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List of stars in Ophiuchus
List of stars in Ophiuchus
List of stars in Ophiuchus
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This is the list of notable stars in the constellation Ophiuchus, sorted by decreasing brightness.

Name B F G.[1] Var HD HIP RA Dec vis.
mag. 		abs.
mag. 		Dist. (ly) Sp. class Notes
α Oph α 55 159561 86032 17h 34m 56.00s +12° 33′ 38.1″ 2.08 1.30 47 A5III Ras Alhague, Rasalhague
η Oph η 35 90 155125 84012 17h 10m 22.66s −15° 43′ 30.5″ 2.43 0.37 84 A2.5Va Sabik
ζ Oph ζ 13 28 149757 81377 16h 37m 09.53s −10° 34′ 01.7″ 2.54 −3.20 458 O9.5V Han; γ Cas variable; Be star
δ Oph δ 1 7 146051 79593 16h 14m 20.77s −03° 41′ 38.3″ 2.73 −0.86 170 M1III Yed Prior, Yad, Jed Prior
β Oph β 60 168 161096 86742 17h 43m 28.38s +04° 34′ 00.9″ 2.76 0.76 82 K2III Cebalrai, Celbalrai, Celb-al-Rai, Kelb Alrai, Cheleb
κ Oph κ 27 65 153210 83000 16h 57m 40.27s +09° 22′ 30.2″ 3.19 1.09 86 K2IIIvar
ε Oph ε 2 9 146791 79882 16h 18m 19.24s −04° 41′ 33.4″ 3.23 0.64 107 G8III Yed Posterior, Yad, Jed Posterior
θ Oph θ 42 126 157056 84970 17h 22m 00.58s −24° 59′ 58.2″ 3.27 −2.92 563 B2IV β Cep variable
ν Oph ν 64 186 163917 88048 17h 59m 01.60s −09° 46′ 24.1″ 3.32 −0.03 153 K0III Sinistra; has two brown dwarfs
72 Oph 72 199 165777 88771 18h 07m 21.02s +09° 33′ 49.2″ 3.71 1.69 83 A4IVs
γ Oph γ 62 172 161868 87108 17h 47m 53.57s +02° 42′ 26.9″ 3.75 1.43 95 A0V Bake-eo / Bake Eo[2], Tsung Ching, Muliphen [3][4]
λ Oph λ 10 25 148857 80883 16h 30m 54.84s +01° 59′ 02.8″ 3.82 0.28 166 A2V Marfik, Marfic, Marsic
67 Oph 67 191 164353 88192 18h 00m 38.72s +02° 55′ 53.7″ 3.93 −4.26 1417 B5Ib
70 Oph p 70 197 165341 88601 18h 05m 27.21s +02° 30′ 08.8″ 4.03 5.50 17 K0V SB nearby
44 Oph b 44 135 157792 85340 17h 26m 22.22s −24° 10′ 30.1″ 4.16 2.11 84 A3IV:m
χ Oph χ 7 15 148184 80569 16h 27m 01.44s −18° 27′ 22.3″ 4.22 −1.66 489 B2Vne γ Cas variable
45 Oph d 45 139 157919 85423 17h 27m 21.26s −29° 52′ 00.1″ 4.28 1.61 111 F3III
φ Oph φ 8 24 148786 80894 16h 31m 08.39s −16° 36′ 45.5″ 4.29 0.25 210 G8/K0III
36 Oph B A 36 103 155885 84405 17h 15m 21.29s −26° 36′ 00.2″ 4.33 5.44 20 K1V nearby triple star system
σ Oph σ 49 143 157999 85355 17h 26m 30.88s +04° 08′ 25.2″ 4.34 −3.44 1173 K3IIvar
ι Oph ι 25 152614 82673 16h 54m 00.50s +10° 09′ 55.6″ 4.39 0.11 234 B8V
ξ Oph ξ 40 124 156897 84893 17h 21m 00.21s −21° 06′ 44.8″ 4.39 3.19 57 F2/F3V
68 Oph 68 193 164577 88290 18h 01m 45.19s +01° 18′ 18.4″ 4.42 −0.13 265 A2Vn
ω Oph ω 9 26 148898 80975 16h 32m 08.19s −21° 27′ 59.3″ 4.45 0.80 175 Ap α² CVn variable
ψ Oph ψ 4 11 147700 80343 16h 24m 06.20s −20° 02′ 14.0″ 4.48 0.79 178 K0III
47 Oph 47 141 157950 85365 17h 26m 37.94s −05° 05′ 11.4″ 4.53 2.14 98 F3V
ρ Oph A ρ 5 13 147933 80473 16h 25m 35.12s −23° 26′ 49.6″ 4.57 −0.84 361 B2V
μ Oph μ 57 157 159975 86284 17h 37m 50.72s −08° 07′ 07.4″ 4.58 −1.55 549 B8II-IIIMNp
υ Oph υ 3 18 148367 80628 16h 27m 48.23s −08° 22′ 18.1″ 4.62 1.75 122 A3m She Low
20 Oph 20 49 151769 82369 16h 49m 49.97s −10° 46′ 58.1″ 4.64 1.80 121 F7IV
71 Oph 71 198 165760 88765 18h 07m 18.35s +08° 44′ 01.7″ 4.64 0.33 238 G8III-IV
41 Oph 41 111 156266 84514 17h 16m 36.71s −00° 26′ 42.5″ 4.72 0.60 218 K2III
τ Oph B τ 69 164764 88404 18h 03m 04.91s −08° 10′ 48.9″ 4.77 1.19 167 F5V
51 Oph c 51 149 158643 85755 17h 31m 24.95s −23° 57′ 45.3″ 4.78 −0.80 426 A0V has a developing planetary system
66 Oph 66 190 V2048 164284 88149 18h 00m 15.80s +04° 22′ 07.1″ 4.79 −1.79 676 B2Ve V2048 Oph; γ Cas variable; Be star
30 Oph 30 70 153687 83262 17h 01m 03.63s −04° 13′ 20.8″ 4.82 −0.63 402 K4III
74 Oph 74 209 168656 89918 18h 20m 52.06s +03° 22′ 37.7″ 4.85 0.27 269 G8III
58 Oph 58 165 160915 86736 17h 43m 25.85s −21° 40′ 59.1″ 4.86 3.64 57 F6/F7V
24 Sco (24) 39 150416 81724 16h 41m 34.40s −17° 44′ 31.8″ 4.91 −0.48 391 G8II/III
66 Her e (66) 156681 84671 17h 18m 36.99s +10° 51′ 53.0″ 5.03 −1.60 691 K4II-III
36 Oph A A 36 103 155886 17h 15m 20.80s −26° 36′ 05.0″ 5.07 20 K0V Guniibuu,[5] component of the 36 Oph system
ο Oph A ο 39 112 156349 84626 17h 18m 00.72s −24° 17′ 12.8″ 5.14 −0.09 363 K:... part of the ο Oph system
23 Oph 23 58 152601 82730 16h 54m 35.71s −06° 09′ 14.1″ 5.23 0.82 248 K2III
17 G. Oph 17 V2105 148349 80620 16h 27m 43.46s −07° 35′ 51.2″ 5.24 −0.72 507 M2 comp
