2016ApJ...827....8N


Query : 2016ApJ...827....8N

2016ApJ...827....8N - Astrophys. J., 827, 8-8 (2016/August-2)

Friends of hot jupiters. IV. Stellar companions beyond 50 au might facilitate giant planet formation, but most are unlikely to cause Kozai-Lidov migration.

NGO H., KNUTSON H.A., HINKLEY S., BRYAN M., CREPP J.R., BATYGIN K., CROSSFIELD I., HANSEN B., HOWARD A.W., JOHNSON J.A., MAWET D., MORTON T.D., MUIRHEAD P.S. and WANG J.

Abstract (from CDS):

Stellar companions can influence the formation and evolution of planetary systems, but there are currently few observational constraints on the properties of planet-hosting binary star systems. We search for stellar companions around 77 transiting hot Jupiter systems to explore the statistical properties of this population of companions as compared to field stars of similar spectral type. After correcting for survey incompleteness, we find that 47 % ±7 % of hot Jupiter systems have stellar companions with semimajor axes between 50 and 2000 au. This is 2.9 times larger than the field star companion fraction in this separation range, with a significance of 4.4σ. In the 1-50 au range, only {3.9}_{-2.0}^{+4.5} % of hot Jupiters host stellar companions, compared to the field star value of 16.4 % ±0.7 % , which is a 2.7σdifference. We find that the distribution of mass ratios for stellar companions to hot Jupiter systems peaks at small values and therefore differs from that of field star binaries which tend to be uniformly distributed across all mass ratios. We conclude that either wide separation stellar binaries are more favorable sites for gas giant planet formation at all separations, or that the presence of stellar companions preferentially causes the inward migration of gas giant planets that formed farther out in the disk via dynamical processes such as Kozai-Lidov oscillations. We determine that less than 20% of hot Jupiters have stellar companions capable of inducing Kozai-Lidov oscillations assuming initial semimajor axes between 1 and 5 au, implying that the enhanced companion occurrence is likely correlated with environments where gas giants can form efficiently.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): binaries: close - binaries: eclipsing - methods: observational - planetary systems - planets and satellites: dynamical evolution and stability - techniques: high angular resolution - techniques: high angular resolution

Simbad objects: 43

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Number of rows : 43
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HAT-P-19 * 00 38 04.0135699416 +34 42 41.553538560   13.834 12.853 12.611   K1V 31 1
2 HAT-P-28 * 00 52 00.1876130976 +34 43 42.205232532   13.4   13.24   ~ 22 1
3 BD+01 316 PM* 01 46 31.8575937456 +02 42 02.030065560   10.13 9.52     F7 52 0
4 BD+01 316b Pl 01 46 31.8576707085 +02 42 02.033178181           ~ 140 0
5 HAT-P-29b Pl 02 12 31.4784785872 +51 46 43.562095527           ~ 28 1
6 HAT-P-29 * 02 12 31.4787454416 +51 46 43.563748620   12.30 11.83 11.82   ~ 30 1
7 HAT-P-38 PM* 02 21 31.9803537360 +32 14 46.093339140   13.34 12.51 12.36   G 18 0
8 HD 15082 dS* 02 26 51.0582618096 +37 33 01.736482032   8.41 8.14     kA5hA8mF4 175 1
9 WASP-11 ** 03 09 28.5433589520 +30 40 24.862993356   12.58 11.57 11.42   K3V 78 1
10 HAT-P-25 * 03 13 44.4981245184 +25 11 50.689343148   14.12 13.15 13.22 11.98 G5 28 1
11 HAT-P-54 * 06 39 35.5181974296 +25 28 57.156510144   14.832 13.505     ~ 18 0
12 HAT-P-9 * 07 20 40.4564614032 +37 08 26.342829060   12.35 12.34 12.08   F 51 1
13 HAT-P-39 * 07 35 01.9793942688 +17 49 48.235016856     12.422     ~ 18 1
14 HAT-P-39b Pl 07 35 01.9794135519 +17 49 48.234882594           ~ 18 1
15 HAT-P-35 * 08 13 00.1784913648 +04 47 13.416267948   12.84 11.59 12.38   ~ 27 1
16 HAT-P-35b Pl 08 13 00.1786456777 +04 47 13.417449950           ~ 21 1
17 HAT-P-43 * 08 35 42.1747382424 +10 12 23.924988648   14.12 13.36 13.17   ~ 19 1
18 WASP-36 V* 08 46 19.2977439552 -08 01 37.015743396   13.1 12.7   12.05 G2 43 1
19 HAT-P-42 * 09 01 22.6491794664 +06 05 50.013869568   12.83 12.17 12.02   ~ 19 1
20 BD+34 1976 V* 09 20 24.7145388600 +33 52 56.696039796   11.21 10.42     G1V 65 1
21 WASP-43 PM* 10 19 38.0088913464 -09 48 22.605801336   13.4 12.4 12.08 11.10 K7V 122 1
22 HAT-P-21 * 11 25 05.9859193536 +41 01 40.664937216   12.56 11.46 11.71   G3 30 1
23 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     A9Ve 250 1
24 HAT-P-36 * 12 33 03.9061156728 +44 54 55.196024616   12.97 12.15 12.27   ~ 42 1
25 HAT-P-3 * 13 44 22.5937349736 +48 01 43.205733624   12.53 11.86     K1V 78 1
26 WASP-39 * 14 29 18.4151689656 -03 26 40.204480380   12.93 12.09 12.17 11.29 ~ 46 1
27 HAT-P-27 * 14 51 04.1870399712 +05 56 50.548526376   13.18 12.19 11.98 11.23 G8 54 1
28 WASP-40b Pl 14 51 04.1870409044 +05 56 50.548178856           ~ 36 1
29 HD 141569 Y*O 15 49 57.7482550392 -03 55 16.341617064 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 508 0
30 BD+28 2507 V* 16 02 11.8462322592 +28 10 10.420201452   11.88 11.25     G1V 98 1
31 WASP-103 * 16 37 15.5765824488 +07 11 00.109678740     12.1     F8V 59 1
32 HAT-P-5 * 18 17 37.3126923960 +36 37 17.170401468   12.92 11.95     G1V 60 1
33 WASP-58 PM* 18 18 48.2529552984 +45 10 19.260291288   12.33 11.66     G2V 26 1
34 WASP-58b Pl 18 18 48.2530627697 +45 10 19.259152747           ~ 23 1
35 HAT-P-37 * 18 57 11.0562256392 +51 16 08.850467640   13.1 13.23 13.58   ~ 24 1
36 NAME V672 Lyr b Pl 19 04 09.8516024106 +36 37 57.445911611           ~ 324 1
37 WASP-48 * 19 24 38.9614451424 +55 28 23.332107108   12.31 11.65 11.61   ~ 41 1
38 HAT-P-41 * 19 49 17.4398486136 +04 40 20.786070360   11.65 11.36     ~ 34 1
39 HAT-P-41b Pl 19 49 17.4399552361 +04 40 20.783585782           ~ 50 1
40 HAT-P-23 * 20 24 29.7234392904 +16 45 43.811510112   13.05 11.94 12.27   G0 56 1
41 HAT-P-40 * 22 22 03.0875673648 +45 27 26.518064616   12.19 11.34     ~ 23 1
42 BD+37 4734B PM* 22 57 46.8442481880 +38 40 30.358351704   10.82 9.87     G0V 156 1
43 WASP-5 V* 23 57 23.7564672192 -41 16 37.743700800   12.808 12.146 12.058 11.44 G4V 109 1

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