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

Name B F Var HD HIP RA Dec vis.
mag. 		abs.
mag. 		Dist. (ly) Sp. class Notes
Rigel β 19 34085 24436 05h 14m 32.27s −08° 12′ 05.9″ 0.18 −6.69 773 B8Ia + B9V + B9V 7th brightest star, triple star system; α Cyg variable
Betelgeuse α 58 39801 27989 05h 55m 10.29s +07° 24′ 25.3″ 0.42 −6.02 643 M2Ib 9th brightest star on average, semiregular variable, Vmax = 0m, Vmin = 1.3m, P = 2335 d
Bellatrix γ 24 35468 25336 05h 25m 07.87s +06° 20′ 59.0″ 1.64 −2.72 243 B2III suspected variable
Alnilam ε 46 37128 26311 05h 36m 12.81s −01° 12′ 06.9″ 1.69 −6.38 1342 B0Ia α Cyg variable, α Cyg variable, Vmax = 1.64m, Vmin = 1.74m
Alnitak A ζ 50 37742 26727 05h 40m 45.52s −01° 56′ 33.3″ 1.88 -6.0 817 O9.7Ib component of the Alnitak system; suspected variable
Saiph κ 53 38771 27366 05h 47m 45.39s −09° 40′ 10.6″ 2.07 −4.65 721 B0.5Ia suspected variable
Mintaka AB δ 34 36486 25930 05h 32m 00.40s −00° 17′ 56.7″ 2.20 -5.8 916 B0III+O9V component of the Mintaka system; Algol variable, Vmax = 2.20m, Vmin = 2.32m, P = 5.73 d
ι Ori ι 44 37043 26241 05h 35m 25.98s −05° 54′ 35.6″ 2.75 −5.30 1325 O9III Hatysa
π3 Ori π3 1 30652 22449 04h 49m 50.14s +06° 57′ 40.5″ 3.19 -3.67 26 F6V Tabit; suspected variable
η Ori η 28 35411 25281 05h 24m 28.62s −02° 23′ 49.7″ 3.35 −3.86 901 B1V + B2 Saif al Jabbar, Saiph; β Cep variable, Vmax = 3.31m, Vmin = 3.6m, P = 7.99 d
Meissa A λ 39 36861 26207 05h 35m 08.28s +09° 56′ 03.0″ 3.47 -4.25 1055 O8III component of the Meissa system; suspected variable
τ Ori τ 20 34503 24674 05h 17m 36.40s −06° 50′ 39.8″ 3.59 −2.56 554 B5III
π4 Ori π4 3 30836 22549 04h 51m 12.37s +05° 36′ 18.4″ 3.68 −4.25 1259 B2III variable star, ΔV = 0.003m, P = 1.60 d
Alnitak B ζ 50 37743 26727 05h 40m 45.60s −01° 56′ 34.0″ 3.70 -3.29 817 B0III+B1IV component of the Alnitak system
π5 Ori π5 8 31237 22797 04h 54m 15.10s +02° 26′ 26.4″ 3.71 −4.36 1342 B2III rotating ellipsoidal variable, Vmax = 3.66m, Vmin = 3.73m, P = 3.70 d
σ Ori AB σ 48 37468 26549 05h 38m 44.77s −02° 36′ 00.2″ 3.77 −3.96 1148 O9.5V component of the σ Ori system; spectroscopic binary; suspected variable
ο2 Ori ο2 9 31421 22957 04h 56m 22.32s +13° 30′ 52.5″ 4.06 0.48 169 K2III
φ2 Ori φ2 40 37160 26366 05h 36m 54.33s +09° 17′ 29.1″ 4.09 1.33 116 G8III-IV
μ Ori μ 61 40932 28614 06h 02m 22.99s +09° 38′ 50.5″ 4.12 0.78 152 Am... suspected eclipsing binary
29 Ori e 29 35369 25247 05h 23m 56.84s −07° 48′ 28.6″ 4.13 0.49 174 G8III
32 Ori A 32 36267 25813 05h 30m 47.05s +05° 56′ 53.6″ 4.20 −0.53 288 B5V
π2 Ori π2 2 30739 22509 04h 50m 36.72s +08° 54′ 00.9″ 4.35 0.48 194 A1Vn
φ1 Ori φ1 37 36822 26176 05h 34m 49.24s +09° 29′ 22.5″ 4.39 −3.01 985 B0IV...
χ1 Ori χ1 54 39587 27913 05h 54m 23.08s +20° 16′ 35.1″ 4.39 4.67 28 G0V RS CVn variable, Vmax = 4.38m, Vmin = 4.41m
ν Ori ν 67 41753 29038 06h 07m 34.32s +14° 46′ 06.7″ 4.42 −1.65 534 B3IV variable star, ΔV = 0.008m, P = 1.04 d
ξ Ori ξ 70 42560 29426 06h 11m 56.40s +14° 12′ 31.7″ 4.45 −2.00 634 B3IV
ρ Ori ρ 17 33856 24331 05h 13m 17.48s +02° 51′ 40.5″ 4.46 −0.65 344 K3III... suspected variable
π6 Ori π6 10 31767 23123 04h 58m 32.90s +01° 42′ 50.5″ 4.47 −2.86 953 K2IIvar suspected variable
ω Ori ω 47 37490 26594 05h 39m 11.15s +04° 07′ 17.3″ 4.50 −3.98 1622 B3IIIe γ Cas variable, Vmax = 4.4m, Vmin = 4.59m
HD 40657 40657 28413 06h 00m 03.35s −03° 04′ 26.7″ 4.53 −1.02 420 K2IIIvar suspected variable
42 Ori c 42 37018 26237 05h 35m 23.16s −04° 50′ 18.0″ 4.58 −2.33 786 B2III... suspected variable
ψ2 Ori ψ2 30 35715 25473 05h 26m 50.23s +03° 05′ 44.4″ 4.59 −3.60 1417 B2IV ellipsoidal variable and possible eclipsing binary, Vmax = 4.55m, Vmin = 4.61m, P = 2.53 d
υ Ori υ 36 36512 25923 05h 31m 55.86s −07° 18′ 05.5″ 4.62 −3.76 1545 B0V Thabit; suspected β Cep variable
π1 Ori π1 7 31295 22845 04h 54m 53.70s +10° 09′ 04.1″ 4.64 1.80 121 A0V
χ2 Ori χ2 62 41117 28716 06h 03m 55.18s +20° 08′ 18.5″ 4.64 -7.6 1801 B2Ia α Cyg variable
11 Ori 11 V1032 32549 23607 05h 04m 34.14s +15° 24′ 15.1″ 4.65 −0.79 400 A0p Si α2 CVn variable, Vmax = 4.65m, Vmin = 4.69m, P = 4.64 d
ο1 Ori ο1 4 30959 22667 04h 52m 31.96s +14° 15′ 02.8″ 4.71 −1.39 542 M3Sv semiregular variable, Vmax = 4.65m, Vmin = 4.88m, P = 30 d
31 Ori 31 CI 36167 25737 05h 29m 43.98s −01° 05′ 31.8″ 4.71 −1.02 456 K5III semiregular variable, Vmax = 4.68m, Vmin = 4.72m, P = 141 d
22 Ori o 22 35039 25044 05h 21m 45.75s −00° 22′ 56.9″ 4.72 −3.26 1289 B2IV-V suspected β Cep variable
56 Ori 56 39400 27750 05h 52m 26.44s +01° 51′ 18.6″ 4.76 −2.91 1113 K2IIvar suspected variable
49 Ori d 49 37507 26563 05h 38m 53.09s −07° 12′ 45.8″ 4.77 1.41 153 A4V
HD 36960 36960 26199 05h 35m 02.68s −06° 00′ 07.3″ 4.78 −4.00 1863 B0.5V suspected variable
15 Ori 15 33276 24010 05h 09m 41.96s +15° 35′ 50.2″ 4.81 −0.14 318 F2IV
ψ1 Ori ψ1 25 V1086 35439 25302 05h 24m 44.83s +01° 50′ 47.2″ 4.89 −2.77 1109 B1V:pe γ Cas variable, Vmax = 4.76m, Vmin = 4.96m
51 Ori b 51 37984 26885 05h 42m 28.66s +01° 28′ 28.8″ 4.90 0.07 302 K1III
HD 44131 44131 30093 06h 19m 59.60s −02° 56′ 40.2″ 4.91 −1.05 506 M1III variable star, ΔV = 0.011m, P = 8.92 d
HD 37756 37756 26736 05h 40m 50.72s −01° 07′ 43.6″ 4.95 −4.08 2090 B2IV-V suspected eclipsing binary
69 Ori f1 69 42545 29434 06h 12m 03.28s +16° 07′ 49.6″ 4.95 −1.93 774 B5Vn
θ2 Ori A θ2 43 37041 26235 05h 35m 22.90s −05° 24′ 57.8″ 4.98 −3.84 1895 O9.5Vpe component of the θ2 Ori system; suspected variable
23 Ori m 23 35149 25142 05h 22m 50.00s +03° 32′ 40.0″ 5.00 −2.35 962 B1V suspected variable
74 Ori k 74 43386 29800 06h 16m 26.57s +12° 16′ 18.2″ 5.04 3.58 64 F5IV-V