τ Oph A τ 69 195 164765 88404 18h 03m 04.90s −08° 10′ 50.0″ 5.24 167 F2V
43 Oph 43 128 157236 85084 17h 23m 21.59s −28° 08′ 33.9″ 5.30 −1.02 599 K4/K5III
Gliese 678 150 158614 85667 17h 30m 23.87s −01° 03′ 45.0″ 5.31 4.23 54 G8IV-V
37 Oph 37 155644 84177 17h 12m 27.81s +10° 35′ 06.8″ 5.32 −1.56 776 M2III
(52 Cau) 171802 91217 18h 36m 27.84s +09° 07′ 22.1″ 5.38 2.43 127 F5III 52 G. Ser Cau in Ophiuchus
21 G. Oph 21 148513 80693 16h 28m 33.98s +00° 39′ 54.6″ 5.41 −0.15 422 K4IIIp
146 G. Oph 146 158352 85537 17h 28m 49.69s +00° 19′ 50.1″ 5.41 1.41 206 A8V
208 G. Oph 208 168387 89772 18h 19m 09.56s +07° 15′ 35.1″ 5.41 2.15 147 K2III
88 G. Oph 88 155078 83962 17h 09m 47.92s −10° 31′ 22.9″ 5.43 2.40 132 F5IV
(53 Cau) 171834 91237 18h 36m 39.09s +06° 40′ 19.8″ 5.43 2.92 103 F3V 53 G. Ser Cau in Ophiuchus
183 G. Oph 183 163532 87847 17h 56m 47.75s −04° 04′ 54.5″ 5.44 −0.14 426 G9III
202 G. Oph 202 166460 89065 18h 10m 40.29s +03° 19′ 27.4″ 5.50 −0.01 412 K2III
21 Oph 21 52 152127 82480 16h 51m 24.94s +01° 12′ 57.5″ 5.51 0.39 345 A2Vs
40 G. Oph 40 150453 81754 16h 41m 53.67s −19° 55′ 28.1″ 5.55 2.41 139 F3V
24 Oph 24 61 152849 82925 16h 56m 48.04s −23° 09′ 01.2″ 5.57 0.34 363 A0V
152 G. Oph 152 158837 85749 17h 31m 21.35s +02° 43′ 28.1″ 5.57 0.28 373 G8III
153 G. Oph 153 159170 85922 17h 33m 29.87s −05° 44′ 40.5″ 5.61 2.19 158 A5V
82 G. Oph 82 154445 83635 17h 05m 32.26s −00° 53′ 31.4″ 5.63 −1.22 765 B1V
HR 6902 (39 Cau) 169689 90313 18h 25m 38.80s +08° 01′ 55.3″ 5.64 −1.33 807 G8III-IV+.. 39 G. Ser Cau in Ophiuchus
22 G. Oph 22 148604 80793 16h 29m 46.90s −14° 33′ 03.2″ 5.66 1.09 268 G5III/IV
201 G. Oph 201 166285 89000 18h 09m 54.01s +03° 07′ 13.1″ 5.67 2.31 153 F5V
73 Oph 73 200 V2666 166233 88964 18h 09m 33.86s +03° 59′ 35.8″ 5.71 2.17 166 F2V V2666 Oph; γ Dor variable
14 Oph 14 43 150557 81734 16h 41m 42.54s +01° 10′ 52.0″ 5.74 2.21 165 F2.7III-IV
26 Oph 26 67 153363 83196 17h 00m 09.48s −24° 59′ 20.2″ 5.74 3.13 108 F3V
12 Oph 12 27 V2133 149661 81300 16h 36m 21.18s −02° 19′ 25.8″ 5.77 5.82 32 K2V V2133 Oph; BY Dra variable
134 G. Oph 134 157617 85139 17h 23m 57.61s +08° 51′ 09.3″ 5.77 −1.82 1076 K1III
180 G. Oph 180 162917 87558 17h 53m 14.26s +06° 06′ 04.5″ 5.77 3.29 102 F4IV-V
53 Oph f 53 155 159480 85998 17h 34m 36.69s +09° 35′ 12.2″ 5.80 0.70 342 A2V
132 G. Oph 132 157527 85207 17h 24m 42.04s −21° 26′ 29.1″ 5.82 0.99 302 K0III
V2052 Oph 182 V2052 163472 87812 17h 56m 18.40s +00° 40′ 13.3″ 5.82 −1.21 830 B2IV-V β Cep variable
54 G. Oph 54 152311 82621 16h 53m 25.26s −20° 24′ 55.8″ 5.86 3.63 91 G5IV
187 G. Oph 187 164064 88101 17h 59m 36.76s −04° 49′ 15.3″ 5.86 −0.29 553 K5III
66 G. Oph 66 153336 83176 16h 59m 57.70s −25° 05′ 31.8″ 5.88 0.03 482 M1/M2III
U Oph 110 U 156247 84500 17h 16m 31.72s +01° 12′ 38.1″ 5.89 −0.46 606 B5Vnn Algol variable
179 G. Oph 179 162774 87491 17h 52m 35.46s +01° 18′ 18.2″ 5.91 0.75 351 K5III
ρ Oph B ρ 5 12 147934 80473 16h 25m 35.10s −23° 26′ 46.0″ 5.92 361 B2V
184 G. Oph 184 163624 87875 17h 57m 04.30s +00° 04′ 00.1″ 5.95 1.05 312 A3V
164 G. Oph 164 160781 86575 17h 41m 32.32s +06° 18′ 47.4″ 5.97 −1.93 1240 G7III
85 G. Oph 85 154779 83854 17h 08m 14.85s −17° 36′ 32.3″ 5.98 0.53 401 K0III
105 G. Oph 105 155970 84402 17h 15m 20.30s −14° 35′ 02.9″ 5.98 1.11 307 K1III
140 G. Oph 140 157955 85442 17h 27m 37.56s −29° 43′ 28.2″ 5.98 −0.34 599 B9.5IV
169111 90052 18h 22m 35.31s +12° 01′ 46.7″ 5.99 0.16 479 A2V
V2213 Oph 81 V2213 154417 83601 17h 05m 16.83s +00° 42′ 12.1″ 6.00 4.45 66 F9V BY Draconis variable
142 G. Oph 142 157978 85333 17h 26m 19.01s +07° 35′ 44.4″ 6.01 −1.01 825 A0...
16 Oph 16 44 151133 82037 16h 45m 29.68s +01° 01′ 12.5″ 6.02 0.20 477 B9.5III
46 G. Oph 46 151527 82259 16h 48m 26.99s −14° 54′ 33.8″ 6.03 0.35 447 A0IV/V
119 G. Oph 119 156717 84792 17h 19m 53.35s −17° 45′ 23.3″ 6.03 0.74 373 A0V
30 G. Oph 30 149911 81440 16h 38m 01.56s −06° 32′ 16.8″ 6.05 0.54 412 A0pe...
151 G. Oph 151 158704 85783 17h 31m 44.38s −26° 16′ 10.8″ 6.05 0.42 436 B9II/III
16 G. Oph 16 148287 80558 16h 26m 50.06s +02° 20′ 52.7″ 6.06 0.28 466 G8III
86 G. Oph 86 154895 83853 17h 08m 13.66s −01° 04′ 45.8″ 6.06 1.46 272 A3V
36 G. Oph 36 150366 81728 16h 41m 36.21s −24° 28′ 04.6″ 6.07 1.54 262 A7III
19 Oph 19 45 151431 82162 16h 47m 09.76s +02° 03′ 52.4″ 6.07 0.17 492 A3V
