Astronomy:List of stars in Cassiopeia

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

Name B F Var HD HIP RA Dec vis.
mag. 		abs.
mag. 		Dist. (ly) Sp. class Notes
α Cas α 18 3712 3179  00h 40m 30.39s +56° 32′ 14.7″ 2.24 −1.99 228 K0II-IIIvar Schedar
β Cas β 11 432 746  00h 09m 10.09s +59° 09′ 00.8″ 2.28 1.17 54 F2III-IV Caph; δ Sct variable, Vmax = 2.25m, Vmin = 2.29m, P = 0.10 d
γ Cas γ 27 5394 4427  00h 56m 42.50s +60° 43′ 00.3″ 2.47 −4.22 613 B0IV:evar Tiansi[1], Tsih, Navi; prototype γ Cas variable, Vmax = 1.6m, Vmin = 3.0m
δ Cas δ 37 8538 6686  01h 25m 48.60s +60° 14′ 07.5″ 2.68 0.26 99 A5Vv SB Ruchbah; Algol variable, Vmax = 2.68m, Vmin = 2.76m, P = 759 d
ε Cas ε 45 11415 8886  01h 54m 23.68s +63° 40′ 12.5″ 3.35 −2.31 442 B2pvar Segin; variable star, ΔV = 0.002m, P = 0.09 d
η Cas η 24 4614 3821  00h 49m 05.10s +57° 48′ 59.6″ 3.46 4.59 19 G0V SB Achird, RS CVn variable
ζ Cas ζ 17 3360 2920  00h 36m 58.27s +53° 53′ 49.0″ 3.69 −2.62 597 B2IV Fùlù (附路),[2] suspected variable
50 Cas 50 12216 9598  02h 03m 26.19s +72° 25′ 16.5″ 3.95 0.47 162 A2V Gang[1], variable star, ΔV = 0.003m, P = 0.80 d
κ Cas κ 15 2905 2599  00h 32m 59.99s +62° 55′ 54.4″ 4.17 −6.34 4127 B1Ia Cexing[1], α Cyg variable, Vmax = 4.12m, Vmin = 4.21m, P = 2.65 d
θ Cas θ 33 6961 5542  01h 11m 05.93s +55° 08′ 59.8″ 4.34 1.22 137 A7Vvar Marfak; suspected variable
ι Cas ι 15089 11569  02h 29m 03.99s +67° 24′ 08.6″ 4.46 1.27 141 A5p Sr Huagai[1], α2 CVn variable, Vmax = 4.45m, Vmin = 4.53m, P = 1.74 d
ο Cas ο 22 4180 3504  00h 44m 43.50s +48° 17′ 03.8″ 4.48 −2.74 906 B5III triple star, γ Cas variable, Vmax = 4.31m, Vmin = 4.62m
48 Cas A 48 12111 9480  02h 01m 57.55s +70° 54′ 25.4″ 4.49 1.72 117 A3IV quadruple star
ρ Cas ρ 7 224014 117863  23h 54m 23.04s +57° 29′ 57.8″ 4.51 −9.5 8500 F8Ia0-M2I yellow hypergiant; semiregular variable, Vmax = 4.1m, Vmin = 6.2m, P = 320 d
υ2 Cas υ2 28 5395 4422  00h 56m 40.01s +59° 10′ 52.2″ 4.62 0.62 206 G8III-IV Castula
χ Cas χ 39 9408 7294  01h 33m 55.93s +59° 13′ 55.5″ 4.68 0.70 204 K0III
ψ Cas ψ 36 8491 6692  01h 25m 55.90s +68° 07′ 47.8″ 4.72 0.86 193 K0III
λ Cas λ 14 2772 2505  00h 31m 46.32s +54° 31′ 20.4″ 4.74 −0.44 354 B8Vn suspected variable
ξ Cas ξ 19 3901 3300  00h 42m 03.88s +50° 30′ 45.1″ 4.80 −2.86 1109 B2.5V suspected variable
HR 244 5015 4151  00h 53m 04.28s +61° 07′ 24.8″ 4.80 3.46 61 F8V spectroscopic binary
R Cas R 224490 118188  23h 58m 24.80s +51° 23′ 19.0″ 4.80 410 M6.5-9e Mira variable, Vmax = 4.7m, Vmin = 13.5m, P = 430 d
υ1 Cas υ1 26 5234 4292  00h 55m 00.19s +58° 58′ 22.1″ 4.83 −0.65 406 K2III
1 Cas 1 218376 114104  23h 06m 36.81s +59° 25′ 11.2″ 4.84 −2.81 1105 B0.5IV
HD 19275 19275 14862  03h 11m 56.24s +74° 23′ 37.9″ 4.85 1.37 162 A2Vnn Shangcheng[1]
τ Cas τ 5 223165 117301  23h 47m 03.39s +58° 39′ 06.7″ 4.88 1.26 173 K1III
σ Cas σ 8 224572 118243  23h 59m 00.53s +55° 45′ 17.8″ 4.88 −3.47 1523 B1V...