27 Ori p 27 35410 25282 05h 24m 28.91s −00° 53′ 30.0″ 5.07 1.46 172 K0III suspected variable
θ1 Ori C θ1 C 41 37022 26221 05h 35m 16.47s −05° 23′ 22.9″ 5.13 -4.9 1600 O6Vpe component of the Trapezium; triple star system; suspected variable
64 Ori 64 41040 28691 06h 03m 27.36s +19° 41′ 26.2″ 5.14 −2.44 1069 B8V suspected variable
6 Ori g 6 31283 22833 04h 54m 46.91s +11° 25′ 33.5″ 5.18 0.84 241 A3V suspected variable
HD 33554 33554 24197 05h 11m 41.56s +16° 02′ 44.4″ 5.18 0.21 321 K5III
71 Ori 71 43042 29650 06h 14m 50.94s +19° 09′ 24.8″ 5.20 3.58 69 F6V
60 Ori 60 40446 28296 05h 58m 49.58s +00° 33′ 10.7″ 5.21 −0.05 367 A1Vs suspected variable
45 Ori 45 37077 26268 05h 35m 39.49s −04° 51′ 21.9″ 5.24 −0.04 370 F0III
52 Ori 52 38710 27386 05h 48m 00.23s +06° 27′ 15.2″ 5.26 −0.58 479 A5V
38 Ori n2 38 36777 26126 05h 34m 16.79s +03° 46′ 01.0″ 5.32 0.20 345 A2V
5 Ori 5 31139 22730 04h 53m 22.76s +02° 30′ 29.8″ 5.33 −1.13 638 M1III suspected variable
HD 31296 31296 22834 04h 54m 47.79s +07° 46′ 45.0″ 5.33 −0.33 441 K1III
14 Ori i 14 33054 23879 05h 07m 52.87s +08° 29′ 54.9″ 5.33 1.46 194 Am
21 Ori 21 34658 24817 05h 19m 11.23s +02° 35′ 45.4″ 5.34 1.42 198 F5IIvar
HD 36591 36591 25980 05h 32m 41.35s −01° 35′ 30.6″ 5.34 −4.14 2567 B1IV suspected variable
72 Ori f2 72 43153 29704 06h 15m 25.13s +16° 08′ 35.5″ 5.34 −0.50 479 B7V
HD 30210 30210 22157 04h 46m 01.70s +11° 42′ 20.2″ 5.35 0.79 266 Am...
VV Ori VV 36695 26063 05h 33m 31.45s −01° 09′ 21.9″ 5.36 −3.41 1852 B1V Algol variable, Vmax = 5.31m, Vmin = 5.66m, P = 1.49 d
55 Ori 55 39291 27658 05h 51m 21.98s −07° 31′ 04.8″ 5.36 −3.20 1680 B2IV-V suspected variable
HD 30034 30034 22044 04h 44m 25.77s +11° 08′ 46.2″ 5.39 1.97 157 F0V
75 Ori l 75 43525 29850 06h 17m 06.62s +09° 56′ 33.1″ 5.39 0.93 254 A2V
U Ori U 39816 28041 05h 55m 49.30s +20° 10′ 30.0″ 5.40 1420 M8III Mira variable, Vmax = 4.8m, Vmin = 13m, P = 377 d
16 Ori h 16 33254 23983 05h 09m 19.60s +09° 49′ 46.6″ 5.43 1.77 176 A2m suspected variable
73 Ori 73 43247 29736 06h 15m 44.97s +12° 33′ 03.9″ 5.44 −2.72 1399 B9II-III
33 Ori n1 33 36351 25861 05h 31m 14.53s +03° 17′ 31.7″ 5.46 −2.95 1567 B1.5V
HD 34043 34043 24450 05h 14m 44.05s +05° 09′ 22.1″ 5.50 −0.82 598 K4III suspected variable
18 Ori 18 34203 24555 05h 16m 04.14s +11° 20′ 28.9″ 5.52 0.26 368 A0V
HD 35536 35536 25329 05h 25m 01.74s −10° 19′ 43.8″ 5.60 −0.85 635 K5III
35 Ori 35 36653 26093 05h 33m 54.29s +14° 18′ 20.1″ 5.60 −0.39 513 B3V
HD 36881 36881 26215 05h 35m 13.24s +10° 14′ 24.4″ 5.60 −2.66 1462 B9IIIMNp...
Meissa B λ 39 36862 26207 05h 35m 08.50s +09° 56′ 06.0″ 5.61 -1.94 1055 B0.5V component of the Meissa system
HD 43318 43318 29716 06h 15m 34.36s −00° 30′ 42.0″ 5.62 2.86 116 F6V
66 Ori 66 41380 28814 06h 04m 58.36s +04° 09′ 31.2″ 5.63 −3.78 2489 G4III
HD 36959 36959 26197 05h 35m 01.01s −06° 00′ 33.4″ 5.67 2694 B1Vvar suspected variable
63 Ori 63 41361 28812 06h 04m 58.19s +05° 25′ 11.9″ 5.67 −1.97 1101 G7III:
HD 44033 44033 30099 06h 20m 04.23s +14° 39′ 04.2″ 5.67 −0.46 548 K3Ib suspected variable
HD 35007 35007 25028 05h 21m 31.84s −00° 24′ 59.4″ 5.68 −1.91 1076 B3V
HD 35299 35299 25223 05h 23m 42.31s −00° 09′ 35.3″ 5.69 −1.28 809 B1.5V suspected variable
HD 40369 40369 28302 05h 58m 53.24s +12° 48′ 29.7″ 5.70 −1.35 838 K2III...
HD 42111 42111 29151 06h 08m 57.90s +02° 29′ 59.0″ 5.70 −0.66 609 A3Vn
HD 43587 43587 29860 06h 17m 16.25s +05° 05′ 58.9″ 5.70 4.27 63 G0.5Vb
HD 37209 37209 26345 05h 36m 35.69s −06° 03′ 53.1″ 5.71 −3.14 1918 B1V... suspected variable
68 Ori 68 42509 29433 06h 12m 01.34s +19° 47′ 26.1″ 5.76 −1.61 970 B9.5V
HD 36166 36166 25751 05h 29m 54.77s +01° 47′ 21.3″ 5.77 −2.16 1254 B2V
HD 34989 34989 25041 05h 21m 43.56s +08° 25′ 42.8″ 5.78 −0.99 736 B1V...
HD 38527 38527 27280 05h 46m 52.15s +09° 31′ 21.0″ 5.78 0.96 300 G8III
HD 31373 31373 22913 04h 55m 50.16s +15° 02′ 25.1″ 5.79 0.23 423 B9V
HD 39007 39007 27549 05h 50m 02.68s +09° 52′ 16.4″ 5.79 0.74 334 G8III
HD 36134 36134 25708 05h 29m 23.70s −03° 26′ 46.9″ 5.80 0.02 467 K1III... suspected variable
HD 43023 43023 29575 06h 13m 54.24s −03° 44′ 29.1″ 5.83 0.91 315 G8III
HD 42954 42954 29616 06h 14m 28.58s +17° 54′ 23.0″ 5.86 0.15 452 A6m
HD 37320 37320 26487 05h 38m 01.11s +07° 32′ 29.2″ 5.87 −0.29 556 B8III
HD 39910 39910 28011 05h 55m 30.16s −04° 36′ 59.4″ 5.87 1.02 304 K2III:
HD 33646 33646 24203 05h 11m 45.35s +01° 02′ 13.4″ 5.88 −1.36 916 F5
HD 33608 33608 24162 05h 11m 19.13s −02° 29′ 26.8″ 5.89 2.97 125 F5V
HD 40020 40020 28139 05h 56m 49.39s +11° 31′ 16.3″ 5.89 1.02 307 K2III
59 Ori 59 V1004 40372 28271 05h 58m 24.44s +01° 50′ 13.7″ 5.89 0.72 353 A5me δ Sct variable, Vmax = 5.88m, Vmin = 5.92m, P = 0.06 d
HD 33833 33833 24294 05h 12m 48.12s −06° 03′ 25.6″ 5.90 0.22 446 G7III
HD 32263 32263 23408 05h 01m 50.35s +00° 43′ 19.8″ 5.91 −0.01 498 K0
HD 43112 43112 29678 06h 15m 08.46s +13° 51′ 03.9″ 5.91 −2.21 1370 B1V suspected variable
HD 36780 36780 26108 05h 34m 04.06s −01° 28′ 12.7″ 5.92 −1.14 842 K5III
57 Ori 57 39698 27965 05h 54m 56.69s +19° 44′ 58.6″ 5.92 −2.25 1405 B2V suspected variable
HD 36162 36162 25790 05h 30m 26.17s +15° 21′ 38.0″ 5.93 0.81 344 A3Vn
HD 37788 37788 26762 05h 41m 05.59s +00° 20′ 15.7″ 5.93 2.38 168 F0IV
HD 38529 38529 27253 05h 46m 34.96s +01° 10′ 06.7″ 5.94 2.80 138 G4V binary star; has a planet and a brown dwarf
HD 39421 39421 27713 05h 52m 07.73s −09° 02′ 31.1″ 5.95 0.62 379 A2Vn
HD 37481 37481 26535 05h 38m 37.97s −06° 34′ 26.2″ 5.96 −2.45 1567 B1.5IV suspected variable
HD 39051 39051 27560 05h 50m 13.06s +04° 25′ 24.6″ 5.96 0.00 507 K2III
HD 39286 39286 27747 05h 52m 23.41s +19° 52′ 04.3″ 5.96 −2.16 1370 B9V + G suspected variable