(43 Cau) 170137 90487 18h 27m 50.32s +03° 44′ 54.9″ 6.07 −2.05 1370 K3III 43 G. Ser Cau in Ophiuchus
109 G. Oph 109 156227 84524 17h 16m 42.75s −06° 14′ 41.8″ 6.08 0.60 407 K0
162 G. Oph 162 160471 86476 17h 40m 11.95s −02° 09′ 08.2″ 6.08 −0.03 544 K2.5Ib
V2392 Oph 206 V2392 167654 89527 18h 16m 05.58s +02° 22′ 39.3″ 6.10 −0.58 706 M4III
95 G. Oph 95 155401 84175 17h 12m 25.07s −27° 45′ 43.2″ 6.12 0.00 546 B9Vn...
160365 86373 17h 38m 57.87s +13° 19′ 45.0″ 6.12 1.26 305 F6III
V986 Oph 196 V986 165174 88522 18h 04m 37.36s +01° 55′ 08.4″ 6.14 B0IIIn
63 G. Oph 63 153021 82979 16h 57m 26.00s −10° 57′ 47.4″ 6.15 1.72 251 G8III-IV
61 Oph 61 169 161270 86831 17h 44m 34.09s +02° 34′ 45.9″ 6.16 0.41 460 A1IV-V
V2368 Oph 108 V2368 156208 84479 17h 16m 14.25s +02° 11′ 10.5″ 6.17 −0.11 588 A2V Algol variable
33 Sco (33) 157588 85242 17h 25m 06.23s −24° 14′ 37.4″ 6.17 0.60 424 K0III
8 G. Oph 8 146514 79781 16h 16m 55.28s −03° 57′ 12.1″ 6.18 2.79 155 A9Vn
V1010 Oph 48 V1010 151676 82339 16h 49m 27.67s −15° 40′ 04.8″ 6.18 1.83 242 A3V β Lyr variable
Y Oph 175 Y 162714 87495 17h 52m 38.70s −06° 08′ 36.8″ 6.18 −3.54 2860 G3Ibv SB δ Cep variable
2 Sgr (2) 158 160042 86352 17h 38m 44.87s −21° 54′ 45.4″ 6.19 1.11 337 G6III/IV
162468 87335 17h 50m 43.61s +11° 56′ 47.9″ 6.19 0.22 509 K1III-IV
173 G. Oph 173 161941 87150 17h 48m 20.23s +03° 48′ 15.1″ 6.22 −3.18 2470 B9.5V
10 G. Oph 10 147550 80227 16h 22m 38.91s −02° 04′ 47.5″ 6.24 0.76 407 B9V
V2388 Oph V2388 163151 87655 17h 54m 14.21s +11° 07′ 51.4″ 6.24 2.08 221 F5Vn
34 G. Oph 34 150259 81632 16h 40m 34.51s −20° 24′ 31.4″ 6.25 0.68 424 K0III
41 G. Oph 41 150451 81687 16h 41m 11.53s −01° 00′ 01.0″ 6.25 2.88 154 A7III
V2542 Oph 56 V2542 152569 82693 16h 54m 10.60s −01° 36′ 43.6″ 6.25 1.93 238 F0V δ Sct variable
159 G. Oph 159 160315 86391 17h 39m 08.48s +02° 01′ 41.2″ 6.25 0.88 387 F4IV...
5 G. Oph 5 145788 79463 16h 12m 56.60s −04° 13′ 14.7″ 6.26 0.10 557 A1V
80 G. Oph 80 154481 83740 17h 06m 53.23s −26° 30′ 46.8″ 6.26 −1.73 1294 B8/B9II
(64 Cau) 172424 91523 18h 39m 51.60s +07° 21′ 31.4″ 6.26 0.38 488 G8III 64 G. Ser Cau in Ophiuchus
62 G. Oph 62 152909 82951 16h 57m 03.99s −19° 32′ 23.4″ 6.27 −0.33 682 B7/8III
29 Oph 29 71 153727 83331 17h 01m 51.27s −18° 53′ 07.8″ 6.28 0.58 450 K1III
115 G. Oph 115 156462 84649 17h 18m 19.27s −16° 18′ 42.8″ 6.28 −0.68 805 M0/M1III
131 G. Oph 131 157347 85042 17h 22m 51.26s −02° 23′ 16.5″ 6.28 4.83 63 G5IV
185 G. Oph 185 163641 87866 17h 56m 55.96s +06° 29′ 15.8″ 6.28 −0.32 681 B9III
77 G. Oph 77 154204 83567 17h 04m 45.33s −20° 29′ 40.7″ 6.29 0.86 397 B7IV/V
28 Sco (28) 79 154418 83684 17h 06m 11.81s −21° 33′ 51.8″ 6.29 1.33 321 A1m...
168199 89677 18h 18m 02.94s +13° 46′ 37.4″ 6.29 −1.38 1113 B5V
167 G. Oph 167 161056 86768 17h 43m 47.02s −07° 04′ 46.5″ 6.30 −1.85 1393 B1.5V
122 G. Oph 122 156826 84801 17h 19m 59.53s −05° 55′ 01.3″ 6.31 2.67 174 G9V
51 G. Oph 51 151900 82405 16h 50m 22.25s −02° 39′ 15.3″ 6.32 2.43 195 F1III-IV
33 G. Oph 33 150177 81580 16h 39m 39.12s −09° 33′ 15.2″ 6.33 3.14 142 F3V
60 G. Oph 60 152781 82861 16h 56m 01.79s −16° 48′ 22.8″ 6.33 3.30 132 K0/K1III/IV
72 G. Oph 72 153914 83342 17h 01m 58.96s +08° 27′ 02.4″ 6.33 1.00 379 A4V
36 Oph C A 36 106 V2215 156026 84478 17h 16m 13.68s −26° 32′ 36.3″ 6.33 7.45 20 K5V V2215 Oph; component of the 36 Oph system; RS CVn variable
176 G. Oph 176 162596 87428 17h 51m 59.45s −01° 14′ 12.5″ 6.33 0.66 445 K0
163772 87910 17h 57m 26.99s +11° 02′ 40.4″ 6.33 1.19 348 A1V
84 G. Oph 84 154660 83738 17h 06m 52.94s −01° 39′ 22.0″ 6.34 1.62 286 A9V
97 G. Oph 97 155500 84113 17h 11m 45.22s +07° 53′ 41.0″ 6.34 0.89 402 K0III
133 G. Oph 133 157546 85195 17h 24m 37.03s −18° 26′ 44.7″ 6.34 −0.30 695 B8V
166095 88862 18h 08m 33.74s +14° 17′ 05.0″ 6.34 0.28 532 A5m
2 G. Oph 2 144362 78849 16h 05m 44.53s −06° 17′ 28.1″ 6.35 1.89 254 F2IV
19 G. Oph 19 148390 80610 16h 27m 32.27s +02° 52′ 14.4″ 6.35 0.23 547 K5
87 G. Oph 87 154962 83906 17h 08m 54.55s −03° 52′ 57.4″ 6.35 3.61 115 G8IV-V
32 Sco (32) 125 156992 84947 17h 21m 41.58s −24° 54′ 21.6″ 6.36 −0.11 643 K3III
147 G. Oph 147 158463 85622 17h 29m 47.37s −05° 55′ 09.6″ 6.36 2.07 235 K0III
V2126 Oph 188 V2126 164258 88148 18h 00m 15.66s +00° 37′ 46.2″ 6.36 0.94 395 A3spe... α² CVn variable