AR Cas AR 221253 115990  23h 30m 01.92s +58° 32′ 56.1″ 4.89 −1.34 575 B3IV septuple star; Algol variable, Vmax = 4.82m, Vmin = 4.96m, P = 6.07 d
ν Cas ν 25 4636 3801  00h 48m 49.99s +50° 58′ 05.5″ 4.90 −0.49 389 B9III
π Cas π 20 4058 3414  00h 43m 28.09s +47° 01′ 28.7″ 4.95 1.31 174 A5V rotating ellipsoidal variable
φ Cas φ 34 7927 6242  01h 20m 04.92s +58° 13′ 53.8″ 4.95 −4.32 2329 F0Ia foreground star appearing among NGC 457; suspected variable
4 Cas 4 220652 115590  23h 24m 50.25s +62° 16′ 58.2″ 4.96 −1.91 771 M1III slow irregular variable, Vmax = 4.95m, Vmin = 5.00m
ω Cas ω 46 11529 9009  01h 56m 00.00s +68° 41′ 07.0″ 4.97 −1.69 701 B8III suspected variable
HD 3240 3240 2854  00h 36m 08.29s +54° 10′ 06.4″ 5.08 −0.87 505 B7III
V509 Cas V509 217476 113561  23h 00m 05.10s +56° 56′ 43.4″ 5.10 −6.77 7723 F80 yellow hypergiant; semiregular variable, Vmax = 4.75m, Vmin = 5.5m
μ Cas μ 30 6582 5336  01h 08m 12.92s +54° 55′ 27.2″ 5.17 5.78 25 G5VIp/M5V Marfak; suspected variable
HD 15920 15920 12273  02h 38m 02.09s +72° 49′ 05.6″ 5.17 0.69 256 G8III
42 Cas 42 10250 8016  01h 42m 55.73s +70° 37′ 21.2″ 5.18 0.51 281 B9V suspected Algol variable
49 Cas 49 12339 9763  02h 05m 31.58s +76° 06′ 54.4″ 5.22 −0.36 426 G8III Rangifer[1]
47 Cas 47 12230 9727  02h 05m 07.05s +77° 16′ 53.2″ 5.27 2.64 109 F0Vn
40 Cas 40 9774 7650  01h 38m 30.94s +73° 02′ 24.3″ 5.28 −0.40 447 G8II-III suspected variable
HD 11946 11946 9312  01h 59m 37.99s +64° 37′ 17.9″ 5.29 0.81 257 A0Vn
31 Cas 31 6829 5518  01h 10m 39.27s +68° 46′ 43.3″ 5.32 0.38 318 A0Vnn
HD 4775 4775 3951  00h 50m 43.57s +64° 14′ 51.3″ 5.35 −1.63 813 A4V comp SB variable star, ΔV = 0.008m, P = 0.96 d
12 Cas 12 2011 1960  00h 24m 47.49s +61° 49′ 51.8″ 5.38 −1.47 763 B9III
HD 4222 4222 3544  00h 45m 17.20s +55° 13′ 17.1″ 5.41 0.25 351 A2Vs
23 Cas 23 4382 3721  00h 47m 46.02s +74° 50′ 51.3″ 5.42 −1.54 803 B8III
6 Cas 6 V566 223385 117447  23h 48m 50.17s +62° 12′ 52.3″ 5.43 −8.06 6150 A3Ia comp α Cyg variable, Vmax = 5.34m, Vmin = 5.45m, P = 37.26 d
HD 3474 3574 3083  00h 39m 09.89s +49° 21′ 16.5″ 5.45 −2.60 1331 K5III
HD 9900 9900 7617  01h 38m 07.56s +57° 58′ 39.5″ 5.55 −2.17 1140 G5II