HD 37171 37171 26386 05h 37m 04.35s +11° 02′ 06.2″ 5.97 −1.04 821 K4II SB variable star, ΔV = 0.013m, P = 1.56 d
HD 38089 38089 26926 05h 42m 53.91s −06° 47′ 46.7″ 5.97 2.47 163 F3V
HD 38858 38858 27435 05h 48m 34.90s −04° 05′ 38.7″ 5.97 5.01 51 G4V has a planet; suspected variable
HD 39118 39118
39119		 27588 05h 50m 30.03s +02° 01′ 29.0″ 5.97 −1.73 1128 G8III+... suspected variable
HD 39885 39985 28110 05h 56m 28.04s +09° 30′ 33.9″ 5.97 −0.68 697 A0IV
HD 31331 31331 22840 04h 54m 50.71s +00° 28′ 01.8″ 5.98 −1.38 964 B5V
HD 35281 35281 25187 05h 23m 18.51s −08° 24′ 56.1″ 5.99 0.09 493 B8+...
HD 37594 37594 26624 05h 39m 31.15s −03° 33′ 53.0″ 5.99 2.91 135 A8Vs
HD 39775 39775 27939 05h 54m 44.04s +00° 58′ 07.0″ 5.99 −1.03 827 K0III
HD 44497 44497 30318 06h 22m 36.42s +12° 34′ 13.1″ 6.00 2.00 205 F0III
HD 37303 37303 26427 05h 37m 27.36s −05° 56′ 18.2″ 6.03 −2.07 1358 B1Vvar suspected variable
HD 30545 30545 22354 04h 48m 44.63s +03° 35′ 18.8″ 6.04 −0.64 707 K1III
HD 32686 32686 23643 05h 04m 54.53s −03° 02′ 22.8″ 6.04 −3.83 3075 B5IV
V1031 Ori V1031 38735 27341 05h 47m 26.90s −10° 31′ 58.5″ 6.04 −0.47 653 A4V Algol variable, Vmax = 6.02m, Vmin = 6.43m, P = 3.41 d
HD 42477 42477 29371 06h 11m 27.91s +13° 38′ 19.0″ 6.04 0.44 430 A0Vnn
HD 43285 43285 29728 06h 15m 40.18s +06° 03′ 58.3″ 6.07 −0.72 743 B6V
HD 33883 33883 24349 05h 13m 31.55s +01° 58′ 03.7″ 6.08 −1.07 879 A5V
HD 38309 38309 27118 05h 45m 01.80s +04° 00′ 29.5″ 6.09 2.57 165 F0III:n γ Dor variable, ΔV = 0.008m, P = 0.36 d
HD 41076 41076 28686 06h 03m 24.77s +11° 40′ 51.9″ 6.09 0.25 480 A0Vs
W Ori W 32736 23680 05h 05m 23.71s +01° 10′ 39.5″ 6.10 −0.56 700 C semiregular variable, Vmax = 5.5m, Vmin = 6.9m, P = 212 d
HD 30870 30870 22597 04h 51m 43.38s +09° 58′ 30.3″ 6.11 −0.56 704 B5V
HD 33419 33419 24041 05h 10m 03.26s −00° 33′ 54.7″ 6.11 1.19 314 K0III
HD 37232 37232 26414 05h 37m 19.31s +08° 57′ 06.8″ 6.11 −1.01 867 B2IV-V
HD 43683 43683 29931 06h 18m 05.61s +14° 22′ 58.3″ 6.12 −0.33 637 A3V
HD 35317 35317 25240 05h 23m 51.33s −00° 51′ 59.8″ 6.13 2.31 189 F7V
HD 39632 39632 27900 05h 54m 13.35s +10° 35′ 11.1″ 6.13 −2.15 1475 G9II
HD 31764 31764 23161 04h 58m 59.41s +14° 32′ 35.7″ 6.14 −0.43 671 B7V suspected variable
13 Ori 13 33021 23852 05h 07m 38.32s +09° 28′ 21.8″ 6.15 3.89 92 G1IV
HD 34180 34180 24493 05h 15m 18.52s −01° 24′ 32.6″ 6.15 2.84 150 F0IV
HD 36558 36558 25976 05h 32m 37.97s +00° 00′ 43.1″ 6.15 −2.16 1495 K5
HD 37356 37356 26477 05h 37m 53.39s −04° 48′ 50.5″ 6.16 −1.52 1120 B2IV-V suspected variable
HD 35588 35588 25378 05h 25m 47.02s +00° 31′ 12.9″ 6.18 −2.25 1583 B2.5V suspected variable
HD 35693 35693 25502 05h 27m 13.90s +15° 15′ 27.6″ 6.18 0.43 461 A1IV
CK Ori CK 36217 25785 05h 30m 19.91s +04° 12′ 17.5″ 6.21 −0.02 574 K2III not variable
HD 40347 40347 28252 05h 58m 11.70s −00° 59′ 38.3″ 6.21 0.77 400 K0 suspected variable
HD 37744 37744 26713 05h 40m 37.29s −02° 49′ 30.9″ 6.22 −2.34 1680 B1.5V suspected variable
HD 40282 40282 28232 05h 57m 54.51s +01° 13′ 27.5″ 6.22 0.21 519 M0III
HD 36430 36430 25869 05h 31m 20.89s −06° 42′ 30.2″ 6.23 −2.43 1762 B2V
HD 33555 33555 24130 05h 10m 57.97s −02° 15′ 13.5″ 6.24 2.82 158 G8III
HD 35640 35640 25401 05h 26m 02.36s −05° 31′ 06.6″ 6.24 −0.31 667 B9.5Vn
HD 36779 36779 26106 05h 34m 03.89s −01° 02′ 08.6″ 6.24 −1.66 1240 B2.5V suspected variable
HD 37016 37016 26234 05h 35m 22.32s −04° 25′ 27.6″ 6.24 −1.46 1128 B2.5V
HD 38495 38495 27212 05h 46m 02.86s −04° 16′ 05.9″ 6.24 0.96 371 K1III...
HD 43821 43821 29982 06h 18m 40.35s +09° 02′ 50.2″ 6.24 1.11 346 K0
HD 31623 31623 23041 04h 57m 17.21s −01° 04′ 01.9″ 6.25 1.63 274 F2
HD 36840 36840 26149 05h 34m 29.29s −00° 00′ 44.4″ 6.25 −1.63 1230 G5
HD 39927 39927 28019 05h 55m 35.38s −04° 47′ 18.7″ 6.28 1.32 321 A2III
HD 30869 30869 22607 04h 51m 49.92s +13° 39′ 18.7″ 6.30 3.19 136 F5
HD 39685 39685 27902 05h 54m 15.72s +03° 13′ 32.8″ 6.30 0.16 552 K0
BL Ori BL 44984 30564 06h 25m 28.18s +14° 43′ 19.2″ 6.30 −1.70 1299 C semiregular variable, Vmax = 5.9m, Vmin = 6.6m, P = 153 d
HD 32115 32115 23296 05h 00m 39.82s −02° 03′ 57.7″ 6.31 2.83 162 A8IV
V1197 Ori V1197 38099 26953 05h 43m 09.32s −01° 36′ 47.4″ 6.31 −0.28 679 K4III rotating ellipsoidal variable, Vmax = 6.21m, Vmin = 6.31m, P = 143 d
HD 43819 V1155 43819 30019 06h 19m 01.85s +17° 19′ 31.0″ 6.32 −0.11 631 B9IIIsp... α2 CVn variable, ΔV = 0.02m, P = 15.03 d
HD 30321 30321 22189 04h 46m 24.15s −02° 57′ 15.8″ 6.33 1.68 277 A2V
HD 33946 33946 24377 05h 13m 47.25s +00° 33′ 37.7″ 6.33 −0.70 832 M0V suspected variable
HD 34648 34748 24847 05h 19m 35.28s −01° 24′ 42.8″ 6.33 −2.45 1863 B1.5Vn
HD 35407 35407 25288 05h 24m 36.10s +02° 21′ 11.4″ 6.33 −1.55 1226 B4IVn
HD 36285 36285 25786 05h 30m 20.75s −07° 26′ 05.3″ 6.33 −1.53 1216 B2IV-V
HD 31739 31739 23092 04h 58m 10.90s −02° 12′ 46.0″ 6.34 0.62 454 A2V
V1649 Ori V1649 35242 25205 05h 23m 31.08s +05° 19′ 23.0″ 6.34 1.96 245 A2V δ Sct variable
HD 35909 35909 25638 05h 28m 34.77s +13° 40′ 44.5″ 6.35 1.38 322 A4V
HD 44867 44867 30517 06h 24m 52.76s +16° 03′ 26.0″ 6.35 0.99 385 G9III
HD 35775 35775 25505 05h 27m 15.40s +02° 20′ 28.3″ 6.36 0.78 425 K0
HD 42351 42351 29326 06h 11m 01.77s +18° 07′ 49.7″ 6.37 −3.18 2650 K1II suspected variable
HD 43358 43358 29746 06h 15m 53.98s +01° 10′ 08.4″ 6.37 1.53 303 F5IV:
HD 36058 36058 25667 05h 28m 56.91s −03° 18′ 26.7″ 6.39 −0.45 762 A0Vn
θ2 Ori B θ2 43 37042 05h 35m 26.40s −05° 25′ 00.7″ 6.38 1895 B2-B5 component of the θ2 Ori system; suspected variable
HD 43335 43335 29798 06h 16m 23.79s +17° 10′ 53.9″ 6.39 −0.35 728 K5II
HD 34880 34880 24925 05h 20m 26.41s −05° 22′ 03.1″ 6.40 −0.19 679 B8III
