dc.contributor.author
Alqasim, A.
dc.contributor.author
Grieves, N.
dc.contributor.author
Rosário, N. M.
dc.contributor.author
Gandolfi, D.
dc.contributor.author
Livingston, J. H.
dc.contributor.author
Sousa, S.
dc.contributor.author
Collins, K. A.
dc.contributor.author
Teske, J. K.
dc.contributor.author
Fridlund, M.
dc.contributor.author
Rauer, Heike
dc.date.accessioned
2025-02-14T09:43:27Z
dc.date.available
2025-02-14T09:43:27Z
dc.identifier.uri
https://refubium.fu-berlin.de/handle/fub188/46612
dc.identifier.uri
http://dx.doi.org/10.17169/refubium-46326
dc.description.abstract
We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of R-p = 2.5 +/- 0.1 R-circle plus and a mass of M-p = 10.5(-2.1)(+2.2) M-circle plus, implying a bulk density of rho(p) = 3.6 +/- 0.8 g cm(-3). Our internal composition modelling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39(-0.07)(+0.08), making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b's formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star-star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI-757.
en
dc.format.extent
26 Seiten
dc.rights.uri
https://creativecommons.org/licenses/by/4.0/
dc.subject
techniques: photometric
en
dc.subject
techniques: radial velocities
en
dc.subject
planets and satellites: composition
en
dc.subject
planets and satellites: interiors
en
dc.subject
stars: individual: TOI-757 (TIC 130924120)
en
dc.subject.ddc
500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften
dc.title
TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit
dc.type
Wissenschaftlicher Artikel
dcterms.bibliographicCitation.doi
10.1093/mnras/stae1767
dcterms.bibliographicCitation.journaltitle
Monthly Notices of the Royal Astronomical Society
dcterms.bibliographicCitation.number
1
dcterms.bibliographicCitation.pagestart
1
dcterms.bibliographicCitation.pageend
26
dcterms.bibliographicCitation.volume
533
dcterms.bibliographicCitation.url
https://doi.org/10.1093/mnras/stae1767
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
1365-2966
refubium.resourceType.provider
WoS-Alert