2018A&A...612A..93M


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.18CET06:02:23

2018A&A...612A..93M - Astronomy and Astrophysics, volume 612A, 93-93 (2018/4-1)

Chemical fingerprints of hot Jupiter planet formation.

MALDONADO J., VILLAVER E. and EIROA C.

Abstract (from CDS):


Context. The current paradigm to explain the presence of Jupiter-like planets with small orbital periods (P<10-days; hot Jupiters), which involves their formation beyond the snow line following inward migration, has been challenged by recent works that explore the possibility of in situ formation.
Aims. We aim to test whether stars harbouring hot Jupiters and stars with more distant gas-giant planets show any chemical peculiarity that could be related to different formation processes.
Methods. Our methodology is based on the analysis of high-resolution echelle spectra. Stellar parameters and abundances of C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, and Zn for a sample of 88 planet hosts are derived. The sample is divided into stars hosting hot (a<0.1au) and cool (a>0.1au) Jupiter-like planets. The metallicity and abundance trends of the two sub-samples are compared and set in the context of current models of planet formation and migration.
Results. Our results show that stars with hot Jupiters have higher metallicities than stars with cool distant gas-giant planets in the metallicity range +0.00/+0.20dex. The data also shows a tendency of stars with cool Jupiters to show larger abundances of α elements. No abundance differences between stars with cool and hot Jupiters are found when considering iron peak, volatile elements or the C/O, and Mg/Si ratios. The corresponding p-values from the statistical tests comparing the cumulative distributions of cool and hot planet hosts are 0.20, <0.01, 0.81, and 0.16 for metallicity, α, iron-peak, and volatile elements, respectively. We confirm previous works suggesting that more distant planets show higher planetary masses as well as larger eccentricities. We note differences in age and spectral type between the hot and cool planet host samples that might affect the abundance comparison.
Conclusions. The differences in the distribution of planetary mass, period, eccentricity, and stellar host metallicity suggest a different formation mechanism for hot and cool Jupiters. The slightly larger α abundances found in stars harbouring cool Jupiters might compensate their lower metallicities allowing the formation of gas-giant planets.

Abstract Copyright: © ESO 2018

Journal keyword(s): techniques: spectroscopic - stars: abundances - stars: late-type - planetary systems

