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:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file:table3.dat
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Bytes Format Units Label Explanations
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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)
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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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
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Acknowledgements:
Carlos Saffe, csaffe(at)conicet.gov.ar
(End) Patricia Vannier [CDS] 13-Jan-2021