Observed Properties of Exoplanets : Masses, Orbits, and Metallicities(Origins : From Early Universe to Extrasolar Planets)

By G. Marcy, R. P. Butler, Debra A. Fischer, S. Vogt, Jason T. Wright, C. Tinney, H. Jones. 2005

191 citations recorded by the source corpus.

precision (3 m s −1 ) and long duration. The 104 planets detected in this survey have minimum masses (M sin i )a s low as 6MEarth, orbiting between 0.02 and 6 AU. The core-accretion model of planet formation is supported by four observations: 1) The mass distribution rises toward the lowest detectable masses, dN /dM ∝ M −1.0 . 2) Stellar metallicity correlates strongly with the presence of planets. 3) One planet (1.3 MSat) has a massive rocky core, MCore ≈ 70 MEarth. 4) A super-Earth of ∼ 7 MEarth has been discovered. The distribution of semi-major axes rises from 0.3 – 3.0 AU (dN /d log a) and extrapolation suggests that ∼12% of the FGK stars harbor gas-giant exoplanets within 20 AU. The median orbital eccentricity .

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/aeaa199211649f23273c008b4c52fe7c97441f8b

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Citations in the corpus

Five Planets Orbiting 55 Cancri (2007, background): “The large eccentricities found in the majority of exoplanets (Marcy et al. 2005; Butler et al. 2006) are not seen in 55 Cnc.”
EVIDENCE FOR DUST CLEARING THROUGH RESOLVED SUBMILLIMETER IMAGING (2008, background): “Such systems can therefore strongly constrain models of planet formation, especially the role of gap formation and disk-planet interactions in various planet migration scenarios that lead to the creation of the “hot Jupiters” found to orbit much older systems (Marcy et al. 2005).”
ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES (2012, methodology): “Taking fb ≃ 0.3, estimated from the tail of the distribution in Duquennoy & Mayor (1991), and fp ≃ 0.07, consistent with the studies from Wright et al. (2012) and Marcy et al. (2005), we find f ≃ 0.0032.”
Exploring the Frequency of Close-in Jovian Planets around M Dwarfs (2006, background): “Marcy et al. (2005) find a frequency of 1:2% 0:2% of ‘‘hot Jupiters’’ with a < 0:1 AU around FGK-type stars, and according to their Figure 2, a frequency of 2:5% 0:4% of planets with a < 1 AU.”
Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “Nowadays we know that roughly 5-10 % (e.g. Marcy et al. 2005; Cumming et al. 2008) of solar-like star in the solar neighborhood harbor a giant planet within a few AU in distance.”
Disk eccentricity and embedded planets (2005, background): “For a recent overview of planetary properties se Marcy et al. (2005) and theExtrasolar Planets Encyclopedia (http://www.obspm.fr/encycl/encycl.html) maintained by J. Schneider.”
Dust filtration at gap edges: Implications for the spectral energy distributions of discs with embedded planets (2006, background): “We estimate the efficiency of this process, and argue that it allows relatively low mass planets – which are observed (Marcy et al. 2005) to be much more common than those planets with Mp > MJ that would start to cut off accretion entirely – to nevertheless create dust-poor inner cavities.”
Science with the Murchison Widefield Array (2012, background): “Observations have established that many of the Jovian planets discovered around other stars (e.g., Marcy et al. 2005) have magnetic fields (Shkolnik et al. 2003), although the field strengths are not known.”
CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER (2011, background): “The crucial role hot Jupiters play in present-day exoplanetary science is not because they are common; the occurrence rate of hot Jupiters in the solar neighborhood is only about 1% (Marcy et al. 2005).”
THE FREQUENCY OF HOT JUPITERS ORBITING NEARBY SOLAR-TYPE STARS (2012, methodology): “They note that this is only 40% of the rate of 1.2 ± 0.1% (or 12 ± 1 per thousand dwarfs) found by Marcy et al. (2005a) from radial veloc- † Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the University of California and the California Institute of…”
A comparative study of disc–planet interaction (2006, background): “Planets orbiting at larger distances from the star show a broad eccentricity distribution reaching roughly e= 0.9 (for recent reviews of the properties of the observed systemsee Marcy et al. 2003, 2005).”
The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, methodology): “We systematically searched for planets by calculating the false alarm probability associated with Keplerian orbit fits to the data for each star (C04; Marcy et al. 2005b; O’Toole et al. 2007).”
PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “Not included here is an analysis of the orbital eccentricities that span the range e = 0–0.93 (e.g., Marcy et al. 2005b; Udry & Santos 2007; Moorhead et al. 2011), and the close-in “hot Jupiters” show a wide distribution of inclinations relative to the equatorial plane of the host star (Winn et al.…”
A New High Contrast Imaging Program at Palomar Observatory (2010, background): “In recent years, astronomers have identified more than 400 planets outside our solar system, launching the new and thriving field of exoplanetary science (Mayor et al. 2008; Marcy et al. 2005).”
SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, background): “The most productive radial velocity planet search surveys concentrated their efforts on the search for planets around solar-type, FGK dwarfs or sub-giants (for some examples see e.g. Udry et al. 2000; Mayor et al. 2003; Marcy et al. 2005; Johnson et al. 2007b).”