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Lista de exoplanetas descobertos em 2019

Esta é uma Lista de exoplanetas descobertos em 2019.[1][2]

Para exoplanetas detectados apenas pela velocidade radial, o valor da massa é na verdade um limite inferior. (Consulte a massa mínima para obter mais informações)

Nome Massa (MJ) Raio (RJ) Período (dais) Semieixo maior (AU) Temp. (K)[3] Método de descoberta Distância (ly) Massa da estrela-mãe (M☉) Temperatura da estrela-mãe (K) Observações
7 Canis Majoris c 0.87 996.00 2.153 Vel. radial 64.6 1.34 4826 [4]
Beta Pictoris c 9 1200 2.7 Vel. radial 64.43 1.76 [5]
DS Tucanae Ab 0.509±0.015 8.138268±0.000011 850 Trânsito 143.89±0.22 1.01±0.06 5428±80 [6]
Epsilon Indi Ab 3.25 16510 11.55 64.25 Vel. radial 11.87 0.75 [7]
G 9-40 b 0.1807 5.746007 0.0385 456 Trânsito 91.1 0.290 3348 [8][9]
Gliese 49 b 0.0177+0.0021
−0.0021 		13.8508+0.0053
−0.0051 		0.0905±0.0011 Vel. radial 32.145±0.01 0.515±0.019 3805±51 [10]
Gliese 357 b 0.00579 0.1086 3.93072 0.035 525 Trânsito 30.80 0.342 3505 [11]
Gliese 357 c 0.0107 9.1247 0.061 401.2 Vel. radial 30.80 0.342 3505 [11]
Gliese 357 d 0.019 55.661 0.204 219.6 Vel. radial 30.80 0.342 3505 Exoplaneta potencialmente habitável[11]
Gliese 378 b 0.04097±0.006 3.822±0.001 0.082±0.002 Vel. radial 48.79 0.56±0.01 3879±67 [12]
Gliese 411 b 0.00941±0.00145 12.9532±0.0079 349.83±0.32 Vel. radial 8.284 0.386±0.039 3563±60 [13] Estrela-mãe também conhecida como Lalande 21185
Gliese 685 b 0.028+0.0053
−0.0057 		24.160+0.061
−0.047 		0.1344+0.0052
−0.0051 		Vel. radial 46.7102 0.3816±0.069 0.55±0.06 [14]
Gliese 686 b 0.022±0.003 15.53209+0.00166
−0.00167 		0.091±0.004 379+24
−25 		Vel. radial 26.612±0.008 0.42±0.05 3663±68 [15]
Gliese 3512 b 0.463 203.59 0.3380 Vel. radial 30.95 0.123 3081 [16]
Gliese 4276 b 0.05213+0.00296
−0.00299 		13.352±0.003 0.082±0.002 Vel. radial 69.6±0.1 0.41±0.03 3387±51 Podem ser dois exoplanetas em ressonância orbital 2:1[17]
HAT-P-69b 3.58 1.676 4.7869491 0.06555 1930 Trânsito 1122 1.65 7394 [18]
HAT-P-70b <6.78 1.87 2.74432452 0.04739 4000 Trânsito 1073 1.89 8450 [18][19]
HD 8326 b 0.210±0.062 158.991±1.440 0.533±0.011 Vel. radial 100.2 0.80±0.05 4914+51
−32 		[20]
HD 13724 b 26.77+4.40
−2.20 		14763.405+4901.655
−1599.795 		12.40+2.60
−0.90 		Vel. radial 141.9±0.17 0.76±0.71 5868±27 [21]
HD 15337 b 0.0236+0.0034
−0.0032 		0.146±0.005 4.75615±0.00017 0.0522±0.0012 1001.0±11.5 Trânsito 146.36±0.23 0.90±0.03 5125±50 Estrela-mãe também conhecida como TOI-402[22]
HD 15337 c 0.0255+0.0057
−0.0053 		0.213±0.011 17.1784±0.0016 0.1268±0.0038 642±10 Trânsito 146.36±0.23 0.90±0.03 5125±50 Estrela-mãe também conhecida como TOI-402[22]
HD 21411 b 0.207±0.081 84.288±0.127 0.362±0.007 Vel. radial ±95.11 0.89±0.05 5605+247
−132 		[20]
HD 21749 b 0.073+0.007
−0.006 		0.254+0.023
−0.020 		35.61253+0.00060
−0.00062 		0.1915+0.0058
−0.0063 		422+15
−14 		Trânsito 53.261±0.023 0.73±0.07 4640±100 [23]
HD 21749 c <0.0116 0.0796+0.0057
−0.0052 		7.78993+0.00051
−0.00044 		0.0695+0.0021
−0.0023 		701+25
−23 		Trânsito 53.261±0.023 0.73±0.07 4640±100 [23]
HD 24085 b 0.0371±0.0098 2.0455±0.0002 0.034±0.001 Vel. radial 179.4 1.22±0.07 6034+32
−53 		[20]
HD 25015 b 4.48+0.30
−0.28 		6019.320+679.365
−262.980 		6.19+0.45
−0.23 		Vel. radial 122.2±0.22 0.86±0.05 5160±63 [20]
HD 39855 b 0.027±0.005 3.2498±0.0004 0.041±0.001 Vel. radial 75.93 0.87±0.05 5576+50
−46 		[20]
HD 64114 b 0.0560±0.0110 45.791±0.070 0.246±0.005 Vel. radial 102.9 0.95±0.05 5676+32
−87 		[20]
HD 65216c 1.295±0.062 577.6±1.328 1.301±0.020 Vel. radial 114.7±0.1 0.95±0.01 5718±8 Redescoberto em 2019 após falso positivo em 2013[24]
HD 85628 A b 1.675±0.241 1.515±0.044 2.8240932±0.0000046 0.0474±0.0013 1865±25 Trânsito 560±3 1.75±0.05 7800±200 Estrela-mãe também conhecida como MASCARA-4[25][26][27]
HD 92788 c 3.67+0.30
−0.25 		11611.2975+5055.06
−905.820 		10.50+2.90
−0.55 		Vel. radial 113.1385 1.15±0.07 5744±24 [28]
HD 92987 b 16.88+0.69
−0.65 		10354.8375+551.5275
−270.2850 		9.62+0.36
−0.26 		Vel. radial 142.2±0.22 1.08±0.06 5770±36 [21][29]
HD 97048 b 2.5 130 Imagem direta 603 2.4 10000 Descoberto usando o estudo da cinemática do disco,[30] Não confirmado.
