This is a List of exoplanets discovered in 2012. [1] For exoplanets detected only by radial velocity, the mass value is actually a lower limit. (See Minimum mass for more information)
Name | Mass (MJ) | Radius (RJ) | Period (days) | Semi-major axis (AU) | Temp. (K) [2] | Discovery method | Distance (ly) | Host star mass (M☉) | Host star temp. (K) | Remarks |
---|---|---|---|---|---|---|---|---|---|---|
75 Ceti b | 3 | 691.9 | 2.1 | radial vel. | 266 | 2.49 | 4846 | [3] | ||
BD+20 274 b | 4.2 | 578.2 | 1.3 | radial vel. | 4500±300 | 0.8 | 4296 | [4] | ||
BD+48 740 b | 1.7±0.7 | 733+5 −8 | 1.7±0.1 | radial vel. | 2214±72 | 1.09±0.16 | 4534±8 | [5] Confirmed in 2018. [6] | ||
CoRoT-21b | 2.26 | 1.3 | 2.72 | 0.0417 | 1867 | transit | 4600±900 | 1.29 | 6200 | [7] |
Epsilon Coronae Borealis b | 6.7 | 417.9 | 1.3 | radial vel. | 229.7 | 1.7 | 4406 | [8] | ||
Gliese 676 Ad | 0.014 | 3.6005 | 0.0413±0.0014 | radial vel. | 52.29±0.03 | 0.71±0.04 | 3734 | [9] | ||
Gliese 676 Ae | 0.025 | 35.39 | 0.187±0.007 | radial vel. | 52.29±0.03 | 0.71±0.04 | 3734 | [9] | ||
Gliese 3470 b | 0.043 | 0.346 | 3.3366487 | 0.031 | radial vel. | 82 | 0.51 | 3652 | [10] | |
HAT-P-34b | 7.01 | 1.35 | 5.45265 | 0.06774 | 1520 | transit | 818.94 | 4.26 | 6442 | [11] Proper name Ġgantija |
HAT-P-35b | 7.52 | 3.55 | 3.64671 | 0.0498 | 1581 | transit | 1677 | 23.56 | 6096 | [11] |
HAT-P-36b | 1.8482 | 1.277 | 1.32734683 | 0.0241 | 1781 | transit | 968.49 | 1.03 | 5620 | [11] Proper name Bran |
HAT-P-37b | 1.169 | 1.178 | 2.797436 | 0.0379 | 1271 | transit | 1341 | 0.93 | 5500 | [11] Additional planets in system are suspected [12] |
HAT-P-38b | 0.267 | 0.825 | 4.640382 | 0.0523 | transit | 810 | 0.89 | 5330 | [13] Proper name Hiisi | |
HAT-P-39b | 0.599 | 1.571 | 3.54387 | 0.0509 | transit | 2090 | 1.4 | 6430 | [14] | |
HAT-P-40b | 0.615 | 1.73 | 4.457243 | 0.0608 | transit | 1630 | 1.51 | 6080 | [14] Proper name Vytis | |
HAT-P-41b | 0.8 | 1.685 | 2.694047 | 0.0426 | transit | 1120 | 1.42 | 6390 | [15] [14] [16] | |
HAT-P-42b | 1.044 | 1.28 | 4.641878 | 0.0575 | 1427 | transit | 1460 | 1.18 | 5743 | [17] Proper name Iolaus |
HAT-P-43b | 0.662 | 1.281 | 3.332687 | 0.0443 | 1361 | transit | 1770 | 1.05 | 5645 | [17] |
HATS-1b | 1.855 | 1.302 | 3.446459 | 0.0444 | transit | 990 | 0.99 | 5870 | [18] | |
HD 142 c | 5.3 | 6005 | 6.8 | radial vel. | 83.6 | 1.23 | 6245 | [19] | ||
