillimeter Array (ALMA) of the disk around CIDA 1, a VLM star in Taurus, show substructures that hint at the presence of a massive planet.
Aims. We aim to reproduce the dust ring of CIDA 1, observed in the dust continuum emission in ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm), along with its 12CO (J = 3−2) and 13CO (J = 3−2) channel maps, assuming the structures are shaped by the interaction of the disk with a massive planet. We seek to retrieve the mass and position of the putative planet, through a global simulation that assesses planet-disk interactions to quantitatively reproduce protoplanetary disk observations of both dust and gas emission in a self-consistent way.
Methods. Using a set of hydrodynamical simulations, we model a protoplanetary disk that hosts an embedded planet with a starting mass of between 0.1 and 4.0 MJup and initially located at a distance of between 9 and 11 au from the central star. We compute the dust and gas emission using radiative transfer simulations, and, finally, we obtain the synthetic observations, treating the images as the actual ALMA observations.
Results. Our models indicate that a planet with a minimum mass of ~1.4 MJup orbiting at a distance of ~9−10 au can explain the morphology and location of the observed dust ring in Band 7 and Band 4. We match the flux of the dust emission observation with a dust-to-gas mass ratio in the disk of ~10−2. We are able to reproduce the low spectral index (~2) observed where the dust ring is detected, with a ~40−50% fraction of optically thick emission. Assuming a 12CO abundance of 5 × 10−5 and a 13CO abundance 70 times lower, our synthetic images reproduce the morphology of the 12CO (J = 3−2) and 13CO (J = 3−2) observed channel maps where the cloud absorption allowed a detection. From our simulations, we estimate that a stellar mass M* = 0.2 M⊙ and a systemic velocity vsys = 6.25 km s−1 are needed to reproduce the gas rotation as retrieved from molecular line observations. Applying an empirical relation between planet mass and gap width in the dust, we predict a maximum planet mass of ~4−8 MJup.
Conclusions. Our results suggest the presence of a massive planet orbiting CIDA 1, thus challenging our understanding of planet formation around VLM stars.
en
dc.format.extent
22 Seiten
dc.rights.uri
https://creativecommons.org/licenses/by/4.0/
dc.subject
protoplanetary disks
en
dc.subject
planet-disk interactions
en
dc.subject
stars: individual: CIDA 1
en
dc.subject
planets and satellites: formation
en
dc.subject
hydrodynamics
en
dc.subject
radiative transfer
en
dc.subject.ddc
500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften
dc.title
A giant planet shaping the disk around the very low-mass star CIDA 1
dc.type
Wissenschaftlicher Artikel
dcterms.bibliographicCitation.articlenumber
A25
dcterms.bibliographicCitation.doi
10.1051/0004-6361/202142748
dcterms.bibliographicCitation.journaltitle
Astronomy & Astrophysics
dcterms.bibliographicCitation.volume
665
dcterms.bibliographicCitation.url
https://doi.org/10.1051/0004-6361/202142748
refubium.affiliation
Geowissenschaften
refubium.affiliation.other
Institut für Geologische Wissenschaften / Fachrichtung Planetologie und Fernerkundung

refubium.resourceType.isindependentpub
no
dcterms.accessRights.openaire
open access
dcterms.isPartOf.eissn
1432-0746
refubium.resourceType.provider
WoS-Alert