2013A&A...552A...6G


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.18CEST12:10:39

2013A&A...552A...6G - Astronomy and Astrophysics, volume 552A, 6-6 (2013/4-1)

Searching for the signatures of terrestrial planets in F-, G-type main-sequence stars.

GONZALEZ HERNANDEZ J.I., DELGADO-MENA E., SOUSA S.G., ISRAELIAN G., SANTOS N.C., ADIBEKYAN V.Zh. and UDRY S.

Abstract (from CDS):

Detailed chemical abundances of volatile and refractory elements have been discussed in the context of terrestrial-planet formation during in past years. The HARPS-GTO high-precision planet-search program has provided an extensive database of stellar spectra, which we have inspected in order to select the best-quality spectra available for late type stars. We study the volatile-to-refractory abundance ratios to investigate their possible relation with the low-mass planetary formation. We present a fully differential chemical abundance analysis using high-quality HARPS and UVES spectra of 61 late F- and early G-type main-sequence stars, where 29 are planet hosts and 32 are stars without detected planets. As for the previous sample of solar analogs, these stars slightly hotter than the Sun also provide very accurate Galactic chemical abundance trends in the metallicity range -0.3<[Fe/H]<0.4. Stars with and without planets show similar mean abundance ratios. Moreover, when removing the Galactic chemical evolution effects, these mean abundance ratios, Δ[X/Fe]SUN–STARS, against condensation temperature, tend to exhibit less steep trends with nearly zero or slightly negative slopes. We have also analyzed a subsample of 26 metal-rich stars, 13 with and 13 without known planets, with spectra at S/N∼850, on average, in the narrow metallicity range 0.04<[Fe/H]<0.19. We find the similar, although not equal, abundance pattern with negative slopes for both samples of stars with and without planets. Using stars at S/N≥550 provides equally steep abundance trends with negative slopes for stars both with and without planets. We revisit the sample of solar analogs to study the abundance patterns of these stars, in particular, 8 stars hosting super-Earth-like planets. Among these stars having very low-mass planets, only four of them reveal clear increasing abundance trends versus condensation temperature. Finally, we compared these observed slopes with those predicted using a simple model that enables us to compute the mass of rocks that have formed terrestrial planets in each planetary system. We do not find any evidence supporting the conclusion that the volatile-to-refractory abundance ratio is related to the presence of rocky planets.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: fundamental parameters - stars: atmospheres - planetary systems

VizieR on-line data: <Available at CDS (J/A+A/552/A6): stars.dat planets.dat single.dat>