HD 4732 b | 2.37 | 360.2 | 1.19 | radial vel. | 184 | 1.74 | 4959 | [20] | ||
HD 4732 c | 2.37 | 2732 | 4.6 | radial vel. | 184 | 1.74 | 4959 | [20] | ||
HD 5608 b | 1.4 | 792.6 | 1.9 | radial vel. | 189.7 | 1.55 | 4854 | [3] | ||
HD 24040 b | 4.10±0.12 | 3490±25 | 4.637±0.067 | radial vel. | 152.3±0.4 | 1.14±0.02 | 5917±52 | [21] Suspected since 2006 | ||
HD 27631 b | 1.45 | 2208 | 3.25 | radial vel. | 145.3 | 0.94 | 5737 | [22] | ||
HD 37605 c | 3.366 | 2720 | 3.814 | radial vel. | 139.9 | 1 | 5448 | [23] | ||
HD 40307 e | 0.0110±0.0044 | 34.62+0.21 −0.20 | 0.1886+0.083 −0.0104 | radial vel. | 41.8 | 0.77 | 4956 | [24] | ||
HD 40307 f | 0.0164 | 51.76 | 0.247 | radial vel. | 41.8 | 0.77 | 4956 | [24] | ||
HD 40307 g | 0.0223 | 197.8 | 0.6 | radial vel. | 41.8 | 0.77 | 4956 | [24] | ||
HD 66141 b | 6 | 480.5 | 1.2 | radial vel. | 261.1 | 1.1 | 4323 | [25] | ||
HD 77338b | 0.05 | 5.7361 | 0.0614 | radial vel. | 134.6 | 0.93 | 5370 | [26] | ||
HD 79498 b | 1.34 | 1807 | 2.98 | radial vel. | 159.89 | 1.08 | 5748 | [27] | ||
HD 98649 b | 6.8 | 4951 | 5.6 | radial vel. | 139.5 | 1 | 5759 | [22] | ||
HD 106515 Ab | 9.61 | 3630 | 4.59 | radial vel. | 118.6 | 0.97 | 5362 | [22] | ||
HD 150706 b | 2.71 | 5894 | 6.7 | radial vel. | 88.8 | 1.17 | 5961 | [21] | ||
HD 159868 c | 0.73 | 352.3 | 1 | radial vel. | 171.9 | 1.09 | 5558 | [19] | ||
HD 166724 b | 3.53 | 5144 | 5.42 | radial vel. | 140.2 | 0.81 | 5127 | [22] | ||
HD 197037 b | 0.79 | 1035.7 | 2.07 | radial vel. | 107.1 | 1.063±0.022 | 6137±20 | [27] | ||
HD 207832 b | 0.56 | 161.97 | 0.57 | radial vel. | 180.4 | 0.94 | 5710 | [28] Suspected false positive [29] | ||
HD 207832 c | 0.73 | 1155.7 | 2.112 | radial vel. | 180.4 | 0.94 | 5710 | [28] Suspected false positive [29] | ||
HD 208527 b | 9.9 | 875.5 | 2.1 | radial vel. | 1148.4 | 1.6 | 4035 | [30] | ||
HD 219077 b | 10.39 | 5501 | 6.22 | radial vel. | 95 | 1.05 | 5362 | [22] | ||
HD 219415 b | 1 | 2093.3 | 3.2 | radial vel. | 553.7 | 1 | 4820 | [4] | ||
HD 220074 b | 11.1 | 672.1 | 1.6 | radial vel. | 942.7 | 1.2 | 3935 | [30] | ||
HD 220689 b | 1.06 | 2209 | 3.36 | radial vel. | 147.5 | 1.04 | 5921 | [22] | ||
HD 220773 b | 1.45 | 3724.7 | 4.94 | radial vel. | 159.82 | 1.16 | 5940 | [27] | ||
HD 222155 b | 2.12 | 3999 | 5.14 | radial vel. | 165.3 | 1.21 | 5701 | [21] | ||
HW Virginis b | 14.3 | 4640 | 4.69 | timing | 590 | 0.485 | [31] Likely false positive [32] | |||