Simbad objects: 88

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Number of rows : 88

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 142 PM* 00 06 19.17544 -49 04 30.6817   6.30 5.76     F7V 204 1
2 HD 1237 PM* 00 16 12.6791488703 -79 51 04.244738563 7.692 7.335 6.578     G8V 190 1
3 HD 2039 PM* 00 24 20.2781992627 -56 39 00.181780096   9.65 8.99     G2/3IV/V 94 1
4 HD 2638 ** 00 29 59.8720587219 -05 45 50.398743428   10.33 9.38 9.10 9.19 K1V 61 1
5 * ups And PM* 01 36 47.84216 +41 24 19.6443 4.70 4.64 4.10 3.64 3.35 F9V 883 1
6 HD 11506 PM* 01 52 50.5345499280 -19 30 25.110796380   8.11 7.51     G0V 63 1
7 HD 12661 PM* 02 04 34.2883519451 +25 24 51.514208219   8.16   7.0   K0V 230 1
8 * 79 Cet PM* 02 35 19.9292617962 -03 33 38.170691640   7.49 6.78     G2V 257 1
9 * 94 Cet PM* 03 12 46.4369076602 -01 11 45.949836281   5.631 5.070     F8.5V 399 1
10 HD 20782 PM* 03 20 03.5777409770 -28 51 14.660409684   8.03 7.38     G1.5V 153 1
11 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1660 1
12 HD 23079 PM* 03 39 43.0960508327 -52 54 57.016146971   7.68 7.11     F9.5V 133 1
13 HD 27631 PM* 04 19 45.4693133676 -41 57 36.951524035   8.914 8.24 8.38   G3IV/V 41 1
14 HD 28185 PM* 04 26 26.3227027269 -10 33 02.945489682   8.52 7.81     G6.5IV-V 153 1
15 HD 30177 PM* 04 41 54.3739541801 -58 01 14.724686984   9.18 8.37     G8V 110 1
16 HD 30669 PM* 04 48 28.4853499332 -28 25 09.461904064   9.93 9.11     G8/K0V 42 0
17 HD 33283 PM* 05 08 01.0122843442 -26 47 50.894096538 8.870 8.640 8.040     G3/5V 72 1
18 * pi. Men PM* 05 37 09.8851202601 -80 28 08.831347245   6.25 5.67     G0V 220 1
19 HD 41004 ** 05 59 49.6473573887 -48 14 22.805780232   9.49 8.65     K1IV 150 1
20 HD 46375 PM* 06 33 12.6225933827 +05 27 46.527797938   8.70 7.84     K1IV 201 2
21 * nu.02 CMa PM* 06 36 41.0375756 -19 15 21.165905 5.96 5.011 3.91 3.13 2.61 K1.5III-IVFe1 236 1
22 HD 49674 PM* 06 51 30.5163382954 +40 52 03.925594792   8.83 8.10     G0 120 1
23 HD 50499 PM* 06 52 02.0243202297 -33 54 56.016399083   7.82 7.20     G0/2V 80 1
24 HD 52265 PM* 07 00 18.0357152121 -05 22 01.778490073   6.845 6.282     G0V 276 1
25 HD 65216 PM* 07 53 41.3193105336 -63 38 50.353209584   8.65 7.96     G5V 104 1
26 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 454 2
27 V* CS Pyx BY* 08 36 23.0163309904 -30 02 15.441850007   8.84 8.06     G8IV-VFe+0.5 127 1
28 HD 73534 PM* 08 39 15.8030495855 +12 57 37.348477409   9.21 8.24     G5 40 1
29 HD 74156 PM* 08 42 25.1221445320 +04 34 41.146391815       7.2   G1V 194 2
30 HD 75289 PM* 08 47 40.3895634256 -41 44 12.456269569 7.04 6.94 6.36     F9VFe+0.3 238 1
31 HD 76700 PM* 08 53 55.5158663272 -66 48 03.574256032   8.88 8.13     G6V 108 1
32 HD 77338 PM* 09 01 12.4937500947 -25 31 37.433309411   9.47 8.59     K0IV 51 1
33 HD 82943 PM* 09 34 50.7352288445 -12 07 46.363303103   7.17 6.53     F9VFe+0.5 395 2
34 HD 83443 PM* 09 37 11.8276134249 -43 16 19.932615823   9.03 8.24     K0/1V+G(III) 193 1
35 HD 86081 PM* 09 56 05.9185287123 -03 48 30.323313278   9.34 8.70     G1V 56 1
36 HD 86226 PM* 09 56 29.8441755158 -24 05 57.795793912   8.563 7.93 7.71   G2V 46 1
37 HD 86264 PM* 09 56 57.8386126022 -15 53 42.422984371   7.92 7.41     F7V 49 1
38 HD 92788 PM* 10 42 48.5280658285 -02 11 01.522096792   8.01 7.30     G6V 192 1
39 BD-10 3166 PM* 10 58 28.7842601404 -10 46 13.391758325   10.88 10.01 9.85 9.19 K3.0V 115 1
40 HD 96167 PM* 11 05 15.0687870608 -10 17 28.694691689   8.82 8.08     G3V 44 1
41 HD 98649 PM* 11 20 51.7687156812 -23 13 02.425068034   8.646 7.99 7.75 8.26 G3/5V 47 1
42 HD 99109 PM* 11 24 17.3586264283 -01 31 44.663474688   9.96 9.06     G8/K0IV 83 1
43 HD 101930 PM* 11 43 30.1133689238 -58 00 24.776845450   9.12 8.21     K2V+ 81 1
44 HD 102195 PM* 11 45 42.2927799874 +02 49 17.326151286       7.6   K0V 98 1
45 V* PR Vir BY* 11 56 41.1855718442 -02 46 44.235013734   10.44 9.49     K1IV/V 35 0