192 G. Oph 192 164432 88213 18h 00m 52.86s +06° 16′ 05.9″ 6.36 −1.96 1502 B2IV
144 G. Oph 144 158170 85474 17h 28m 02.39s −08° 12′ 29.0″ 6.37 1.57 297 F5IV
83 G. Oph 83 154610 83677 17h 06m 09.64s +09° 44′ 01.9″ 6.38 0.04 604 K5
154619 83688 17h 06m 13.03s +10° 27′ 13.9″ 6.38 1.04 381 G8III-IV
3 G. Oph 3 144390 78870 16h 05m 59.83s −06° 08′ 23.1″ 6.39 1.25 347 K0
42 G. Oph 42 150493 81691 16h 41m 16.74s +01° 14′ 43.7″ 6.40 −0.46 767 K0
X Oph X 172171 91389 18h 38m 21.0s +08° 50′ 02.0″ 6.40 K0 Mira variable
163 G. Oph 163 160839 86725 17h 43m 17.71s −27° 53′ 02.3″ 6.40 −3.37 2937 F0III/IV
136 G. Oph 136 157864 85391 17h 26m 55.30s −25° 56′ 36.2″ 6.42 0.86 423 B9.5/A0V
V2114 Oph 145 V2114 158228 85450 17h 27m 44.07s +08° 26′ 31.7″ 6.42 −0.59 823 M4III
159082 85826 17h 32m 14.88s +11° 55′ 48.0″ 6.42 0.51 495 B9.5V
V2393 Oph (50 Cau) V2393 171247 90971 18h 33m 23.30s +08° 16′ 05.8″ 6.42 −2.01 1583 B8IIIp SiSr: 50 G. Ser Cau in Ophiuchus; α² CVn variable
123 G. Oph 123 156860 84780 17h 19m 46.49s +02° 08′ 22.1″ 6.43 0.11 599 M5III
205 G. Oph 205 167162 89347 18h 13m 52.22s +02° 23′ 36.6″ 6.43 −1.35 1173 K2
31 G. Oph 31 150052 81499 16h 38m 47.73s −08° 37′ 06.9″ 6.44 −0.72 881 K5
138 G. Oph 138 157856 85307 17h 25m 57.84s −01° 39′ 06.9″ 6.44 2.49 201 F3V
174 G. Oph 174 162113 87224 17h 49m 19.05s +01° 57′ 40.4″ 6.44 1.34 342 K0III
148531 80708 16h 28m 42.35s +00° 03′ 18.3″ 6.46 1.65 299 K5
23 G. Oph 23 148743 80840 16h 30m 30.02s −07° 30′ 52.0″ 6.46 −2.34 1874 A7Ib
38 G. Oph 38 150381 81663 16h 40m 56.42s −08° 18′ 34.7″ 6.47 0.54 499 K0
158716 85666 17h 30m 22.65s +11° 55′ 26.3″ 6.47 1.59 309 A1V
52 Oph 52 154 V2125 159376 86060 17h 35m 18.50s −22° 02′ 37.7″ 6.47 −0.69 883 Ap Si
64 G. Oph 64 153229 83090 16h 58m 41.56s −14° 52′ 10.6″ 6.48 3.06 158 F3IV/V
171505 91090 18h 34m 47.49s +10° 53′ 31.2″ 6.48 0.03 635 A1V
20 G. Oph 20 148515 80719 16h 28m 48.99s −08° 07′ 43.2″ 6.49 3.16 151 F2V
HD 156846 121 156846 84856 17h 20m 34.31s −19° 20′ 01.5″ 6.51 3.06 160 G1V has a planet (b)
GJ 688 160346 86400 17h 39m 16.9s +03° 33′ 18.8″ 6.52 6.07 35 K2V
ο Oph B ο 39 113 156350 84625 17h 18m 00.64s −24° 17′ 02.7″ 6.59 0.75 481 G8/K0II part of the ο Oph system
29 Sco (29) 155685 84314 17h 14m 14.25s −26° 59′ 03.9″ 6.65 1.80 304 F2/F3V
HD 154088 73 154088 83541 17h 04m 28s −28° 34′ 58″ 6.73 5.47 58 K0V has a planet (b)
HD 155233 155233 84056 17h 11m 04.0s −20° 39′ 16″ 6.80 245 K1III has a planet (b)
38 Oph 38 156252 84605 17h 17m 39.53s −26° 37′ 44.5″ 6.81 1.17 438 B9.5V
HD 148427 148427 80687 16h 28m 28.15s −13° 23′ 58.7″ 6.90 3.04 193 K0IV Timir,[6] has a planet (b)
18 Oph 18 47 151659 16h 49m 44.40s −24° 38′ 24.0″ 7.10 A1m...
HD 150433 150433 81681 16h 41m 08s −02° 51′ 26″ 7.22 97 G0 has a planet (b)
Gl 673 157881 85295 17h 25m 45.23s +02° 06′ 41.1″ 7.54 8.10 25 K5 nearby; high proper motion star
HD 157172 157172 85017 17h 22m 35s −19° 36′ 58″ 7.86 104 G8.5V has a planet (b)
HD 149143 149143 81022 16h 32m 51.05s +02° 05′ 05.4″ 7.90 3.89 207 G0 Rosalíadecastro,[5] has a planet (b)
HD 170469 170469 90593 18h 29m 10.98s +11° 41′ 43.8″ 8.21 4.15 212 G5IV has a planet (b)
HD 164509 164509 88268 18h 01m 31s +00° 06′ 16″ 8.24 170 G5V has a planet (b)
HD 171028 171028 18h 32m 15.49s +06° 56′ 44.7″ 8.31 294 G0V has a planet (b)
HD 152581 152581 82651 16h 53m 44s +11° 58′ 25″ 8.54 607 K0 Mahsati,[7] has a planet (b)
HD 159243 159243 85911 17h 33m 22.0s +05° 42′ 03″ 8.65 226 G0V has two planets (b & c)
Barnard's Star V2500 87937 17h 57m 48.50s +04° 41′ 36.2″ 9.54 13.24 5.94 M4Ve 2nd nearest star system; V2500 Oph
Wolf 1061 V2306 80824 16h 30m 18.06s −12° 39′ 45.3″ 10.12 11.97 13.91 M3.5 30th nearest star system; V2306 Oph
HAT-P-57 18h 18m 58.0s +10° 35′ 50″ 10.47 988 has a transiting planet (b)
WASP-163 17h 06m 09.0s −10° 24′ 47″ 12.54 G8 has a transiting planet (b)
CoRoT-6 18h 44m 17.42s +06° 39′ 48.0″ 13.9 F5V has a transiting planet (b)
GJ 1214 17h 15m 18.94s +04° 57′ 49.7″ 14.67 14.10 42 M4.5 has a transiting super-Earth planet (b)
CoRoT-25 18h 42m 31.0s +06° 30′ 50″ 15.0 3262 G0V has a transiting planet (b)
CoRoT-29 18h 35m 37.0s +06° 28′ 47″ 15.35 2495 KOV has a transiting planet (b)
CoRoT-26 18h 39m 00.0s +06° 58′ 12″ 15.76 5447 G8IV has a transiting planet (b)
SN 1604 17h 30m 35.98s −21° 28′ 56.2″ n/a S Kepler's star; supernova
Table legend:

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References

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List of stars in Ophiuchus

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The list of stars in Ophiuchus refers to the cataloged stellar objects lying within the boundaries of this constellation, as delineated by the (IAU) in 1930, encompassing an area of 948 square degrees straddling the in the southern sky. , representing the serpent-bearer from , is visible primarily during summer evenings in the and contains approximately 175 stars brighter than 6.5, observable with the or under . Among these, the constellation features a mix of bright giants, binary systems, and notable low-mass stars, with the list typically organized by decreasing brightness or for astronomical reference. The brightest star in Ophiuchus is Rasalhague (α Ophiuchi), a consisting of a giant (A5 III spectral type) and an orange dwarf companion, located about 48.6 light-years away and shining at an of 2.07. This rapidly rotating star marks the head of the serpent-bearer figure and is a key navigational point in the constellation. Following it in brightness is Cebalrai (β Ophiuchi), an orange giant (K2 III) at magnitude 2.75–2.77, situated 81.8 light-years distant and notable for its evolved stage, having expanded to over 12 times the Sun's . Another prominent member is Sabik (η Ophiuchi), a binary pair of main-sequence stars (A1 V and A3 V) with a combined magnitude of 2.43, orbiting each other every 87.58 years at a distance of 88 light-years. Beyond these luminaries, the list includes variable and high-proper-motion stars like (V2500 Ophiuchi), a (M4.0Ve) just 5.96 light-years away—the fourth-closest known star to the Sun—and renowned for its record-breaking of 10.3 arcseconds per year, making it appear to shift position rapidly across the sky. Other noteworthy entries encompass ζ Ophiuchi, a massive (O9.5 V) and Beta Cephei variable at magnitude 2.57, and red giants such as Yed Prior (δ Ophiuchi, M0.5 III, magnitude 2.75). These stars highlight Ophiuchus's diversity, from nearby neighbors to distant massive objects, and the constellation's list serves as a valuable resource for stargazers, researchers, and catalogers studying and dynamics.

Overview

Constellation Context

is a large constellation occupying an area of 948 square degrees, making it the 11th largest among the 88 modern constellations recognized by the (IAU). It lies along the in the southern sky, positioned between the constellations of to the south and to the north, with coordinates spanning from 17h 01.3m to 18h 44.3m and from +18° to -30.7°. The IAU formalized the boundaries of in 1930 under the direction of astronomer Eugène Delporte, who delineated them along lines of and ; this definition notably incorporates the division of the neighboring into Caput (head) and Cauda (tail) sections to accommodate 's central figure grasping the serpent. In , represents , the skilled healer and son of the god Apollo and the mortal Coronis, who was renowned for his ability to revive the dead using knowledge gained from observing serpents shed their skins. Depicted as a serpent-bearer, the constellation shows the figure holding the snake that forms , symbolizing themes of and renewal that led to Asclepius's eventual deification. This ancient imagery traces back to Ptolemy's 48 constellations in the 2nd century CE, though has roots in even earlier Mesopotamian and Egyptian sky lore. Ophiuchus is visible to observers at latitudes between +80° and -80°, with optimal viewing from the during July evenings when it reaches its highest point overhead. In the , it appears prominently during winter months and remains partially visible year-round from latitudes south of about 10°S. The region's dense stellar fields, including notable globular clusters such as M10 and M12, contribute to its richness as a target for astronomical observation.

Stellar Characteristics

The stars within the boundaries of predominantly originate from the galactic , given the constellation's position at low galactic latitudes near the plane. Their ages typically range from 1 to 10 billion years, a distribution consistent with the protracted history in the local galactic disk, as derived from kinematic and spectroscopic analyses of nearby F and G dwarfs. This age spread reflects multiple episodes of , with younger populations contributing to the observed diversity in evolutionary stages. Metallicity levels among these stars vary from near-solar to slightly subsolar, averaging around [Fe/H] ≈ -0.2, as measured in spectroscopic surveys of disk field stars in similar galactic directions. This mild depletion may arise from contributions by older, metal-poor components. Dominant spectral types among the brighter, more visible stars include A and F giants, which represent evolved, luminous members of the disk population; for instance, Rasalhague (α Ophiuchi) exemplifies an A5 III giant. In contrast, fainter stars, detectable in deeper surveys, are chiefly K and M dwarfs, comprising the bulk of the low-mass, long-lived component of the local disk. The evolutionary context of Ophiuchus stars encompasses main-sequence objects alongside post-main-sequence phases, such as giants in the K spectral range, positioning them across the Hertzsprung-Russell diagram in a manner that underscores the disk's bimodal history with peaks around 1-3 Gyr and 7-10 Gyr ago. Distances to principal stars generally fall between 50 and 200 light-years, based on measurements, while comprehensive surveys extend to populations up to 1,000 light-years, sampling a broader cross-section of the disk.

Principal Stars

Brightest Stars by Magnitude

The brightest stars in , with apparent visual magnitudes ranging from 2.07 to 3.5, are easily visible to the and form the constellation's prominent skeletal structure, often likened to a giant figure holding a serpent. These stars exhibit a variety of types, from hot O and types appearing blue-white to cooler and giants with orange or red hues, reflecting their evolutionary stages and temperatures. Observational prominence is enhanced by their positions near the , making them accessible from both hemispheres during summer months in the . Precise parameters, including and parallaxes, are provided by the DR3 catalog, which measured parallaxes with uncertainties typically below 1 mas for these bright objects. Absolute magnitudes, calculated as MV=mV+5−5log⁡10(d)M_V = m_V + 5 - 5\log_{10}(d) where dd is in parsecs, indicate their intrinsic luminosities relative to the Sun.
RankNameBayer DesignationApparent Magnitude (mVm_V)Absolute Magnitude (MVM_V)Spectral TypeDistance (ly)Parallax (mas)Observational Notes
1Rasalhagueα Oph2.071.21A5IVnn48.667.13 ± 1.06White subgiant; binary system; prominent naked-eye star with steady light.
2Sabikη Oph2.433.25A2IV-V88.436.91 ± 0.80White main-sequence binary; appears as a single point of light; multiple system.
3-ζ Oph2.57-3.09O9.2IVnn4407.41 ± 0.66Blue supergiant; rapid rotator; appears brilliant white-blue, high luminosity.
4Yed Priorδ Oph2.74-1.91M0.5III16020.41 ± 0.54Orange-red giant; variable brightness; forms "hand" with ε Oph.
5Cebalraiβ Oph2.770.41K2III83.239.23 ± 0.20Orange giant; steady light; marks the "head" of Ophiuchus.
6-κ Oph3.200.95K2III87.937.11 ± 0.20Orange giant; long-period variable candidate; faint orange hue visible in binoculars.
7Yed Posteriorε Oph3.24-0.30G9.5IIIbFe-0.5106.930.51 ± 0.20Yellow giant; binary; pairs with δ Oph to form "left hand."
8-θ Oph3.270.84A0V10928.96 ± 0.25White main-sequence; steady; part of the "body" pattern.
9-ν Oph3.33-0.78B9.5V7442.5 ± 0.3Blue-white dwarf; appears as a sharp point; near the "foot."
10-72 Oph3.734.82K0V74.244.18 ± ?Orange dwarf; steady light; contributes to constellation pattern.
The table continues with additional stars up to magnitude 3.5, such as γ Oph (3.75, A0V, 103 ly, white main-sequence star), ι Oph (3.41, K0III, 98 ly, orange giant), μ Oph (4.21, but borderline for principal), and others like 19 Oph (3.22, F8V, 145 ly, yellow-white), all contributing to the constellation's visibility and used historically for . These stars' parallaxes from DR3 enable accurate distance determinations, with typical errors under 1% for the nearest ones, highlighting Ophiuchus's mix of nearby giants and more distant hot stars.

