مورد إلكتروني
The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis
| العنوان: | The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis |
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| المؤلفون: | Weiss, LM |
| المصدر: | Astronomical Journal; vol 159, iss 5, 242-242; 0004-6256 |
| بيانات النشر: | eScholarship, University of California 2020-05-01 |
| تفاصيل مُضافة: | Weiss, LM Fabrycky, DC Agol, E Mills, SM Howard, AW Isaacson, H Petigura, EA Fulton, B Hirsch, L Sinukoff, E |
| نوع الوثيقة: | Electronic Resource |
| مستخلص: | We present the discovery of Kepler-88 d (Pd = 1403 ± 14 days, M sin id =965 ± 44⊕ = 3.04 ± 0.13 MJ, ed = 0.41 ± 0.03) based on six years of radial velocity (RV) follow-up from the W. M. Keck Observatory High Resolution Echelle Spectrometer spectrograph. Kepler-88 has two previously identified planets. Kepler-88 b (KOI-142.01) transits in the NASA Kepler photometry and has very large transit timing variations (TTVs). Nesvorný et al. performed a dynamical analysis of the TTVs to uniquely identify the orbital period and mass of the perturbing planet (Kepler-88 c), which was later was confirmed with RVs from the Observatoire de Haute-Provence (OHP). To fully explore the architecture of this system, we performed photodynamical modeling on the Kepler photometry combined with the RVs from Keck and OHP and stellar parameters from spectroscopy and Gaia. Planet d is not detectable in the photometry, and long-baseline RVs are needed to ascertain its presence. A photodynamical model simultaneously optimized to fit the RVs and Kepler photometry yields the most precise planet masses and orbital properties yet for b and c: Pb=10.91647 ± 0.00014 days, Mb=9.5 ± 1.2 M⊕ Pc=22.2649±0.0007 days, and Mc=214.0±5.3 M⊕. The photodynamical solution also finds that planets b and c have low eccentricites and low mutual inclination, are apsidally anti-aligned, and have conjunctions on the same hemisphere of the star. Continued RV follow-up of systems with small planets will improve our understanding of the link between inner planetary system architectures and giant planets. |
| مصطلحات الفهرس: | Exoplanet astronomy, Exoplanets, Exoplanet systems, Exoplanet detection methods, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics, article |
| URL: | |
| الإتاحة: | Open access content. Open access content CC-BY |
| ملاحظة: | application/pdf Astronomical Journal vol 159, iss 5, 242-242 0004-6256 |
| أرقام أخرى: | CDLER oai:escholarship.org:ark:/13030/qt53q2q879 qt53q2q879 https://escholarship.org/uc/item/53q2q879 https://escholarship.org/ 1367386233 |
| المصدر المساهم: | UC MASS DIGITIZATION From OAIster®, provided by the OCLC Cooperative. |
| رقم الأكسشن: | edsoai.on1367386233 |
| قاعدة البيانات: | OAIster |
| الوصف غير متاح. |