46 HD 103774 PM* 11 56 55.5894945689 -12 06 28.470004762   7.61 7.12     F6V 32 1
47 HD 108147 PM* 12 25 46.2670326229 -64 01 19.515027395   7.532 6.994     F8/G0V 150 1
48 HD 109749 PM* 12 37 16.3786075146 -40 48 43.624370244   8.864 8.208 8.96   G3V 72 1
49 HD 111232 PM* 12 48 51.7525840250 -68 25 30.547067196   8.29 7.61     G8VFe-1.0 114 1
50 HD 114783 PM* 13 12 43.7856018216 -02 15 54.129940644 9.137 8.469 7.550 7.053 6.627 K1V 154 1
51 HD 114729 PM* 13 12 44.25696 -31 52 24.0555   7.31 6.69     G0V 152 1
52 HD 117207 PM* 13 29 21.1129830405 -35 34 15.586278234   7.98 7.25     G7IV-V 102 1
53 HD 117618 PM* 13 32 25.5555942170 -47 16 16.913384391   7.77 7.17     G0V 97 1
54 HD 118203 PM* 13 34 02.5394311294 +53 43 42.698368523   8.75 8.06     K0 62 1
55 * tau Boo ** 13 47 15.74340 +17 27 24.8552 5.02 4.98 4.49 4.09 3.85 F7IV-V 863 1
56 HD 126525 PM* 14 27 32.9718177113 -51 55 59.107520674   8.529 7.85 7.56 8.31 G4V 78 1
57 HD 128311 BY* 14 36 00.5607343227 +09 44 47.453643485 9.232 8.441 7.446 6.895 6.425 K3V 262 1
58 HD 130322 PM* 14 47 32.7265637197 -00 16 53.305928889   8.82 8.04     K0V 224 1
59 * 23 Lib PM* 15 13 28.6671093171 -25 18 33.654699099   7.168 6.46 6.43   G6IV-V 252 1
60 HD 330075 PM* 15 49 37.6938243823 -49 57 48.677088732   10.23 9.33     G5 73 1
61 HD 143105 * 15 53 36.5588770309 +68 43 12.411637723   7.27 6.75     F5 21 0
62 HD 142415 PM* 15 57 40.7918993254 -60 12 00.922769552   7.94 7.34     G1V 89 1
63 HD 143361 PM* 16 01 50.3482052938 -44 26 04.343500265   9.93 9.16     G6V 48 1
64 HD 147513 PM* 16 24 01.2905970257 -39 11 34.734611237 6.17 6.02 5.376     G5V 306 1
65 HD 148156 PM* 16 28 17.2846186438 -46 19 03.463378236   8.26 7.69     G0/2V 54 1
66 HD 149143 PM* 16 32 51.0508085515 +02 05 05.381400381   8.56 7.89     G3V 73 1
67 HD 154672 PM* 17 10 04.9104594412 -56 26 57.373212880   8.91 8.20     G3IV 43 1
68 HD 164604 PM* 18 03 06.9331415426 -28 33 38.357588084   10.88 9.83     K3.5Vk: 34 1
69 HD 168746 PM* 18 21 49.7828389501 -11 55 21.653794976   8.66 7.95     G5V 158 2
70 HD 170469 PM* 18 29 10.9812401099 +11 41 43.798483675   8.86 8.18     G5 66 1
71 BD+61 1762 PM* 18 36 53.1542192147 +61 42 09.015575427       8.1   G5 15 1
72 HD 179949 PM* 19 15 33.2300861317 -24 10 45.673372382   6.772 6.237     F8V 338 1
73 HD 187123 PM* 19 46 58.1122608389 +34 25 10.279867125       7.4   G2V 210 1
74 HD 187085 PM* 19 49 33.9664782612 -37 46 49.973931792   7.78 7.21     G0V 71 1
75 HD 190647 PM* 20 07 19.6698192687 -35 32 19.078587550   8.54 7.78     G5V 65 1
76 HD 192263 BY* 20 13 59.8455148268 -00 52 00.771665295 9.447 8.724 7.767 7.231 6.771 K1/2V 208 1
77 HD 196050 ** 20 37 51.7098385539 -60 38 04.147300896   8.16 7.49     G3V 118 2
78 * mu.02 Oct PM* 20 41 44.1008440862 -75 21 02.884884826   7.05 6.44     G0V 38 1
79 HD 207832 PM* 21 52 36.2809985142 -26 01 35.613253912   9.48 8.79     G5V 58 1
80 HD 210277 PM* 22 09 29.8657193934 -07 32 55.163014863   8.85 8.57 7.36   G8V 293 2
81 HD 212301 PM* 22 27 30.9215928401 -77 43 04.529817437   8.31 7.76     F8V 71 1
82 HD 213240 PM* 22 31 00.3665162994 -49 25 59.767492660   7.41 6.80     G0/1V 144 1
83 * tau01 Gru PM* 22 53 37.9322277750 -48 35 53.824643522 6.85 6.66 6.04     G0V 162 1
84 * rho Ind PM* 22 54 39.4829644814 -70 04 25.356610041 6.95 6.71 6.05     G1VFe+0.3 163 1
85 HD 216770 PM* 22 55 53.7082013969 -26 39 31.548008089   8.92 8.10     G9VCN+1 107 1
86 * 51 Peg ** 22 57 27.9804167474 +20 46 07.782240714 6.39 6.16 5.46 4.97 4.61 G2IV 1059 1
87 HD 217107 ** 22 58 15.5411942071 -02 23 43.387117210   6.919 6.163     G8IV/V 327 1
88 HD 220689 PM* 23 25 52.9921486658 -20 36 57.701216544   8.355 7.76 7.65 8.59 G3V 37 1

    Equat.    Gal    SGal    Ecl

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2019.11.18-06:02:23

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