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List of stars in Taurus
List of stars in Taurus
List of stars in Taurus
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These are the stars in the constellation Taurus, sorted by decreasing brightness:

Name B F G. Var HD HIP RA Dec vis.
mag. 		abs.
mag. 		Dist. (ly) Sp. class Notes
Aldebaran α 87 29139 21421 04h 35m 55.20s +16° 30′ 35.1″ 0.87 −0.63 65 K5III Cor Tauri, Parilicium; 13th-brightest star, variable
β Tau β 112 35497 25428 05h 26m 17.50s +28° 36′ 28.3″ 1.65 −1.37 131 B7III El Nath, Alnath, Nath
Alcyone A η 25 23630 17702 03h 47m 29.06s +24° 06′ 18.9″ 2.85 −2.41 368 B7III member of the Pleiades star cluster, binary star
ζ Tau ζ 123 37202 26451 05h 37m 38.68s +21° 08′ 33.3″ 2.97 −2.56 417 B4IIIp Tianguan; γ Cas variable
θ2 Tau θ2 78 28319 20894 04h 28m 39.67s +15° 52′ 15.4″ 3.40 0.10 149 A7III Chamukuy, member of the Hyades star cluster; δ Sct variable
λ Tau λ 35 25204 18724 04h 00m 40.82s +12° 29′ 25.4″ 3.41 −1.87 370 B3V + A Sadr al Tauri, Pectus Tauri; eclipsing binary; Algol variable
ε Tau ε 74 28305 20889 04h 28m 36.93s +19° 10′ 49.9″ 3.53 0.15 155 K0III Ain, Oculus Borealis; member of the Hyades star cluster; has a planet (b)
ο Tau ο 1 3 21120 15900 03h 24m 48.84s +09° 01′ 44.6″ 3.61 −0.45 211 G8III
Atlas A 27 23850 17847 03h 49m 09.73s +24° 03′ 12.7″ 3.62 −1.72 380 B8III member of the Pleiades star cluster; triple star
γ Tau γ 54 27371 20205 04h 19m 47.53s +15° 37′ 39.7″ 3.65 0.28 154 G8III Hyadum I, Prima Hyadum, Primus Hyadum; member of the Hyades star cluster
Electra 17 23302 17499 03h 44m 52.52s +24° 06′ 48.4″ 3.72 −1.56 370 B6III member of the Pleiades star cluster
ξ Tau ξ 2 4 21364 16083 03h 27m 10.12s +09° 43′ 58.0″ 3.73 −0.44 222 B9Vn Ushakaron; eclipsing binary
δ1 Tau δ1 61 27697 20455 04h 22m 56.03s +17° 32′ 33.3″ 3.77 0.41 153 G8III Hyadum II, Secunda Hyadum, Secundus Hyadum; member of the Hyades star cluster
θ1 Tau θ1 77 28307 20885 04h 28m 34.43s +15° 57′ 44.0″ 3.84 0.42 158 G7III member of the Hyades star cluster
Maia 20 23408 17573 03h 45m 49.59s +24° 22′ 04.3″ 3.87 −1.34 360 B8III member of the Pleiades star cluster
ν Tau ν 38 30 25490 18907 04h 03m 09.38s +05° 59′ 21.5″ 3.91 0.92 129 A1V
5 Tau f 5 21754 16369 03h 30m 52.37s +12° 56′ 12.1″ 4.14 −1.08 360 K0II-III...
Merope 23 V971 23480 17608 03h 46m 19.56s +23° 56′ 54.5″ 4.14 −1.07 359 B6IV V971 Tau; member of the Pleiades star cluster; β Cep variable
κ1 Tau κ1 65 27934 20635 04h 25m 22.10s +22° 17′ 38.3″ 4.21 0.85 153 A7IV-V member of the Hyades star cluster; sextuple star
88 Tau d 88 61 29140 21402 04h 35m 39.23s +10° 09′ 39.3″ 4.25 0.93 150 A5m
μ Tau μ 49 44 26912 19860 04h 15m 32.05s +08° 53′ 32.7″ 4.27 −1.35 435 B3IV
90 Tau c 90 29388 21589 04h 38m 09.40s +12° 30′ 39.1″ 4.27 0.96 150 A6V member of the Hyades star cluster
τ Tau τ 94 29763 21881 04h 42m 14.70s +22° 57′ 25.1″ 4.27 −1.18 400 B3V
υ Tau υ 69 28024 20711 04h 26m 18.39s +22° 48′ 49.3″ 4.28 0.90 155 A8Vn member of the Hyades star cluster; δ Sct variable
10 Tau 10 11 22484 16852 03h 36m 52.52s +00° 24′ 10.2″ 4.29 3.60 45 F9V
Taygeta q 19 23338 17531 03h 45m 12.48s +24° 28′ 02.6″ 4.30 −0.99 373 B6V Taÿgete; member of the Pleiades star cluster
68 Tau δ3 68 V776 27962 20648 04h 25m 29.32s +17° 55′ 40.8″ 4.30 1.02 148 A2IV V776 Tau; member of the Hyades star cluster; α2 CVn variable
119 Tau 119 CE 36389 25945 05h 32m 12.75s +18° 35′ 39.3″ 4.32 −4.53 1918 M2Ib Ruby Star, CE Tau; semiregular variable
37 Tau A1 37 25604 19038 04h 04m 41.66s +22° 04′ 55.4″ 4.36 0.64 181 K0III Yuè (月)[1]
71 Tau 71 V777 28052 20713 04h 26m 20.67s +15° 37′ 06.0″ 4.48 1.08 156 F0V... V777 Tau; member of the Hyades star cluster; spectroscopic binary; δ Sct variable
136 Tau 136 39357 27830 05h 53m 19.64s +27° 36′ 44.2″ 4.56 −1.08 438 A0V
ι Tau ι 102 32301 23497 05h 03m 05.70s +21° 35′ 24.2″ 4.62 1.13 163 A7V member of the Hyades star cluster
ρ Tau ρ 86 28910 21273 04h 33m 50.86s +14° 50′ 40.2″ 4.65 1.30 152 A8V member of the Hyades star cluster; δ Sct variable
σ2 Tau σ2 92 29488 21683 04h 39m 16.45s +15° 55′ 04.9″ 4.67 1.23 159 A5Vn Fùěr (附耳),[2] member of the Hyades star cluster
π Tau π 73 28100 20732 04h 26m 36.38s +14° 42′ 49.9″ 4.69 −1.03 455 G8III
HD 28527 28527 21029 04h 30m 33.57s +16° 11′ 38.7″ 4.78 1.54 145 A6IV member of the Hyades star cluster
64 Tau δ2 64 27819 20542 04h 24m 05.69s +17° 26′ 39.2″ 4.80 1.55 146 A7V member of the Hyades star cluster
139 Tau 139 40111 28237 05h 57m 59.66s +25° 57′ 14.1″ 4.81 −4.24 2103 B1Ib
47 Tau 47 42 26722 19740 04h 13m 56.39s +09° 15′ 50.0″ 4.84 −0.44 371 G5III
126 Tau 126 37711 26777 05h 41m 17.72s +16° 32′ 03.1″ 4.84 −1.96 748 B3IV...
114 Tau o 114 35708 25539 05h 27m 38.08s +21° 56′ 13.1″ 4.88 −1.76 695 B2.5IV
132 Tau 132 38751 27468 05h 49m 00.96s +24° 34′ 03.2″ 4.88 −1.14 522 G8IIIvar
134 Tau 134 38899 27511 05h 49m 32.94s +12° 39′ 04.9″ 4.89 0.29 272 B9IV
104 Tau m 104 32923 23835 05h 07m 26.68s +18° 38′ 42.0″ 4.91 3.91 52 G4V
ω2 Tau ω2 50 27045 19990 04h 17m 15.69s +20° 34′ 43.5″ 4.93 2.64 93 A3m
75 Tau 75 28292 20877 04h 28m 26.37s +16° 21′ 34.7″ 4.96 1.08 194 K2IIIvar
109 Tau n 109 34559 24822 05h 19m 16.59s +22° 05′ 48.1″ 4.96 0.96 206 G8III
φ Tau φ 52 27382 20250 04h 20m 21.23s +27° 21′ 03.4″ 4.97 −0.13 342 K1III
111 Tau 111 V1119 35296 25278 05h 24m 25.31s +17° 23′ 00.8″ 5.00 4.17 48 F8V SB V1119 Tau; BY Draconis variable
79 Tau b 79 28355 20901 04h 28m 50.10s +13° 02′ 51.5″ 5.02 1.56 160 A7V member of the Hyades star cluster
