A Planet at 5 AU around 55 Cancri

By G. Marcy, R. P. Butler, Debra A. Fischer, G. Laughlin, S. Vogt, G. Henry, Dimitri Pourbaix. 2002

167 citations recorded by the source corpus.

We report precise Doppler-shift measurements of 55 Cancri (G8 V) obtained from 1989 to 2002 at Lick Observatory. The velocities reveal evidence for an outer planetary companion to 55 Cancri orbiting at 5.5 AU. The velocities also confirm a second, inner planet at 0.11 AU. The outer planet is the first extrasolar planet found that orbits near or beyond the orbit of Jupiter. It was drawn from a sample of ~50 stars observed with sufficient duration and quality to detect a giant planet at 5 AU, implying that such planets are not rare. The properties of this Jupiter analog may be compared directly to those of the Jovian planets in our solar system. Its eccentricity is modest, e = 0.16, compared with e = 0.05 for both Jupiter and Saturn. Its mass is at least 4.0 MJUP (M sin i). The two planets do not perturb each other significantly. Moreover, a third planet of sub-Jupiter mass could easily survive between these two known planets. Indeed, a third periodicity remains in the velocity measurements with P = 44.3 days and a semiamplitude of 13 m s-1. This periodicity is caused either by a third planet at a = 0.24 AU or by inhomogeneities on the stellar surface that rotate with period 42 days. The planet interpretation is more likely, as the stellar surface is quiet both chromospherically [log(R) = -5.0] and photospherically (brightness variations less than 1 mmag). Moreover, any hypothetical surface inhomogeneity would have to persist in longitude for 14 yr. Even with all three planets, an additional planet of terrestrial mass could orbit stably at ~1 AU. The star 55 Cancri is apparently a normal, middle-aged main-sequence star with a mass of 0.95 M☉, rich in heavy elements ([Fe/H] = +0.27). This high metallicity raises the issue of the precise relationship between its age, rotation, and chromosphere.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/78221be0112ee93b3dc6e4f20f817ac52ae515c3

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Citations in the corpus

Secular Evolution of Hierarchical Planetary Systems (2002, background): “The two planets about GJ 876 are deep in three orbital resonances at the 2 : 1 mean-motion commensurability (Laughlin &Chambers 2001; Lee & Peale 2002), and there are possibly two other systems with meanmotion resonances: 2 : 1 for the two planets about HD 829432 (Goździewski & Maciejewski 2001) an”
Detection of a Neptune-Mass Planet in the ρ1 Cancri System Using the Hobby-Eberly Telescope (2004, methodology): “These results are partially based on data obtained with the UCO/Lick Observatory Telescope, the ELODIE spectrograph at Observatoire de Haute-Provence (OHP, France), the Apache Point Observatory 3.5m telescope which is owned and operated by the Astrophysical Research Consortium), and the NASA/ESA Hub”
Five Planets Orbiting 55 Cancri (2007, methodology): “A detailed description of the setup of the Hamilton spectrometer, its calibrating iodine absorption cell, and the method of extracting Doppler measurements for 55 Cnc are given in Butler et al. (1996) and in Marcy et al. (2002).”
Theoretical Spectra and Atmospheres of Extrasolar Giant Planets (2002, background): “The recently discovered outer planet (Marcy et al. 2002) is the first EGP found to orbit its primary at a distance greater than Jupiter’s distance from the Sun.”
A SUPER-EARTH TRANSITING A NAKED-EYE STAR (2011, background): “INTRODUCTION Precise Doppler observations have revealed five planets orbiting the nearby G8 V star 55 Cnc (Butler et al. 1997, Marcy et al. 2002, McArthur et al. 2004, Wisdom 2005, Fischer et al. 2008).”
THE TWENTY-FIVE YEAR LICK PLANET SEARCH (2013, unknown): “…al. 1996), the first multi-planet system around a normal star, Ups And b, c, d (Butler et al. 1997, 1999), 55 Cnc b, c, d, f, g (Butler et al. 1997; Marcy et al. 2002; Fischer et al. 2008), HD 195019 b and HD 217107 b (Fischer et al. 1999), HD 89744 b (Korzennik et al. 2000), GJ 876 b, c, d…”
Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, background): “55 Cancri (HD75732) 55Cnc is the richest planet-host star known to date, harboring four Neptune- to Jupiter-size planets (Butler et al. 1997; Marcy et al. 2002; McArthur et al. 2004).”
Quantifying the Uncertainty in the Orbits of Extrasolar Planets (2003, background): “Already, one known planet (55 Cancri d) has an orbital period of over 14 years (Marcy et al. 2002).”
Extrasolar Planets in Mean-Motion Resonance: Apses Alignment and Asymmetric Stationary Solutions (2002, methodology): “As an additional example of this application, in Figure 10 we have plotted (in full circles) the three best dynamical fits of the two resonant planets of the 55Cnc system (Marcy et al. 2002).”
RADIAL VELOCITY PLANETS DE-ALIASED: A NEW, SHORT PERIOD FOR SUPER-EARTH 55 Cnc e (2010, methodology): “Measurements from the Hobby-Eberly Telescope (McArthur et al. 2004) (HET) revealed, on their own and combined with the Lick measurements by Marcy et al. (2002) and ELODIE measurements by Naef et al. (2004), the presence of planet e, with a reported orbital period of 2.8 days.”
Five New Extrasolar Planets (2005, background): “…HD 16141 and HD 46375 (Marcy et al. 2000), HD 168746 (Pepe et al. 2002), HD 76700 (Tinney et al. 2003), HD 49674 (Butler et al. 2003), 55 Cnc c (Marcy et al. 2002), and HD 3651 (Fischer et al. 2003a), along with the three planets having M sin i near 1MNep (Butler et al. 2004; McArthur et al.…”
DHP Framework: Digital Health Passports Using Blockchain - Use case on international tourism during the COVID-19 pandemic (2004, background): “The orbit of planet b is approximately circular while planet c is somewhat eccentric (Marcy et al. 2002).”
DETECTION OF AN ATMOSPHERE AROUND THE SUPER-EARTH 55 CANCRI E (2015, background): “At a distance of only 12 pc, 55 Cancri is an extremely interesting planetary system hosting five planets, all discovered via radial velocity measurements (Butler et al. 1997; Marcy et al. 2002; McArthur et al. 2004; Fischer et al. 2008).”
The HARPS search for southern extra-solar planets - VI. A Neptune-mass planet around the nearby M dwarf Gl 581 (2005, background): “The multiple systems range from strongly resonant to fully hierarchical (Rivera et al., 2005; Marcy et al., 2002).”