Kappa Andromedae b | 13.616 | 55 | 1850 | imaging | 169.7 | 2.6 | 10900 | Has a reddish color, and may be a brown dwarf [33] | ||
KELT-1b | 27.23 | 1.11 | 1.217514 | 0.02466 | 2423 | transit | 850 | 1.32 | 6518 | [34] |
KELT-2Ab | 1.522 | 1.286 | 4.1137912 | 0.05496 | transit | 405.2 | 1.31 | 6151 | [35] | |
Kepler-30b | 0.036 | 0.348 | 29.33434 | 0.18 | transit | 4600 | 0.99 | 5498 | [36] | |
Kepler-30c | 2.01 | 1.097 | 60.323105 | 0.3 | transit | 4600 | 0.99 | 5498 | [36] | |
Kepler-30d | 0.073 | 0.785 | 143.34394 | 0.5 | transit | 4600 | 0.99 | 5498 | [36] | |
Kepler-32d | 0.241 | 22.7802 | 0.13 | transit | 990 | 0.58 | 3900 | [36] | ||
Kepler-32e | 0.134 | 2.896 | 0.033 | transit | 990 | 0.58 | 3900 | Weak evidence [36] | ||
Kepler-32f | 0.073 | 0.74296 | 0.013 | transit | 990 | 0.58 | 3900 | Weak evidence [36] | ||
Kepler-33f | 0.03036 | 0.398 | 41.02902 | 0.2535 | transit | 4086 | 1.29 | 5904 | [37] | |
Kepler-34b | 0.22 | 0.764 | 288.822 | 1.0896 | transit | 4889 | 1.05 | 5913 | [38] | |
Kepler-35b | 0.127 | 0.728 | 131.458 | 0.60347 | transit | 5365 | 0.89 | 5606 | [38] | |
Kepler-36b | 0.014 | 0.133 | 13.83989 | 0.1153 | transit | 1500 | 1.07 | 5911 | [39] | |
Kepler-36c | 0.025 | 0.328 | 16.23855 | 0.1283 | transit | 1500 | 1.07 | 5911 | [39] | |
Kepler-38b | 0.384 | 0.384 | 105.599 | 0.4632 | transit | 2000 | 0.94 | 5623 | [40] | |
Kepler-46b | 6 | 0.808 | 33.60134 | 0.1968 | transit | 2790 | 0.9 | 5309 | [41] | |
Kepler-46c | 0.376 | 57.011 | 0.2799 | timing | 2790 | 0.9 | 5309 | [41] | ||
Kepler-47b | 2 | 0.27 | 49.532 | 0.2962 | transit | 4900 | 1.05 | 5636 | [42] | |
Kepler-47c | 28 | 0.411 | 303.137 | 0.991 | transit | 4900 | 1.05 | 5636 | [42] | |
Kepler-48b | 0.0124 | 0.168 | 4.778 | transit | 1009±5 | 0.88 | 5194 | [43] [44] | ||
Kepler-48c | 0.04597 | 0.242 | 9.67395 | transit | 1009±5 | 0.88 | 5194 | [43] [44] | ||
Kepler-49b | 0.98 | 0.243 | 7.2037945 | transit | 1024±8 | 0.55 | 4252 | [43] [44] | ||
Kepler-49c | 0.72 | 0.227 | 10.9129343 | transit | 1024±8 | 0.55 | 4252 | [43] [44] | ||
Kepler-50b | 0.153 | 7.81254 | 0.077 | transit | 821±6 | 1.24 | 6225 | [44] | ||
Kepler-50c | 0.194 | 9.37647 | 0.087 | transit | 821±6 | 1.24 | 6225 | [44] | ||
Kepler-51b | 0.007 | 0.633 | 45.154 | 0.2514 | 543 | transit | 2610±50 | 1.04 | 6018 | [44] |