Bayer-Designated Stars

The Bayer designations for stars in originate from 's 1603 star atlas Uranometria, where he systematically assigned Greek letters from α to ω to the constellation's brighter members, primarily ordered by apparent visual magnitude as observed from northern latitudes. This convention facilitated precise identification of s for navigation and cataloging, building on earlier Ptolemaic traditions. The (IAU) has formalized proper names for select stars, drawing from , Persian, and other historical sources to preserve cultural significance while standardizing nomenclature globally. The table below catalogs all Bayer-designated stars in , arranged alphabetically by Greek letter. It includes the IAU-approved proper name (if assigned), Flamsteed number (where applicable), and equatorial coordinates ( in hours:minutes:seconds and in degrees:arcminutes:arcseconds for J2000.0). Coordinates are derived from the and cross-verified astronomical databases.
Bayer SymbolProper Name (IAU-approved)Flamsteed NumberRA (J2000.0)Dec (J2000.0)
α OphRasalhague6717:34:56+12:33:36
β OphCebalrai5417:43:28+04:34:02
γ OphBake-eo6217:59:40+02:41:47
δ OphYed Prior3616:14:21-03:41:39
ε OphYed Posterior3716:18:25-04:35:12
ζ Oph-4816:37:10-10:34:02
η OphSabik2817:10:22-15:43:29
θ Oph-4317:22:27-25:00:23
ι Oph-2917:00:36+10:17:29
κ Oph-3117:02:24+09:21:34
λ OphMarfik4117:30:43+01:04:54
μ Oph-5817:38:20-08:07:31
ν Oph-6518:05:31-09:49:41
ξ Oph-4017:14:24-22:54:07
ο Oph-3417:31:09-24:14:42
π Oph-4917:26:24+04:08:24
ρ Oph-616:25:35-23:26:39
σ Oph-1116:54:04-21:46:30
τ Oph-7018:04:52-08:18:08
υ Oph-1416:35:08-18:35:06
φ Oph-816:31:08-16:36:46
χ Oph-2016:57:49-18:35:23
ψ Oph-1516:11:45-20:32:39
ω Oph-1916:31:25-18:34:53

Variable Stars

Long-Period Variables

Long-period variables (LPVs) in Ophiuchus are primarily cool, evolved giants and supergiants that exhibit pulsational variability on timescales exceeding 100 days, often associated with the asymptotic giant branch (AGB) phase of stellar evolution. These stars, including Mira types and semiregular variables, display radial pulsations driven by opacity changes in their outer layers, leading to significant brightness variations observable from Earth. In Ophiuchus, notable examples include R Oph, a classic Mira variable with a pulsation period of approximately 310 days, during which its visual magnitude fluctuates from about 7.0 at maximum to ~13.0, and a spectral type of M5-7e; this star lies at a distance of roughly 1,730 light-years (Gaia DR3 parallax 1.886 mas, as of 2023). Another prominent LPV is S Oph, classified as a Mira variable with a period around 233 days, showing amplitude changes from visual magnitudes ~9.6 to ~13.5 and a spectral type of M5+e, located approximately 6,200 light-years away (Gaia DR3 parallax 0.524 mas, as of 2023). T Oph, also a Mira-type LPV, has a longer period of about 372 days, with magnitude variations from ~10.4 to ~14.5 and a spectral type of M6.5e, located approximately 2,670 light-years away (Gaia DR3 parallax 1.223 mas, as of 2023). The pulsations in these stars arise from radial expansions and contractions triggered by the ionization of helium in a partial ionization zone beneath the photosphere, where increased opacity during compression traps heat and drives the cycle. This mechanism, known as the kappa mechanism, leads to periodic luminosity changes that follow a period-luminosity (P-L) relation for Mira variables, empirically expressed as Mbol≈−3.3log⁡P+CM_{\rm bol} \approx -3.3 \log P + C, where PP is the pulsation period in days and CC is a constant depending on the calibration (typically around 2.8 for Galactic Miras in bolometric magnitudes). For Ophiuchus LPVs like R Oph and T Oph, this relation implies luminosities consistent with AGB stars, with periods correlating to brighter absolute magnitudes for longer cycles. Amplitude ranges for Ophiuchus LPVs vary widely, with Miras like R Oph and T Oph showing large variations of 4-6 magnitudes in visual light due to their extended atmospheres, while variables such as S Oph exhibit ~4 mag swings. Spectral changes accompany these cycles, particularly in cooler phases when molecular bands like TiO strengthen, causing the star to appear redder and fainter as the atmosphere expands and cools to temperatures below 3,000 K. The American Association of Variable Star Observers (AAVSO) maintains extensive monitoring programs for these stars, compiling visual and photometric data spanning decades to track cycle timings, amplitudes, and any deviations that may indicate mass loss or binary interactions. For instance, AAVSO light curves of R Oph reveal consistent 310-day cycles with occasional cycle-to-cycle variations of up to 20 days, aiding in refined P-L calibrations and evolutionary studies.

Pulsating Variables

Pulsating variables in Ophiuchus encompass short-period stars that exhibit radial and non-radial oscillations, primarily δ Scuti types in the of the Hertzsprung-Russell diagram and RR Lyrae types on the . These stars, with periods typically under one day, provide insights into stellar interiors and serve as probes for galactic structure. δ Scuti variables are main-sequence or stars of I, pulsating due to the mechanism, where opacity variations in the outer helium ionization zones drive energy blocking and release, leading to periodic expansion and contraction. In contrast, RR Lyrae stars represent evolved, low-mass II objects that have undergone a at the tip of the , transitioning to the where core helium burning sustains their luminosity while they pulsate in the . A representative δ Scuti star in Ophiuchus is V567 Oph, which pulsates with a primary period of 0.1495 days and a visual magnitude range of 11.02 to 11.47, classified as type G5 at a distance of approximately 3,500 light-years. For RR Lyrae examples, V530 Oph is an RRab subtype with a period of 0.666 days, varying in the G band from 13.36 to 14.09 magnitude (corresponding to roughly V ~13.5-14.2), located about 13,200 light-years away in a field near globular clusters like M10. RR Lyrae light curves are analyzed using the Bailey diagram, which plots period against amplitude to distinguish subtypes: RRab stars show asymmetric profiles with longer periods (~0.5-1 day) and higher amplitudes, while RRc subtypes have shorter periods (~0.2-0.5 days) and more symmetric shapes, reflecting fundamental versus first-overtone pulsations. Fourier decomposition of these curves yields parameters like the phase differences φ_{21} and φ_{31}, which quantify light curve asymmetry and correlate with , aiding in classifying evolutionary stages and chemical compositions. These stars function as standard candles through their , particularly for RR Lyrae in Population II environments, where absolute magnitudes near M_V ≈ 0.5 enable precise distance estimates to globular clusters and the , with minimal dependence on for calibrated relations.

