TOI-2109: An Ultrahot Gas Giant on a 16 hr Orbit

Wong, Ian; Shporer, Avi; Zhou, George; Kitzmann, Daniel; Komacek, Thaddeus D.; Tan, Xianyu; Tronsgaard, R.; Buchhave, Lars A.; Vissapragada, Shreyas; Greklek-McKeon, Michael; Rodriguez, Joseph E.; Ahlers, John P.; Quinn, Samuel N.; Furlan, Elise; Howell, Steve B.; Bieryla, Allyson; Heng, Kevin; Knutson, Heather A.; Collins, Karen A.; McLeod, Kim K.; Berlind, P.; Brown, P. Lancaster; Calkins, M.; Leon, Jerome P. de; Esparza-Borges, E.; Esquerdo, Gilbert A.; Fukui, A.; Gan, Tianjun; Girardin, Éric; Gnilka, Crystal L.; Ikoma, Masahiro; Jensen, Eric L. N.; Kielkopf, John F.; Kodama, Takanori; Kurita, S.; Lester, Kathryn V.; Lewin, Pablo; Marino, G.; Murgas, F.; Narita, Norio; Πάλλη, Ε.; Schwarz, Richard P.; Stassun, Keivan G.; Tamura, Motohide; Watanabe, Noriharu; Benneke, Björn; Ricker, G.; Latham, David W.; Vanderspek, R.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Caldwell, Douglas A.; Fong, William; Huang, Chelsea X.; Mireles, Ismael; Schlieder, Joshua E.; Shiao, Bernie; Villaseñor, J.

doi:10.3847/1538-3881/ac26bd

Cited by 31 publications

(15 citation statements)

References 158 publications

(209 reference statements)

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“…Based on the forecast of Yee et al (2021), to assemble a sample of 400 hot Jupiters (an order of magnitude more planets than the Kepler sample), a magnitude-limited survey would need to be complete down to G = 12.5. The 10 planets described here, along with the other new TESS hot Jupiters that have been described in the literature (e.g., Rodriguez et al 2019;Zhou et al 2019;Brahm et al 2020;Davis et al 2020;Nielsen et al 2020;Ikwut-Ukwa et al 2021;Rodriguez et al 2021;Sha et al 2021;Wong et al 2021;Knudstrup et al 2022;Rodriguez et al 2022) are steps toward realizing the promise of TESS for hot Jupiter demographics. Note.…”

Section: Discussionmentioning

confidence: 99%

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Yee

Winn

Hartman

et al. 2022

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Hot Jupiters—short-period giant planets—were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA’s Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, T eff between 4800 and 6200 K). The planets’ orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a “sub-Saturn,” with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.

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Section: Discussionmentioning

confidence: 99%

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Yee

Winn

Hartman

et al. 2022

Self Cite

View full text Add to dashboard Cite

show abstract

“…Based on the forecast of Yee et al (2021), to assemble a sample of 400 hot Jupiters (an orderof-magnitude more planets than the Kepler sample), a magnitude-limited survey would need to be complete down to G = 12.5. The ten planets described here, along with the other new TESS hot Jupiters that have been described in the literature (e.g., Rodriguez et al 2019;Zhou et al 2019;Brahm et al 2020;Davis et al 2020;Nielsen et al 2020;Ikwut-Ukwa et al 2021;Rodriguez et al 2021;Sha et al 2021;Wong et al 2021;Knudstrup et al 2022;Rodriguez et al 2022) are steps toward realizing the promise of TESS for hot Jupiter demographics.…”

Section: Discussionmentioning

confidence: 99%

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Yee,

Winn,

Hartman

et al. 2022

Preprint

Self Cite

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Hot Jupiters -short-period giant planets -were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS ), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of ten new hot Jupiters (TOI-2193A b, TOI-2207 b, TOI-2236 b, TOI-2421 b, TOI-2567 b, TOI-2570 b, TOI-3331 b, TOI-3540A b, TOI-3693 b, TOI-4137 b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS , and were subsequently confirmed using ground-based time-series photometry, high angular resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The ten newly discovered planets orbit relatively bright F and G stars (G < 12.5, T eff between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421 b is notable for being a Saturn-mass planet and TOI-2567 b for being a "sub-Saturn', with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17±0.05) for TOI-2207 b, a planet on an 8-day orbit, while placing an upper limit of e < 0.052 for TOI-3693 b, which has a 9-day orbital period. The ten planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters. TOI-2421 b TOI-2567 b Planet Parameters P (days) Period 2.1225735 ± 0.0000016 8.001968 +0.000024 −0.000025 3.5315902 ± 0.0000026 4.3474032 +0.0000079 −0.0000078 5.983944 ± 0.000013 Tc (BJD TDB ) Time of conjunction 2459052.42122 ± 0.

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“…A key finding of GCM studies is that tidally locked planets within the HZ of M-class stars can retain temperate climates in spite of their uneven thermal forcing as a result of winds redistributing heat from their hot daysides to their cold nightsides (Joshi et al 1997;Merlis & Schneider 2010;Wordsworth 2015;Pierrehumbert & Hammond 2019). The day-night temperature gradient of a tidally locked exoplanet has already been observed for some hot Jupiters (Komacek et al 2017;Wong et al 2021), and even for a rocky planet (Demory et al 2016). However, most past studies have examined mean climate states, masking time-dependent phenomena that may impact observations by upcoming instruments such as the James Webb Space Telescope's Near Infrared Spectrograph (NIRSpec) (Mollière et al 2017;Morley et al 2017) and the ESA Atmospheric Remote-sensing Infrared Exoplanet Large-survey mission (Tinetti et al 2018;Venot et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Longitudinally Asymmetric Stratospheric Oscillation on a Tidally Locked Exoplanet

Cohen

Bollasina

Palmer

et al. 2022

ApJ

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Using a three-dimensional general circulation model, we show that the atmospheric dynamics on a tidally locked Earth-like exoplanet, simulated with the planetary and orbital parameters of Proxima Centauri b, support a longitudinally asymmetric stratospheric wind oscillation (LASO), analogous to Earth’s quasi-biennial oscillation (QBO). In our simulations, the LASO has a vertical extent of 35–55 km, a period of 5–6.5 months, and a peak-to-peak wind speed amplitude of −70 to +130 m s−1 with a maximum at an altitude of 41 km. Unlike the QBO, the LASO displays longitudinal asymmetries related to the asymmetric thermal forcing of the planet and to interactions with the resulting stationary Rossby waves. The equatorial gravity wave sources driving the LASO are localized in the deep convection region at the substellar point and in a jet exit region near the western terminator, unlike the QBO, for which these sources are distributed uniformly around the planet. Longitudinally, the western terminator experiences the highest wind speeds and undergoes reversals earlier than other longitudes. The antistellar point only experiences a weak oscillation with a very brief, low-speed westward phase. The QBO on Earth is associated with fluctuations in the abundances of water vapor and trace gases such as ozone, which are also likely to occur on exoplanets if these gases are present. Strong fluctuations in temperature and the abundances of atmospheric species at the terminators will need to be considered when interpreting atmospheric observations of tidally locked exoplanets.

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TOI-2109: An Ultrahot Gas Giant on a 16 hr Orbit

Cited by 31 publications

References 158 publications

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Longitudinally Asymmetric Stratospheric Oscillation on a Tidally Locked Exoplanet

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