Kepler-51c | 0.013 | 0.803 | 85.312 | 0.384 | 439 | transit | 2610±50 | 1.04 | 6018 | [44] |
Kepler-52b | 8.7 | 0.187 | 7.8773565 | transit | 1058±7 | 0.54 | 4263 | [44] | ||
Kepler-52c | 10.41 | 0.164 | 16.3850021 | transit | 1058±7 | 0.54 | 4263 | [44] | ||
Kepler-53b | 18.41 | 0.258 | 18.6489525 | transit | 4600±200 | 0.98 | 5858 | [43] [44] | ||
Kepler-53c | 15.74 | 0.283 | 38.5583038 | transit | 4600±200 | 0.98 | 5858 | [43] [44] | ||
Kepler-54b | 0.92 | 0.187 | 8.0109434 | transit | 893±9 | 0.51 | 4252 | [44] | ||
Kepler-54c | 0.37 | 0.11 | 12.0717249 | transit | 893±9 | 0.51 | 4252 | [44] | ||
Kepler-55b | 1.49 | 0.217 | 27.9481449 | transit | 1920±30 | 0.62 | 4503 | [44] | ||
Kepler-55c | 1.11 | 0.197 | 42.1516418 | transit | 1920±30 | 0.62 | 4503 | [44] | ||
Kepler-56b | 0.07 | 0.581 | 10.5016 | 0.1028 | transit | 3060±80 | 1.32 | 4840 | [44] | |
Kepler-56c | 0.57 | 0.874 | 21.40239 | 0.1652 | transit | 3060±80 | 1.32 | 4840 | [44] | |
Kepler-57b | 18.86 | 0.195 | 5.7293196 | 0.057 | transit | 3140±30 | 0.83 | 5145 | [43] [44] | |
Kepler-57c | 6.95 | 0.138 | 11.6092567 | 0.092 | 631 | transit | 3140±30 | 0.83 | 5145 | [43] [44] |
Kepler-58b | 1.39 | 0.248 | 10.2184954 | transit | 3250±80 | 0.95 | 6099 | [43] [44] | ||
Kepler-58c | 2.19 | 0.255 | 15.5741568 | transit | 3250±80 | 0.95 | 6099 | [43] [44] | ||
Kepler-59b | 2.05 | 0.098 | 11.8681707 | transit | 3925±75 | 1.04 | 6074 | [44] | ||
Kepler-59c | 1.37 | 0.177 | 17.9801235 | transit | 3925±75 | 1.04 | 6074 | [44] | ||
Kepler-60b | 0.01318 | 0.153 | 7.1334 | transit | 3440±70 | 1.04 | 5905 | [44] | ||
Kepler-60c | 0.01211 | 0.17 | 8.9187 | transit | 3440±70 | 1.04 | 5905 | [44] | ||
Kepler-60d | 0.01309 | 0.178 | 11.8981 | transit | 3440±70 | 1.04 | 5905 | [44] | ||
Kepler-64b | 0.531 | 0.551 | 138.317 | 0.652 | transit | 6200±1000 | 1.53 | 6407 | [45] Quadruple star system | |
Kepler-79b | 0.0343 | 0.31 | 13.4845 | 0.117 | 868 | transit | 3430±60 | 1.17 | 6174 | [43] |
Kepler-79c | 0.019 | 0.332 | 27.4029 | 0.187 | 685 | transit | 3430±60 | 1.17 | 6174 | [43] |
Kepler-80b | 0.0218 | 0.238 | 7.05246 | 0.0648 | transit | 1160 | 0.73 | 4540 | [43] | |
Kepler-80c | 0.02121 | 0.244 | 9.52355 | 0.0792 | transit | 1160 | 0.73 | 4540 | [43] | |
Kepler-81b | 0.216 | 5.955 | 646 | transit | 1147±10 | 0.64 | 4500 | [43] | ||
Kepler-81c | 0.211 | 12.04 | 513 | transit | 1147±10 | 0.64 | 4500 | [43] | ||