Nearby and High-Motion Stars

Closest Stars to

The closest stars to in the constellation lie within 20 parsecs, providing key insights into the local stellar neighborhood dominated by low-mass dwarfs and binary systems. These proximity allows precise measurements via , revealing their roles in understanding Galactic and in the solar vicinity. stands out as the nearest individual star in , followed by the binary systems and 36 Ophiuchi, all characterized by modest luminosities and masses ranging from 0.1 to 1 solar masses (M⊙).
Star NameDistance (pc)Parallax (mas)Spectral TypeApparent MagnitudeApproximate Mass (M⊙)
(V2500 Oph, HD 173416)1.83 ± 0.01M4V
(HD 155358)5.11 ± 0.01G1V + K7V (binary)
36 Ophiuchi (HD 147513)5.95 ± 0.01K1V + K2V + M0V (triple)
Barnard's Star, the fourth-nearest known star to the Sun overall, is a prototypical low-mass with a radius about 20% of the Sun's and an of approximately 3,100 K, making it one of the faintest visible to amateur telescopes. Its , measured by the mission (DR3), confirms its exceptional proximity, enabling detailed studies of flare activity and magnetic fields typical of M dwarfs. This star exhibits a high space velocity of over 140 km/s relative to the Sun, indicative of its halo population origins and rapid transit through the disk. The binary system consists of a primary G1V dwarf similar in mass and temperature to the young Sun (around 5,900 K) orbiting a cooler K7V companion with a period of 88 years and semi-major axis of about 12 AU. refines their shared , highlighting the system's stability and potential for stable orbital zones around each component, where temperatures could support liquid water on hypothetical . With a combined roughly 1.5 times solar, it represents a common G-K binary archetype in the local census. Farther out, the 36 Ophiuchi triple system features a wide K1V + K2V binary pair (period ~471 years, semi-major axis ~82 AU) with a distant M0V companion at ~15,700 AU, all sharing a common and per DR3 data. The binary has masses and luminosities (0.4-0.8 solar each) conducive to habitable zones spanning 0.5-2 AU, influenced by their eccentric orbits (e=0.64). This configuration exemplifies multiple systems prevalent among nearby K dwarfs, with space velocities around 50 km/s suggesting thin-disk membership. These stars collectively underscore the prevalence of low-mass, metal-rich objects in Ophiuchus's local volume, with masses below 1 M⊙ dominating due to the initial mass function's peak at ~0.3 M⊙. Their high space velocities (40-140 km/s) relative to the local standard of rest imply diverse kinematic histories, from disk populations to possible halo interlopers like , aiding calibrations of stellar age and distributions in the solar neighborhood.

Stars with High Proper Motion

Stars in exhibiting high , defined here as greater than 1 arcsecond per year relative to the solar neighborhood, are predominantly low-mass M-type dwarfs belonging to the old disk population of the . These stars provide valuable insights into the dynamics of nearby , as their rapid apparent motion across the sky stems from their proximity and significant tangential velocities. from the DR3 catalog reveal components (μ_α and μ_δ) for such objects, with the total proper motion calculated as μ = √(μ_α² + μ_δ²). A quintessential example is (Gliese 699, V2500 Ophiuchi), an located approximately 1.83 parsecs from the Sun. Its DR3 proper motion components are μ_α = -801.551 mas/yr and μ_δ = 10362.394 mas/yr, yielding a total μ ≈ 10.39 arcsec/yr—the highest known for any star. This motion corresponds to a tangential v_t ≈ 90 km/s, computed via v_t = 4.74 × μ × d (with μ in arcsec/yr and d in pc), and a total space of approximately 142 km/s when combined with its of -110 km/s. Barnard's Star's kinematics align with the old thin-disk population, characterized by moderate velocities indicative of long-term orbital stability in the Galaxy's disk rather than membership in younger streams like the Hercules group. These high-proper-motion stars in , including , are typically ancient (ages exceeding several billion years) and show signs of depletion in their atmospheres, a hallmark of low-mass dwarfs that have undergone significant convective mixing over time. Their depleted abundances (often A(Li) < 1.0 dex) reflect evolutionary processes in metal-poor, cool stars, contrasting with lithium-rich younger populations. Such objects trace the solar neighborhood's dynamical history, with space velocities suggesting origins in the Galactic disk's early formation phases.

Exoplanet-Hosting Stars

Confirmed Planetary Systems

Ophiuchus hosts several stars with confirmed exoplanetary systems, primarily detected through (RV) and transit methods, providing insights into diverse architectures from compact multi-planet setups around cool dwarfs to wide-orbit giants around solar analogs. These systems span a range of host star types, including red dwarfs with short-period terrestrial worlds and G-type stars with massive companions, often exhibiting metallicities [Fe/H] around solar or slightly enhanced, which influences planet formation efficiency in RV surveys. Ages of these hosts typically range from 5 to 10 billion years, allowing for mature system evolution observable today. One of the most prominent systems is that around (Gliese 699), an M3.5V located 5.96 light-years away, the closest single star to the Sun. In March 2025, observations with the MAROON-X spectrograph on Gemini North and on the confirmed four sub-Earth rocky planets: Barnard's Star b (period 3.15 days, mass ~0.4 masses, semi-major axis 0.015 AU), c (4.12 days, ~0.5 M⊕, 0.019 AU), d (2.34 days, ~0.3 M⊕, 0.012 AU), and e (6.74 days, ~0.6 M⊕, 0.030 AU). All orbit interior to the , with low eccentricities (<0.1) and minimum masses derived from RV semi-amplitudes K on the order of 0.5–1 m/s; the system architecture suggests a resonant chain formed via disk migration. This RV detection, building on decades of searches since a disputed 1963 claim, highlights the challenges of detecting low-mass planets around active M dwarfs but confirms a compact, dynamically stable configuration. Another notable system orbits GJ 1214, an M4.5V 48 light-years distant with super-solar [Fe/H] = +0.25 and an age estimated at 6–10 Gyr. The confirmed planet, , is a (radius 2.7 radii, mass 8.2 M⊕, period 1.58 days, semi-major axis 0.014 AU, eccentricity ~0) detected via transits by the MEarth array in 2009, marking one of the first super-Earths found. Transmission spectroscopy with Hubble and JWST has revealed a hazy hydrogen-helium atmosphere rich in , potentially comprising up to 50% by mass, distinguishing it as a key example of a "ocean world" or high-metallicity gas envelope. The RV follow-up yielded a precise mass, with semi-amplitude K ≈ 13 m/s, confirming no additional close-in companions. Additional confirmed systems include the three-planet setup around Wolf 1061 (GJ 628), an M3V star 14 light-years away discovered via RV in 2015 with HARPS, featuring Wolf 1061 b (1.36 M⊕, 4.89 days), c (3.98 M⊕, 17.87 days, habitable zone candidate), and d (5.72 M⊕, 217 days); and GJ 3998 (M3V, 58 light-years), with three short-period planets (b: 1.1 M⊕, 2.65 days; c: 2.3 M⊕, 13.73 days; d: ~4 M⊕, 41.78 days) confirmed by TESS transits and RV in 2023. These underscore Ophiuchus's role in probing terrestrial planet demographics around nearby M dwarfs. The general RV detection formula, K = (28.4 m/s) (P/1 yr)^{-1/2} (m sin i / M_J) (M_*/M_⊙)^{-2/3} (1 - e^2)^{-1/2}, illustrates the sensitivity to planet mass and period in these surveys.
StarSpectral TypeDistance (ly)PlanetsDetection MethodKey Architecture Notes
M3.5V5.964 (all <1 M⊕, P<7 days)RV (2025)Compact rocky chain, inner orbits
GJ 1214M4.5V481 (, P=1.58 d)Transit (2009)Hazy atmosphere, water-rich
M3V143 (terrestrials, P=4.9–217 d)RV (2015)HZ candidate at c
GJ 3998M3V583 (super-Earths, P=2.7–42 d)Transit+RV (2023)Multi-transiting, close-in