V1377 Ori V1377 37055 26263 05h 35m 35.90s −03° 15′ 10.2″ 6.40 −3.12 2608 B3IV slowly pulsating B star
HD 35656 35656 25453 05h 26m 38.82s +06° 52′ 07.5″ 6.41 1.55 305 A0Vn
HD 35912 35912 25582 05h 28m 01.47s +01° 17′ 53.7″ 6.41 −1.35 1160 B2V
HD 37904 37904 26820 05h 41m 40.31s −02° 53′ 47.5″ 6.41 1.80 273 A9IV-V suspected variable
HD 31423 31423 22938 04h 56m 09.02s +07° 54′ 17.3″ 6.42 2.57 192 F5
HD 34317 34317 24607 05h 16m 41.05s +01° 56′ 50.4″ 6.42 0.07 608 A0V variable star, ΔV = 0.008m, P = 1.75 d
HD 34878 34878 24960 05h 20m 43.74s +02° 32′ 41.0″ 6.43 0.91 415 G8IV
V1357 Ori V1357 42807 29525 06h 13m 12.46s +10° 37′ 40.3″ 6.44 5.15 59 G8V RS CVn variable, Vmax = 6.44m, Vmin = 6.49m
HD 35575 35575 25368 05h 25m 36.50s −01° 29′ 28.7″ 6.44 −0.49 791 B3V
HD 32273 32273 23419 05h 02m 00.03s +01° 36′ 31.8″ 6.45 0.49 508 B8V suspected variable
HD 36814 36814 26104 05h 34m 02.48s −07° 01′ 25.1″ 6.45 0.00 637 K0
V1389 Ori V1389 42787 29509 06h 12m 59.57s +06° 00′ 58.6″ 6.45 −0.24 709 M... semiregular variable
HD 37808 V1051 37808 26728 05h 40m 46.19s −10° 24′ 31.20″ 6.46 0.38 536 B9.5IIIp Si α2 CVn variable, ΔV = 0.02m, P = 1.10 d
V1369 Ori V1369 34959 25011 05h 21m 19.31s +04° 00′ 43.1″ 6.49 −1.42 1244 B5Vp Be star
HD 36150 36150 25732 05h 29m 41.59s −00° 48′ 08.7″ 6.49 1.09 391 A2 variable star
HD 37635 37635 26623 05h 39m 30.84s −09° 42′ 23.8″ 6.49 0.29 566 B7V
HD 31411 31411 22923 04h 55m 58.36s +05° 23′ 56.6″ 6.50 0.62 489 A0V
HD 37150 37150 26314 05h 36m 15.03s −05° 38′ 52.5″ 6.51 1270 B3Vv suspected variable
HD 37017 V1046 37017 26233 05h 35m 21.87s −04° 29′ 39.02″ 6.56 1240 B1.5V eclipsing binary and SX Ari variable, Vmax = 6.54m, Vmin = 6.58m, P = 0.95 d
σ Ori E σ 48 V1030 37479 05h 38m 47.19s −02° 35′ 40.5″ 6.61 1148 B2Vp component of the σ Ori system; prototype helium-rich star; SX Ari variable, Vmax = 6.61m, Vmin = 6.77m, P = 1.19 d
HD 43317 43317 29739 06h 15m 47.01s +04° 17′ 01.1″ 6.62 1200 B3IV slowly pulsating B star and β Cep variable, ΔV = 0.01m, P = 0.91 d
σ Ori D σ 48 37468 05h 38m 45.62s −02° 35′ 58.9″ 6.62 1148 B2V component of the σ Ori system
θ1 Ori D θ1 D 41 37023 26224 05h 35m 17.20s −05° 23′ 15.7″ 6.71 1600 B1.5Vp component of the Trapezium; suspected variable
θ1 Ori A θ1 A 41 37020 26220 05h 35m 15.82s −05° 23′ 14.3″ 6.73 1600 B0.5V component of the Trapezium; triple star system; Algol variable, Vmax = 6.72m, Vmin = 7.65m, P = 65.43 d
HD 35155 V1261 35155 25092 05h 22m 18.64s −08° 35′ 58.0″ 6.77 939 S4,1 Z And and rotating ellipsoidal variable, Vmax = 6.68m, Vmin = 7.08m, P = 641 d
Mintaka C δ 34 36485 25930 05h 32m 00.50s −00° 17′ 04.0″ 6.83 916 B2V component of the Mintaka system; suspected variable
HD 42618 42618 29432 06h 12m 01.0s +06° 46′ 59″ 6.84 77 G4V has a planet (b)
KX Ori KX 36958 05h 35m 04.79s −04° 43′ 54.6″ 6.90 B3V Orion variable
Gliese 205 36395 25878 05h 31m 27.50s −03° 40′ 38.0″ 6.97 19 M1.5V
V901 Ori V901 37776 26742 05h 40m 56.37s −01° 30′ 25.9″ 6.97 1080 B2IV SX Ari variable, Vmax = 6.97m, Vmin = 7.02m, P = 1.54 d
HD 33636 33636 24205 05h 11m 46.45s +04° 24′ 12.7″ 7.06 92 G0VCH-0.3 binary star
HD 31253 31253 22826 04h 54m 44s +12° 21′ 08″ 7.13 175.5 F8 has a planet (b)
S Ori S 36090 25673 05h 29m 00.89s −04° 41′ 32.8″ 7.20 3662 M6.5-7.5e Mira variable, Vmax = 7.2m, Vmin = 13.1m, P = 444 d
HD 37824 V1149 37824 26795 05h 41m 26.79s +03° 46′ 40.9″ 7.2 446 G5 RS CVn variable, ΔV = 0.11m, P = 3.88 d
HD 34137 34137 24482 05h 15m 11.87s +01° 33′ 22.14″ 7.24 −0.34 2300 K2III
HD 37058 V359 37058 05h 35m 33.36s −04° 50′ 15.2″ 7.30 B3Vp SX Ari variable, Vmax = 7.25m, Vmin = 7.36m, P = 15.26 d
HD 34445 34445 24681 05h 17m 40.98s +07° 21′ 12.0″ 7.31 3.97 152 G0 has six planets (b, c, d, e, f & g)
HD 37151 V1179 37151 26304 05h 36m 06.23s −07° 43′ 27.3″ 7.37 627 B8V α2 CVn variable, ΔV = 0.1m
V1192 Ori V1192 31993 23245 05h 00m 08.22s +03° 17′ 12.0″ 7.50 721 K2III RS CVn variable, Vmax = 7.5m, Vmin = 7.57m, P = 29.5 d
HD 36629 36629 26000 05h 32m 57.08s −04° 34′ 59.3″ 7.65 B2Vv has a subdwarf companion; suspected variable
HD 37903 37903 26816 05h 41m 38.39s −02° 15′ 32.5″ 7.83 970 B1.5V illuminates NGC 2023; suspected variable
HD 35298 V1156 35298 25235 05h 23m 50.36s +02° 04′ 55.8″ 7.89 1730 B7IV SX Ari variable, ΔV = 0.03m, P = 1.85 d
HD 37806 37806 26752 05h 41m 02.29s −02° 43′ 00.7″ 7.90 1600 A2Vpe Orion variable, Vmax = 7.86m, Vmin = 8.08m
θ1 Ori B θ1 B 41 BM 37021 05h 35m 16.10s −05° 23′ 07.0″ 7.96 1600 B1V component of the Trapezium; quintuple star system; Algol variable, Vmax = 7.9m, Vmin = 8.65m, P = 6.47 d
HD 38677 38677 27305 05h 47m 06.0s −10° 37′ 49″ 8.0 202 F8V has four planets (b, c, d & e)
V372 Ori V372 36917 05h 34m 46.98s −05° 34′ 14.59″ 8.03 A0V Orion variable, Vmax = 7.94m, Vmin = 8.13m
HD 36668 V1107 36668 26048 05h 33m 26.06s +00° 37′ 16.9″ 8.06 811 B8V SX Ari variable, ΔV = 0.02m, P = 2.12 d
HD 38801 38801 27384 05h 47m 59.18s −08° 19′ 39.7″ 8.26 3.47 296 K0IV has a planet (b)
HD 39392 39392 27828 05h 53m 19.0s +22° 04′ 20″ 8.38 307 F8 has a planet (b)
RS Ori RS 44415 30286 06h 22m 13.19s +14° 40′ 41.3″ 8.42 4020 F4Ib classical Cepheid, Vmax = 8.01m, Vmin = 8.88m, P = 7.57 d
σ Ori C σ 48 05h 38m 44.12s −02° 36′ 06.3″ 8.79 1148 A2V component of the σ Ori system
HD 37605 37605 26664 05h 40m 01.73s +06° 03′ 38.1″ 8.69 5.53 140 K0 has two planets
V351 Ori V351 38238 27059 05h 44m 18.79s +00° 08′ 40.4″ 8.87 547 A7IIIe UX Ori star and δ Sct variable, Vmax = 8.7m, Vmin = 9.8m, P = 0.06 d
V2689 Ori V2689 245409 26335 05h 36m 30.99s +11° 19′ 40.32″ 8.90 37 K7-M0V passed near the sun 500,000 years ago; BY Dra variable, Vmax = 8.80m, Vmin = 9.85m, P = 12.13 d
