The Mass of the Convective Zone in FGK Main-Sequence Stars and the Effect of Accreted Planetary Material on Apparent Metallicity Determinations

By M. Pinsonneault, D. DePoy, M. Coffee. 2001

163 citations recorded by the source corpus.

The mass of the outer convective zone in FGK main-sequence stars decreases dramatically with stellar mass. Therefore, any contamination of a star's atmosphere by accreted planetary material should affect hotter stars much more than cool stars. If high metal abundances in stars with planets were from planetesimal accretion, then metallicity enhancements in earlier type stars with planets should be very pronounced. No such trend is seen, however.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6f082c3f14dadfdb2f454c8ba58a6ac3f7b1ff56

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. J. Johnson
2. Debra A. Fischer
3. J. Winn
4. G. Marcy
5. Andrew W. Howard
6. M. Mayor
7. Nuno C. Santos
8. J. Southworth

In Instrumentation

1. J. Johnson
2. G. Marcy
3. Andrew W. Howard
4. Debra A. Fischer
5. J. Winn
6. Nuno C. Santos
7. M. Mayor
8. R. P. Butler

Citations in the corpus

• Searching for Planets in the Hyades. IV. Differential Abundance Analysis of Hyades Dwarfs (2003, background): “At this time the convective region has decreased in size (Murray & Chaboyer 2002; Pinsonneault et al. 2001; Laughlin & Adams 1997).”
• THE COMPOSITIONAL DIVERSITY OF EXTRASOLAR TERRESTRIAL PLANETS. I. IN SITU SIMULATIONS (2010, methodology): “Values for the masses of the convective zone for each of the target stars were thus obtained from Pinsonneault et al. (2001) using the Teff values from Santos et al. (2004).”
• Spectroscopic metallicities for planet-host stars: Extending the samples (2005, background): “The fact that we do not find a clear difference between PIB stars and single planet-hosts suggests that strong planetesimal accretion is not usual both for single planet-hosts (Pinsonneault et al. 2001; Santos et al. 2003; Cody & Sasselov 2004) nor for planet-host stars in multiple stellar systems.”
• OBLIQUITIES OF HOT JUPITER HOST STARS: EVIDENCE FOR TIDAL INTERACTIONS AND PRIMORDIAL MISALIGNMENTS (2012, methodology): “Stars hotter than this level have very thin or absent convective envelopes, with the mass of the envelope dropping below about 0.002 M at 6250 K (Pinsonneault et al. 2001).”
• The Planet-Metallicity Correlation (2005, background): “Pinsonneault et al. (2001) questioned the existence of an accretion signature aftermodeling the increase inmetallicity arising from accretion of 10 Mearth of material onto zero-age mainsequence stars.”
• A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER (2014, background): “The probability of this occurring by chance is only 0.3%, and it is intriguing that these hotter stars are distinguished from the cooler stars by the lack of a convective envelope (Pinsonneault et al. 2001).”
• Spectroscopic [Fe/H] for 98 extra-solar planet-host stars. Exploring the probability of planet formation (2003, methodology): “5 (where we plot the stellar metallicity as a function of Teff ) was used by several authors (e.g. Pinsonneault et al. 2001; Santos et al. 2001; Gonzalez et al. 2001; Santos et al. 2003a) to try to decide whether the excess metallicity observed in planet-host stars is of “primordial origin”…”
• Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog (2006, methodology): “Pinsonneault et al. (2001) computed the mass of convective zone for stars with masses in the range 0.6 – 1.3M⊙ and showed that Mce is a sensitive function of the effective temperature.”
• Planet formation and migration (2005, background): “This metallicity excess appears to have a “primordial” origin (Pinsonneault et al 2001; Santos et al 2001; Santos et al 2002; Sadakane et al 2002), rather than being due to the infall of planetary material onto the star which might result in observed heavy element polution for stars in the mass…”