HD 102843 b 0.3584±0.0456 3090.942±295.049 4.074±0.270 Vel. radial 205.05 0.95±0.05 5436+144
−69 		[20]
HD 103949 b 0.0352±0.0072 120.878±0.446 0.439±0.009 Vel. radial 86.50 0.77±0.04 4792+66
−54 		[20]
HD 181234 b 8.37+0.34
−0.36 		7462.0575+80.3550
−76.7025 		12.40+2.60
−0.90 		Vel. radial 155.9±0.42 1.01±0.06 5386±60 [21]
HD 202696 b 1.996+0.220
−0.100 		517.8+8.9
−3.9 		1.566+0.016
−0.007 		Vel. radial 618.3±5.2 1.91+0.09
−0.14 		5040+71
−85 		[31]
HD 202696 c 1.864+0.177
−0.227 		946.6+20.7
−20.9 		2.342+0.034
−0.035 		Vel. radial 618.3±5.2 1.91+0.09
−0.14 		5040+71
−85 		[31]
HD 206255 b 0.108±0.022 96.045±0.317 0.461±0.009 Vel. radial 245.9 1.42±0.08 5635+82
−99 		[20]
HD 210193 b 0.4817±0.0733 649.918±8.599 1.487±0.031 Vel. radial 137.8 1.04±0.06 5790+38
−50 		[20]
HD 211970 b 0.0409±0.0079 25.201±0.025 0.143±0.003 Vel. radial 42.4 0.61±0.04 4127+149
−94 		[20]
HD 213885 b 0.0278+0.0021
−0.0020 		0.1557+0.0045
−0.0046 		1.008035+0.000021
−0.000020 		0.02012+0.00015
−0.00012 		Trânsito 156.45721±0.4566189 1.068+0.020
−0.018 		5978±50 Uma super-Terra em trânsito com um período de 1 dia com uma composição semelhante à da Terra em torno de uma estrela brilhante (V=7.9) revelada por TESS[32]
HD 213885 c 0.06277+0.00434
−0.00428 		4.78503+0.00056
−0.000051 		0.056798+0.00044
−0.00032 		1265.4+7.3
−8.4 		Vel. radial 156.45721±0.4566189 1.068+0.020
−0.018 		5978±50 [32]
HD 221416 b 0.190±0.018 0.836+0.031
−0.028 		14.2767±0.0037 0.1228+0.00025
−0.00026 		Trânsito 310.0931 1.212±0.074 5080±90 Estrela-mãe também conhecida como TOI-197 ou HIP 116158[33]
HD 221420 b 9.70+1.10
−1.00 		22482+4200
−4100 		18.5±2.3 Vel. radial 101.7±0.12 1.67±0.11 5830±44 [29]
HIP 35173 b 0.0400±0.0085 41.516±0.077 0.217±0.004 Vel. radial 108.25 0.79±0.05 4881+55
−81 		[20]
HIP 54373 b 0.02712±0.00579 7.760±0.003 0.063±0.001 Vel. radial 61.09 0.57±0.03 4021+226
−146 		[20]
HIP 54373 c 0.03914±0.00664 15.144±0.008 0.0990±0.0020 Vel. radial 61.09 0.57±0.03 4021+226
−146 		[20]
HIP 71135 b 0.0592±0.0129 87.190±0.381 0.335±0.007 Vel. radial 105.5 0.66±0.04 4146+107
−110 		[20]
HIP 79098 (AB)b 20.5±4.5 345±6 2450±150 Imagem direta 477.2±8.2 3.75±1.25 Anã marrom[34]
HR 858 b 0.1860+0.0061
−0.0057 		3.58599±0.00015 0.0480+0.0010
−0.0011 		1572+22
−19 		Trânsito 104.35 1.145+0.074
−0.080 		6201±50 [35]
HR 858 c 0.1730±0.0062 5.97293+0.00060
−0.00053 		0.0674+0.0014
−0.0016 		1326+18
−16 		Trânsito 104.35 1.145+0.074
−0.080 		6201±50 [35]
HR 858 d 0.1931+0.0077
−0.0074 		11.2300+0.0011
−0.0010 		0.1027+0.0022
−0.0025 		1075+15
−13 		Trânsito 104.35 1.145+0.074
−0.080 		6201±50 [35]
HR 5183 b 3.23 27000 18 171 Vel. radial 102.7 1.07 5794 Exoplaneta encontrado com uma das órbitas mais elípticas em 2019[36]
K2-32e 0.0901+0.0089
−0.008 		4.34882+0.00069
−0.00075 		0.04951±0.00055 Trânsito 516.6±4.2 0.856±0.028 Com um raio quase idêntico ao da Terra, é quase certamente um exoplaneta terrestre[37]
K2-43c 0.216 2.198884 1093.7 Trânsito 598 0.57 3841 [38]
K2-50c 0.089+0.011
−0.01 		3.96151+0.00046
−0.00051 		Trânsito 845.82±10.63 0.61±0.06 [39]
K2-63c 0.35±0.11 25.4556±0.0047 0.189±0.011 Trânsito 524.414±21 1.40±0.25 6771±303 Não confirmado
K2-133e 0.154+0.012
−0.012 		26.5841+0.0018
−0.0017 		0.1346±0.0011 296±10 Trânsito 245.3±0.7 0.46±0.01 3655±80 [40] Estrela-mãe também conhecida como LP 358-499
K2-146c 0.02358 0.195 4.00498 1093.7 Trânsito 259 0.33 3385 [41]
K2-166c 0.109+0.019
−0.015 		3.80464+0.00091
−0.00105 		Trânsito 1568.81+31.64
−29.03 		1.07±0.03 [39]
K2-168c 0.105+0.012
−0.009 		8.0468+0.0024
−0.0025 		Trânsito 800.91±13.67 0.91±0.03 [38][39]
K2-198c 0.1270 3.3596055 1229.9 Trânsito 362 0.80 5213 [38]
K2-198d 0.2175 7.4500177 943.2 Trânsito 362 0.80 5213 [38]
K2-282c 0.132+0.012
−0.009 		0.70531±0.00005 Trânsito 1638.22±25.34 0.94±0.04 5499±109 [39]3.º exoplaneta descoberto em 2020[42]
K2-286b 0.0214±0.0135 0.1873±0.0178 27.359±0.005 0.1768+0.0175
−0.0205 		347+21
