Dataset Information

A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

ABSTRACT: Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations¹. These 'hot Jupiter' planets are instead thought to have migrated inward from beyond the ice line and several viable migration channels have been proposed, including eccentricity excitation through angular-momentum exchange with a third body followed by tidally driven orbital circularization^2,3. The discovery of the extremely eccentric (e = 0.93) giant exoplanet HD 80606 b (ref. ⁴) provided observational evidence that hot Jupiters may have formed through this high-eccentricity tidal-migration pathway⁵. However, no similar hot-Jupiter progenitors have been found and simulations predict that one factor affecting the efficacy of this mechanism is exoplanet mass, as low-mass planets are more likely to be tidally disrupted during periastron passage^6-8. Here we present spectroscopic and photometric observations of TIC 241249530 b, a high-mass, transiting warm Jupiter with an extreme orbital eccentricity of e = 0.94. The orbit of TIC 241249530 b is consistent with a history of eccentricity oscillations and a future tidal circularization trajectory. Our analysis of the mass and eccentricity distributions of the transiting-warm-Jupiter population further reveals a correlation between high mass and high eccentricity.

SUBMITTER: Gupta AF

PROVIDER: S-EPMC11291287 | biostudies-literature | 2024 Jul

REPOSITORIES: biostudies-literature

ACCESS DATA

Publications

A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

Gupta Arvind F AF Millholland Sarah C SC Im Haedam H Dong Jiayin J Jackson Jonathan M JM Carleo Ilaria I Libby-Roberts Jessica J Delamer Megan M Giovinazzi Mark R MR Lin Andrea S J ASJ Kanodia Shubham S Wang Xian-Yu XY Stassun Keivan K Masseron Thomas T Dragomir Diana D Mahadevan Suvrath S Wright Jason J Alvarado-Montes Jaime A JA Bender Chad C Blake Cullen H CH Caldwell Douglas D Cañas Caleb I CI Cochran William D WD Dalba Paul P Everett Mark E ME Fernandez Pipa P Golub Eli E Guillet Bruno B Halverson Samuel S Hebb Leslie L Higuera Jesus J Huang Chelsea X CX Klusmeyer Jessica J Knight Rachel R Leroux Liouba L Logsdon Sarah E SE Loose Margaret M McElwain Michael W MW Monson Andrew A Ninan Joe P JP Nowak Grzegorz G Palle Enric E Patel Yatrik Y Pepper Joshua J Primm Michael M Rajagopal Jayadev J Robertson Paul P Roy Arpita A Schneider Donald P DP Schwab Christian C Schweiker Heidi H Sgro Lauren L Shimizu Masao M Simard Georges G Stefánsson Guðmundur G Stevens Daniel J DJ Villanueva Steven S Wisniewski John J Will Stefan S Ziegler Carl C

Nature 20240717 8023

Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations<sup>1</sup>. These 'hot Jupiter' planets are instead thought to have migrated inward from beyond the ice line and several viable migration channels have been proposed, including eccentricity excitation through angular-momentum exchange with a third body followed by tidally driven orbital circularization<sup>2,3</sup>. The discovery of the extremely eccentric (e = 0.93) giant exoplanet ...[more]

PMID: 39020171

Similar Datasets

Project description:Recent observations at subarcsecond resolution, now possible also at submillimeter wavelengths, have shown intricate circumstellar structures around asymptotic giant branch (AGB) stars, mostly attributed to binary interaction. The results presented here are part of a larger project aimed at investigating the effects of a binary companion on the morphology of circumstellar envelopes (CSEs) of AGB stars. AGB stars are characterized by intense stellar winds that build CSEs around the stars. Here, the CO(J = 3→2) emission from the CSE of the binary S-type AGB star W Aql has been observed at subarcsecond resolution using ALMA. The aim of this paper is to investigate the wind properties of the AGB star and to analyse how the known companion has shaped the CSE. The average mass-loss rate during the creation of the detected CSE is estimated through modelling, using the ALMA brightness distribution and previously published single-dish measurements as observational constraints. The ALMA observations are presented and compared to the results from a 3D smoothed particle hydrodynamics (SPH) binary interaction model with the same properties as the W Aql system and with two different orbital eccentricities. Three-dimensional radiative transfer modelling is performed and the response of the interferometer is modelled and discussed. The estimated average mass-loss rate of W Aql is Ṁ = 3.0×10-6 M⊙ yr-1 and agrees with previous results based on single-dish CO line emission observations. The size of the emitting region is consistent with photodissociation models. The inner 10″ of the CSE is asymmetric with arc-like structures at separations of 2-3″ scattered across the denser sections. Further out, weaker spiral structures at greater separations are found, but this is at the limit of the sensitivity and field of view of the ALMA observations. The CO(J = 3→2) emission is dominated by a smooth component overlayed with two weak arc patterns with different separations. The larger pattern is predicted by the binary interaction model with separations of ~10″ and therefore likely due to the known companion. It is consistent with a binary orbit with low eccentricity. The smaller separation pattern is asymmetric and coincides with the dust distribution, but the separation timescale (200 yrs) is not consistent with any known process of the system. The separation of the known companions of the system is large enough to not have a very strong effect on the circumstellar morphology. The density contrast across the envelope of a binary with an even larger separation will not be easily detectable, even with ALMA, unless the orbit is strongly asymmetric or the AGB star has a much larger mass-loss rate.

Dataset Information

A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

Publications

A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

Similar Datasets

OmicsDI is part of the ELIXIR infrastructure

Tweets