Kepler-82b | 0.357 | 26.444 | 581 | transit | 3030±80 | 0.85 | 5428 | [43] | ||
Kepler-82c | 0.477 | 51.538 | 464 | transit | 3030±80 | 0.85 | 5428 | [43] | ||
Kepler-83b | 0.252 | 9.77 | transit | 1320±17 | 0.66 | 4648 | [43] [46] | |||
Kepler-83c | 0.211 | 20.09 | transit | 1320±17 | 0.66 | 4648 | [43] [46] | |||
Kepler-84b | 0.199 | 8.726 | 937 | transit | 4700±500 | 1 | 6031 | [43] [46] | ||
Kepler-84c | 0.211 | 12.883 | 821 | transit | 4700±500 | 1 | 6031 | [43] [46] | ||
Kepler-85b | 0.176 | 8.306 | transit | 2550±50 | 0.92 | 5436 | [43] KOI-2038 [47] | |||
Kepler-85c | 0.194 | 12.513 | transit | 2550±50 | 0.92 | 5436 | [43] KOI-2038 [47] | |||
MOA-2011-BLG-293Lb | 2.4+1.4 −0.9 | 1.0±0.1 | microlensing | 23000±2000 | 0.675±0.525 | [48] | ||||
MOA-2010-BLG-073Lb | 11 | 1.21 | microlensing | 9100 | 0.16 | Possibly brown dwarf [49] | ||||
MOA-2010-BLG-477Lb | 1.4±0.3 | 2.8±0.5 | microlensing | 7500±2000 | 0.53±0.11 | 5950±150 | [50] White dwarf host star [51] | |||
MOA-bin-1Lb | 3.7±2.1 | 8.3+4.5 −2.7 | microlensing | 17000 | 0.75+0.33 −0.41 | [52] | ||||
Mu2 Octantis b | 6.9 | 3638 | 5.02 | radial vel. | 142.1 | 1.29 | 6017 | [22] | ||
Nu Ophiuchi b | 24 | 530.32 | 1.9 | radial vel. | 152.8 | 3.04 | 4928 | Brown dwarf or small star [3] | ||
Nu Ophiuchi c | 27 | 3186 | 6.1 | radial vel. | 152.8 | 3.04 | 4928 | Brown dwarf or small star [3] | ||
OGLE-2012-BLG-0026Lb | 0.145 | 4 | microlensing | 13110 | 1.06 | [53] | ||||
OGLE-2012-BLG-0026Lc | 0.86 | 4.8 | microlensing | 13110 | 1.06 | [53] | ||||
Omicron Coronae Borealis b | 1.5 | 187.83 | 0.83 | radial vel. | 274.1 | 2.13 | 4749 | [3] | ||
Omicron Ursae Majoris b | 4.1 | 1630 | 3.9 | radial vel. | 183.7 | 3.09 | 5242 | [3] | ||
Pr0201 b | 0.54 | 4.4264 | radial vel. | 610 | 1.23 | 6174 | [54] In Beehive Cluster | |||
Pr0211 b | 1.88 | 2.1461 | 0.03176 | radial vel. | 610 | 0.94 | 5300 | [54] Multi-planet system In Beehive Cluster | ||
RR Caeli b | 3.0±0.3 | 1900±40 | 5.2±0.1 | timing | 69.10±0.03 | 0.18+0.44 | 3100+7540 | Circumbinary planet around red and white dwarfs. [55] [56] | ||
Tau Ceti e | 0.0124 | 162.87 | 0.538 | radial vel. | 12 | 0.78 | [57] Potentially habitable exoplanet | |||
Tau Ceti f | 0.0124 | 636.13 | 1.334 | radial vel. | 12 | 0.78 | [57] | |||
WASP-42b | 0.527 | 1.122 | 4.9816819 | 0.0561 | 1021±19 | transit | 520 | 0.95 | 5315 | [58] |