−11 		Trânsito 248.9±0.8 0.64±0.02 3926±100 [43]
K2-288Bb 0.17±0.03 31.393463+0.000067
−0.000069 		0.164±0.030 226.36±22.30 Trânsito 214.3±2.8 0.33±0.02 3341±276 [44]
K2-290b 0.0664 0.273±0.014 9.21165+0.00033
−0.00034 		0.0923±0.0066 1230±38 Trânsito 897±12 1.19+0.07
−0.08 		6302±120 [45] Dois planetas em órbita retrógrada[46]
K2-290c 0.774±0.047 1.006±0.050 48.36685+0.00041
−0.00040 		0.0923±0.0066 676±16 Trânsito 897±12 1.19+0.07
−0.08 		6302±120 [45] Dois planetas em órbita retrógrada[46]
K2-291b 0.0204±0.0036 0.1418+0.0085
−0.0064 		2.225177+0.000066
−0.000068 		0.03261±0.00044 Trânsito 295±2 0.93±0.04 5520±60 [47]
K2-293b 0.219+0.031
−0.022 		13.1225+0.0011
−0.0012 		750+170
−50 		Trânsito 1290±22 0.96+0.04
−0.03 		5532±78 [48]
K2-294b 0.148+0.019
−0.017 		2.50387+0.00022
−0.00023 		1425+79
−54 		Trânsito 1230±20 0.99+0.03
−0.03 		5612±50 [48]
K2-296b 0.167+0.018
−0.04 		28.1656+0.0027
−0.0028 		Trânsito 521.78±4.57 0.41+0.11
−0.05 		Estrela-mãe também conhecida como EPIC 201238110[39]
K2-297b 0.062+0.005
−0.004 		2.13174±0.00022 Trânsito 831.31±5.48 0.78+0.09
−0.17 		Estrela-mãe também conhecida como EPIC 201497682[39]
K2-298b 0.098+0.012
−0.011 		4.16959+0.00051
−0.00053 		Trânsito 1441.42±26.65 0.8+0.08
−0.16 		[39]
K2-299b 0.152+0.053
−0.028 		4.50756+0.00062
−0.0006 		Trânsito 1219.21±16.28 0.93+0.08
−0.1 		5724±72 [39]Mais dois exoplanetas no sistema estelar descobertos em 2020[42]
K2-300b 0.09+0.021
−0.012 		2.87814+0.00023
−0.00026 		Trânsito 528.67±5.87 0.22+0.04
−0.06 		[39]
K2-301b 0.145+0.015
−0.017 		5.29711+0.00074
−0.0007 		Trânsito 1491.42±44.98 0.56±0.05 4114±99 [39]
K2-302b 0.08+0.017
−0.018 		2.25372±0.00047 Trânsito 359.49±3.52 0.41+0.1
−0.08 		[39]Mais dois exoplanetas no sistema descobertos em 2020[42]
K2-303b 0.086+0.01
−0.013 		1.58252+0.00017
−0.00018 		Trânsito 1034.57±9.59 0.71+0.09
−0.03 		[39]
K2-304b 0.118+0.007
−0.008 		2.28943±0.00019 Trânsito 1380.78±23.94 0.83+0.09
−0.12 		[39]
K2-305b 0.194+0.06
−0.037 		18.0983+0.006
−0.0058 		Trânsito 2030.88±33.92 1.11+0.14
−0.12 		[39]
K2-306b 0.143+0.012
−0.014 		34.885+0.011
−0.01 		Trânsito 931.54±6.69 0.91+0.04
−0.16 		[39]
K2-307b 0.1+0.011
−0.008 		15.2841+0.0037
−0.0029 		Trânsito 1053.09±20.65 0.98+0.04
−0.03 		6004+77
−78 		[39]Suspeita-se de mais dois exoplanetas no sistema,[49] segundo exoplaneta no sistema confirmado em 2021[50]
K2-308b 0.884±0.087 3.38628±0.00002 Trânsito 1.09±0.09 6100±263 [51]
K2-310b 0.2307±0.0112 13.6030±0.0013 0.0980±0.0040 536±18 Trânsito 1133.22 0.690±0.038 4684±79 [52]
K2-310c 0.2400±0.0130 65.5500±0.0089 0.280±0.006 316±10 Trânsito 1133.22 0.690±0.038 4684±79 [52]
KELT-23Ab 0.938+0.048
−0.044 		1.323±0.025 2.255251+0.000011
−0.000012 		0.03302+0.00068
−0.00064 		1561±20 Trânsito 409.07±1.14 0.94+0.06
−0.05 		5899±49 [53]
KELT-24b 5.18 1.272 5.5514926 0.06969 1459 Trânsito 313.2 1.46 6509
Kepler-47d 0.05984+0.07501
−0.03672 		0.628+0.059
−0.044 		187.366+0.069
−0.051 		0.6992+0.0031
−0.0033 		Trânsito 4900 0.957+0.013
−0.015
Kepler-65e 0.653+0.056
−0.055 		258.8+1.5
−1.3 		0.362±0.007 Vel. radial 999.3±8.8 1.25±0.06 6211±66
Kepler-82f 0.0658±0.0031 75.732±0.012 0.3395±0.0041 Tempo 3026.64 0.91±0.03 5401±108
Kepler-88d 3.15±0.15 1409+14
−13 		2.45±0.02 Vel. radial 1243±7 1.022+0.023
−0.026 		5513±67 [54]
Kepler-411d 0.0478±0.0160 0.2961±0.0093 58.02035±0.00056 0.279±0.004 410±10 Trânsito 500.94±1.57 0.87±0.04 [55]
Kepler-411e 0.0340±0.0035 31.509728±0.000085 0.186±0.003 503±9 Tempo 500.94±1.57 0.87±0.04 [55]
Kepler-448c 22 2500 4.2 Tempo 1318 1.5
Kepler-1659b 0.028±0.001 0.17±0.02 13.608±0.00006 0.11229 Trânsito 3812.7570 1.02
Kepler-1659c 0.0014±0.001 0.17±0.03 20.4415±0.0013 0.1472 Trânsito 3812.7570 1.02
Kepler-1660b 7.693±0.054 237.68977±0.08237 Tempo 4013.68±73.27 1.21 Esta detecção surgiu de uma busca por variações de tempo de eclipse entre os mais de 2.000 binários eclipsantes observados pelo Kepler.