Pleione 28 BU 23862 17851 03h 49m 11.20s +24° 08′ 12.6″ 5.05 −0.32 387 B7p BU Tau; member of the Pleiades star cluster; γ Cas variable
30 Tau e 30 23793 17771 03h 48m 16.25s +11° 08′ 36.1″ 5.08 −1.11 565 B3V
σ1 Tau σ1 91 29479 21673 04h 39m 09.20s +15° 48′ 00.1″ 5.08 1.74 152 A4m member of the Hyades star cluster
97 Tau i 97 V480 30780 22565 04h 51m 22.41s +18° 50′ 23.8″ 5.08 1.27 189 A7IV-V V480 Tau; member of the Hyades star cluster; δ Sct variable
66 Tau r 66 50 27820 20522 04h 23m 51.84s +09° 27′ 39.5″ 5.10 −0.32 396 A3V
4 Tau s 4 21686 16322 03h 30m 24.48s +11° 20′ 11.3″ 5.14 −0.39 417 A0Vn
41 Tau 41 GS 25823 19171 04h 06m 36.40s +27° 36′ 00.1″ 5.18 −0.72 494 B9p Si GS Tau; α² CVn variable
125 Tau 125 37438 26640 05h 39m 44.19s +25° 53′ 49.7″ 5.18 −0.73 495 B3IV
ψ Tau ψ 42 25867 19205 04h 07m 00.52s +29° 00′ 04.6″ 5.21 3.01 90 F1V
43 G. Tau 43 26793 19799 04h 14m 36.24s +10° 00′ 41.2″ 5.22 −0.59 474 B9Vn
23985 17954 03h 50m 18.91s +25° 34′ 46.7″ 5.24 1.39 192 A2V
58 Tau 58 V696 27459 20261 04h 20m 36.24s +15° 05′ 43.8″ 5.26 1.89 154 F0V V696 Tau; member of the Hyades star cluster; δ Sct variable
κ2 Tau κ2 67 27946 20641 04h 25m 24.94s +22° 12′ 00.4″ 5.27 2.05 144 A7V member of the Hyades star cluster
l Tau l 106 32977 23871 05h 07m 48.43s +20° 25′ 06.4″ 5.28 1.65 173 A5V
133 Tau 133 38622 27364 05h 47m 42.90s +13° 53′ 58.7″ 5.28 −1.67 799 B2IV-V
46 Tau 46 41 26690 19719 04h 13m 33.11s +07° 42′ 57.7″ 5.29 2.45 121 F3V... Solar sibling candidate
40 Tau 40 32 V1133 25558 18957 04h 03m 44.60s +05° 26′ 08.3″ 5.32 −2.21 1045 B3V V1133 Tau
49 Eri (49) 62 29335 21515 04h 37m 13.68s +00° 59′ 54.0″ 5.32 −1.75 847 B7V
29 Tau u 29 17 23466 17563 03h 45m 40.43s +06° 03′ 00.1″ 5.34 −0.94 588 B3V
56 Tau 56 V724 27309 20186 04h 19m 36.69s +21° 46′ 24.9″ 5.34 0.41 316 A0p Si V724 Tau; α² CVn variable
34 G. Tau 34 25621 18993 04h 04m 09.79s +02° 49′ 38.1″ 5.36 2.66 113 F6IV
121 Tau 121 36819 26248 05h 35m 27.12s +24° 02′ 22.7″ 5.37 −0.95 599 B2.5IV
χ Tau χ 59 27638 20430 04h 22m 34.93s +25° 37′ 45.7″ 5.38 0.81 267 B9V
63 G. Tau 63 29499 21670 04h 39m 06.10s +07° 52′ 15.6″ 5.38 1.82 168 A5m member of the Hyades star cluster
44 Tau p 44 IM 26322 19513 04h 10m 49.88s +26° 28′ 51.7″ 5.39 1.51 195 F2IV-V IM Tau; δ Sct variable
83 Tau 83 28556 21036 04h 30m 37.30s +13° 43′ 28.0″ 5.40 2.10 149 F0V member of the Hyades star cluster
115 Tau 115 35671 25499 05h 27m 10.09s +17° 57′ 44.2″ 5.40 −1.16 668 B5V
23753 17776 03h 48m 20.80s +23° 25′ 16.9″ 5.44 0.36 338 B8V
Celaeno 16 23288 17489 03h 44m 48.20s +24° 17′ 22.5″ 5.45 0.40 334 B7IV member of the Pleiades star cluster
33 G. Tau 33 25570 18975 04h 03m 56.51s +08° 11′ 49.9″ 5.45 2.67 117 F2V member of the Hyades star cluster
93 Tau 93 29589 21735 04h 40m 03.42s +12° 11′ 51.5″ 5.45 0.33 345 B8IV
36 Tau 36 25555 19009 04h 04m 21.67s +24° 06′ 21.7″ 5.46 −1.87 953 G0III...
81 Tau 81 28546 21039 04h 30m 38.83s +15° 41′ 31.0″ 5.47 2.24 145 Am member of the Pleiades star cluster
118 Tau 118 35943 25695 05h 29m 16.49s +25° 09′ 01.1″ 5.47 −0.15 434 B9Vn
130 Tau 130 38558 27338 05h 47m 26.20s +17° 43′ 44.9″ 5.47 −2.48 1268 F0III
53 Tau 53 V1024 27295 20171 04h 19m 26.08s +21° 08′ 32.7″ 5.50 0.93 267 B9IV V1024 Tau; α² CVn variable; on 29 May 2032, it will be occulted by Venus but in daylight and with Venus too close to the Sun[3]: 166 
103 Tau 103 32990 23900 05h 08m 06.62s +24° 15′ 54.7″ 5.50 −4.48 3228 B2V...
36408 25950 05h 32m 14.14s +17° 03′ 29.4″ 5.50 −2.17 1116 B7III
ω1 Tau ω1 43 26162 19388 04h 09m 09.90s +19° 36′ 33.5″ 5.51 0.76 291 K2III
31539 23043 04h 57m 22.35s +17° 09′ 13.3″ 5.51 −0.29 472 K1III
116 Tau 116 35770 25555 05h 27m 45.61s +15° 52′ 26.8″ 5.52 −0.67 565 B9.5Vn
72 Tau 72 28149 20789 04h 27m 17.45s +22° 59′ 46.9″ 5.53 0.01 415 B7V
44 Eri (44) 54 28375 20884 04h 28m 32.11s +01° 22′ 51.1″ 5.53 0.17 385 B3V
122 Tau 122 37147 26382 05h 37m 03.71s +17° 02′ 25.5″ 5.53 1.87 176 F0V member of the Hyades star cluster
135 Tau 135 39019 27581 05h 50m 28.90s +14° 18′ 20.5″ 5.54 0.63 312 G9III:
12 Tau 12 13 22796 17103 03h 39m 51.14s +03° 03′ 24.6″ 5.55 0.10 400 G6III:
57 Tau h 57 V483 27397 20219 04h 19m 57.63s +14° 02′ 06.9″ 5.58 2.32 146 F3V... V483 Tau; member of the Hyades star cluster; δ Sct variable
80 Tau 80 28485 20995 04h 30m 08.53s +15° 38′ 16.4″ 5.58 2.38 142 F0V... member of the Hyades star cluster
39004 27629 05h 50m 58.11s +27° 58′ 04.2″ 5.60 0.29 376 G7III:
137 Tau 137 V809 39317 27743 05h 52m 22.30s +14° 10′ 18.5″ 5.60 −0.39 515 B9p... V809 Tau; α² CVn variable
32 Tau 32 24740 18471 03h 56m 52.03s +22° 28′ 41.7″ 5.62 2.36 146 F2IV
51 Tau 51 27176 20087 04h 18m 23.14s +21° 34′ 45.8″ 5.64 1.95 179 F0V member of the Hyades star cluster
63 Tau 63 27749 20484 04h 23m 25.00s +16° 46′ 38.4″ 5.64 2.27 154 A1m member of the Hyades star cluster
18 Tau 18 23324 17527 03h 45m 09.73s +24° 50′ 21.7″ 5.66 0.40 368 B8V
31 Tau 31 21 24263 18089 03h 52m 00.22s +06° 32′ 05.7″ 5.66 −1.01 704 B5V
26 G. Tau 26 25330 18805 04h 01m 46.13s +09° 59′ 52.9″ 5.67 −0.52 565 B5V
60 G. Tau 60 28978 21295 04h 34m 08.28s +05° 34′ 07.1″ 5.67 0.18 408 A2Vs
120 Tau 120 V960 36576 26064 05h 33m 31.63s +18° 32′ 24.8″ 5.67 −3.13 1874 B2IV-Ve V960 Tau; Be star
13 Tau 13 23016 17309 03h 42m 18.94s +19° 42′ 01.0″ 5.68 0.19 409 B9Vn
45 Tau 45 38 26462 19554 04h 11m 20.20s +05° 31′ 22.9″ 5.71 2.78 126 F4V member of the Hyades star cluster
60 Tau 60 V775 27628 20400 04h 22m 03.45s +14° 04′ 38.1″ 5.72 2.42 149 A3m V775 Tau; member of the Hyades star cluster; spectroscopic binary; δ Sct variable