Candidate Systems

Several stars in the constellation host candidates identified through transit surveys, particularly from NASA's extension of the Kepler mission and the (TESS). These candidates represent tentative detections requiring further validation via measurements, imaging, or to rule out false positives such as eclipsing binaries. The transit method detects periodic dips in stellar brightness caused by a passing in front of its host , with the depth of the transit δ=(Rp/R∗)2\delta = (R_p / R_*)^2 providing an estimate of the planet-to-star radius ratio, where RpR_p is the radius and R∗R_* is the stellar radius. Vetting processes assess false positive rates through techniques like centroid shifts, which check if the transit signal originates from the target or a background source, typically achieving false positive probabilities below 1% for high-confidence candidates. The Kepler mission's primary field focused on the northern sky in Cygnus and , with limited direct overlap into , but the K2 mission's repointed campaigns (e.g., Campaigns 2–19) covered southern and equatorial fields, including portions of for targeted searches of cool dwarfs. Similarly, TESS's all-sky survey, conducted in 26 sectors per year, includes coverage of in sectors 14–15 during its southern hemisphere observations, enabling detection of brighter, nearby hosts amenable to ground-based follow-up. These candidates hold implications for understanding planetary formation around cool stars, where habitable zones lie closer to the host, potentially allowing Earth-sized worlds to receive insolation similar to Earth's. Future confirmations could leverage the (JWST) for transmission spectroscopy, probing atmospheric compositions for biosignatures or volatile content in these systems.

Other Notable Stars

Multiple Systems

Ophiuchus hosts several hierarchical multiple star systems, ranging from visual binaries resolvable with moderate telescopes to more complex triples identified through . These systems provide insights into stellar formation and evolution, with orbital parameters often determined via speckle and measurements. For instance, is a nearby visual binary consisting of a K0V primary and K5V secondary, with an of 88.38 years, semi-major axis of 4.526 arcseconds, and eccentricity of 0.5005. The system's masses are approximately 0.89 M⊙ for the primary and 0.73 M⊙ for the secondary, yielding a of about 1.22, and its proximity at roughly 16.6 light-years underscores its value for detailed study. Another prominent example is 36 Ophiuchi, a wide visual binary with a K1.5 primary and K secondary separated by about 5 arcseconds (corresponding to a mean physical of 82.3 AU at a of 19.3 light-years), orbiting with a period of 471 years. A more distant K5 companion (36 Ophiuchi C) orbits the A-B pair at approximately 732 arcseconds, with an estimated period exceeding 180,000 years, forming a hierarchical triple. Theta Ophiuchi represents a triple system with a B2 primary and companions, resolved through observations that reveal an inner binary , though precise orbital periods for the inner pair remain under refinement from ongoing speckle data. Visual orbits for such systems in , including semi-major axis a in arcseconds, inclination i, and eccentricity e, are frequently derived from speckle , enabling precise tracking of relative positions over decades. The dynamical stability of these hierarchical multiples is evaluated using the Hill radius, which approximates the region of gravitational influence around a companion; stable configurations typically require outer separations exceeding 3–5 times the Hill radius of the inner subsystem to prevent perturbations leading to ejection. Physical association in wider systems is confirmed through common , where components share similar tangential velocities across the sky, distinguishing bound pairs from chance alignments. In the Rho Ophiuchi cloud, a prolific star-forming region, numerous pre-main-sequence binaries exhibit separations of 90–250 AU, with orbital dynamics reflecting early fragmentation processes during collapse. These young systems, often triples, highlight evolutionary stages from protostellar disks to main-sequence companions, with surveys tabulating over a dozen such multiples to assess binary fractions around 25–30% in this environment.

Spectroscopically Interesting Stars

Stars in the constellation exhibit a range of spectroscopic peculiarities, including rapid rotation and chemical abundance anomalies that deviate from standard main-sequence compositions. These features provide insights into , atmospheric processes, and mixing mechanisms. Notable examples include rapidly rotating O-type stars with enhanced surface abundances and chemically peculiar B-type stars showing overabundances of heavy elements like mercury and . ζ Ophiuchi (HD 149757), classified as an O9.5 Vnn star, is a prominent rapid rotator with a projected rotational velocity of v sin i ≥ 340 km/s, leading to significant in its spectral lines. This broadening affects the profiles of and lines, complicating abundance determinations but revealing surface enhancements in due to rotational mixing during its . The abundance is elevated compared to solar values, consistent with models of massive star where transports processed material to the surface. Spectral analyses using high-resolution and optical data show equivalent widths for N III and N IV lines that exceed expectations for non-rotating O stars, highlighting the role of in altering photospheric compositions. Another example is μ Ophiuchi, a B9.5 Vp Mn star with an apparent magnitude of 4.62, classified as a mercury-manganese (HgMn) chemically peculiar object. Its spectrum displays strong absorption lines from singly ionized mercury (Hg II) at wavelengths such as 3984 Å and manganese (Mn II) around 4783 Å, with equivalent widths indicating overabundances by factors of 100 to 1000 relative to solar abundances. These anomalies arise from atomic processes, where radiative acceleration on heavy ions like Hg and Mn counteracts gravitational settling, leading to vertical separation of elements in the stable atmospheres of main-sequence B stars. Diffusion models predict such stratification, with radiative forces separating lighter elements downward while heavier ones accumulate near the surface. In addition to abundance anomalies, spectroscopic peculiarities in Ophiuchus stars often involve magnetic effects observable in cooler types. For instance, Am and Fm stars, which exhibit enhanced metallic lines due to diffusion in their atmospheres, can show Zeeman splitting in spectral lines when are present, with splitting widths proportional to field strength via the relation Δλ = 4.67 × 10^{-13} g λ² B, where g is the Landé factor, λ the in Å, and B the field in gauss. These fields, typically 100–1000 G, influence diffusion by confining plasma and altering element transport. Studies of such stars probe stellar interiors, revealing how diffusion and magnetic braking regulate and chemical homogeneity. Overall, these objects serve as natural laboratories for testing theories of radiative levitation and rotational dynamics, contributing to our understanding of upper main-sequence .

References

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