KMT-2016-BLG-0212Lb 18 2.2 Microlente 21000 0.48
KMT-2016-BLG-1107Lb 3.283+3.468
−1.835 		0.342+0.070
−0.085 		Microlente 21700+3090
−4400 		0.087+0.092
−0.049
KMT-2017-BLG-0165Lb 0.11+0.05
−0.04 		3.45+0.98
−0.95 		Microlente 14774.88 0.760+0.340
−0.270 		[56][57]
KMT-2017-BLG-1038Lb 2.0+2.0
−1.1 		1.8+0.6
−0.5 		Microlente 19569.3826 0.37+0.36
−0.20
KMT-2017-BLG-1146Lb 0.710+0.800
−0.420 		1.6±0.6 Microlente 21200.16 0.33+0.36
−0.20
KMT-2018-BLG-1990Lb 0.348 0.763 Microlente 3150 0.09
LHS 3844 b 0.1162±0.0020 0.46292913±0.00000190 0.00622±0.00017 805±20 Trânsito 48.60±0.03 0.15±0.01 3036±77
LP 791-18 b 0.0999 0.9480050 0.009690 650 Trânsito 86.41 0.14 2960 [58]
LP 791-18 c 0.206 4.989963 0.029392 370 Trânsito 86.41 0.14 2960 [58]
L 98-59 b 0.00157+0.00094
−0.00063 		0.071±0.004 2.25314±0.00002 0.0233±0.0017 Trânsito 34.64 0.31±0.01 3367±150 [59]
L 98-59 c 0.00755+0.00566
−0.00252 		0.12+0.007
−0.006 		3.690621+0.000013
−0.000014 		0.0324±0.0023-0.0024 Trânsito 34.64 0.31±0.01 3367±150 [59]
L 98-59 d 0.0107+0.0085
−0.0044 		0.14±0.012 7.45086+0.00004
−0.00005 		0.052±0.004 Trânsito 34.64 0.31±0.01 3367±150 [59]
LSPM J2116+0234 b 0.04185+0.00315
−0.00346 		14.4399+0.0078
−0.0087 		0.0876+0.0022
−0.0021 		Vel. radial 57.53±0.07 0.43±0.03 3475±51
LTT 1445 Ab 0.0069 0.123 5.35882 0.03807 433 Trânsito 22.4 0.26 3337 [60]
MOA-bin-29b 0.600 0.48 Microlente 23200 0.03 [61]
NGTS-5b 0.229±0.037 1.136±0.023 3.3569866±0.0000026 0.0382±0.0013 952±24 Trânsito 309.5±8.5 0.66+0.07
−0.06 		4987±41 [62]
NGTS-6b 1.339 1.326 0.8820590 0.01677 Trânsito 1010 0.77 4730 [63]
NGTS-8b 0.93 1.09 2.49970 0.035 1345 Trânsito 1420 0.89 5241 [64]
NGTS-9b 2.90 1.07 4.43527 0.058 1448 Trânsito 1420 1.34 6330 [64]
NSVS 14256825 b 14.15±0.16 3225±22 3.12±0.07 Tempo 2734.2±137.31 0.42±0.07 40000 Disputado[65]
NY Virginis c 5.54 8799 Tempo 1800 Disputado[66]
OGLE-2015-BLG-1649L 2.54 2.07 Microlente 1380 0.34 [67]
OGLE-2016-BLG-1067Lb 0.43 1.70 Microlente 3730 0.30
OGLE-2018-BLG-0532Lb 0.02062+0.00285
−0.00254 		1.103+0.118
−0.107 		Microlente [68]
OGLE-2018-BLG-0596Lb 0.04383±0.00491 0.97±0.13 Microlente 18400±2400 0.23±0.03 [69]
OGLE-2018-BLG-0740Lb 4.8 5480 6.1 Microlente 10400 1.0 5912 [70]
OGLE-2018-BLG-1011Lb 1.8 6.1 Microlente 23000 0.18 [71]
OGLE-2018-BLG-1011Lc 2.8 0.80 Microlente 23000 0.18

[71]

PDS 70c 8.0±4.0 34.5±2 Imagem direta 369.96±1.7 0.76±0.02 3972±36 [72]
Qatar-8b 0.371±0.062 1.285±0.022 3.71495±0.00100 0.0474±0.0008 1457±14 Trânsito 902.5±11 1.03±0.05 5738±51 [73]
Qatar-9b 1.19±0.16 1.009±0.014 1.540731±0.000038 0.0234±0.0003 1134±9 Trânsito 689.5±5.2 0.72±0.02 4309±31 [73]
Qatar-10b 0.736±0.090 1.543±0.040 1.645321±0.000010 0.0286±0.0006 1955±25 Trânsito 1760±33 1.16±0.07 6124±46 [73]
SDSS J1228+1040 b 0.0009+0.0045
−0.000758 		0.0857±0.00021 0.0034±0.000009 1800 Tempo 413.337977±0.4892346 0.705±0.05 O menor exoplaneta conhecido descoberto[74]
Teegarden b 0.00330+0.00041
−0.00038 		4.9100±0.0014 0.0252+0.0008
−0.0009 		Vel. radial 12.50±0.013 0.09±0.01 2904±51 [75]
Teegarden c 0.00349+0.00050
−0.00047 		11.409±0.009 0.0443+0.0014
−0.0015 		226 Vel. radial 12.50±0.013 0.09±0.01 2904±51 Exoplaneta potencialmente habitável[75]
TOI-125 b 0.0299±0.00277 0.2432±0.00669 4.65382±0.00033 0.05186+0.00086
−0.00077 		1037±11 Trânsito 363.3382±1.435088 0.859+0.044
−0.038 		5320±39 [76][77]
TOI-125 c 0.02086±0.00311 0.24614±0.009 9.15059+0.0007
−0.00082 		0.814±0.0013 827.8±8.6 Trânsito 363.3382±1.435088 0.859+0.044
−0.038 		5320±39 [77][78]
TOI-125 d 0.0428±0.0038 0.2614±0.0152 19.98+0.005
−0.0056 		0.05186+0.00086
−0.00077 		638.1±6.6 Trânsito 363.3382±1.435088 0.859+0.044
−0.038 		5320±39 [77][79]
TOI-150b 1.75+0.14
−0.17 		1.38±0.04 5.857342+0.000065
−0.000066 		0.0583+0.0013
−0.0018 		1493+29
−32 		Trânsito 1095.89±6.52 1.25+0.07
−0.12 		6003+104
−98 		[80]
TOI-163b 1.22 1.489 4.231306 0.0580 1669 Trânsito 1359 1.44 6495 [80]
TOI-172b 5.42+0.22
−0.20 		0.965+0.032
−0.029 		9.47725+0.00064
−0.00079 		0.0914±0.0017 Trânsito 1097.418 1.128+0.065
−0.061 		5645±50 [81]
TOI-216 b 0.059±0.002 0.714+0.268
−0.179 		17.1607 0.1293+0.0067
−0.0051 		628+13
−11 		Trânsito 583±3 0.77 5026±125 Semieixo maior são fortemente variáveis devido à interação do exoplaneta em uma escala de tempo de alguns anos[82][83][84]
TOI-216 c 0.56±0.02 0.902±0.018 34.525528 0.2069+0.0107
−0.0082 		497+10
−8 		Trânsito 583±3 0.77 5026±125 Semieixo maior são fortemente variáveis devido à interação do exoplaneta em uma escala de tempo de alguns anos[82][83][84]
TOI-270b 0.0050 0.1112 3.360080 0.0306 528 Trânsito 73.23 0.40 3386 [85][86]
