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

Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations . 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 eccentricit...

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Published inNature (London) Vol. 632; no. 8023; pp. 50 - 54
Main Authors Gupta, Arvind F, Millholland, Sarah C, Im, Haedam, Dong, Jiayin, Jackson, Jonathan M, Carleo, Ilaria, Libby-Roberts, Jessica, Delamer, Megan, Giovinazzi, Mark R, Lin, Andrea S J, Kanodia, Shubham, Wang, Xian-Yu, Stassun, Keivan, Masseron, Thomas, Dragomir, Diana, Mahadevan, Suvrath, Wright, Jason, Alvarado-Montes, Jaime A, Bender, Chad, Blake, Cullen H, Caldwell, Douglas, Cañas, Caleb I, Cochran, William D, Dalba, Paul, Everett, Mark E, Fernandez, Pipa, Golub, Eli, Guillet, Bruno, Halverson, Samuel, Hebb, Leslie, Higuera, Jesus, Huang, Chelsea X, Klusmeyer, Jessica, Knight, Rachel, Leroux, Liouba, Logsdon, Sarah E, Loose, Margaret, McElwain, Michael W, Monson, Andrew, Ninan, Joe P, Nowak, Grzegorz, Palle, Enric, Patel, Yatrik, Pepper, Joshua, Primm, Michael, Rajagopal, Jayadev, Robertson, Paul, Roy, Arpita, Schneider, Donald P, Schwab, Christian, Schweiker, Heidi, Sgro, Lauren, Shimizu, Masao, Simard, Georges, Stefánsson, Guðmundur, Stevens, Daniel J, Villanueva, Steven, Wisniewski, John, Will, Stefan, Ziegler, Carl
Format Journal Article
LanguageEnglish
Published England Nature Publishing Group 01.08.2024
Nature Publishing Group UK
Subjects
Angular momentum
Extrasolar planets
Gas giant planets
Ice formation
Jupiter
Orbits
Oscillations
Photometric observations
Planetary orbits
Retrograde orbits
Simulation
Trajectory analysis
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Abstract Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations . 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 . The discovery of the extremely eccentric (e = 0.93) giant exoplanet HD 80606 b (ref.  ) provided observational evidence that hot Jupiters may have formed through this high-eccentricity tidal-migration pathway . 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 . 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.
AbstractList Abstract Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations 1 . 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 pathway 5 . 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.
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 circularization2,3. 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 passage6-8. 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.
Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations . 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 . The discovery of the extremely eccentric (e = 0.93) giant exoplanet HD 80606 b (ref.  ) provided observational evidence that hot Jupiters may have formed through this high-eccentricity tidal-migration pathway . 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 . 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.
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 circularization2,3. 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 passage6-8. 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.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 circularization2,3. 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 passage6-8. 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.
Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations 1 . 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 pathway 5 . 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. The spectroscopic and photometric observations of a high-mass, transiting warm Jupiter, TIC 241249530 b, with an orbital eccentricity of 0.94, provide evidence that hot Jupiters may have formed by means of a high-eccentricity tidal-migration pathway.
Author Stassun, Keivan
Bender, Chad
Patel, Yatrik
Gupta, Arvind F
Libby-Roberts, Jessica
Simard, Georges
Higuera, Jesus
Nowak, Grzegorz
Masseron, Thomas
Dalba, Paul
McElwain, Michael W
Robertson, Paul
Huang, Chelsea X
Jackson, Jonathan M
Ziegler, Carl
Schweiker, Heidi
Millholland, Sarah C
Lin, Andrea S J
Blake, Cullen H
Im, Haedam
Hebb, Leslie
Primm, Michael
Mahadevan, Suvrath
Caldwell, Douglas
Carleo, Ilaria
Halverson, Samuel
Delamer, Megan
Schneider, Donald P
Wisniewski, John
Will, Stefan
Golub, Eli
Klusmeyer, Jessica
Villanueva, Steven
Guillet, Bruno
Rajagopal, Jayadev
Loose, Margaret
Knight, Rachel
Alvarado-Montes, Jaime A
Giovinazzi, Mark R
Cañas, Caleb I
Cochran, William D
Monson, Andrew
Wang, Xian-Yu
Wright, Jason
Fernandez, Pipa
Ninan, Joe P
Logsdon, Sarah E
Stefánsson, Guðmundur
Dragomir, Diana
Everett, Mark E
Pepper, Joshua
Palle, Enric
Dong, Jiayin
Shimizu, Masao
Leroux, Liouba
Roy, Arpita
Stevens, Daniel J
Sgro, Lauren
Schwab, Christian
Kanodia, Shubham
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BackLink https://www.ncbi.nlm.nih.gov/pubmed/39020171$$D View this record in MEDLINE/PubMed
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SSID ssj0005174
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Snippet Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations . These 'hot Jupiter' planets are instead...
Abstract Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations 1 . These ‘hot Jupiter’ planets are...
Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations1. These 'hot Jupiter' planets are instead...
Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations 1 . These ‘hot Jupiter’ planets are instead...
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StartPage 50
SubjectTerms Angular momentum
Extrasolar planets
Gas giant planets
Ice formation
Jupiter
Orbits
Oscillations
Photometric observations
Planetary orbits
Retrograde orbits
Simulation
Trajectory analysis
Title A hot-Jupiter progenitor on a super-eccentric retrograde orbit
URI https://www.ncbi.nlm.nih.gov/pubmed/39020171
https://www.proquest.com/docview/3091181887/abstract/
https://www.proquest.com/docview/3082307392/abstract/
https://pubmed.ncbi.nlm.nih.gov/PMC11291287
Volume 632
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