Simbad objects: 73

goto Full paper

goto View the reference in ADS

Number of rows : 73

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 1388 PM* 00 17 58.8690394826 -13 27 20.308710371   7.09 6.50     G0V 103 0
2 HD 1461 PM* 00 18 41.8673684261 -08 03 10.805762856   7.14 6.46     G3VFe0.5 328 1
3 * zet Tuc PM* 00 20 04.2599713 -64 52 29.254760 4.82 4.80 4.23 3.73 3.40 F9.5V 351 0
4 HD 2039 PM* 00 24 20.2781992627 -56 39 00.181780096   9.65 8.99     G2/3IV/V 101 1
5 HD 3823 PM* 00 40 25.6702570458 -59 27 16.565812842   6.44 5.88     G0VFe-0.9CH-0.4 154 0
6 HD 6735 PM* 01 07 32.0518935701 -41 44 48.127363003   7.56 7.00     F9V 57 0
7 HD 7449 PM* 01 14 29.3222250437 -05 02 50.614804562   8.08 7.48     F9.5V 85 2
8 HD 9782 PM* 01 35 26.3082160890 -13 22 51.702585599   7.77 7.17     F9V 55 0
9 * ups And PM* 01 36 47.84216 +41 24 19.6443 4.70 4.64 4.10 3.64 3.35 F9V 904 1
10 HD 10180 * 01 37 53.5773715933 -60 30 41.485438420   7.95 7.32     G1V 162 2
11 * q01 Eri PM* 01 42 29.3148822519 -53 44 26.991165270   6.05 5.52     F9V 279 1
12 HD 11226 PM* 01 50 15.4483557846 -06 42 14.722510137   7.64 7.06     K4III 62 0
13 * iot Hor PM* 02 42 33.4664838826 -50 48 01.056222150   5.97 5.40     F8V 351 1
14 * 94 Cet PM* 03 12 46.4369076602 -01 11 45.949836281   5.631 5.070     F8.5V 415 1
15 HD 23079 PM* 03 39 43.0960508327 -52 54 57.016146971   7.68 7.11     F9.5V 146 1
16 HD 23596 PM* 03 48 00.3743574570 +40 31 50.300542774   7.85 7.24     F8 111 1
17 HD 31527 PM* 04 55 38.3827517884 -23 14 30.758953907   8.071 7.484 7.24 8.88 G0V 77 1
18 HD 31822 PM* 04 58 35.7660454116 -09 20 03.464109537   8.50 7.93     G1V 51 0
19 HD 33636 Pe* 05 11 46.4489745849 +04 24 12.759759957   7.64   6.6   G0V_CH-0.3 171 1
20 HD 36379 PM* 05 30 59.9404041031 -10 04 51.904429406   7.47 6.91     G2V 71 0
21 * pi. Men PM* 05 37 09.8851202601 -80 28 08.831347245   6.25 5.67     G0V 264 1
22 HD 38973 PM* 05 46 27.9906103524 -53 13 09.569229756   7.22 6.63     G0V 75 0
23 HD 44447 PM* 06 15 06.0182841360 -71 42 09.951988664   7.182 6.615     G0VFe-0.8CH-0.3 67 0
24 HD 44120 PM* 06 16 18.7861155187 -59 12 48.606746714   7.02 6.43     F9.5V 91 0
25 HD 45184 PM* 06 24 43.8797456693 -28 46 48.416253741   7.01 6.39 6.24 8.94 G2Va 171 1
26 HD 50554 PM* 06 54 42.8262327211 +24 14 44.008992953   7.41 6.84     F8V 174 1
27 HD 52265 PM* 07 00 18.0357152121 -05 22 01.778490073   6.845 6.282     G0V 296 1
28 HD 68978 PM* 08 13 34.4987340538 -31 44 07.381417481   7.36 6.75     G0.5V 76 0
29 HD 69655 PM* 08 15 25.2141947631 -52 03 37.072808906   7.190 6.619     G1V 67 0
30 HD 70889 PM* 08 23 31.8109268603 -27 49 20.475493888   7.68 7.09     F9.5V 59 0
31 HD 71479 PM* 08 27 35.1263989929 -05 08 55.088095382   7.81 7.18     G2/3V 77 0
32 HD 72659 PM* 08 34 03.1900792374 -01 34 05.579345170   8.08 7.47     G2V 134 1
33 HD 73121 PM* 08 35 12.5373815165 -39 58 13.620573526   7.007 6.431     F9.5V 75 0
34 HD 73524 PM* 08 37 19.9931199573 -40 08 51.600168904 7.29 7.15 6.55     G0Vp 126 0
35 HD 74156 PM* 08 42 25.1221445320 +04 34 41.146391815       7.2   G1V 208 2
36 HD 75289 PM* 08 47 40.3895634256 -41 44 12.456269569 7.04 6.94 6.36     F9VFe+0.3 254 1
37 HD 82943 PM* 09 34 50.7352288445 -12 07 46.363303103   7.17 6.53     F9VFe+0.5 419 2