TOI-270c 0.0193 0.216 5.660172 0.0472 424 Trânsito 73.23 0.40 3386 [85][86]
TOI-270d 0.0150 0.190 11.38014 0.0733 340 Trânsito 73.23 0.40 3386 [85][86]Atmosfera de vapor e hidrogênio[87]
TOI-564b 1.463+0.10
−0.096 		1.02+0.71
−0.29 		1.651144±0.000018 0.02734+0.00061
−0.00053 		1714+20
−21 		Trânsito 643.8±5.9 0.998+0.068
−0.057 		5640+34
−37 		[88]
TOI-905b 0.667+0.042
−0.041 		1.171+0.052
−0.051 		3.739494±0.000038 0.04666+0.00096
−0.0011 		1192+39
−36 		Trânsito 489.9+23.5
−22.5 		0.968+0.061
−0.068 		5570+150
−140 		[88]
V1298 Tauri b 0.911+0.049
−0.053 		24.13861+0.00102
−0.00090 		0.1687+0.0025
−0.0026 		668±22 Trânsito 353.9±2.3 1.10±0.05 4970±120 [89]
V1298 Tauri c 0.499 8.24958 0.0825 845±27 Trânsito 353.9 1.10 4970 [90]
V1298 Tauri d 0.572 12.4032 0.1083 677±22 Trânsito 353.9 1.10 4970 [90]
V1298 Tauri e 0.780 60 0.308 492+66
−104 		Trânsito 353.9 1.10 4970 [90]
WASP-18Ac 0.174±0.039 2.1558 0.035 Tempo 404 1.22 6400 [91]
WASP-126c 0.202±0.077 7.63±0.17 Tempo 763.206±48.9235 1.12 5800 [91]False positive[92]
WASP-169b 0.561 1.304 5.6114118 0.0681 1604 Trânsito 2080 1.34 6110 [93]
WASP-171b 1.084 0.980 3.8186244 0.05040 1642 Trânsito 2530 1.17 5965 [93]
WASP-175b 0.990 1.208 3.0652907 0.04403 1571 Trânsito 2080 1.21 6229 [93]
WASP-177b 0.508±0.038 1.58+0.66
−0.83 		3.071722±0.000001 0.03957±0.00058 1142±32 Trânsito 580.5583 0.876±0.038 5017±70 [94]
WASP-178b 1.66 1.81 3.3448285 0.0558 2470 Trânsito 1360 2.07 9360 [95]
WASP-180Ab 0.9 1.24 3.409264 0.048 Trânsito 830 1.3 6600 [96]
WASP-181b 0.299±0.034 1.184+0.071
−0.059 		4.159±0.0000034 0.00542±0.00069 1186+32
−26 		Trânsito 1444.872 1.04±0.04 5839±70 [94]
WASP-182b 0.148 0.850 3.3769848 0.0451 1479 Trânsito 1080 1.08 5638 [93]
WASP-183b 0.502±0.047 1.47+0.94
−0.33 		4.11177±0.0000051 0.0463±0.00075 1111±30 Trânsito 1069.79292 1.00±0.03 0.784±0.038 [94]
WASP-184b 0.57 1.33 5.18170 0.0627 1480 Trânsito 2090 1.23 6000 [95]
WASP-185b 0.980 1.25 9.38755 0.0904 1160 Trânsito 897 1.12 5900 [95]
WASP-192b 2.30 1.23 2.8786765 0.0408 1620 Trânsito 1610 1.09 5910 [95]
KMT-2016-BLG-1836L b 2.2+1.9
−1.1 		3.5+1.1
−0.9 		Microlente 23157.1+2609.25
−7827.753 		0.49+0.38
−0.25 		[97]
HD 85628 A b 3.1±0.9 1.53+0.07
−0.04 		2.82406±0.00003 0.047±0.004 2100±100 Trânsito 559.47±3.05 1.75±0.05 7800±200 Mascara-4b: estrela gigante A3V e um exoplaneta em órbita retrógrada.[98]
OGLE-2016-BLG-1227 b 0.79+1.3
−0.39 		3.4+2.1
−1 		Microlente 0.1+0.17
−0.05 		[99]
OGLE-2013-BLG-0911L b 9.51+2.72
−1.69 		Microlente 10500+1500
−1100 		0.29+0.07
−0.05 		[100]
L 1159-16 b 0.088+0.060
−0.035 		241.59+4.6
−4.0 		0.403+0.039
−0.047 		Vel. radial 14.584±0.007 0.15 3158 [101][102] Refutado em 202[103]
L 1159-16 c 0.23±0.02 772.05+2.41
−1.84 		0.88±0.02 Vel. radial 14.578±0.005 0.15±0.01 3154±54 [101][102] Confirmado em 2022 como L 1159-16 b[103]
TOI-175b 0.00126+0.00050
−0.00048 		0.0642+0.0046
−0.0035 		2.2531136+0.0000012
−0.0000015 		0.02191+0.00080
−0.00084 		627+33
−36 		Trânsito 34.636±0.010 0.273±0.030 3415±135 [104] Até o momento, é o exoplaneta de menor massa confirmado, ou medido, usando a técnica da velocidade radial.[105] Estrela-mãe também conhecida como L 98-59.[106]

Listas específicas de exoplanetas editar


Referências

  1. ↑ «NASA Exoplanet Archive». exoplanetarchive.ipac.caltech.edu. California Institute of Technology. Consultado em 27 de março de 2018 
  2. ↑ «Extrasolar Planet's Catalogue (sic)». Kyoto University. Consultado em 20 de dezembro de 2019 
  3. ↑ «The Extrasolar Planets Encyclopaedia». Consultado em 20 de janeiro de 2018 
  4. ↑ Luque, R.; Trifonov, T.; Reffert, S.; Quirrenbach, A.; Lee, M. H.; Albrecht, S.; Andersen, M. Fredslund; Antoci, V.; Grundahl, F.; Schwab, C.; Wolthoff, V. (13 de outubro de 2019). «Precise radial velocities of giant stars XIII. A second Jupiter orbiting in 4:3 resonance in the 7 CMa system». Astronomy & Astrophysics. A136. 631 páginas. Bibcode:2019A&A...631A.136L. arXiv:1910.05853 . doi:10.1051/0004-6361/201936464 
  5. ↑ «A second planet in the Beta Pictoris system». Nanowerk. 19 de agosto de 2019. Consultado em 20 de agosto de 2019 
  6. ↑ Benatti, S.; Nardiello, D.; Malavolta, L.; Desidera, S.; Borsato, L.; Nascimbeni, V.; Damasso, M.; D'Orazi, V.; Mesa, D.; Messina, S.; Esposito, M.; Bignamini, A.; Claudi, R.; Covino, E.; Lovis, C.; Sabotta, S. (outubro de 2019). «A possibly inflated planet around the bright young star DS Tucanae A». Astronomy & Astrophysics (em inglês). 630: A81. Bibcode:2019A&A...630A..81B. ISSN 0004-6361. arXiv:1904.01591 . doi:10.1051/0004-6361/201935598 