HD 290327 290327 25191 05h 23m 21.56s −02° 16′ 39.4″ 8.96 5.26 179 G5IV has a planet
DN Ori DN 40632 28456 06h 00m 28.35s +10° 13′ 05.0″ 9.15 942 A2e Algol variable
V1355 Ori V1355 291095 06h 02m 40.36s −00° 51′ 37.3″ 9.19 K0-2IV RS CVn variable, Vmax = 8.97m, Vmin = 9.35m
FT Ori FT 42858 06h 13m 58.15s +21° 25′ 39.2″ 9.29 A0 Algol variable, Vmax = 9.1m, Vmin = 9.9m, P = 3.15 d
ER Ori ER 24156 05h 11m 14.51s −08° 33′ 24.7″ 9.46 1340 G1V: W UMa variable, Vmax = 9.28m, Vmin = 10.01m, P = 0.42 d
HD 250550 V1307 250550 28582 06h 01m 59.99s +16° 30′ 56.7″ 9.48 B9e Orion variable, ΔV = 0.35m
UX Ori UX 293782 23602 05h 04m 29.99s −03° 47′ 14.3″ 9.48 913 A4IVe prototype UX Ori star, Vmax = 9.48m, Vmin = 12.5m
EY Ori EY 36412 25863 05h 31m 18.41s −05° 42′ 13.5″ 9.49 A7V Algol variable, Vmax = 9.43m, Vmin = 10.13m, P = 16.79 d
BN Ori BN 05h 36m 29.35s +06° 50′ 02.2″ 9.60 F4e T Tau star, Vmax = 9.60m, Vmin = 9.70m, P = 0.65 d
FU Ori FU 05h 45m 22.36s +09° 04′ 12.4″ 9.60 F0Iab prototype FU Orionis star
BF Ori BF 26403 05h 37m 13.26s −06° 35′ 00.6″ 9.69 A7III UX Ori star, Vmax = 9.69m, Vmin = 13.47m
Gliese 221 27803 05h 53m 00.28s −05° 59′ 41.4″ 9.69 66 K7V/M0V has 2 planets
V586 Ori V586 37258 05h 36m 59.25s −06° 09′ 16.4″ 9.77 A3V UX Orionis star, Vmax = 9.48m, Vmin = 11.41m
HD 37411 V1788 37411 05h 38m 14.51s −05° 25′ 13.3″ 9.79 B9Ve Orion variable, Vmax = 9.76m, Vmin = 9.85m
BD +03 740 23344 05h 01m 16.62s +04° 06′ 37.0″ 9.81 371 sd:F0 metal-poor star
HD 34282 V1366 34282 24552 05h 16m 00.48s −09° 48′ 35.4″ 9.84 622 A0 UX Ori star and δ Sct variable, Vmax = 9.75m, Vmin = 10.62m
EW Ori EW 287727 05h 20m 09.15s +02° 02′ 40.0″ 9.9 F8 Algol variable, Vmax = 9.9m, Vmin = 10.6m, P = 6.94 d
V1162 Ori V1162 05h 32m 01.99s −07° 15′ 24.6″ 9.9 A6mF2 δ Sct variable
Z Ori Z 249313 28045 05h 55m 50.93s +13° 41′ 42.0″ 9.98 B4V... Algol variable
GW Ori GW 244138 25689 05h 29m 08.39s +11° 52′ 12.7″ 10.10 896 G5/8Ve triple star; T Tau star
WASP-82 04h 50m 39.0s +01° 53′ 38″ 10.1 652 F5 has a transiting planet (b)
V1005 Ori V1005 23200 04h 59m 34.83s +01° 47′ 00.7″ 10.11 84 M0Ve T Tau star and flare star, ΔV = 0.067m, P = 4.41 d
V346 Ori V346 287841 25299 05h 24m 42.80s +01° 43′ 48.3″ 10.17 1570 A UX Ori star and δ Sct variable, Vmax = 10.1m, Vmin = 10.9m, P = 0.03 d
CO Ori CO 25540 05h 27m 38.34s +11° 25′ 39.0″ 10.30 1060 F7Ve UX Ori star, Vmax = 10.0m, Vmin = 12.8m
FZ Ori FZ 288166 05h 41m 21.01s +02° 36′ 23.0″ 10.70 G0 W UMa variable, Vmax = 10.7m, Vmin = 11.3m, P = 0.40 d
V380 Ori V380 26327 05h 36m 25.43s −06° 52′ 57.7″ 10.7 A1e quadruple star; UX Ori star
GG Ori GG 290842 05h 43m 10.22s −00° 41′ 14.9″ A2 Algol variable
HK Ori HK 05h 31m 28.05s +12° 09′ 10.3″ 11.20 A2?e+G0?e UX Ori star, Vmax = 11.2m, Vmin = 12.3m
T Ori T 05h 35m 50.44s −05° 28′ 34.9″ 11.25 A3IVeb UX Ori star, Vmax = 9.5m, Vmin = 12.6m
DY Ori DY 06h 06m 14.91s +13° 54′ 19.1″ 11.29 RV Tau variable, Vmax = 11.2m, Vmin = 12.2m, P = 60.84 d
LkHα 208 06h 07m 49.54s +18° 39′ 26.5″ 11.30 1000 F0Ve associated with a bipolar nebula
GJ 3379 06h 00m 03.50s +02° 42′ 23.7″ 11.31 17 M4.0V
FH Ori FH 243229 05h 23m 18.62s +04° 15′ 38.2″ 11.37 A2 Algol variable
θ1 Ori E θ1 E 41 05h 35m 15.77s −05° 23′ 10.02″ 11.4 1600 G2IV+G2IV component of the Trapezium; Algol variable and T Tau star, ΔV = 0.1m, P = 9.90 d
V371 Ori V371 26081 05h 33m 44.81s +01° 56′ 43.4″ 11.50 51 M2.5V Wachmann's Flare Star; flare star
Ross 87 V1352 26857 05h 42m 09.27s +12° 29′ 21.6″ 11.51 19 M4.0V BY Dra variable, Vmax = 11.48m, Vmin = 11.55m
Gliese 179 22627 04h 52m 05.73s +06° 28′ 35.5″ 11.96 7.41 40 M3.5 has a planet
GP Ori GP 286340 05h 02m 48.07s +15° 19′ 12.6″ 12.20 SC7/8 semiregular variable
RX J0529.4+0041 V1642 05h 29m 20.65s +00° 41′ 28.0″ 12.30 K2 Algol variable, Vmax = 12.03m, Vmin = 13.07m, P = 3.04 d
GU Ori GU 06h 10m 04.62s +12° 49′ 46.6″ W UMa variable, Vmax = 12.5m, Vmin = 13.3m, P = 0.47 d
YY Ori YY 05h 34m 47.53s −05° 57′ 56.9″ 13.20 K2IVe prototype YY Orionis star
LV 2 θ1 G 41 05h 35m 16.72s −05° 23′ 16.6″ 13.68 1600 K0.7 component of the Trapezium; has a protoplanetary disk
G 99-47 V1201 05h 56m 25.47s +05° 21′ 48.6″ 14.10 26 DA8P variable white dwarf, Vmax = 13m, Vmin = 14.12m
V1118 Ori V1118 05h 34m 44.75s −05° 33′ 42.2″ 14.43 M1e EXor
LP 658-2 05h 55m 09.49s −04° 10′ 04.3″ 14.45 21 DZ11
G 99-37 05h 51m 19.48s −00° 10′ 21.3″ 14.60 36 DQ8P strongly magnetized white dwarf
V1159 Ori V1159 05h 28m 59.57s −03° 33′ 52.3″ ER UMa variable
VY Ori VY 05h 33m 35.89s −05° 01′ 32.49″ 14.9 variable star
V1309 Ori V1309 05h 15m 41.41s +01° 04′ 40.5″ 15.2 WD+M0V polar, Vmax = 15.2m, Vmin = 18.2m
CN Ori CN 05h 52m 07.79s −05° 25′ 00.5″ 16.2 SS Cyg variable, Vmax = 12.1m, Vmin = 16.2m
CZ Ori CZ 06h 16m 43.23s +15° 24′ 11.3″ 17.6 SS Cygni variable, Vmax = 12.1m, Vmin = 17.6m
V1647 Ori V1647 05h 46m 13.14s −00° 06′ 04.8″ 18.1 EXor, Vmax = 18.1m, Vmin = <20m
4U 0614+091 V1055 06h 17m 07.3s +09° 08′ 13″ 18.5 low-mass X-ray binary; producing relativistic jets
Becklin–Neugebauer Object V2254 05h 35m 14.11s −05° 22′ 22.7″ B Orion variable; well-studied protostar
2MASS J05352184-0546085 V2384 05h 35m 21.84s −05° 46′ 08.6″ M7 eclipsing binary brown dwarf
OMC-2 FIR 4 V2457 05h 35m 26.97s −05° 09′ 54.5″ M7 has a circumstellar disk; Orion variable
Orion Source I 05h 35m 14.51s −05° 22′ 30.4″ protostellar binary
Reipurth 50 05h 40m 27.45s −07° 27′ 30.1″ suspected FU Ori star
S Ori 70 05h 38m 10.10s −02° 26′ 26.0″ T6 possibly a rogue planet
WISE J0521+1025 05h 21m 26.30s +10° 25′ 28.5″ 16 brown dwarf
Table legend:

See also

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References

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List of stars in Orion

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The list of stars in Orion encompasses the cataloged stellar members within the boundaries of Orion, one of the 88 modern constellations and a prominent winter asterism visible primarily in the from to , recognized for its distinctive shape formed by a rectangular frame of bright stars and a linear belt of three aligned stars. This constellation, spanning 594 square degrees on the and named after the Greek mythological hunter Orion as one of the 48 constellations listed by in the , is home to numerous hot, luminous blue supergiants belonging to the , making it a key region for studying young, massive stars and . Among its most notable stars are Rigel (Beta Orionis), the brightest in the constellation at an apparent magnitude of 0.13 and the seventh-brightest star in the night sky overall, a blue supergiant of spectral type B8 Ia located approximately 848 light-years away and part of a multiple star system marking the hunter's left foot. Betelgeuse (Alpha Orionis), the second-brightest at a variable magnitude of 0.50, is a red supergiant of type M1–M2 Ia–ab about 548 light-years distant, known for its distinctive orange-red hue and semiregular variability, positioning it as the tenth-brightest star visible. In 2025, a companion star was directly imaged approximately 52 AU from Betelgeuse, confirming it as part of a binary system. Other prominent members include Bellatrix (Gamma Orionis), a blue main-sequence star of type B2 V with magnitude 1.64 at 250 light-years, forming the right shoulder; Saiph (Kappa Orionis), a blue supergiant of type B0.5 Ia at magnitude 2.09 and 650 light-years, denoting the left leg; and Meissa (Lambda Orionis), marking the head at magnitude 3.33. The iconic Orion's Belt consists of three nearly equidistant stars: Alnitak (Zeta Orionis), an O9.5 Iab blue supergiant triple system at magnitude 1.77 and 1,260 light-years, representing the easternmost "girdle"; Alnilam (Epsilon Orionis), the central and brightest belt star at magnitude 1.69, a B0 Ia blue supergiant 1,180 light-years away known as the "string of pearls"; and Mintaka (Delta Orionis), the faintest at magnitude 2.23, an O9.5 II blue giant multiple system about 1,200 light-years distant, signifying the western "belt." Additional significant stars in the list include Hatysa (Iota Orionis), a blue giant of type O9 III at magnitude 2.77 and 1,340 light-years, the brightest in Orion's Sword hanging from the belt. This compilation typically includes all stars with Bayer or Flamsteed designations brighter than magnitude 6.5, alongside variable and multiple systems, highlighting Orion's role as a benchmark for naked-eye astronomy and deep-sky observation.

Constellation Context

Location and Visibility

Orion occupies a defined region of the , spanning from 04h 43m 25s to 06h 25m 47s and from -10° 58' to +22° 52', encompassing an area of 594 square degrees and ranking as the 26th largest among constellations officially recognized by the (IAU). This equatorial position places Orion prominently in the winter sky for northern observers, with its boundaries set along lines of and to ensure complete coverage of the sky without overlap. In the , Orion is most visible during winter evenings from to February, rising in the east after sunset and reaching its highest point in the southern sky around midnight, offering optimal viewing conditions for up to 60°N. Conversely, in the , the constellation appears during summer evenings, positioned in the northern sky and appearing inverted compared to northern views, with visibility extending to down to 75°S. Its proximity to the ensures broad accessibility from both hemispheres, though it never becomes circumpolar at any due to its moderate range. Key asterisms within Orion facilitate star identification for amateur astronomers: , a linear arrangement of three bright stars aligned nearly horizontally, serves as a central reference point, while , a shorter vertical chain of fainter stars dangling below the belt, points toward notable deep-sky objects like the . These patterns are easily recognizable even under moderate , making Orion one of the most identifiable constellations for beginners. For naked-eye observation, Orion's brightest , including those in the belt and shoulders, are discernible from most locations between 85°N and 75°S, particularly from dark-sky sites away from urban areas where can dim fainter members of the asterism. Observers are advised to allow 20-30 minutes for dark adaptation, use for subtle details, and seek rural or elevated vantage points to mitigate , enhancing the view of the constellation's outline against the backdrop.

Historical Significance

In , the constellation Orion is depicted as a mighty hunter, often portrayed wielding a club and shield while pursuing celestial prey, with its prominent stars representing key anatomical features such as marking the right shoulder and the left foot. The three stars forming —Alnitak, Alnilam, and Mintaka—are central to this figure, symbolizing the hunter's girdle and serving as a key identifier in ancient sky lore. Orion held significant roles in various ancient astronomical traditions beyond Greece. In Babylonian astronomy, it was known as SIPA.ZI.AN.NA, or the "True Shepherd of Heaven," a figure associated with guidance and protection in early Mesopotamian star catalogs. Ancient Egyptians identified the constellation with Osiris, the god of resurrection and light, linking its annual appearances to cycles of death and rebirth in their religious cosmology. Chinese astronomers referred to Orion's belt stars as Shen, or "The Three Stars," integrating them into broader stellar lore for seasonal and imperial divination. Polynesian navigators relied on Orion's stars, including Betelgeuse (known as 'Aua in Hawaiian), for wayfinding across the Pacific, using their risings and settings to maintain course on long voyages. The constellation's visibility influenced early calendars and agriculture, particularly through its heliacal rising, which ancient Greek poets like Hesiod cited as a signal for autumn sowing and vintaging around late October. Homer referenced Orion in the Iliad and Odyssey as a formidable hunter among the stars, embedding it in epic narratives that underscored its cultural prominence. Though not part of the zodiac, Orion's proximity to zodiacal signs like Taurus reinforced its role in seasonal timing and mythological storytelling across Mediterranean traditions. Many of its star names trace to origins, transmitted via medieval astronomers like al-Sufi; for instance, derives from "al-nitaq" meaning "the belt," from "yad al-Jawza'" or "hand of the central figure," and from "rijl" or "foot."

Designation Systems

Bayer and Flamsteed Designations

The designation system was introduced by German astronomer in his 1603 star atlas Uranometria, the first comprehensive modern celestial atlas containing maps of 51 constellations. In this system, stars are labeled with lowercase Greek letters from α (alpha) to ω (omega), followed by the Latin genitive form of the constellation name, such as α Orionis for the star . The letters were intended to be assigned roughly in order of decreasing apparent brightness, with α reserved for the brightest star in the constellation and subsequent letters for progressively fainter ones, though this ordering was not always strictly followed due to observational limitations of the era. For Orion, a prominent winter constellation visible from both hemispheres and thus favorable for early cataloging, Bayer applied the full set of 24 Greek letters to denote its brighter stars. Notable irregularities appear in Orion's Bayer designations, reflecting the challenges of pre-telescopic observations. For instance, β Orionis (), the constellation's brightest star at an of about 0.13, received the beta label, while α Orionis () was assigned alpha despite its typical magnitude of 0.50; this anomaly likely occurred because , an irregular , was temporarily brighter than during Bayer's observations around 1603, possibly enhanced by the in low-light conditions that makes red stars appear relatively brighter. Such deviations highlight that 's system prioritized positional and approximate brightness ordering over , and in Orion, it also grouped multiple stars under shared designations like π Orionis for components of the hunter's shield. Complementing the Bayer system, the Flamsteed designation was established by English astronomer , the first , in his posthumously published Historia Coelestis Britannica in 1725, which cataloged nearly 3,000 stars based on telescopic observations from Greenwich. This system assigns sequential (starting from 1) to stars within each constellation, ordered by increasing , followed by the genitive constellation name; for example, is 19 Orionis, reflecting its position eastward of several other notable stars like (24 Orionis). Unlike Bayer's brightness-based approach, Flamsteed's method provided a more systematic spatial sequence, aiding navigation and further mapping, though it too focused on brighter stars visible to the or early telescopes. Both systems are limited to Orion's more prominent stars, collectively designating around 80 brighter objects but leaving fainter ones (below magnitude 6) unnamed until later catalogs; for instance, Bayer omitted 10 stars from Orion's printed list due to mapping errors, and Flamsteed's numbering extends only to about 74 in the constellation. These 17th- and 18th-century conventions remain foundational for identifying Orion's key stars, emphasizing its role as a benchmark for early stellar .

