2021A&A...647A..49S


Query : 2021A&A...647A..49S

2021A&A...647A..49S - Astronomy and Astrophysics, volume 647A, 49-49 (2021/3-1)

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. and COLLADO A.

Abstract (from CDS):


Aims. Our goal is to explore the chemical pattern of early-type stars with planets, searching for a possible signature of planet formation. In particular, we study a likely relation between the λ Bootis chemical pattern and the presence of giant planets.
Methods. We performed a detailed abundance determination in a sample of early-type stars with and without planets via spectral synthesis. Fundamental parameters were initially estimated using Stromgren photometry or literature values and then refined by requiring excitation and ionization balances of Fe lines. We derived chemical abundances for 23 different species by fitting observed spectra with an iterative process. Synthetic spectra were calculated using the program SYNTHE together with local thermodynamic equilibrium ATLAS12 model atmospheres. We used specific opacities calculated for each star, depending on the individual composition and microturbulence velocity vmicro through the opacity sampling method. The complete chemical pattern of the stars were then compared to those of λ Bootis stars and other chemically peculiar stars.
Results. We compared the chemical pattern of the stars in our sample (13 stars with planets and 24 stars without detected planets) with those of λ Bootis and other chemically peculiar stars. We have found four λ Bootis stars in our sample, two of which present planets and circumstellar disks (HR 8799 and HD 169142) and one without planets detected (HD 110058). We have also identified the first λ Bootis star orbited by a brown dwarf (ζ Del). This interesting pair, the λ Bootis star and brown dwarf, could help to test stellar formation scenarios. 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 λ Bootis-like pattern. On the other hand, we do not find a λ 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 λ Bootis pattern between main-sequence stars. Finally, we suggest that the formation of planets around λ Bootis stars, such as HR 8799 and HD 169142, is also possible through the core accretion process and not only gravitational instability.

Abstract Copyright: © ESO 2021

Journal keyword(s): stars: early-type - stars: abundances - planetary systems

VizieR on-line data: <Available at CDS (J/A+A/647/A49): table3.dat tablea1.dat>

Simbad objects: 41

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Number of rows : 41
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 V* BU Psc gD* 00 02 02.6171019192 -02 45 58.215204612   7.20 6.92     A9V/IV 56 0
2 * ome And ** 01 27 39.3807155195 +45 24 24.065127426 5.25 5.25 4.83 4.42 4.19 F4IV 145 0
3 HD 15082 EB* 02 26 51.0582618096 +37 33 01.736482032   8.41 8.14     kA5hA8mF4 198 1
4 HD 23281 * 03 43 33.8338762320 -10 29 08.365157736 5.88 5.80 5.61 5.40 5.30 A5III-IV 89 0
5 * 51 Eri PM* 04 37 36.1326090888 -02 28 24.775726260   5.486 5.209     F0IV 241 0
6 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1899 1
7 V* V435 Car dS* 06 21 50.0593461744 -51 14 15.751606740   6.95 6.73     A5V 38 0
8 HD 50445 PM* 06 51 42.4207334784 -36 13 48.979898580   6.120 5.940     A3V 35 0
9 * lam Gem PM* 07 18 05.5789195368 +16 32 25.389581244   3.674 3.559     A4IV 255 0
10 BD+07 1721 EB* 07 26 02.2901761080 +07 36 56.815027668   10.21 9.86     A8V+G9V/K1V 23 0
11 BD+14 1881 Pe* 08 22 28.2046820904 +13 44 07.143774288   9.53 9.23   8.948 kA1hA5mA9Si 36 0
12 * q Vel PM* 10 14 44.1557297 -42 07 18.993292 3.98 3.90 3.85 3.83 3.81 A2Va 135 0
13 HD 95086 * 10 57 03.0215719872 -68 40 02.449216128   7.60 7.36     A8III 176 1
14 HD 101615 EB* 11 41 19.7910777168 -43 05 44.397442968   5.57 5.53     A0V 54 0
15 * 3 Crv PM* 12 11 03.8390016096 -23 36 08.715836340   5.52 5.47     A1V 57 0
16 HD 110058 * 12 39 46.1962525608 -49 11 55.550898744   8.12 7.97     A0V 84 0
17 CD-34 8618 * 13 04 10.5339280776 -35 32 58.322148612   10.93 10.52     ~ 16 0
18 HD 115820 * 13 20 26.8121687568 -49 13 25.207170420   8.19 7.95     A7/8V 40 0
19 HD 120326 * 13 49 54.5032282344 -50 14 23.876991348   8.75 8.39     F0V 64 0
20 * lam Boo dS* 14 16 23.0184083839 +46 05 17.895459693 4.31 4.26 4.18 4.16 4.13 A0Va_lB 348 0
21 * m Hya ** 14 46 00.07998 -25 26 35.4355           F0VSr+G1V 69 0
22 HD 133112 PM* 15 02 44.8678907928 -03 01 52.986571896   6.788 6.618     A4/5IV/V 60 0
23 HD 133803 gD* 15 07 14.9365580040 -29 30 16.132469112   8.47 8.12     F2IVm-2 55 0
24 HD 134004 * 15 09 04.8933581184 -42 42 17.789374620   10.05 9.95     A1V 21 0
25 * bet Cir PM* 15 17 30.8501567 -58 48 04.337319   4.153 4.057     A3Va 128 0
26 HD 139614 Ae? 15 40 46.3820275416 -42 29 53.538761832   8.47 8.24     A9VekA5mA5(_lB) 209 0
27 * d Sco PM* 16 18 17.8991603537 -28 36 50.471996469   4.804 4.782     A1Va 161 0
28 HD 153053 PM* 17 00 06.2792932296 -54 35 49.837300800   5.816 5.633     A5IV/V 42 0
29 HD 156751 PM* 17 22 47.8854372504 -58 28 23.679597756   7.05 6.84 7.75   A7II/III 27 0
30 * pi. Ara PM* 17 38 05.5153908936 -54 30 01.562028048   5.431 5.242     A5IV/V 96 0
31 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 448 0
32 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2686 1
33 * 59 Dra PM* 19 09 09.8814606288 +76 33 37.813819608   5.400 5.107     A7V 125 1
34 HD 185603 EB* 19 38 38.7352230144 +31 13 09.217127532   7.67 7.58     A0 54 0
35 * eps Pav PM* 20 00 35.5555788 -72 54 37.819779   3.927 3.940     A0Va 130 0
36 HD 340099 * 20 21 45.9296022840 +26 41 33.605958552   10.675 10.326   9.597 A8 24 0
37 HD 195689 SB* 20 31 26.3534153736 +39 56 19.773037500   7.59 7.56     A0 120 0
38 * zet Del * 20 35 18.5362051999 +14 40 27.173946047   4.738 4.647     A3Va 81 0
39 HD 201585 * 21 10 12.3723073896 +10 44 19.949472816   8.51 8.27     A8 37 0
40 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1234 3
41 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1135 0

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