  7. ↑ Feng, Fabo; Anglada-Escudé, Guillem; Tuomi, Mikko; Jones, Hugh R. A.; Chanamé, Julio; Butler, Paul R.; Janson, Markus (14 de outubro de 2019), «Detection of the nearest Jupiter analog in radial velocity and astrometry data», Monthly Notices of the Royal Astronomical Society, 490 (4): 5002–5016, Bibcode:2019MNRAS.490.5002F, arXiv:1910.06804 , doi:10.1093/mnras/stz2912 
  8. ↑ Stefansson, Gudmundur; et al. (2020), «A Sub-Neptune-sized Planet Transiting the M2.5 Dwarf G 9-40: Validation with the Habitable-zone Planet Finder», The Astronomical Journal, 159 (3): 100, Bibcode:2020AJ....159..100S, arXiv:1912.00291 , doi:10.3847/1538-3881/ab5f15 
  9. ↑ G 9-40 b
  10. ↑ Perger, M.; et al. (abril de 2019). «Gliese 49: Activity evolution and detection of a super-Earth». Astronomy & Astrophysics. 624. 19 páginas. Bibcode:2019A&A...624A.123P. ISSN 0004-6361. arXiv:1903.04808 . doi:10.1051/0004-6361/201935192. A123 
  11. ↑ a b c Jenkins, J. S.; Pozuelos, F. J.; Tuomi, M.; Berdiñas, Z. M.; Díaz, M. R.; Vines, J. I.; Suárez, Juan C.; Peña Rojas, P. A. (2019), «GJ 357: A low-mass planetary system uncovered by precision radial velocities and dynamical simulations», Monthly Notices of the Royal Astronomical Society, 490 (4): 5585–5595, arXiv:1909.00831 , doi:10.1093/mnras/stz2937 
  12. ↑ Hobson, M. J.; et al. (2019), «The SOPHIE search for northern extrasolar planets», Astronomy & Astrophysics, 625: A18, arXiv:1902.05998 , doi:10.1051/0004-6361/201834890 
  13. ↑ Díaz, R. F.; et al. (2019), «The SOPHIE search for northern extrasolar planets», Astronomy & Astrophysics, 625: A17, arXiv:1902.06004 , doi:10.1051/0004-6361/201935019 
  14. ↑ Pinamonti, M.; Sozzetti, A.; Giacobbe, P.; Damasso, M.; Scandariato, G.; Perger, M.; González Hernández, J. I.; Lanza, A. F.; Maldonado, J.; Micela, G.; Suárez Mascareño, A.; Toledo-Padrón, B.; Affer, L.; Benatti, S.; Bignamini, A.; Bonomo, A. S.; Claudi, R.; Cosentino, R.; Desidera, S.; Maggio, A.; Martinez Fiorenzano, A.; Pagano, I.; Piotto, G.; Rainer, M.; Rebolo, R.; Ribas, I. (2019), «The HADES RV programme with HARPS-N at TNG», Astronomy & Astrophysics, 625: A126, arXiv:1903.11853 , doi:10.1051/0004-6361/201834969 
  15. ↑ Affer, L.; Damasso, M.; Micela, G.; Poretti, E.; Scandariato, G.; Maldonado, J.; Lanza, A. F.; Covino, E.; Rubio, A. Garrido (31 de janeiro de 2019). «HADES RV program with HARPS-N at TNG. IX. A super-Earth around the M dwarf Gl686». Astronomy & Astrophysics. 622: A193. Bibcode:2019A&A...622A.193A. ISSN 0004-6361. arXiv:1901.05338 . doi:10.1051/0004-6361/201834868 
  16. ↑ Morales, J. C.; et al. (2019). «A giant exoplanet orbiting a very-low-mass star challenges planet formation models». Science. 365 (6460): 1441–1445. Bibcode:2019Sci...365.1441M. ISSN 0036-8075. PMID 31604272. arXiv:1909.12174 . doi:10.1126/science.aax3198 
  17. ↑ Nagel, E.; Czesla, S.; Schmitt, J. H. M. M.; Dreizler, S.; Anglada-Escudé, G.; Rodríguez, E.; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J.; Caballero, J. A.; Aceituno, J.; Béjar, V. J. S.; Cortés-Contreras, M.; González-Cuesta, L.; Guenther, E. W.; Henning, T.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; López-González, M. J.; Montes, D.; Morales, J. C.; Passegger, V. M.; Rodríguez-López, C.; Schweitzer, A.; Zechmeister, M. (2019), «The CARMENES search for exoplanets around M dwarfs», Astronomy & Astrophysics, 622, pp. A153, arXiv:1901.02367 , doi:10.1051/0004-6361/201834569 
  18. ↑ a b Zhou, G.; et al. (2019), «Two New HATNet Hot Jupiters around a Stars and the First Glimpse at the Occurrence Rate of Hot Jupiters from TESS», The Astronomical Journal, 158 (4): 141, Bibcode:2019AJ....158..141Z, arXiv:1906.00462 , doi:10.3847/1538-3881/ab36b5 
  19. ↑ Bello-Arufe, Aaron; Cabot, Samuel H. C.; Mendonça, João M.; Buchhave, Lars A.; Rathcke, Alexander D. (2022), «Mining the Ultrahot Skies of HAT-P-70b: Detection of a Profusion of Neutral and Ionized Species», The Astronomical Journal, 163 (2): 96, Bibcode:2022AJ....163...96B, arXiv:2112.03292 , doi:10.3847/1538-3881/ac402e 
  20. ↑ a b c d e f g h i j k l m n o Feng, Fabo; Crane, Jeffrey D.; Wang, Sharon Xuesong; Teske, Johanna K.; Shectman, Stephen A.; Díaz, Matías R.; Thompson, Ian B.; Jones, Hugh R. A.; Butler, R. Paul (2019), «Search for Nearby Earth Analogs. I. 15 Planet Candidates Found in PFS Data», The Astrophysical Journal Supplement Series, 242 (2), p. 25, Bibcode:2019ApJS..242...25F, arXiv:1904.08567 , doi:10.3847/1538-4365/ab1b16 
  21. ↑ a b c Rickman, E. L.; et al. (2019), «The CORALIE survey for southern extrasolar planets», Astronomy & Astrophysics, 625, pp. A71, arXiv:1904.01573 , doi:10.1051/0004-6361/201935356 