WASP-47b | 1.21 | 1.15 | 4.16071 | 0.052 | 1275 | transit | 650 | 1.11 | 5576 | [59] |
WASP-49b | 0.378 | 1.115 | 2.7817387 | 0.0379 | 1369±39 | transit | 550 | 0.94 | 5600 | [58] |
WASP-52b | 0.46 | 1.27 | 1.7497798 | 0.0272 | 1315±35 | transit | 460 | 0.87 | 5000 | [60] Proper name Göktürk |
WASP-54b | 0.636 | 1.653 | 3.6936411 | 0.04987 | 1742+49 −69 | transit | 650 | 1.21 | 6100 | [61] |
WASP-55b | 0.627 | 1.335 | 4.4656291 | 0.0558 | 1290 | transit | 1100 | 1.16 | 6070 | [59] |
WASP-56b | 0.571 | 1.092 | 4.617101 | 0.05458 | 1200 | transit | 830 | 1.03 | 5600 | [61] |
WASP-57b | 0.644 | 1.05 | 2.83891856 | 0.03769 | 1338±29 | transit | 1480 | 0.89 | 5600 | [61] |
WASP-58b | 0.89 | 1.37 | 5.01718 | 0.0561 | 1270±80 | transit | 980 | 0.94 | 5800 | [60] |
WASP-59b | 0.863 | 0.775 | 7.919585 | 0.0697 | 670±35 | transit | 410 | 0.72 | 4650 | [60] |
WASP-60b | 0.514 | 0.86 | 4.3050011 | 0.0531 | 1479±35 | transit | 1300 | 1.08 | 5900 | [60] Proper name Vlasina |
WASP-61b | 2.06 | 1.24 | 3.8559 | 0.0514 | 1565±35 | transit | 1600 | 1.22 | 6320 | [59] |
WASP-62b | 0.57 | 1.39 | 4.411953 | 0.0567 | 1329.6±44.8 | transit | 520 | 1.25 | 6280 | [59] Proper name Krotoa |
WASP-63b | 0.38 | 1.43 | 4.37809 | 0.0574 | 1536±37 | transit | 1100 | 1.32 | 5570 | [59] |
WASP-64b | 1.271 | 1.271 | 1.5732918 | 0.02648 | 1989+87 −88 | transit | 1100 | 1 | 5400 | [62] Proper name Agouto |
WASP-66b | 2.32 | 1.39 | 4.086052 | 0.0546 | 1790±60 | transit | 1200 | 1.3 | 6580 | [59] |
WASP-67b | 0.42 | 1.4 | 4.61442 | 0.0517 | 1050 | transit | 730 | 0.87 | 5240 | [59] |
WASP-71b | 2.242 | 1.46 | 2.9036747 | 0.04619 | 2016.1+67.0 −52.5 | transit | 1130 | 1.56 | 6059 | [63] Proper name Tanzanite |
WASP-72b | 1.5461 | 1.27 | 2.2167421 | 0.03708 | 2210+120 −130 | transit | 1100 | 1.39 | 6250 | [62] Proper name Cuptor |
WASP-77Ab | 1.76 | 1.21 | 1.3600309 | 0.024 | 1715 | transit | 300 | 1 | 5500 | Orbiting primary star of binary star system [64] |
WASP-78b | 0.89 | 1.7 | 2.17517632 | 0.0362 | 2350 | transit | 1800 | 1.17 | 6100 | [65] |
WASP-79b | 0.9 | 2.09 | 3.6623866 | 0.0535 | 1900±50 | transit | 780 | 1.38 | 6600 | [65] Proper name Pollera |
WISE 1217+1626 B | 22 | 0.934 | 8 | 450 | imaging | 29±3 | 0.03 | 575 | Brown dwarf [66] | |
WTS-1b | 4.01 | 1.49 | 3.352057 | 0.047 | 1500±100 | transit | 8100±1000 | 1.2 | 6250 | [67] |
The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.