38 HD 88742 PM* 10 13 24.7292010413 -33 01 54.193510617 7.06 6.97 6.38     G0V 140 0
39 HD 89744 PM* 10 22 10.5623067078 +41 13 46.308754730       5.4   F7V 309 1
40 HD 93385 PM* 10 46 15.1160197580 -41 27 51.726112295   8.08 7.486 7.61 8.82 G2/3V 76 1
41 HD 95456 PM* 11 00 40.7833785848 -31 50 21.728365315   6.575 6.051     F8V 73 0
42 HD 96700 PM* 11 07 54.4269492842 -30 10 28.445136193   7.11 6.503 6.59 8.95 G1VFe-0.5 132 1
43 HD 101364 PM* 11 40 28.4842891594 +69 00 30.600485781   9.32 8.67     G5 67 0
44 HD 108147 PM* 12 25 46.2670326229 -64 01 19.515027395   7.532 6.994     F8/G0V 160 1
45 HD 117618 PM* 13 32 25.5555942170 -47 16 16.913384391   7.77 7.17     G0V 106 1
46 HD 119638 PM* 13 44 44.6014824006 -14 13 30.649428385   7.40 6.92     F8.5V 57 0
47 HD 121504 PM* 13 57 17.2384093173 -56 02 24.156313081   8.12 7.52     G2V 152 1
48 HD 122862 PM* 14 08 27.1622887824 -74 51 01.032345398   6.60 6.02     F9.5V 105 0
49 HD 125881 PM* 14 24 45.9776416423 -63 42 23.637275986   7.85 7.25     G2V 65 0
50 HD 134060 PM* 15 10 44.7429942541 -61 25 20.361553963   6.91 6.285 6.16 8.68 G0VFe+0.4 110 1
51 HD 134606 PM* 15 15 15.0442916033 -70 31 10.643946773   7.61 6.854 6.69 8.89 G6IV 72 1
52 HD 145666 PM* 16 15 04.1593855561 -56 22 28.352532928   8.361 7.80     G2V 62 1
53 HD 157338 PM* 17 24 08.7399924603 -34 47 54.438253370   7.50 6.92     F9.5V 66 0
54 * mu. Ara PM* 17 44 08.7036342277 -51 50 02.591049123   5.85 5.15     G3IV-V 482 2
55 HD 168871 PM* 18 24 33.1377476498 -49 39 10.361256463   7.036 6.454     G1/2V 75 0
56 HD 169830 * 18 27 49.4852008378 -29 49 00.705771732   6.406 5.902 7.01   F7V 253 1
57 HD 171990 PM* 18 47 49.1311457626 -77 52 05.702768139   6.974 6.392     F8V 71 0
58 HD 179949 BY* 19 15 33.2300861317 -24 10 45.673372382   6.772 6.237     F8V 365 1
59 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 693 1
60 * 16 Cyg ** 19 41 49.09 +50 31 31.6           ~ 125 0
61 * 16 Cyg B PM* 19 41 51.9731830550 +50 31 03.086127222 7.07 6.86 6.20 5.76 5.42 G3V 815 1
62 HD 189567 PM* 20 05 32.7652367983 -67 19 15.228862402 6.79 6.71 6.07     G2V 204 1
63 HD 193193 PM* 20 19 45.1837570848 -25 13 42.972480422   9.030 8.571     G2V 76 0
64 HD 196800 PM* 20 40 22.3335773458 -24 07 04.902229061   7.82 7.23     G1/2V 77 0
65 * 11 Aqr PM* 21 00 33.8407622601 -04 43 48.940823425   6.819 6.192     G1V 191 0
66 HD 204385 PM* 21 30 47.9297993054 -62 10 03.373030468   7.74 7.15     G0VCH-0.3 68 0
67 HD 208487 PM* 21 57 19.8475392496 -37 45 49.047988735   8.02 7.47     G1/3(V) 101 1
68 HD 209458 V* 22 03 10.7729598762 +18 53 03.548248479   8.21 7.63     F9V 1021 1
69 HD 212301 PM* 22 27 30.9215928401 -77 43 04.529817437   8.31 7.76     F8V 81 1
70 HD 213240 PM* 22 31 00.3665162994 -49 25 59.767492660   7.41 6.80     G0/1V 157 1
71 * tau01 Gru PM* 22 53 37.9322277750 -48 35 53.824643522 6.85 6.66 6.04     G0V 177 1
72 HD 221287 PM* 23 31 20.3381873379 -58 12 35.032427169   8.31 7.81     F7V 66 1
73 HD 221356 PM* 23 31 31.5028338070 -04 05 14.655967513   7.03 6.49     F7V 142 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2013A&A...552A...6G and select 'bookmark this link' or equivalent in the popup menu


2021.06.18-12:10:39

© Université de Strasbourg/CNRS

    • Contact