  22. ↑ a b Dumusque, Xavier; et al. (2019), «Hot, rocky and warm, puffy super-Earths orbiting TOI-402 (HD 15337)», Astronomy & Astrophysics, 627, pp. A43, Bibcode:2019A&A...627A..43D, arXiv:1903.05419 , doi:10.1051/0004-6361/201935457 
  23. ↑ a b Dragomir, Diana; et al. (2019), «TESS Delivers Its First Earth-sized Planet and a Warm Sub-Neptune», The Astrophysical Journal, 875 (2): L7, Bibcode:2019ApJ...875L...7D, arXiv:1901.00051 , doi:10.3847/2041-8213/ab12ed 
  24. ↑ Wittenmyer, Robert A.; et al. (2019). «Truly eccentric – I. Revisiting eight single-eccentric planetary systems». Monthly Notices of the Royal Astronomical Society. 484 (4): 5859–5867. Bibcode:2019MNRAS.484.5859W. arXiv:1901.08471 . doi:10.1093/mnras/stz290 
  25. ↑ Dorval, P.; Talens, G. J. J.; Otten, G. P. P. L.; Brahm, R.; Jordán, A.; Torres, P.; Vanzi, L.; Zapata, A.; Henry, T.; Paredes, L.; Jao, W. C.; James, H.; Hinojosa, R.; Bakos, G. A.; Csubry, Z.; Bhatti, W.; Suc, V.; Osip, D.; Mamajek, E. E.; Mellon, S. N.; Wyttenbach, A.; Stuik, R.; Kenworthy, M.; Bailey, J.; Ireland, M.; Crawford, S.; Lomberg, B.; Kuhn, R.; Snellen, I. (2020), «MASCARA-4 b/B Ring-1 b: A retrograde hot Jupiter around a bright A-type star», Astronomy & Astrophysics, 635: A60, Bibcode:2020A&A...635A..60D, arXiv:1904.02733 , doi:10.1051/0004-6361/201935611 
  26. ↑ Ahlers, John P.; Kruse, Ethan; Colón, Knicole D.; Dorval, Patrick; Talens, Geert Jan; Snellen, Ignas; Albrecht, Simon; Otten, Gilles; Ricker, George; Vanderspek, Roland; Latham, David; Seager, Sara; Winn, Joshua; Jenkins, Jon M.; Haworth, Kari; Cartwright, Scott; Morris, Robert; Rowden, Pam; Tenenbaum, Peter; Ting, Eric B. (2020), «Gravity-darkening Analysis of the Misaligned Hot Jupiter MASCARA-4 B», The Astrophysical Journal, 888 (2): 63, Bibcode:2020ApJ...888...63A, arXiv:1911.05025 , doi:10.3847/1538-4357/ab59d0 
  27. ↑ Zhang, Yapeng; Snellen, Ignas A. G.; Wyttenbach, Aurèlien; Nielsen, Louise D.; Lendl, Monika; Casasayas-Barris, Núria; Chaverot, Guillaume; Kesseli, Aurora Y.; Lovis, Christophe; Pepe, Francesco A.; Psaridi, Angelica; Seidel, Julia V.; Udry, Stéphane; Ulmer-Moll, Solène (2022), «Transmission spectroscopy of the ultra-hot Jupiter MASCARA-4 B», Astronomy & Astrophysics, 666: A47, arXiv:2208.11427 , doi:10.1051/0004-6361/202244203 
  28. ↑ Rickman, E. L.; et al. (maio de 2019). «The CORALIE survey for southern extrasolar planets. XVIII. Three new massive planets and two low-mass brown dwarfs at greater than 5 AU separation». Astronomy & Astrophysics. 625. 16 páginas. Bibcode:2019A&A...625A..71R. arXiv:1904.01573 . doi:10.1051/0004-6361/201935356. A71 
  29. ↑ a b Kane, Stephen R.; Dalba, Paul A.; Li, Zhexing; Horch, Elliott P.; Hirsch, Lea A.; Horner, Jonathan; Wittenmyer, Robert A.; Howell, Steve B.; Everett, Mark E.; Butler, R. Paul; Tinney, Christopher G.; Carter, Brad D.; Wright, Duncan J.; Jones, Hugh R. A.; Bailey, Jeremy; o'Toole, Simon J. (2019), «Detection of Planetary and Stellar Companions to Neighboring Stars via a Combination of Radial Velocity and Direct Imaging Techniques», The Astronomical Journal, 157 (6), p. 252, Bibcode:2019AJ....157..252K, arXiv:1904.12931 , doi:10.3847/1538-3881/ab1ddf 
  30. ↑ Pinte, C.; Van Der Plas, G.; Ménard, F.; Price, D. J.; Christiaens, V.; Hill, T.; Mentiplay, D.; Ginski, C.; Choquet, E.; Boehler, Y.; Duchêne, G.; Perez, S.; Casassus, S. (2023), «Kinematic detection of a planet carving a gap in a protoplanetary disk», Nature Astronomy, 3 (12), pp. 1109–1114, arXiv:1907.02538 , doi:10.1038/s41550-019-0852-6 
  31. ↑ a b Trifonov, Trifon; Stock, Stephan; Henning, Thomas; Reffert, Sabine; Kürster, Martin; Lee, Man Hoi; Bitsch, Bertram; Butler, R. Paul; Vogt, Steven S. (2019), «Two Jovian Planets around the Giant Star HD 202696: A Growing Population of Packed Massive Planetary Pairs around Massive Stars?», The Astronomical Journal, 157 (3): 93, Bibcode:2019AJ....157...93T, arXiv:1901.01935 , doi:10.3847/1538-3881/aafa11 
  32. ↑ a b Espinoza, Néstor; et al. (2019), «HD 213885b: A transiting 1-d-period super-Earth with an Earth-like composition around a bright (V = 7.9) star unveiled by TESS», Monthly Notices of the Royal Astronomical Society, 491 (2), pp. 2982–2999, arXiv:1903.07694 , doi:10.1093/mnras/stz3150 
  33. ↑ Huber, Daniel; et al. (2019), «A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered byTESS», The Astronomical Journal, 157 (6), p. 245, Bibcode:2019AJ....157..245H, arXiv:1901.01643 , doi:10.3847/1538-3881/ab1488 