WASP-4b is an exoplanet, specifically a hot Jupiter, approximately 891 light-years away in the constellation of Phoenix.
WASP-6b, also named Boinayel, is an exoplanet approximately 650 light years away in the constellation Aquarius. It was discovered in 2008, by the WASP survey, by astronomical transit across its parent star WASP-6. This planet orbits at only 4% of the Earth-Sun distance. The planet has a mass half that of Jupiter, but its insolation has forced a thermal expansion of its radius to greater than that of Jupiter. Thus, this planet is an inflated hot Jupiter. Starspots on the host star WASP-6 helped to refine the measurements of the mass and the radius of the planet.
WASP-7b is an extrasolar planet discovered in 2008. This 5-day period planet is slightly smaller than Jupiter, roughly the same mass and more dense.
WASP-8b is an exoplanet orbiting the star WASP-8A in the constellation of Sculptor. The star is similar to the Sun and forms a binary star with a red dwarf star (WASP-8B) of half the Sun's mass that orbits WASP-8A 4.5 arcseconds away. The system is 294 light-years away and is therefore located closer to Earth than many other star systems that are known to feature planets similar to WASP-8b. The planet and its parent star were discovered in the SuperWASP batch -6b to -15b. On 1 April 2008, Dr. Don Pollacco of Queen's University Belfast announced them at the RAS National Astronomy Meeting.
WASP-11/HAT-P-10 is a binary star. It is a primary main-sequence orange dwarf star. Secondary is M-dwarf with a projected separation of 42 AU. The system is located about 424 light-years away in the constellation Aries.
HAT-P-8 is a magnitude 10 star located 700 light-years away in Pegasus. It is a F-type star about 28% more massive than the Sun. Two red dwarf companions have been detected around HAT-P-8. The first has a spectral type of M5V and has a mass of 0.22 M☉. The second is even less massive, at 0.18 M☉, and its spectral type is M6V.
WASP-17 is an F-type main sequence star approximately 1,310 light-years away in the constellation Scorpius.
WASP-17b is an exoplanet in the constellation Scorpius that is orbiting the star WASP-17. Its discovery was announced on 11 August 2009. It is the first planet discovered to have a retrograde orbit, meaning it orbits in a direction counter to the rotation of its host star. This discovery challenged traditional planetary formation theory. In terms of diameter, WASP-17b is one of the largest exoplanets discovered and at half Jupiter's mass, this made it the most puffy planet known in 2010. On 3 December 2013, scientists working with the Hubble Space Telescope reported detecting water in the exoplanet's atmosphere.
WASP-19, formally named Wattle, is a magnitude 12.3 star about 869 light-years away, located in the Vela constellation of the southern hemisphere. This star has been found to host a transiting hot Jupiter-type planet in tight orbit.
HAT-P-14b, officially named Sissi also known as WASP-27b, is an extrasolar planet located approximately 224.2 ± 0.6 parsecs (731.2 ± 2.0 ly) away in the constellation of Hercules, orbiting the 10th magnitude F-type main-sequence star HAT-P-14. This planet was discovered in 2010 by the HATNet Project using the transit method. It was independently detected by the SuperWASP project.
HAT-P-17 is a K-type main-sequence star about 92.4 parsecs (301 ly) away. It has a mass of about 0.857 ± 0.039 M☉. It is the host of two planets, HAT-P-17b and HAT-P-17c, both discovered in 2010. A search for a binary companion star using adaptive optics at the MMT Observatory was negative. A candidate companion was detected by a spectroscopic search of high-resolution K band infrared spectra taken at the Keck observatory.
HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.
HAT-P-16 is a F-type main-sequence star about 725 light-years away. The star has a concentration of heavy elements slightly higher than solar abundance, and low starspot activity. The survey in 2015 have failed to find any stellar companions to it. The spectral analysis in 2014 have discovered the HAT-P-16 has a carbon to oxygen molar ratio of 0.58±0.08, close to Sun`s value of 0.55.