Modern Catalog References

The Henry Draper Catalogue (), published between 1918 and 1924, provides spectroscopic classifications for approximately 225,000 stars down to ninth magnitude, including over 200 entries within the boundaries of Orion based on its systematic survey of stellar spectra. This 20th-century resource, developed at Observatory, assigns HD numbers to stars like HD 39771 (corresponding to 42 Orionis) and emphasizes spectral types, enabling early insights into stellar temperatures and compositions in regions like Orion. The mission, launched by the in 1989, produced the Hipparcos Catalogue with high-precision for about 118,000 stars brighter than 12th magnitude, while its companion Tycho-2 Catalogue extended coverage to 2.5 million stars down to 11th magnitude, including proper motions and two-color photometry. For Orion, these 1990s datasets include astrometric parameters such as parallaxes and proper motions for roughly 120 stars brighter than seventh magnitude, facilitating distance estimates and kinematic studies of the constellation's prominent members. The mission, ongoing since 2013, has revolutionized stellar catalogs through its space-based , photometry, and . 's Data Release 3 (DR3) from delivers precise positions, distances, and radial velocities for over 1.8 billion sources, encompassing thousands of in Orion and enabling detailed mapping of cluster memberships within its dense stellar populations. Data Release 4 (DR4), anticipated in late 2026, will incorporate 66 months of observations to refine these measurements further, including time-series for variable and enhanced binary orbit solutions relevant to Orion's systems. Specialized catalogs complement these general surveys for Orion's binary stars and data access. The Washington Double Star Catalog (WDS), maintained by the U.S. Naval Observatory, serves as the primary global database for astrometric doubles and multiples, recording positions, separations, and for over 150,000 systems, many of which are queried within Orion's rich binary population. For cross-referencing and queries, tools like provide unified identifiers and basic data for Orion stars, while enables access to multiple catalogs, allowing researchers to link designations to modern measurements efficiently. Orion's proximity and star-forming activity underscore the value of these catalogs, as the Orion OB1 association lies at about 400 parsecs, hosting a high density of young stars that Gaia and earlier surveys have helped characterize through membership probabilities and evolutionary stages.

Principal Stars

Shoulder and Head Stars

The shoulder and head stars of Orion represent the constellation's upper body, featuring prominent supergiants and giants that dominate the winter sky due to their brightness and distinctive colors. Alpha Orionis, commonly known as , marks the hunter's right shoulder and is a prototypical with an apparent visual magnitude averaging 0.50 but varying between 0.0 and 1.6 due to pulsations. Recent interferometric observations suggest the presence of a companion star orbiting at about 4 AU, potentially contributing to its variability. Its spectral type is classified as M1-2 Ia-Iab, indicating a cool, luminous atmosphere rich in molecular bands. At an estimated distance of approximately 548 light-years, Betelgeuse has a radius of about 724 solar radii and a mass ranging from 14 to 20 solar masses, making it one of the largest known stars. It gained significant attention for the "Great Dimming" event from late 2019 to early 2020, when its brightness dropped by about 1.2 magnitudes, attributed to dust ejection or surface activity rather than an imminent . As a massive evolved star, Betelgeuse is a prime candidate for a future explosion within the next million years, though precise timing remains uncertain. Positioned as Orion's left shoulder, Gamma Orionis, or , is a with an apparent magnitude of 1.64, providing a stark contrast to Betelgeuse's ruddy hue. Its type is B2 III, characteristic of a hot, hydrogen-fusing star with strong lines. Located at about 250 light-years away, Bellatrix exhibits rapid rotation with a projected equatorial velocity (v sin i) of approximately 52 km/s, contributing to its broadened lines. Historically, it has served as a standard comparison star for photometric measurements due to its relative stability in brightness. Lambda Orionis, known as , crowns Orion's head as a with a combined of 3.39. The primary is an O8 III giant paired with a B3 V main-sequence companion, forming a binary that ionizes surrounding gas. At a distance of roughly 1,300 light-years, anchors the Lambda Orionis Cluster (Collinder 69), a young of about 5 million years old embedded in the Sh2-264 , which spans over 100 light-years and glows from excitation by the system's hot stars. This association highlights Meissa's role in recent within Orion's complex. These upper stars differ from the hotter, aligned belt stars that form Orion's midsection.
Star NameBayer DesignationCoordinates (J2000, RA/Dec)Proper Motion (mas/yr, RA/Dec)Spectral Peculiarities
Betelgeuseα Ori05h 55m 10.3s / +07° 24' 25"+27.54 / +11.30Variable red supergiant with molecular bands and pulsations
Bellatrixγ Ori05h 25m 07.9s / +06° 20' 59"-8.11 / -12.88Blue giant with broadened lines from rotation
Meissaλ Ori05h 35m 08.3s / +09° 56' 03"-0.34 / -2.94O+B binary ionizing emission nebula

Belt Stars

The three stars forming —Delta Orionis (Mintaka), Epsilon Orionis (), and Zeta Orionis ()—create a distinctive linear asterism that is one of the most recognizable features in the . These hot, massive O- and B-type stars are aligned nearly perfectly along the , with a positional error of less than 1° from a straight line, spanning about 3° of arc. Known culturally as the "Three Kings" or "Three Magi" in Western traditions, particularly linked to the Biblical story of the following a star, the asterism has served as a navigational guide for millennia; extending the line downward from the belt points toward Sirius, the brightest star in the sky. All three stars are young, belonging to the Orion OB1 association, a vast complex of approximately 1,300 light-years distant, highlighting the region's active stellar birth processes. Delta Orionis, or , is the westernmost belt star with an apparent visual magnitude of 2.23, making it visible to the under . Classified as an O9.5 II primary paired with a B0 III companion in a , it exhibits variability due to eclipses, with an of approximately 5.7 days for the close pair. Located about 1,200 light-years away, is a member of the Orion OB1b subgroup, characterized by stars aged 4–5 million years, and contributes to the association's collective feedback that triggers further in the region. Epsilon Orionis, known as , anchors the center of the belt as the brightest member at magnitude 1.69. This B0 Ia blue supergiant, situated roughly 1,340 light-years distant, boasts a of 375,000 times that of the Sun and displays a helium-rich indicative of its high exceeding 27,000 K, where ionized lines dominate. Alnilam resides in the Orion OB1a subgroup, slightly older at around 12 million years, and its intense radiation illuminates surrounding nebulosity, underscoring its role in the association's evolutionary sequence. Zeta Orionis, or , forms the eastern end of the belt with a magnitude of 1.74. As an O9.5 Iab primary accompanied by multiple companions—forming a system with four components total—it lies approximately 1,260 light-years away and is part of the Orion OB1b subgroup. The primary's high mass and rapid contribute to its status as one of the hottest visible stars, with surface temperatures around 30,000 K, influencing the dynamics of nearby .

Leg and Sword Stars

The leg and sword stars delineate the lower outline of Orion, forming a distinctive trapezoidal extension below the belt that enhances the constellation's recognizable hunter silhouette. Beta Orionis, commonly known as , anchors the right leg as a brilliant with an apparent visual magnitude of 0.13, varying slightly between 0.05 and 0.18 due to its semiregular pulsations. Classified as spectral type B8 Ia, lies approximately 860 light-years away and exhibits an extraordinary luminosity of 120,000 times that of the Sun, powered by a around 18 solar masses. It forms part of a multiple system, with a visual companion separated by 9.5 arcseconds. 's intense blue-white glow rivals the variable in overall brightness, providing a striking color contrast in the constellation. Kappa Orionis, or , marks the left foot with an apparent magnitude of 2.07 and spectral type B0.5 II, characterizing it as a hot . Positioned about 650 light-years distant, Saiph displays a of approximately 1.9 mas/yr. The sword, hanging below the belt, features prominent stars that add depth to Orion's form. , dubbed Hatsya, tips the sword with a magnitude of 2.75 and spectral type O9 III, situated roughly 1,360 light-years away as a luminous O-type giant. This star heads a multiple system with an of 28.9 years for its close companions, contributing to its observed variability and complexity. Further along the sword, Sigma Orionis appears as a combined magnitude 3.81 visual system dominated by an O9.5 V primary paired with a B0.2 V companion, located at about 1,260 light-years. It anchors a young open cluster rich in low-mass members, including several brown dwarfs identified through deep photometric surveys, underscoring the region's active star formation. ===== END CLEANED SECTION =====

Variable and Multiple Stars

Notable Variable Stars

Orion hosts several notable variable stars, with variability arising primarily from intrinsic pulsations in their atmospheres. Among the brightest, (Alpha Orionis) is a semiregular variable exhibiting pulsations with a dominant period of approximately 400 days and typical amplitude of about 0.5 magnitudes in the visual band. This star's variability has been monitored since 1836, when it was first noted by . A particularly dramatic event was the Great Dimming of 2019–2020, during which faded by over 1 magnitude due to a surface mass ejection forming a dust veil that obscured part of the star. The pulsations are driven by convective motions in the star's extended envelope, occasionally leading to dust ejections that enhance the amplitude. Rigel (Beta Orionis), the constellation's brightest star, is an Alpha Cygni-type variable blue showing non-radial pulsations with a quasi-period of roughly 22 days and small of about 0.1 magnitudes. These variations stem from complex atmospheric instabilities rather than simple radial expansion and contraction, resulting in irregular light curves superimposed on the short-term pulsations. Other notable variables in Orion include long-period types like RR Orionis, a Mira-type variable with a pulsation period of 251 days and amplitude spanning 4.8 magnitudes in V (from 9.7 to 14.5). This asymptotic giant branch star's variability is characteristic of thermal pulsations in its outer layers, leading to significant brightness changes over months. Less prominent examples encompass short-period pulsators such as Upsilon Orionis (Thabit), a Beta Cephei-type variable with a period of approximately 0.51 days and amplitude up to 0.05 magnitudes (4.55–4.65 V), driven by radial and non-radial modes in its hot main-sequence atmosphere. Additionally, V851 Orionis displays irregular variability with multi-periodic behavior akin to delta Scuti stars, fluctuating by about 0.6 magnitudes (6.2–6.8 V) over hours to days due to low-amplitude pulsations.
Star NameTypePeriod (days)Amplitude (mag, V)Discovery/Monitoring Notes
Betelgeuse (α Ori)Semiregular~400~0.5Monitored since 1836; Great Dimming 2019–2020
Rigel (β Ori)Alpha Cygni~22~0.1Irregular pulsations noted in 20th-century surveys
Upsilon Orionis (Thabit)Beta Cephei~0.51~0.05 (4.55–4.65)Identified as pulsator in mid-20th-century studies
RR OrionisMira2514.8 (9.7–14.5)Long-period variability cataloged in AAVSO records
V851 OrionisDelta Scuti (irregular)Multi-period (<1)~0.6 (6.2–6.8)UV-irregular variations observed in 2010s

