Are beryllium abundances anomalous in stars with giant planets?

• Published in: Astronomy and astrophysics (Berlin) 2004-12, Vol.427 (3), p.1085-1096
• Main Authors: Santos, N. C., Israelian, G., García López, R. J., Mayor, M., Rebolo, R., Randich, S., Ecuvillon, A., Domínguez Cerdeña, C.
• Format: Article
• Language: English
• Subjects: stars: abundances; stars: atmospheres; stars: fundamental parameters; stars: planetary systems; stars: planetary systems: formation
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361:20040509

In this paper we present beryllium (Be) abundances in a large sample of 41 extra-solar planet host stars, and for 29 stars without any known planetary-mass companion, spanning a large range of effective temperatures. The Be abundances were derived through spectral synthesis done in standard Local Thermodynamic Equilibrium, using spectra obtained with various instruments. The results seem to confirm that overall, planet-host stars have “normal” Be abundances, although a small, but not significant, difference might be present. This result is discussed, and we show that this difference is probably not due to any stellar “pollution” events. In other words, our results support the idea that the high-metal content of planet-host stars has, overall, a “primordial” origin. However, we also find a small subset of planet-host late-F and early-G dwarfs that might have higher than average Be abundances. The reason for the offset is not clear, and might be related either to the engulfment of planetary material, to galactic chemical evolution effects, or to stellar-mass differences for stars of similar temperature.