28226 20842 04h 28m 00.72s +21° 37′ 12.0″ 5.72 2.32 156 Am member of the Hyades star cluster
131 Tau 131 38545 27316 05h 47m 13.15s +14° 29′ 18.3″ 5.72 0.16 422 A3Vn
29646 21819 04h 41m 19.74s +28° 36′ 54.2″ 5.73 0.67 335 A2V
6 Tau t 6 8 21933 16511 03h 32m 35.93s +09° 22′ 24.8″ 5.76 0.57 355 B9IV
Sterope I 21 23432 17579 03h 45m 54.46s +24° 33′ 16.6″ 5.76 0.39 387 B8V Asterope; member of the Pleiades star cluster
49 G. Tau 49 27497 20268 04h 20m 41.25s +06° 07′ 51.3″ 5.76 0.17 428 G8III-IV
117 Tau 117 35802 25583 05h 28m 01.60s +17° 14′ 21.3″ 5.77 −0.90 704 M1III
89 Tau 89 29375 21588 04h 38m 09.38s +16° 02′ 00.2″ 5.78 2.49 148 F0V member of the Hyades star cluster
99 Tau 99 31553 23068 04h 57m 48.65s +23° 56′ 54.9″ 5.79 −0.01 471 G8III:
98 Tau k 98 31592 23088 04h 58m 09.38s +25° 03′ 01.9″ 5.79 1.00 296 A0V
V711 Tau 10 V711 22468 16846 03h 36m 47.31s +00° 35′ 17.4″ 5.82 3.51 94 G5IV/V +K1IV RS CVn variable
37098 26396 05h 37m 08.84s +26° 55′ 28.3″ 5.83 0.00 477 B9IV-V
105 Tau 105 V1155 32991 23883 05h 07m 55.43s +21° 42′ 17.4″ 5.84 −1.66 1032 B2Ve V1155 Tau; Be star; on 7 April 2032, it will be occulted by Saturn over New Zealand, the Pacific Ocean, the NW half of North America, Greenland[3]: 165 
HU Tau HU 29365 21604 04h 38m 15.84s +20° 41′ 05.1″ 5.85 0.63 361 B8V Algol variable
28217 20804 04h 27m 28.77s +11° 12′ 44.4″ 5.87 0.00 487 B8IV
28929 21323 04h 34m 37.99s +28° 57′ 40.3″ 5.88 0.11 466 B9p...
25202 18735 04h 00m 48.69s +18° 11′ 38.6″ 5.89 2.60 148 F4V... member of the Hyades star cluster
26038 19284 04h 07m 59.41s +17° 20′ 23.7″ 5.89 0.77 345 K5III
39 Tau A2 39 25680 19076 04h 05m 20.15s +22° 00′ 33.2″ 5.90 4.78 55 G5V
76 Tau 76 28294 20873 04h 28m 23.34s +14° 44′ 27.7″ 5.90 2.23 177 F0IV member of the Hyades star cluster
18 G. Tau 18 23526 17595 03h 46m 09.36s +06° 48′ 13.2″ 5.91 0.84 337 G9III
27639 20417 04h 22m 22.73s +20° 49′ 17.1″ 5.91 −2.74 1753 M0III
6 G. Tau 6 21755 16358 03h 30m 45.40s +06° 11′ 19.5″ 5.93 −0.07 517 G8III
V1156 Tau V1156 33204 24019 05h 09m 45.06s +28° 01′ 50.2″ 5.93 2.24 178 A5m member of the Hyades star cluster
26171 19376 04h 09m 01.56s +13° 23′ 53.9″ 5.94 0.26 445 B9.5V
7 Tau 7 22091 16664 03h 34m 26.62s +24° 27′ 52.1″ 5.95 −0.06 519 A3V
24357 18170 03h 53m 09.96s +17° 19′ 37.8″ 5.97 2.88 135 F4V member of the Hyades star cluster
27901 20614 04h 24m 57.06s +19° 02′ 31.5″ 5.97 2.52 160 F4V member of the Hyades star cluster
30912 22697 04h 52m 47.09s +27° 53′ 51.3″ 5.97 0.81 352 F2IV
30197 22176 04h 46m 16.78s +18° 44′ 05.5″ 5.99 1.16 302 K4III
V1141 Tau V1141 27742 20493 04h 23m 32.36s +20° 58′ 55.7″ 6.00 0.15 482 B8IV-V
129 Tau 129 38478 27265 05h 46m 45.49s +15° 49′ 21.0″ 6.00 −1.15 879 B8IIIMNp...
85 Tau 85 28677 21137 04h 31m 51.69s +15° 51′ 05.9″ 6.01 2.75 147 F4V... member of the Hyades star cluster
59 G. Tau 59 28930 21269 04h 33m 48.18s +09° 24′ 49.0″ 6.01 0.21 470 G8III
V1116 Tau V1116 29169 21459 04h 36m 29.07s +23° 20′ 27.5″ 6.01 2.78 144 F5IV δ Sct variable; member of the Hyades star cluster
26015 19261 04h 07m 41.91s +15° 09′ 46.2″ 6.02 2.66 153 F3V member of the Hyades star cluster
21051 15850 03h 24m 10.11s +12° 37′ 46.7″ 6.03 0.27 462 K0III-IV
38670 27421 05h 48m 22.36s +20° 52′ 10.3″ 6.03 −0.28 595 B9Vn
39970 28154 05h 56m 56.12s +24° 14′ 58.9″ 6.03 A0Ia
23950 17921 03h 49m 55.06s +22° 14′ 39.3″ 6.05 1.08 321 B8III
33 Tau 33 V817 24769 18485 03h 57m 03.80s +23° 10′ 32.1″ 6.05 −0.01 531 B9.5IV V817 Tau
V1143 Tau 51 V1143 28114 20715 04h 26m 21.10s +08° 35′ 25.0″ 6.06 −0.25 597 B6IV β Cep variable
23258 17453 03h 44m 28.19s +20° 55′ 43.6″ 6.09 1.72 243 A0V
24 G. Tau 24 24817 18481 03h 57m 01.70s +06° 02′ 24.5″ 6.09 1.70 246 A2Vn
26546 19641 04h 12m 31.32s +17° 16′ 39.0″ 6.09 1.38 285 K0III
96 Tau 96 30605 22441 04h 49m 44.08s +15° 54′ 15.3″ 6.09 −2.09 1411 K3III
110 Tau 110 35189 25216 05h 23m 37.72s +16° 41′ 57.7″ 6.09 0.41 445 A2IV
11 Tau 11 22805 17181 03h 40m 46.30s +25° 19′ 46.3″ 6.11 0.09 522 A2IV
27429 20255 04h 20m 25.04s +18° 44′ 33.8″ 6.11 2.73 154 F3:V... member of the Hyades star cluster
14 G. Tau 14 22819 17120 03h 39m 59.55s −01° 07′ 16.4″ 6.12 0.56 421 G5
34579 24820 05h 19m 14.71s +20° 08′ 04.8″ 6.12 0.51 431 G8III+...
14 Tau 14 23183 17408 03h 43m 47.14s +19° 39′ 54.6″ 6.13 0.99 347 G8III
22072 16641 03h 34m 08.32s +17° 50′ 00.9″ 6.14 3.00 138 K1IVe...
V1137 Tau V1137 26571 19672 04h 12m 51.25s +22° 24′ 48.5″ 6.14 −1.36 1032 B9IIIsp... α² CVn variable
53 G. Tau 53 28322 20848 04h 28m 03.62s +01° 51′ 30.9″ 6.14 0.99 349 G9III
27483 20284 04h 20m 52.66s +13° 51′ 52.1″ 6.15 2.84 150 F6V... member of the Hyades star cluster
23923 17900 03h 49m 43.52s +23° 42′ 43.1″ 6.17 0.84 380 B8V
22695 17058 03h 39m 25.73s +16° 32′ 12.4″ 6.18 0.72 403 K0III
95 Tau 95 29859 21961 04h 43m 13.75s +24° 05′ 20.3″ 6.18 2.69 163 F7IV-V
24802 18508 03h 57m 26.39s +24° 27′ 43.0″ 6.19 −1.40 1072 K0
36589 26072 05h 33m 38.84s +20° 28′ 27.2″ 6.19 −0.76 799 B6V
32482 23589 05h 04m 21.58s +21° 16′ 40.8″ 6.20 −0.18 615 K0
34810 24977 05h 20m 56.62s +19° 48′ 51.7″ 6.20 −0.21 625 K0III
29459 21689 04h 39m 23.14s +25° 13′ 05.9″ 6.21 0.97 363 A5Vn
52 G. Tau 52 28191 20771 04h 27m 00.66s +02° 04′ 46.4″ 6.23 0.81 395 K1III
113 Tau 113 35532 25410 05h 26m 05.72s +16° 42′ 00.6″ 6.23 −0.28 655 B2Vn
V731 Tau V731 37967 26964 05h 43m 19.50s +23° 12′ 15.9″ 6.23 −1.41 1098 B2.5Ve γ Cas variable; Be star
40 G. Tau 40 26676 19720 04h 13m 34.55s +10° 12′ 45.1″ 6.24 0.30 502 B8Vn
28867 21251 04h 33m 33.04s +18° 01′ 00.3″ 6.24 0.68 423 B9IVn