Prominent Multiple Star Systems

Delta Orionis, commonly known as , forms a triple star system designated as [(Aa1 + Aa2) + Ab], where the inner spectroscopic binary consists of two massive O-type stars orbiting each other with a period of 5.732 days. The primary component Aa1 has a of approximately 17.8 M⊙, while the secondary Aa2 is about 8.5 M⊙; the orbit has a low eccentricity of 0.081 and a semi-major axis of roughly 0.2 AU, determined from combined spectroscopic and photometric analyses. The outer companion Ab, a B-type star of ~8.8 M⊙, orbits the inner pair with a period of approximately 152 years, an eccentricity of 0.589, and a semi-major axis of approximately 93 AU, as refined by recent astrometric measurements including data. Zeta Orionis, or , is a quadruple system comprising the bright O9.7 Aa, accompanied by Ab (a B1 III star), and more distant companions B and C. The inner visual binary Aa-Ab has an of about 7.36 years with a semi-major axis of 0.036 arcseconds (≈14 AU at the system's distance of 387 pc), exhibiting low eccentricity based on speckle interferometry and long-term monitoring. The outer components B and C are separated from the primary by 2.73 arcseconds (≈1060 AU) and 31 arcseconds (≈12,000 AU), respectively, with no tightly constrained s but evidence of common suggesting gravitational binding; recent DR3 confirms relative accelerations indicative of a wide spanning centuries. This configuration resembles the Trapezium Cluster's dynamics but remains a distinct field multiple system. Iota Orionis, known as Hatsya, constitutes a multiple system with the primary an O9 III giant in a close spectroscopic binary (Aa1 + Aa2) orbited by B-type companions. The inner spectroscopic binary has an orbital period of 29.13 days, a semi-major axis of 132 R⊙ (≈0.0006 AU), and eccentricity of 0.745, resolved through spectroscopy. The outer companion B is at 11 arcseconds (≈4500 AU at 412 pc distance), with orbital elements suggesting a period of several millennia; Gaia DR3-updated proper motions indicate a bound hierarchy with the primary dominating the system's dynamics. Some orbital phases may produce brief photometric variability due to eclipses, though primarily gravitational interactions drive the system's evolution. Sigma Orionis represents one of the most complex multiple systems in Orion, a hierarchical quintuple (or higher) arrangement embedded in a young cluster spanning ~30 arcminutes. The core triple subsystem [Aa + Ab + B] features the inner eccentric binary Aa-Ab (O9.5 V + B0.5 V, masses ~36 M⊙ and ~13 M⊙ combined) with a period of 143.2 days and semi-major axis ~1 AU, alongside B at ~100 AU on a near-circular orbit of ~157 years. Components D and E form a wide visual pair at ~40 arcseconds (~8000 AU) with a period of ~288 years, while F is a more distant, unbound interloper; post-2022 Gaia DR3 data refines relative orbits, confirming short-period spectroscopic motion in Aa-Ab and long-term drifts in the outer hierarchy.
SystemTypeKey ComponentsOrbital Period(s)Separation(s)Notes (Gaia DR3 Updates)
δ Ori (Mintaka)Spectroscopic + Visual TripleAa1 (O9 V), Aa2 (B1 V), Ab (B2 V)Inner: 5.73 d; Outer: ~152 yrInner: ~0.2 AU; Outer: ~93 AURefined eccentricity and masses from combined spectroscopy; proper motion anomaly confirms binding.
ζ Ori (Alnitak)Visual QuadrupleAa (O9.7 Ib), Ab (B1 III), B (B3 V), C (B5 V)Inner: ~7.36 yr; Outer: CenturiesInner: ~14 AU; B: ~1060 AU; C: ~12,000 AUAstrometric perturbations indicate wide orbit; no significant change in inner period.
ι Ori (Hatsya)Spectroscopic + Visual MultipleA (O9 III), B (B1 III), C (B3 V)Inner: 29.13 d; Outer: MillenniaInner: ~0.0006 AU; Outer: ~4500 AUUpdated semi-major axis from spectroscopy; cluster membership refined.
σ OriSpectroscopic + Visual Quintuple+Aa (O9.5 V), Ab (B0.5 V), B (B2 V), D/E (A/F)Inner: 143 d; Mid: 157 yr; Outer: ~288 yrInner: ~1 AU; Mid: ~100 AU; Outer: ~8000 AUConfirmed hierarchical stability; short-period orbit unchanged, wide orbits tightened by parallax.

Additional Notable Stars

Fainter Visible Stars

The fainter visible stars in Orion encompass those with apparent magnitudes roughly between 4 and 6, observable to the in or with , contributing to the constellation's rich field without dominating its prominent asterisms. These stars often include hot blue giants or main-sequence objects, many of which are multiple systems, and they populate the Orion OB1 association subgroups. Their distances range from a few hundred to over a thousand light-years, providing a glimpse into the region's star-forming history. Theta Orionis, known as the Trapezium, features fainter components beyond its brightest members, with apparent magnitudes ranging from 5.1 to 8.3. The system is a quadruple consisting of an O6pe primary and B0.5V companions, located at a distance of 1,344 light-years, where the stars collectively ionize the surrounding through their intense ultraviolet radiation. Mu Orionis is a quadruple system with a combined apparent magnitude of 4.13, comprising an A2 V metallic-line primary and companions of spectral types including F5 V, situated 155 light-years away. Nu Orionis has an of 4.42 and spectral type B3 V, lying approximately 534 light-years distant. 42 Orionis exhibits an of 4.59 and spectral type B1 V, forming a system with a separation of about 1.5 arcseconds. Other naked-eye in the magnitude 4-6 range include approximately 20 objects, such as the following representative examples sorted by increasing magnitude (data drawn from astronomical catalogs for basic parameters; updated with DR3 where available):
DesignationApparent MagnitudeSpectral TypeNotes
42 Ori4.59B1 Double system in sword region.
θ¹ Ori C5.13O7 Trapezium component, nebula ionizer.
9 Ori5.16B1 Sword area star.
20 Ori5.21B5 OB association member.
37 Ori5.40A0 White main-sequence.
45 Ori5.47B8 Optical double with 42 Ori.
58 Ori--Removed: incorrect designation (refers to bright α Ori ).
68 Ori4.88B9 III in belt vicinity (verified approximate).
These stars enhance Orion's visual depth, with spectral types spanning O to F classes, reflecting a mix of young, hot objects and cooler giants.

Stars Associated with Deep-Sky Objects

The at the heart of the (M42) is dominated by the multiple star system θ¹ Orionis, whose four brightest components (A–D) have visual magnitudes ranging from 5.1 to 8.7 and spectral types O7 V (C), O8 V (D), O9.5 V (A), B3 V (B), with an estimated age of approximately 1 million years that places them in early pre-main-sequence evolutionary stages. These stars emit intense that ionizes the surrounding gas, illuminating the and driving its expansion. Fainter components E and F, with magnitudes around 10–11, are additional low-mass members contributing to the cluster's dynamics. The λ Orionis association surrounds the star (λ Orionis), encompassing roughly 20 early-type stars embedded in the Sh2-296 , at a of about 394 pc and an age of ~6.8 million years, as refined by DR3 confirming its OB membership and coherent expansion. This group represents a young OB association with ongoing low-level influenced by the nebula's ionized shell. Orion OB1, a vast association spanning the constellation, divides into subgroups with distinct ages and positions; for instance, the belt and sword stars belong primarily to the OB1b subgroup, where ε Orionis () serves as a key B0 Ia supergiant member with a current mass of ~35 M⊙ and an age of ~5 million years, marking the main-sequence phase of massive star evolution in this ~390 pc distant region ( DR3 refined). Other primaries in OB1b exhibit masses of 10–40 M⊙, highlighting the subgroup's role in recent massive . Additional associations link stars to expansive structures like (Sh2-276), a faint emission arc ionized partly by distant OB1 members, including a faint O9.5 Vp star in the reflection nebula near σ Orionis, which contributes to the Horsehead region's illumination at ~360 pc and an age of ~3 million years in pre-main-sequence development. Similarly, ζ Orionis (), an O9.7 Ib , provides the ultraviolet radiation that ionizes the (NGC 2024), exciting its hydrogen emissions ~390 pc away in a ~6 million-year-old environment.
Star/SystemAssociated ObjectDistance (pc)Age (Myr)Evolutionary Stage
θ¹ Orionis (A–D)414~1Pre-main-sequence O/B stars
λ OrionisSh2-296 nebula394~6.8OB association expansion
ε Orionis ()Orion OB1b subgroup390~5Main-sequence B supergiant
ζ Orionis ()390~6Main-sequence O supergiant
σ Orionis360~3Pre-main-sequence O9 system

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