  34. ↑ Janson, Markus; Asensio-Torres, Ruben; André, Damien; Bonnefoy, Mickaël; Delorme, Philippe; Reffert, Sabine; Desidera, Silvano; Langlois, Maud; Chauvin, Gaël; Gratton, Raffaele; Bohn, Alexander J.; Eriksson, Simon C.; Marleau, Gabriel-Dominique; Mamajek, Eric E.; Vigan, Arthur; Carson, Joseph C. (2019), «The B-Star Exoplanet Abundance Study: A co-moving 16–25 MJup companion to the young binary system HIP 79098», Astronomy & Astrophysics, 626, pp. A99, Bibcode:2019A&A...626A..99J, arXiv:1906.02787 , doi:10.1051/0004-6361/201935687 
  35. ↑ a b c Vanderburg, Andrew; et al. (2019). «TESS Spots a Compact System of Super-Earths around the Naked-Eye Star HR 858». The Astrophysical Journal. 881 (1): L19. Bibcode:2019ApJ...881L..19V. arXiv:1905.05193 . doi:10.3847/2041-8213/ab322d 
  36. ↑ Blunt, Sarah; Endl, Michael; Weiss, Lauren M.; Cochran, William D.; Howard, Andrew W.; MacQueen, Phillip J.; et al. (agosto 2019). «Radial Velocity Discovery of an Eccentric Jovian World Orbiting at 18 au». The Astronomical Journal. 158 (5): 181. Bibcode:2019AJ....158..181B. arXiv:1908.09925 . doi:10.3847/1538-3881/ab3e63 
  37. ↑ Heller, René; Rodenbeck, Kai; Hippke, Michael (2019), «Transit least-squares survey», Astronomy & Astrophysics, 625, pp. A31, arXiv:1904.00651 , doi:10.1051/0004-6361/201935276 
  38. ↑ a b c d Hedges, Christina; Saunders, Nicholas; Barentsen, Geert; Coughlin, Jeffrey L.; De Miranda Cardoso, Josè Vinícius; Kostov, Veselin B.; Dotson, Jessie; Cody, Ann Marie (2019), «Four Small Planets Buried in K2 Systems: What Can We Learn for TESS?», The Astrophysical Journal, 880 (1), pp. L5, Bibcode:2019ApJ...880L...5H, arXiv:1907.08244 , doi:10.3847/2041-8213/ab2a74 
  39. ↑ a b c d e f g h i j k l m n o p Heller, René; Hippke, Michael; Rodenbeck, Kai (2019), «Transit least-squares survey», Astronomy & Astrophysics, 627, pp. A66, arXiv:1905.09038 , doi:10.1051/0004-6361/201935600 
  40. ↑ Wells, R.; Poppenhaeger, K.; Watson, C. A. (2019), «Validation of a temperate fourth planet in the K2-133 multiplanet system», Monthly Notices of the Royal Astronomical Society, 487 (2): 1865–1873, arXiv:1905.05206 , doi:10.1093/mnras/stz1334 
  41. ↑ Hamann, Aaron; Montet, Benjamin T.; Fabrycky, Daniel C.; Agol, Eric; Kruse, Ethan (2019), «K2-146: Discovery of Planet c, Precise Masses from Transit Timing, and Observed Precession», The Astronomical Journal, 158 (3), p. 133, Bibcode:2019AJ....158..133H, arXiv:1907.10620 , doi:10.3847/1538-3881/ab32e3 
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  100. ↑ «The Extrasolar Planet Encyclopaedia — OGLE-2013-BLG-0911L b». exoplanet.eu 
  101. ↑ a b Barnes, J. R.; et al. (11 de junho de 2019), Frequency of planets orbiting M dwarfs in the Solar neighbourhood (em inglês), Bibcode:2019arXiv190604644T, arXiv:1906.04644v1 . 
  102. ↑ a b Feng, Fabo; Shectman, Stephen A.; Clement, Matthew S.; Vogt, Steven S.; Tuomi, Mikko; Teske, Johanna K.; Burt, Jennifer; Crane, Jeffrey D.; Holden, Bradford; Sharon Xuesong Wang; Thompson, Ian B.; Diaz, Matias R.; Paul Butler, R. (2020), «Search for Nearby Earth Analogs. III. Detection of ten new planets, three planet candidates, and confirmation of three planets around eleven nearby M dwarfs», The Astrophysical Journal Supplement Series, 250 (2): 29, Bibcode:2020ApJS..250...29F, arXiv:2008.07998 , doi:10.3847/1538-4365/abb139 
  103. ↑ a b Quirrenbach, A.; Passegger, V. M.; Trifonov, T.; Amado, P. J.; Caballero, J. A.; Reiners, A.; Ribas, I.; Aceituno, J.; Béjar, V. J. S.; Chaturvedi, P.; González-Cuesta, L.; Henning, T.; Herrero, E.; Kaminski, A.; Kürster, M.; Lalitha, S.; Lodieu, N.; López-González, M. J.; Montes, D.; Pallé, E.; Perger, M.; Pollacco, D.; Reffert, S.; Rodríguez, E.; López, C. Rodríguez; Shan, Y.; Tal-Or, L.; Osorio, M. R. Zapatero; Zechmeister, M. (2022), «The CARMENES search for exoplanets around M dwarfs», Astronomy & Astrophysics, 663: A48, arXiv:2203.16504 , doi:10.1051/0004-6361/202142915 
  104. ↑ Kostov, Veselin B.; Schlieder, Joshua E.; et al. (2019). «The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf». The Astronomical Journal. 158 (1). 32 páginas. Bibcode:2019AJ....158...32K. ISSN 1538-3881. arXiv:1903.08017 . doi:10.3847/1538-3881/ab2459. hdl:1721.1/124742  
  105. ↑ Demangeon, O. D. S.; Zapatero Osorio, M. R.; Alibert, Y.; Barros, S. C. C.; Adibekyan, V.; Tabernero, H. M.; Antoniadis-Karnavas, A.; Camacho, J. D.; al, et (2021). «Warm terrestrial planet with half the mass of Venus transiting a nearby star» (PDF). Astronomy & Astrophysics. 653: A41. Bibcode:2021A&A...653A..41D. arXiv:2108.03323 . doi:10.1051/0004-6361/202140728 
  106. ↑ «Planet L 98-59 b». exoplanet.eu. Consultado em 6 de agosto de 2021 
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