26703 19736 04h 13m 49.83s +12° 45′ 13.5″ 6.25 1.04 359 K0
108 Tau 108 34053 24512 05h 15m 27.66s +22° 17′ 05.5″ 6.26 −0.26 657 A2V
36859 26291 05h 35m 55.52s +27° 39′ 44.7″ 6.27 −0.68 799 K0
24 Tau 24 23629 03h 47m 20.90s +24° 06′ 58.0″ 6.28 A0V
84 Tau 84 V1146 28595 21082 04h 31m 07.16s +15° 06′ 18.6″ 6.28 0.55 455 M3III V1146 Tau
21379 16095 03h 27m 18.67s +12° 44′ 07.1″ 6.29 1.20 340 A0Vs
36160 25806 05h 30m 43.32s +22° 27′ 44.3″ 6.29 0.87 395 K0
V766 Tau V766 24155 18033 03h 51m 15.86s +13° 02′ 46.1″ 6.30 0.63 443 B9p Si α² CVn variable
25175 18717 04h 00m 36.89s +17° 17′ 48.2″ 6.31 −0.95 924 A0V
48 Tau 48 V1099 26911 19877 04h 15m 46.21s +15° 24′ 02.7″ 6.31 3.07 145 F5Vvar V1099 Tau; member of the Hyades star cluster
47 G. Tau 47 27386 20188 04h 19m 37.43s +10° 07′ 17.5″ 6.31 0.05 583 K0
V774 Tau 45 V774 26923 19859 04h 15m 28.86s +06° 11′ 13.6″ 6.32 4.69 69 G0IV... BY Draconis variable
29104 21408 04h 35m 42.57s +19° 52′ 54.6″ 6.33 0.56 464 G5II-III+...
31362 22949 04h 56m 15.59s +24° 35′ 32.1″ 6.33 3.15 141 F0
62 Tau 62 27778 20533 04h 23m 59.76s +24° 18′ 03.7″ 6.34 −0.40 726 B3V
30122 22128 04h 45m 42.46s +23° 37′ 40.9″ 6.34 −0.33 704 B5III
24368 18201 03h 53m 34.46s +25° 40′ 58.7″ 6.35 0.52 478 A2V
25 G. Tau 25 25102 18658 03h 59m 40.41s +10° 19′ 49.5″ 6.35 3.38 128 F5V member of the Hyades star cluster
34762 24984 05h 20m 59.34s +27° 57′ 26.3″ 6.35 −0.29 695 B9IV
37784 26853 05h 42m 03.99s +22° 39′ 37.4″ 6.35 1.14 359 K2
31236 22850 04h 54m 58.32s +19° 29′ 07.6″ 6.36 2.19 222 F3IV member of the Hyades star cluster
1 G. Tau 1 21018 15807 03h 23m 38.99s +04° 52′ 55.6″ 6.37 −1.30 1116 G5III
28086 20698 04h 26m 01.34s +04° 22′ 24.6″ 6.37 −0.06 631 K0
58 G. Tau 58 28736 21152 04h 32m 04.74s +05° 24′ 36.1″ 6.37 3.19 141 F5V member of the Hyades star cluster
28271 20904 04h 28m 51.98s +30° 21′ 41.5″ 6.38 2.71 177 F7V
22522 16924 03h 37m 47.82s +15° 25′ 50.2″ 6.40 2.05 241 A5IV
5 G. Tau 5 21585 16226 03h 29m 03.80s +03° 14′ 55.3″ 6.41 0.68 455 G5
27860 20558 04h 24m 14.47s +12° 09′ 28.9″ 6.42 −0.28 713 K0
37439 26616 05h 39m 27.11s +21° 45′ 46.8″ 6.42 −0.11 660 A1Vn
Sterope II 22 23441 17588 03h 46m 02.89s +24° 31′ 40.8″ 6.43 1.25 354 A0Vn Asterope; member of the Pleiades star cluster
23712 17759 03h 48m 06.56s +24° 59′ 18.5″ 6.44 −0.33 738 K5
70 Tau 70 27991 20661 04h 25m 37.25s +15° 56′ 27.9″ 6.44 3.10 152 F7V member of the Hyades star cluster
37329 26571 05h 38m 57.36s +26° 37′ 05.1″ 6.45 0.87 426 G9III
2 G. Tau 2 21032 15800 03h 23m 36.31s +00° 54′ 37.1″ 6.47 1.20 369 K0
26 Tau 26 23822 17832 03h 48m 56.91s +23° 51′ 26.2″ 6.47 2.11 243 F0
55 G. Tau 55 28505 20985 04h 30m 02.30s +10° 15′ 44.7″ 6.47 1.22 365 G8III
38263 27116 05h 45m 01.30s +12° 53′ 18.1″ 6.47 1.33 348 A3
32642 23695 05h 05m 32.11s +19° 48′ 24.3″ 6.48 0.71 464 A5m
38524 27353 05h 47m 34.66s +25° 34′ 07.1″ 6.48 −0.95 997 K1III
9 G. Tau 9 22211 16695 03h 34m 49.10s +06° 25′ 03.8″ 6.49 0.84 439 G0
37 G. Tau 37 26292 19434 04h 09m 43.04s +03° 19′ 22.2″ 6.49 2.51 204 F2
SZ Tau SZ 29260 21517 04h 37m 14.78s +18° 32′ 35.0″ 6.49 −1.04 1045 F5Ib δ Cep variable
Y Tau 38307 27181 05h 45m 39.41s +20° 41′ 41.1″ 6.5 −1.1 2170 C6.5 carbon star
22615 17026 03h 39m 00.06s +20° 54′ 57.1″ 6.50 0.60 494 Am...
28568 21053 04h 30m 46.74s +16° 08′ 55.5″ 6.50 3.43 134 F5V member of the Hyades star cluster
9 Tau 9 22374 16859 03h 36m 58.03s +23° 12′ 40.0″ 6.72 1.08 437 A2p
101 Tau 101 31845 23214 04h 59m 44.27s +15° 55′ 00.5″ 6.75 3.57 141 F5V member of the Hyades star cluster
HD 24496 24496 18267 03h 54m 28.03s +16° 36′ 57.8″ 6.81 3.36 160 G5 binary star
55 Tau 55 27383 20215 04h 19m 54.78s +16° 31′ 21.6″ 6.85 3.68 140 F7V+... member of the Hyades star cluster
HD 24040 24040 17960 03h 50m 22.97s +17° 28′ 34.9″ 7.52 4.18 152 G0 has a planet (b)
HD 32963 32963 26381 05h 07m 56.0s +26° 19′ 41″ 7.6 G5IV has a planet (b)
HD 37124 37124 23884 05h 37m 02.49s +20° 43′ 50.8″ 7.68 5.07 108 G4V has three planets (b, c & d)
Alcyone B η 23607 03h 47m 19.20s +24° 08′ 22.0″ 8.30 component of the Alcyone system
HD 28678 28678 21109 04h 31m 25 s +04° 34′ 31″ 8.54 740 K0D Hoggar,[4] has a planet (b)
RV Tauri RV 283868 04h 47m 06.73s +26° 10′ 45.6″ 9.41 ~20000 K3pv prototype of the RV Tauri-type variables; Vmax = 9.8m, Vmin = 13.3m
HD 283668 283668 20834 04h 27m 53.0s +24° 26′ 41″ 9.44 138 has a planet (b)
T Tauri T 284419 20390 04h 21m 59.43s +19° 32′ 06.4″ 9.60 3.36 576 G5Ve prototype of the T Tauri-type variables
HD 284149 284149 19176 04h 06m 39.0s +20° 18′ 11″ 9.63 353 F8 has a planet (b)
HD 286123 286123 04h 55m 04.0s +18° 39′ 16″ 9.8 434 F9V has a planet (b)
Gliese 176 285968 21932 04h 42m 55.78s +18° 57′ 29.4″ 9.97 10.10 31 M2.5V has a planet (b)
HD 285507 285507 19207 04h 07m 01.0s +15° 20′ 06″ 10.5 135 K5 has a planet (b)
HD 283869 283869 22271 04h 47m 42.0s +26° 09′ 00″ 10.6 155 has a planet (b)
K2-136 04h 29m 38.99s +22° 52′ 57.8″ 11.20 192 K5V member of the Hyades star cluster; has three transiting planets (b, c, d)
V830 Tau 04h 33m 10.0s +24° 33′ 43″ 12.1 427 M0 has a planet (b)
WASP-152 04h 10m 41.0s +24° 24′ 07″ 12.56 603 G7V has a transiting planet (b)
CL Tau CL 04h 38m 45.0s +08° 05′ 46″ 13 T Tau has a planet (b)
CI Tau CI 04h 33m 52.0s +22° 50′ 30″ 13 K4IV has a planet (b)
FW Tau FW 04h 29m 30.0s +26° 16′ 53″ 15.5 473 M4 has a planet (b)
Crab Pulsar 05h 34m 31.95s +22° 00′ 52.1″ 16.5 6500 F Baade's Star; PSR B0531+21, CM Tau; pulsar in the Crab Nebula
2M J044144 04h 41m 44.90s +23° 01′ 51.4″ 455 M8.5 has a planet
Table legend:

See also

[edit]

References

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Revisions and contributorsEdit on WikipediaRead on Wikipedia

List of stars in Taurus

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The list of stars in Taurus encompasses the cataloged stellar objects lying within the International Astronomical Union-defined boundaries of Taurus, a prominent zodiac constellation representing a and ranking as the 17th largest in the sky with an area of 797 square degrees. Visible primarily in the from latitudes between +90° and -65° during winter evenings, Taurus is renowned for its bright stars and open clusters, including the Hyades—the nearest such cluster to at 153 light-years—and the (Messier 45), a striking group of hot, young stars about 444 light-years distant. Among its 17 formally named stars, the most prominent is Aldebaran (α Tauri), the constellation's brightest at an apparent visual magnitude of 0.85, an orange giant located 65 light-years away that marks the bull's eye in the V-shaped Hyades asterism. The second-brightest is Elnath (β Tauri), a blue giant with magnitude 1.68 situated 131 light-years distant, which also serves as the tip of Auriga's horn due to its position on the shared border. Other notable named stars include Alcyone (η Tauri, magnitude 2.85), the brightest in the Pleiades; Ain (ε Tauri, magnitude 3.53), a member of the Hyades; and Taygeta (19 Tauri, magnitude 4.30), part of the Pleiades (Seven Sisters) cluster, as well as variable stars like T Tauri, the prototype for pre-main-sequence stellar variables approximately 471 light-years away. This compilation typically includes Bayer and Flamsteed designations, apparent magnitudes, spectral types, distances, and proper motions for stars brighter than sixth magnitude, drawing from surveys like the catalog, while highlighting Taurus's role in studies of and galactic structure due to its rich clusters containing hundreds of members.

Overview of Taurus Constellation

Location and Visibility

Taurus is a prominent zodiac constellation spanning 797 square degrees of the , making it the 17th largest among the 88 modern constellations defined by the . It occupies the first quadrant of the , positioned between Aries to the west and Gemini to the east, with boundaries extending from right ascension 3h 24m to 5h 53m and declination +11° to +37°. This positioning places Taurus along the plane, facilitating its observation from a wide range of latitudes. In the , Taurus is best visible from through , when it rises in the eastern sky after sunset and reaches —its highest point—at midnight around . Due to its location on the , the constellation remains observable worldwide except from extreme southern latitudes below about 65° south. Observers can locate it easily by following the line from toward the bright star , which marks the constellation's alpha star at an of 0.85. Key asterisms within Taurus aid in its identification: the V-shaped Hyades open cluster forms the bull's face, with the reddish serving as the bull's eye at the V's apex. The constellation's horns extend northward from this face, delineated by the stars at the northern tip and (Elnath) at the southern. Major features like the Hyades lie approximately 150 light-years distant, while the prominent cluster, representing the bull's shoulder, is situated about 440 light-years away. A November 2025 study using data has shown that the forms the core of a larger stellar complex spanning about 1,950 light-years.

