The Planet-Metallicity Correlation

By Debra A. Fischer, J. Valenti. 2005

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In Astronomy and Astrophysics

Citations in the corpus

Target Selection for the SDSS-IV APOGEE-2 Survey (2017, background): “…the demographics of substellar companions of evolved stars, including the companions’ survivability as the stellar hosts evolve and their prevalence as a function of stellar metallicity (like the metallicity-planet frequency trend seen in dwarf stars; Fischer & Valenti 2005; Reffert et al. 2015).”
REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, background): “For example, studies found that gas-giant planets occur more frequently around metal-rich stars (Gonzalez 1997; Santos et al. 2004; Fischer & Valenti 2005; Johnson et al. 2010).”
THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, methodology): “While such planets do exist (e.g., Lafrenière et al. 2008; Ireland et al. 2011), they are much less common than planets detected via radial velocity at closer separations (Fischer & Valenti 2005; Cumming et al. 2008; Nielsen & Close 2010).”
Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, methodology): “Such samples can have a different metallicity distribution than volume limited samples as shown by Fischer & Valenti (2005) who find that their planet search sample is shifted by ∼ 0.1 dex towards higher metallicities relative to a volume limited subset.”
GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, methodology): “The null hypoth- 4 Where possible, we have updated the data from Fischer & Valenti (2005) using the improved orbital parameters given in Butler et al.(2006). esis is again not strongly rejected by a KS test, but the KS probability of 2% is somewhat lower than before: this illustrates the typical…”
State of the Field: Extreme Precision Radial Velocities (2016, methodology): “Keck data have been used to derive planet occurrence rates (Cumming et al. 2008; Howard et al. 2012) and spectra have been used for characterization of host star metallicity and activity (Fischer & Valenti 2005; Valenti & Fischer 2005; Isaacson & Fischer 2010).”
Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “Such a possible absence was noted by Udry et al. (2002), Santos et al. (2003) and Fischer & Valenti (2005).”
TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS (2010, background): “While the fraction of solar-type stars with known gas giants increases with their metallicity (e.g., Fischer & Valenti 2005, also see Paper II), there is no analogous correlation between stellar metallicity and the presence of debris disks around them (Greaves et al. 2007).”
Atmosphere, Interior, and Evolution of the Metal-rich Transiting Planet HD 149026b (2005, background): “The high metallicity of the parent star [Fe/H]=0.36±0.05 (Sato et al. 2005) suggests that this system is very favorable to planet formation as the current fraction of stars with detected planets increases strongly with stellar metallicity (Gonzalez 1997; Santos et al. 2004; Fischer & Valenti 2005).”
Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks (2006, background): “…high resolution visual spectra, sensitive to stellar semiamplitudes > 30 m s−1 and orbital periods shorter than 4 yr, find that fewer than 3% of stars with -0.5 < [Fe/H] < 0.0 have Doppler-detected planets while 25% of stars with [Fe/H] > +0.3 – 23 – possess giant planets (Fischer & Valenti 2005).”
Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “Additional evidence is provided by the observed dependence of giant exoplanet occurrence on the host star metallicity, which is a proxy for the dust mass enrichment of the protoplanetary disc (Fischer & Valenti 2005; Buchhave et al. 2012).”
Mass-Radius Relationships for Solid Exoplanets (2007, result): “In contrast to our 2% best case scenario, current typical stellar mass and radius uncertainties are on the order of 5–10% (Ford et al. 1999; Cody & Sasselov 2002; Fischer & Valenti 2005).”
The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, methodology): “(19) This model extends the following exponential model: df dM = C10βM , (20) which was used in Fischer & Valenti (2005) and in several subsequent works.”
A Decreased Probability of Habitable Planet Formation around Low-Mass Stars (2007, background): “2004; Fischer & Valenti 2005) allow for 70-90% of stars to have planetary systems without Jovians, and an even larger fraction for lower-mass stars (Endl et al. 2006; Butler et al. 2006).”
The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets (2017, background): “…stars, those early surveys mapped out the strong correlation between giant-planet occurrence and stellar metallicity (Valenti & Fischer 2005; Fischer & Valenti 2005) and planet occurrence as a function of planet mass, stellar mass, and orbital distance (Cumming et al. 2008; Howard et al.…”