J/A+A/647/A49  Chemical analysis of early-type stars with planets (Saffe+, 2021)

Chemical analysis of early-type stars with planets. Saffe C., Miquelarena P., Alacoria J., Flores M., Jaque Arancibia M., Calvo D., Martin Girardi G., Grosso M., Collado A. <Astron. Astrophys. 647, A49 (2021)> =2021A&A...647A..49S 2021A&A...647A..49S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, early-type ; Exoplanets ; Abundances Keywords: stars: early-type - stars: abundances - stars: planetary systems Abstract: We performed a detailed abundance determination in a sample of early-type stars with and without planets via spectral synthesis, searching for a likely relation between lambda Bootis stars and the presence of planets. We found no unique chemical pattern for the group of early-type stars bearing giant planets. However, our results support, in principle, a suggested scenario in which giant planets orbiting pre-main-sequence stars possibly block the dust of the disk and result in a lambda Bootis-like pattern. On the other hand, we do not find a lambda Bootis pattern in different hot-Jupiter planet host stars, which does not support the idea of possible accretion from the winds of hot-Jupiters, recently proposed in the literature. As a result, other mechanisms should account for the presence of the lambda Bootis pattern between main-sequence stars. Finally, we suggest that the formation of planets around lambda Bootis stars, such as HR 8799 and HD 169142, is also possible through the core accretion process and not only gravitational instability. Description: Detailed chemical abundances for the sample of early-type stars with and without planets. For each chemical specie, we present the average abundance [N/H] derived from different lines (relative to the Sun), the total abundance error (Etot), the dispersion originated by different lines (e1), the uncertainty due to the error of effective temperature (e2), the uncertainty due to the error of superficial gravity (e3), and the uncertainty due to the error in microturbulence velocity (e4). The total error Etot is estimated as the quadratic sum of e1, e2, e3 and e4. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table3.dat 76 37 Fundamental parameters derived for the stars in this work tablea1.dat 62 605 Chemical abundances of early-type stars -------------------------------------------------------------------------------- Byte-by-byte Description of file:table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- Star Star name 14- 18 I5 K Teff Effective temperature 20- 22 I3 K e_Teff Effective temperature error 24- 27 F4.2 [cm/s2] logg Surface gravity 29- 32 F4.2 [cm/s2] e_logg Surface gravity error 34- 37 F4.2 km/s vmicro Microturbulent velocity 39- 42 F4.2 km/s e_vmicro Microturbulent velocity error 44- 48 F5.1 km/s vsini Rotational velocity 50- 52 F3.1 km/s e_vsini Rotational velocity error 54- 55 I2 h RAh Simbad right ascension (J2000) 57- 58 I2 min RAm Simbad right ascension (J2000) 60- 64 F5.2 s RAs Simbad right ascension (J2000) 66 A1 --- DE- Simbad declination sign (J2000) 67- 68 I2 deg DEd Simbad declination (J2000) 70- 71 I2 arcmin DEm Simbad declination (J2000) 73- 76 F4.1 arcsec DEs Simbad declination (J2000) -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablea1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 13 A13 --- Star Star name 14- 20 A7 --- Element Chemical specie 21- 27 F7.2 --- [N/H] Abundance relative to the Sun 28- 34 F7.2 --- Etot Total abundance error 35- 41 F7.2 --- e1 Dispersion of different lines 42- 48 F7.2 --- e2 Uncertainty due to temperature 49- 55 F7.2 --- e3 Uncertainty due to gravity 56- 62 F7.2 --- e4 Uncertainty due to microturbulence -------------------------------------------------------------------------------- Acknowledgements: Carlos Saffe, csaffe(at)conicet.gov.ar
(End) Patricia Vannier [CDS] 13-Jan-2021
The document above follows the rules of the Standard Description for Astronomical Catalogues; from this documentation it is possible to generate f77 program to load files into arrays or line by line