Historical and Mythological Context

In , the constellation Taurus represents the white bull into which transformed to abduct the Phoenician princess Europa, carrying her across the sea to where she became the first queen of the island. This tale, recounted in ancient texts like Ovid's , symbolizes themes of divine pursuit and fertility, with the bull's form enduring as a celestial marker. Earlier, in , Taurus was cataloged in the compendium around the BCE as GU.AN.NA, or "Bull of Heaven," a prominent figure in Mesopotamian lore associated with the , where it embodies a celestial beast sent by the goddess Ishtar. The constellation's position also tied it to the of the es; from approximately 4000 BCE to 1700 BCE during the and Early , the vernal equinox occurred within Taurus, marking the onset of spring and agricultural renewal in ancient calendars. Taurus formed part of the 48 ancient constellations enumerated by the Greek astronomer in his around 150 CE, drawing from earlier Hellenistic and Babylonian traditions to standardize stellar patterns for navigation and astrology. In 1603, introduced Greek letter designations for stars, assigning Alpha Tauri to the prominent red giant now known as , derived from the Arabic al-dabarān meaning "the follower," reflecting its apparent pursuit of the cluster in the sky. By 1725, English Astronomer Royal expanded cataloging with numerical designations in his Historia Coelestis Britannica, assigning sequential numbers to stars within constellations like Taurus based on , facilitating precise identification for observers. Across cultures, Taurus held varied symbolic roles; in Hindu astronomy, it corresponds to Vrishabha , the second zodiac sign embodying the as a of stability and the mount of Shiva's consort , integrated into Vedic sidereal . In Chinese astronomy, it is known as Jin Niu Zuo, or "Golden Ox," part of the lunar mansion and representing diligence and prosperity in traditional asterisms. Modern standardization by the (IAU) in 2016 approved proper names for key stars, such as for Epsilon Tauri (meaning "the eye" in ) and Elnath for (from an-naṭḥ, "the butting one"), preserving Arabic heritage while ensuring global consistency. The cataloging of Taurus stars evolved from qualitative ancient Greek descriptions in Ptolemy's work, which listed about 1,028 stars with rough positions, to quantitative modern surveys. The satellite mission in 1997 provided parallax measurements for over 118,000 stars, including those in Taurus, achieving sub-arcsecond accuracy for the first time. Subsequent missions, launched in 2013, have refined this further with data releases cataloging billions of stars, offering microarcsecond precision on positions, proper motions, and distances for Taurus members, revolutionizing our understanding of the constellation's .

Brightest Stars

Table of Principal Stars

The principal stars in the constellation Taurus, comprising those with apparent visual magnitudes brighter than 4.1, are presented in the following table. Data includes designations, proper names, magnitudes, spectral classifications, distances, radial velocities, coordinates, absolute magnitudes, and relevant notes, primarily sourced from astronomical catalogs incorporating DR3 measurements as of 2022.
Bayer/FlamsteedProper NameVisual MagnitudeSpectral TypeDistance (ly)Radial Velocity (km/s)RA (h:m)Dec (°:' )Absolute MagnitudeNotes
α TauriAldebaran0.85K5 III6754.304:36+16:31-0.75Variable; multiple system
β TauriElnath1.65B7 III134-11.905:26+28:36-1.45Double; also γ Aurigae
η TauriAlcyone2.87B3 III4405.403:47+24:06-2.36Multiple; Pleiades member
ζ TauriTianguan3.00B2 III410-11.005:38+21:09-2.81Variable; shell star
θ² TauriChamukuy3.40A7 III15539.004:29+15:53-0.25Variable; multiple
λ Tauri-3.47B3 V350-13.004:01+12:24-2.25Variable
ε TauriAin3.53K0 III15341.204:29+19:11-0.71Double
ο Tauri-3.60B3 V260-10.004:07+20:49-1.90Variable
27 TauriAtlas3.63B8 III4406.003:49+24:03-2.10Variable; multiple; Pleiades member
γ TauriPrima Hyadum3.65G8 III15335.804:20+15:53-0.70Variable; Hyades member
17 TauriElectra3.70B6 III4405.503:45+24:20-2.30Pleiades member
ξ Tauri-3.74B9 V220-5.004:04+20:01-1.50-
δ¹ TauriSecunda Hyadum3.76G8 III15332.004:23+17:49-0.50Variable; multiple; Hyades member
θ¹ Tauri-3.84A7 III16038.004:29+15:52-0.30Multiple; Hyades member
20 TauriMaia3.87B7 III4406.003:46+24:22-2.40Variable; Pleiades member
ν Tauri-3.91B8 V210-8.004:07+19:09-1.60-
5 Tauri-4.11A7 V13020.004:12+18:47-0.80-

Individual Descriptions

Aldebaran, or , is a prominent classified as spectral type K5 III, marking it as an evolved in the late stages of its life cycle. With a mass of approximately 1.16 solar masses and an age estimated at around 6.6 billion years, it has expanded to a diameter of about 44 solar radii, making it roughly 44 times larger than the Sun in radius. Its measures approximately 20 milliarcseconds, allowing direct imaging of its extended atmosphere through . Observations suggest the presence of a possible dust disk surrounding the , though no confirmed planets have been detected. Elnath, designated , is a hot of spectral type B7 III, characterized by rapid rotation with a projected velocity of about 60 km/s. It exhibits a mercury-manganese peculiarity, a chemical anomaly where its atmosphere is enriched in heavy elements like mercury and due to diffusion processes in its stable outer layers. As a , Elnath consists of a primary giant paired with a companion separated by roughly 1.8 arcseconds, with an on the order of 1,000 years, though precise orbital parameters remain challenging to determine due to the wide separation. Alcyone, or Eta Tauri, serves as the brightest member of the cluster and is classified as a blue-white giant of spectral type B3 III, featuring exceptionally rapid rotation at around 145 km/s that shapes its ellipsoidal form. This high rotational speed contributes to its status as a , with emission lines indicating circumstellar material. Alcyone forms part of a triple system, where the primary is accompanied by two fainter companions at angular separations of approximately 35 arcseconds and 78 arcseconds, enhancing its visual appeal in small telescopes. Tianguan, known as Zeta Tauri, stands out as a shell star of spectral type B2 IIIpe, notable for its equatorial disk of gas that produces characteristic shell absorption lines in its spectrum due to rapid rotation and mass ejection. The disk, formed from material flung from the star's equator at velocities up to 125 km/s, creates a dynamic environment observable through variability in emission lines. Interferometric studies confirm the disk's flattened, equatorial structure, aligning with models of Be star evolution. Hyadum I, or Gamma Tauri, is an orange giant classified as G8 III, representing a more advanced evolutionary stage among the Hyades cluster members with enhanced compared to the Sun. As a multiple , it displays spectroscopic lines indicative of its giant status, with surface abundances analyzed to reveal carbon and enhancements typical of post-main-sequence evolution. Many of the brightest in Taurus, including these examples, are giants or subgiants owing to the constellation's mix of older clusters like the Hyades and younger ones like the , with luminosities typically ranging from several hundred to over a thousand solar luminosities, underscoring their advanced nuclear burning phases.

Stars in Notable Clusters

Hyades Cluster

The Hyades Cluster is the nearest to the Sun, situated at a distance of approximately 153 light-years (47 parsecs). It comprises around 200 that share a common origin, age, chemical composition, and motion through space, spanning an angular diameter of 5.5 degrees. The cluster's brightest members form a prominent V-shaped asterism, traditionally identified as the face or head of Taurus the Bull. With an estimated age ranging from 625 to 790 million years, the Hyades provides a key benchmark for studying in an intermediate-age population. Among its notable members are several bright stars that contribute to the asterism. Gamma Tauri, also known as Hyadum I or Prima Hyadum, is a K0 III giant with an of 3.65, marking the tip of the V. Delta Tauri forms a triple system, featuring an A7 IV primary accompanied by two M-type dwarf companions, with the overall system appearing as part of the cluster's northern arm. Theta¹ Tauri is a complex multiple system comprising four components, including a III giant primary and a B9 V companion in a close binary, along with two additional fainter stars. Epsilon Tauri, called , is a K0 III giant shining at magnitude 3.53 and is noteworthy as the host of a candidate, Amateru (Epsilon Tauri b), with a mass of about 7.2 masses orbiting at 1.7 AU—the first such detection in an . The cluster's stellar population is dominated by main-sequence dwarfs and evolved giants spanning spectral types A through K, with an average of roughly 0.7 solar masses, reflecting the remnants of a progenitor population that has lost higher-mass members to . The Hyades exhibits a coherent of about 45 mas/yr directed toward its apex near Orion, facilitating membership determination via kinematic criteria. It also harbors several dwarfs, such as those identified through imaging, which represent the cooled endpoints of stars originally more massive than about 2 solar masses that have completed their main-sequence lifetimes. As part of the broader Taurus moving group (also known as the Hyades Stream), the cluster co-moves with dispersed field stars sharing similar space velocities, suggesting they originated from the same star-forming region before dynamical interactions scattered the group. , the prominent at the V's base, appears embedded in the asterism but is foreground and unrelated, residing about 65 light-years closer to .

