HD 80606 b, a planet on an extremely elongated orbit

By D. Naef, D. Latham, M. Mayor, T. Mazeh, J. Beuzit, G. Drukier, C. Perrier-Bellet, D. Queloz, J. Sivan, G. Torres and 2 more. 2001

190 citations recorded by the source corpus.

We report the detection of a planetary companion orbiting the solar-type star HD 80606, the brighter component of a wide binary with a projected separation of about 2000 AU. Using high-signal spectroscopic observations of the two components of the visual binary, we show that they are nearly identical. The planet has an orbital period of 111.8 days and a minimum mass of 3.9 M_Jup. With e=0.927, this planet has the highest orbital eccentricity among the extrasolar planets detected so far. We finally list several processes this extreme eccentricity could result from.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/92ed62776c61b9e3b18bde9cdea4c485bf595d31

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In Astronomy and Astrophysics

1. J. Winn
2. J. Johnson
3. J. Southworth
4. D. Charbonneau
5. G. Marcy
6. Andrew W. Howard
7. Timothy Morton
8. Jon Fortney

In Instrumentation

1. J. Winn
2. J. Southworth
3. J. Johnson
4. Andrew W. Howard
5. G. Marcy
6. Timothy Morton
7. D. Charbonneau
8. Y. Lithwick

In Statistical and Nonlinear Physics

1. J. Winn
2. Y. Lithwick
3. J. Southworth
4. Yanqin Wu
5. F. Rasio
6. Andrew W. Howard
7. G. Torres
8. G. Marcy

Citations in the corpus

• HAT-P-16b: A 4 MJ PLANET TRANSITING A BRIGHT STAR ON AN ECCENTRIC ORBIT, (2010, background): “HD80606 (Naef et al. 2001) and HD17156 (Fischer et al. 2007) are also similar in mass, but both planets have long periods and very eccentric orbits.”
• SECULAR CHAOS AND THE PRODUCTION OF HOT JUPITERS (2010, background): “…including ones that are retrograde in projection (Triaud et al. 2010), and is likely responsible in a number of specific cases (such as HD 80606b Naef et al. 2001; Laughlin et al. 2009; Pont et al. 2009; Winn et al. 2009; Hebrard et al. 2010b), it does not preferentially yield low-mass hot…”
• Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “Two of them are the very highly eccentric planets HD 80606b (Naef et al. 2001) and HD 20782b (Jones et al. 2006), both with an eccentricity of 0.92, and the third one is HD 41004Bb — a planet with one of the shortest periods, 1.3 days, with a small but significant eccentricity of 0.081 ± 0.012…”
• Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, methodology): “Spectral synthesis analyses of the parent star have been performed by Naef et al. (2001), Santos et al. (2004) and Gonzalez et al. (2010): I adopt theTeff from Santos et al. (2004) as it is the middle of the three values and its errorbar encompasses the other two; I use the Gonzalez et al. (2010)…”
• The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, background): “We find a period of 15 rather than 111 days for the highly eccentric planet around HD 80606 (which hase = 0.93; Naef et al. 2001).”
• ECCENTRICITY FROM TRANSIT PHOTOMETRY: SMALL PLANETS IN KEPLER MULTI-PLANET SYSTEMS HAVE LOW ECCENTRICITIES (2015, background): “Planets on orbits with e = 0.5 are 33% more likely to transit, and in the extreme case of HD 80606b (e = 0.92) (Naef et al. 2001) the transit probability increased by 640%.”
• Planet Migration and Binary Companions: The Case of HD 80606b (2003, background): “The object HD 80606b (Naef et al. 2001, hereafter NLM01; period 111.8 days, mp sin i ¼ 3:4MJ),4 the focus of this article, has the highest eccentricity (e ¼ 0:927 0:012) and the smallest pericenter distance ( 7 R ) among all known exoplanet candidates.”
• The Occurrence and Architecture of Exoplanetary Systems (2014, background): “Among the systems with very secure measurements, the most eccentric orbit (e = 0.93) belongs to HD 80606b (Naef et al. 2001, Hébrard et al. 2010).”
• Detectability of extrasolar planets in radial velocity surveys (2004, background): “In this regard, it is worth noting that the most eccentric orbit discovered so far, withe = 0.93 (HD 80606; Naef et al. 2001), also has one of the largest amplitudesK = 411m/s (M sin i = 4MJ ).”
• Calculating the Tidal, Spin, and Dynamical Evolution of Extrasolar Planetary Systems (2002, background): “Other configurations may be studied such as the highly eccentric system HD 80606 with e ’ 0:927 and periastron separation 0.03 AU (Naef et al. 2001), for which a binary companion may be responsible for the high eccentricity via the Kozai effect, or which may have been left in this state after a…”
• Catalog of Nearby Exoplanets (2006, unknown): “; K0: Korzennik et al. (2000); LC5: Lo Curto (2005); Le5: Lee et al. (2005); Lt9: Latham et al. (1989); Lv5: Lovis et al. (2005); MA4: McArthur et al. (2004); MC4: McCarthy et al. (2004), Mo5: Moutou et al. (2005); My3: http://obswww.unige.ch/∼naef/planet/geneva planets.html; My4: Mayor et al. (2004”
• Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model (2007, background): “…the 86 planets with orbital periods greater than 10 days and best-fit orbital eccentricities exceeding 0.2, two planets have eccentricities that are currently estimated to be greater than 0.8, HD 80606b (e = 0.935±0.0023; Naef et al. 2001) and HD 20782b (e = 0.925±0.03; Jones et al. 2006).”
• Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity (2010, background): “In particular, the orbital evolution of planetary systems such as HD 80 606, with an orbital eccentricity of 0.9337 (Naef et al. 2001), and XO-3, with a stellar obliquity ε?”