C.D.S. - SIMBAD4 rel 1.7 - 2021.03.09CET11:22:20

2015A&A...582A..17S - Astronomy and Astrophysics, volume 582A, 17-17 (2015/10-1)

HD 80606: searching for the chemical signature of planet formation.


Abstract (from CDS):

Binary systems with similar components are ideal laboratories that allow several physical processes to be tested, such as the possible chemical pattern imprinted by the planet formation process. We explore the probable chemical signature of planet formation in the remarkable binary system HD80606-HD80607. The star HD80606 hosts a giant planet with ∼4MJup detected by both transit and radial velocity techniques, which is one of the most eccentric planets detected to date. We study condensation temperature Tc trends of volatile and refractory element abundances to determine whether there is a depletion of refractories, which could be related to the terrestrial planet formation. We carried out a high-precision abundance determination in both components of the binary system via a line-by-line, strictly differential approach. First, we used the Sun as a reference and then we used HD80606. The stellar parameters Teff, logg, [Fe/H] and vturb were determined by imposing differential ionization and excitation equilibrium of Fe I and Fe II lines, with an updated version of the program FUNDPAR, together with plane-parallel local thermodynamic equilibrium (LTE) ATLAS9 model atmospheres and the MOOG code. Then, we derived detailed abundances of 24 different species with equivalent widths and spectral synthesis with the program MOOG. The chemical patterns were compared with the solar-twins Tc trends of Melendez et al. (2009ApJ...704L..66M) and with a sample of solar-analogue stars with [Fe/H]~+0.2dex from Neves et al. (2009A&A...497..563N). The Tc trends were also compared mutually between both stars of the binary system. From the study of Tc trends, we concluded that the stars HD80606 and HD80607 do not seem to be depleted in refractory elements, which is different for the case of the Sun. Then, following the interpretation of Melendez et al. (2009ApJ...704L..66M), the terrestrial planet formation would have been less efficient in the components of this binary system than in the Sun. The lack of a trend in refractory elements with Tc between both stars implies that the presence of a giant planet do not neccesarily imprint a chemical signature in their host stars, similar to the recent result of Liu et al. (2014MNRAS.442L..51L). This is also in agreement with Melendez et al. (2009ApJ...704L..66M), who suggest that the presence of close-in giant planets might prevent the formation of terrestrial planets. Finally, we speculate about a possible, ejected or non-detected, planet around the star HD80607.

Abstract Copyright:

Journal keyword(s): stars: abundances - planetary systems - binaries: general - stars: individual: HD80606

VizieR on-line data: <Available at CDS (J/A+A/582/A17): list.dat fits/*>

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 BD+50 1471 PM* 07 48 06.4726006390 +50 13 32.921121328   12.002 11.138 10.669 10.243 G9V 142 1
2 HD 80606b Pl 09 22 37.5769478105 +50 36 13.434928660           ~ 282 1
3 HD 80606 PM* 09 22 37.5769478105 +50 36 13.434928660   9.78 9.00     G5 291 2
4 HD 80607 PM* 09 22 39.7367015092 +50 36 13.952617706   9.937 9.070     G5 84 2
5 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 690 1
6 * 16 Cyg ** 19 41 49.09 +50 31 31.6           ~ 123 0
7 * 16 Cyg Bb Pl 19 41 51.9731830550 +50 31 03.086127222           ~ 120 1
8 NAME BD+37 4734Bb Pl 22 57 46.8443014981 +38 40 30.355384717           ~ 208 1
9 BD+37 4734B PM* 22 57 46.8443014981 +38 40 30.355384717   10.82 9.87     G0V 145 1

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