Pleiades Cluster

The , also known as Messier 45 or the "Seven Sisters," is a prominent open star cluster located approximately 440 light-years from in the constellation Taurus. It is estimated to be about 100 million years old and contains roughly 1,000 stars spread across a 2-degree , with the cluster's young age contributing to its cohesive structure bound loosely by gravity. Surrounding several of its brighter members is a , consisting of interstellar dust that scatters blue light from the stars, creating a hazy veil visible in long-exposure images. Among the cluster's notable stars are the bright giants named after figures from . Eta Tauri, or Alcyone, is the brightest at an of 2.87 and is classified as a B7 III giant, emitting intense blue-white light due to its high surface temperature. Nearby, 27 Tauri, known as Atlas, shines at magnitude 3.63 as a B8 III giant, forming part of a triple system. Further out, 16 Tauri, or , appears at magnitude 5.45 with a B7 IV classification as a , while the other sisters—Electra (17 Tauri), (20 Tauri), Merope (23 Tauri), Taygeta (19 Tauri), and Asterope (21 Tauri)—range from magnitudes 3.86 to 5.65 and are primarily B6 to B8 types, all exhibiting the hot, luminous characteristics typical of young main-sequence and giant stars in the cluster. The is dominated by hot B-type stars, which constitute the majority of its brighter members and contribute to its total mass of approximately 800 solar masses, reflecting the cluster's formation from a massive . Many of these stars exhibit rapid rotation, with equatorial velocities often exceeding 100 km/s, a trait common in young clusters where magnetic braking has yet to fully slow them. Additionally, the cluster hosts lower-mass objects, including that failed to ignite fusion, and debris disks around some members, such as the silica-rich disk detected around HD 23514, an F5 V star indicating recent planetary formation activity. Culturally, the holds iconic status worldwide, often visible to the as 6 to 7 stars under good conditions, inspiring myths of sister deities across civilizations. In , it is called Subaru, meaning "unite," which inspired the naming of the on , an 8.2-meter instrument operated by the National Astronomical Observatory of .

Variable Stars

Classification and Types

Variable stars in the constellation Taurus encompass a range of types, predominantly influenced by the region's prominent star-forming molecular clouds. The most characteristic are T Tauri variables, which are pre-main-sequence, low-mass stars (0.2–3 solar masses) undergoing contraction toward the main sequence. These irregular variables exhibit erratic brightness changes of up to 3 magnitudes, driven by instabilities in circumstellar accretion disks, atmospheric activity, and obscuration by surrounding dust or gas clouds. As prototypical young stellar objects embedded in the Taurus-Auriga molecular clouds, T Tauri stars typically display visual magnitudes between 9 and 13, with light curves varying on timescales from days to years. Eclipsing binaries represent another significant category, where variability arises from geometric eclipses in binary systems rather than intrinsic stellar changes. For instance, Algol-type systems like Lambda Tauri produce periodic brightness dips of approximately 0.5 to 2 magnitudes, with orbital periods typically spanning 2 to 10 days, as the cooler companion partially occults the primary star. These systems highlight Taurus's abundance of close binary pairs among its stellar population. Pulsating giants, including RV Tauri variables such as R Tauri, contribute to the constellation's long-period variables. These evolved post-AGB stars undergo radial pulsations with periods of 30 to 150 days, often showing alternating deep and shallow minima with amplitude variations up to several magnitudes, resulting from the expansion and contraction of their outer layers. Classical Cepheids, while present (e.g., EU Tauri with a short period of about 2 days), are not prominent in Taurus compared to other types. Additional types include rotational variables, common among young, spotted T Tauri stars, where photometric modulation from star spots yields periods of 0.57 to 7.4 days, and delta Scuti pulsators in clusters like the Hyades, which exhibit high-frequency oscillations due to partial helium ionization in their envelopes. Overall, the AAVSO International Variable Star Index catalogs around 50 well-documented s in Taurus brighter than 10th magnitude, many tied to its active star-forming regions.

Prominent Examples

T Tauri serves as the prototype for the class of young, pre-main-sequence variable stars known as variables, located approximately 1.8° west of ε Tauri in the constellation, at a distance of about 436 light-years. Discovered in 1852 by astronomer John Russell Hind during a search for nebulae, its irregular photometric variability was first noted in 1890 through observations that revealed fluctuations in brightness. The star exhibits a visual magnitude range of 9.5 to 13, driven by accretion processes from its surrounding onto the stellar surface, which also powers outflows and jets observable in its associated Hind's Variable Nebula (vdB 28). As a hierarchical triple system, with the primary being a K5Ve star and companions including a close binary, T Tauri provides critical insights into the early stages of stellar and planetary formation, particularly the dynamics of circumstellar disks. ζ Tauri, also known as Tianguan, is a prominent Be shell star in Taurus, characterized by a circumstellar disk that contributes to its spectroscopic variability and emission-line . Classified as B1IVe_shell, it displays irregular changes with a visual magnitude ranging from 2.97 to 3.17, influenced by the evolving structure of its decretion disk rather than eclipses. As a single-lined spectroscopic binary with a companion orbiting at a separation corresponding to a period of about 0.36 years, the system's variability is tied to disk oscillations, including one-armed modes that alter the violet-to-red intensity ratios in Balmer lines over cycles of roughly 1400 days. This behavior makes ζ Tauri a key example for studying mass ejection and transport in rapidly rotating early-type stars. λ Tauri represents a classic case of an within Taurus, featuring an inner pair of stars that orbit each other with a period of 3.95 days, resulting in magnitude variations from about 3.7 to 4.2. The primary component is a B3V star, while the secondary is cooler, approximately A-type, forming a detached system where eclipses cause the observed light dips without significant . As part of a wider triple configuration, with a distant tertiary companion, λ Tauri's photometric and spectroscopic monitoring has refined models of in intermediate-mass stars, highlighting the role of in producing observable variability. RY Tauri exemplifies FU Orionis-type eruptive variables among the young stars of Taurus, displaying irregular outbursts with a visual magnitude fluctuating between 9 and 12, embedded in the dark clouds of the Taurus-Auriga complex near vdB 27. As a low-mass pre-main-sequence object, its variability stems from episodic increases in accretion rate from the , leading to temporary spectral type changes and enhanced over decades-long phases. Observations reveal associated jets and outflows, underscoring RY Tauri's importance in understanding outburst mechanisms in regions. Many in Taurus, including these examples, were systematically identified through efforts by the American Association of Variable Star Observers (AAVSO) via ground-based photometry and the satellite mission, which detected over 11,000 potential variables, including new entries in the region. T Tauri-type variables like these are particularly valuable for probing protoplanetary disks, as their variability traces accretion, disk instabilities, and planet-forming processes in real time.

Multiple and Binary Systems

Characteristics of Multiples in Taurus

Multiple star systems are prevalent in the constellation Taurus, with approximately 40–60% of stars participating in binaries or higher-order multiples, a fraction comparable to or elevated relative to that in the solar neighborhood (~45% for solar-type stars) particularly in its younger populations. In the Taurus-Auriga star-forming region, the completeness-corrected multiplicity fraction reaches about 62% ± 14% for stars with masses between 0.7 and 1.4 M⊙, reflecting the region's low-density environment that preserves primordial companions. This high incidence is particularly notable in young clusters such as the Hyades and , where dynamical interactions in relatively sparse conditions help maintain wide binaries that might otherwise disrupt in denser environments. Taurus multiples encompass a variety of types, including visual binaries with wide separations exceeding 1 arcsecond, detectable through direct imaging; spectroscopic binaries identified via Doppler shifts in measurements; and eclipsing binaries when orbital planes align with the , though the latter are less emphasized here. Many systems exhibit hierarchical structures, such as or quadruples, where inner close pairs are orbited by more distant companions, stabilizing the configuration against perturbations. These systems primarily form primordially through turbulent fragmentation of cores during the early collapse phase, rather than through later dynamical capture, leading to the observed high multiplicity in the Taurus-Auriga complex. The region's filamentary structure in the facilitates this process, producing companions with similar masses and ages to their primaries. Observationally, close multiples are probed using speckle interferometry to resolve sub-arcsecond separations, while provides precise for wider systems through long-term tracking. Orbital periods span from mere days for tight spectroscopic pairs to thousands of years for distant visual companions. Statistically, average separations in Taurus T Tauri binaries cluster around 100–500 AU, with mass ratios frequently in the range 0.5–1.0, indicating formation from comparable cloud fragments.

