تقرير
HD 28109 Hosts A Trio of Transiting Neptunian Planets Including A Near-Resonant Pair, Confirmed By ASTEP From Antarctica
| العنوان: | HD 28109 Hosts A Trio of Transiting Neptunian Planets Including A Near-Resonant Pair, Confirmed By ASTEP From Antarctica |
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| المؤلفون: | Georgina Dransfield, Amaury H M J Triaud, Tristan Guillot, Djamel Mekarnia, David Nesvorny, Nicolas Crouzet, Lyu Abe, Karim Agabi, Marco Buttu, Juan Cabrera, Davide Gandolfi, Maximilian Gunther, Florian Rodler, Francois-Xavier Schmider, Philippe Stee, Olga Suarez, Karen A Collins, Martin Devora-Pajares, Steve B Howell, Elisabeth C Matthews, Matthew R Standing, Keivan G Stassun, Chris Stockdale, Samuel N Quinn, Carl Ziegler, Ian J M Crossfield, Jack J Lissauer, Andrew W Mann, Rachel Matson, Joshua Schlieder, George Zhou |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 515(1) |
| بيانات النشر: | United States: NASA Center for Aerospace Information (CASI), 2022. |
| سنة النشر: | 2022 |
| مصطلحات موضوعية: | Astronomy |
| الوصف: | We report on the discovery and characterization of three planets orbiting the F8 star HD 28109, which sits comfortably in TESS ’s continuous viewing zone. The two outer planets have periods of 56 . 0067 ±0 . 0003 d and 84 . 2597 + 0 . 0010 −0 . 0008 d, which implies a period ratio very close to that of the first-order 3:2 mean motion resonance, exciting transit timing variations (TTVs) of up to 60 min. These two planets were first identified by TESS , and we identified a third planet in the TESS photometry with a period of 22 . 8911 ±0 . 0004 d. We confirm the planetary nature of all three planetary candidates using ground-based photometry from Hazelwood , ASTEP , and LCO , including a full detection of the ∼9 h transit of HD 28109 c from Antarctica. The radii of the three planets are R b = 2 . 199 + 0 . 098 −0 . 10 R ⊕, R c = 4 . 23 ±0 . 11 R ⊕, and R d = 3 . 25 ±0 . 11 R ⊕; we characterize their masses using TTVs and precise radial velocities from ESPRESSO and HARPS, and find them to be M b = 18 . 5 + 9 . 1 −7 . 6 M ⊕, M c = 7 . 9 + 4 . 2 −3 . 0 M ⊕, and M d = 5 . 7 + 2 . 7 −2 . 1 M ⊕, making planet b a dense, massive planet while c and d are both underdense. We also demonstrate that the two outer planets are ripe for atmospheric characterization using transmission spectroscopy, especially given their position in the CVZ of James Webb Space Telescope . The data obtained to date are consistent with resonant (librating) and non-resonant (circulating) solutions; additional observations will show whether the pair is actually locked in resonance or just near-resonant. |
| نوع الوثيقة: | Report |
| اللغة: | English |
| تدمد: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stac1383 |
| الوصول الحر: | https://ntrs.nasa.gov/citations/20230004232Test |
| ملاحظات: | 134180 SPEC5732 |
| رقم الانضمام: | edsnas.20230004232 |
| قاعدة البيانات: | NASA Technical Reports |
| تدمد: | 13652966 00358711 |
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| DOI: | 10.1093/mnras/stac1383 |