Key Systems

δ Tauri refers to three separate stars (δ¹, δ², δ³ Tauri) in the Hyades cluster, not a bound multiple system. δ¹ Tauri (mag 3.77) is a spectroscopic binary consisting of an A7 III giant primary and a companion with an of 529.8 days and eccentricity of 0.42. δ² Tauri (A2 V, mag 4.80) and δ³ Tauri (A2 IV-Vs, mag 4.30) are single stars separated by ~120" and ~310" from δ¹, respectively, but unbound. ξ Tauri (mag 3.3) is a hierarchical quadruple consisting of an inner eclipsing binary pair of B9 V dwarfs (period 7.14 days), orbited by a B8 V companion (period 145 days), and an outer F5 V companion (period ~51 years). The is associated with the older population in Taurus, not the young star-forming region. β Tauri (Elnath, mag 1.68) is a single-lined spectroscopic binary with a B7 III mercury-manganese primary; the companion remains undetected, with no known visual separation or . θ Tauri (mag 3.4 combined) is a wide system (separation 5.6') in the Hyades, forming a quadruple overall: θ¹ Tauri (K0 III spectroscopic binary with G5 companion) and θ² Tauri (A7 III spectroscopic binary). The inner pairs have short periods (~days), resolved via ; the wide pair is physical. A notable example is V471 Tauri, a post-common-envelope binary in the Hyades consisting of a and K2 V dwarf (period 12.5 days, separation ~0.8" as of 2025), highlighting processes.

Stars Hosting Exoplanets

Overview of Exoplanet Discoveries

As of November 2025, the NASA Exoplanet Archive lists 18 confirmed host stars within the boundaries of the Taurus constellation harboring a total of over 100 exoplanets, with radial velocity and transit photometry comprising the majority of detection methods. Radial velocity measurements, particularly using high-precision spectrographs like HARPS on the ESO 3.6-meter telescope, have been dominant for detecting massive companions around evolved giant stars in Taurus, revealing planets through the star's gravitational wobble. Transit methods, employed by space-based surveys, have proven effective for identifying smaller planets orbiting members of Taurus's prominent clusters, such as the Hyades and Pleiades. Direct imaging remains rare, hindered by the circumstellar dust and protoplanetary disks prevalent in the region's young stellar populations. The timeline of discoveries in Taurus began in the early , with the first confirmed planet, HD 37124 b, detected in 2002 via observations of its host star, a solar-type dwarf. The pace accelerated during the through NASA's Kepler and missions, which identified transiting systems like those around K2-155, contributing several multi-planet setups amid Taurus's field stars. The (TESS), launched in 2018, further boosted detections by targeting brighter nearby hosts, uncovering candidates such as K2-288Bb in 2019. More recently, Gaia's astrometric data has aided in validating young systems, including potential companions in the Taurus-Auriga star-forming region, by refining stellar distances and proper motions. Exoplanet demographics in Taurus reflect the constellation's mix of evolved and pre-main-sequence stars, featuring hot Jupiters orbiting older giants, often with short periods under 10 days, while younger systems host super-Earths and mini-Neptunes with radii between 1.5 and 4 radii. Host stars generally exhibit elevated metallicities, correlating with higher planet occurrence rates, consistent with broader trends where metal-rich environments favor giant planet formation. Detection challenges persist, especially for stars in Taurus's molecular clouds, where magnetic activity and starspots produce jitter that mimics planetary signals, complicating confirmation. Approximately five candidates await validation as of 2025, primarily from TESS and ground-based follow-up.

Specific Host Stars

One prominent example of an exoplanet host in Taurus is HD 37124, a G5 IV with an apparent visual magnitude of 8.5 and a distance of approximately 92 light years. This system hosts three confirmed planets discovered via (RV) observations between 2002 and 2016. The innermost planet, HD 37124 d, is a with a semi-major axis of 0.04 AU and an orbital period of 23 days, while HD 37124 b orbits at 0.75 AU with a period of 155 days, and the outermost, HD 37124 c, has a semi-major axis of 3.4 AU and a period of 2.3 years. The architecture features a close-in alongside two longer-period companions, with the outer planets exhibiting near-resonant configurations suggestive of dynamical interactions during migration. Another notable system is that of ε Tauri (Ain), a K0 III with a visual magnitude of 3.53, located about 147 light years away and aged around 0.6 billion years as a member of the Hyades cluster. It hosts a single confirmed , ε Tauri b, discovered by RV in 2007, with a minimum mass of 6.6 masses, a semi-major axis of 1.9 AU, and an of 595 days. This planet orbits a evolved host, providing insights into planetary survival around expanding giants, though its high mass places it near the planet-brown dwarf boundary. K2-155, a metal-poor K7 V with a visual magnitude of 12.8 and of 290 years, exemplifies a multi- system of s detected by transit photometry during the K2 mission in 2018. The system includes three confirmed planets: K2-155 b (, 1.6 radii, 6.3-day period, 0.056 AU), K2-155 c (, 1.9 radii, 13.4-day period, 0.10 AU), and K2-155 d ( to , 2.0 radii, 40.8-day period, 0.19 AU). These worlds form a compact chain with periods in a near 1:2:3 , orbiting a host estimated at 0.6-1.0 billion years old and highlighting planet formation in low-metallicity environments. The young V 1298 Tauri system, centered on a kT4Ve (K7 pre-main sequence) (visual magnitude ~10, distance ~354 light years, age ~20-30 million years), represents one of the youngest confirmed multi-planet systems, discovered by TESS transits in 2019 with follow-up RV confirmation. It features four confirmed planets in a compact architecture: V 1298 Tau d (, ~5.4 radii, 8.2-day period, 0.08 AU), c (~6.4 radii, 12.4-day period, 0.11 AU), b (~8.5 radii, 24.1-day period, 0.16 AU), and e (Neptune-sized, ~9.6 radii, 53-day period, 0.32 AU), with masses ~10-25 Earth masses for the inner three from 2023 RV data. This pre-main-sequence setup, embedded in the Taurus-Auriga star-forming region, offers a rare view of early planetary dynamics, including potential mean-motion resonances among the inner worlds. Recent JWST/NIRSpec observations (2024-2025) of V1298 Tau b reveal a primordial H/He-dominated atmosphere with low (~10x solar), providing insights into early evolution. GJ 176, an M2.5 V red dwarf host with visual magnitude 9.97 and distance of 30 light years, hosts two confirmed super-Earths detected by RV between 2007 and 2009. The inner planet, GJ 176 b, has a minimum mass of 7.8 Earth masses, orbital period of 8.8 days, and semi-major axis of 0.066 AU, while the outer GJ 176 c (minimum mass 6.8 Earth masses, 28.6-day period, 0.15 AU) lies near the inner edge of the habitable zone. The system's age of 3-10 billion years underscores the prevalence of close-in rocky worlds around cool stars in Taurus. These host stars in Taurus are predominantly FGK dwarfs and giants, with ages spanning 0.6-10 billion years, though M dwarfs like K2-155 and GJ 176 add diversity; notably, V 1298 Tau marks a confirmed host, challenging earlier assumptions of no such detections. Recent JWST observations of hot Jupiters in similar systems, including transmission spectroscopy for atmospheric characterization, have targeted architectures like HD 37124's to probe migration histories and compositions.

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