HD 223173 223173 117299  23h 47m 01.91s +57° 27′ 05.0″ 5.55 −3.00 1672 K3II slow irregular variable, Vmax = 5.51m, Vmin = 5.54m
HD 5408 5408 4440  00h 56m 46.94s +60° 21′ 46.3″ 5.56 −0.81 614 B8V
HD 6960 6960 5566  01h 11m 25.52s +64° 12′ 09.8″ 5.56 0.06 410 B9.5V suspected eclipsing binary
HD 220369 220369 115395  23h 22m 32.52s +60° 08′ 00.6″ 5.56 −2.73 1482 K3II suspected variable
10 Cas 10 144 531  00h 06m 26.53s +64° 11′ 46.2″ 5.57 −1.82 982 B9III suspected variable
32 Cas 32 RU 6972 5589  01h 11m 41.37s +65° 01′ 08.0″ 5.57 0.34 363 B9IV RU Cas, suspected constant
43 Cas 43 V557 10221 7965  01h 42m 20.44s +68° 02′ 35.0″ 5.57 −0.10 444 A0p SiSr α2 CVn variable, Vmax = 5.55m, Vmin = 5.64m, P = 3.18 d
HD 219134 219134 114622  23h 13m 14.74s +57° 10′ 03.5″ 5.57 6.50 21 K3Vvar suspected variable; has 5-6 planets
HR 9059 V1022 224355 118077  23h 57m 08.49s +55° 42′ 20.6″ 5.57 1.45 218 G8Ib Algol variable, Vmax = 5.56m, Vmin = 5.68m, P = 12.16 d
HD 224893 224893 124  00h 01m 37.02s +61° 13′ 22.1″ 5.58 −4.75 3791 F0III suspected variable
HD 1976 V746 1976 1921  00h 24m 15.64s +52° 01′ 11.7″ 5.58 −2.54 1370 B5IV spectroscopic binary; slowly pulsating B star
HD 219623 219623 114924  23h 16m 42.19s +53° 12′ 50.6″ 5.58 4.04 66 F7V
HD 2774 2774 2497  00h 31m 41.21s +52° 50′ 22.4″ 5.59 0.18 393 K2III
53 Cas 53 12301 9573  02h 03m 00.19s +64° 23′ 24.1″ 5.59 −4.54 3468 B8Ib
HD 17948 17948 13665  02h 55m 56.74s +61° 31′ 15.8″ 5.59 3.48 86 F4V
HR 511 V987 10780 8362  01h 47m 44.06s +63° 51′ 11.2″ 5.63 5.64 33 K0V BY Draconis variable, ΔV = 0.05m, P = 21.7 d
YZ Cas 21 YZ 4161 3572  00h 45m 39.11s +74° 59′ 17.3″ 5.64 0.89 290 A2IV triple system; Algol variable
68 Cas 68 4142 3478  00h 44m 26.23s +47° 51′ 50.3″ 5.66 −1.18 760 B5V...
2 Cas 2 218753 114365  23h 09m 44.14s +59° 19′ 57.7″ 5.68 −3.23 1976 A5III suspected variable
HD 9352 9352 7251  01h 33m 25.71s +58° 19′ 38.4″ 5.69 −3.20 1952 K0Ib+... slow irregular variable, Vmax = 5.68m, Vmin = 5.72m
HD 2054 2054 1982  00h 25m 06.39s +53° 02′ 48.4″ 5.72 −0.33 528 B9IV suspected variable
HD 1239 1239 1354  00h 16m 57.05s +61° 31′ 59.5″ 5.74 −0.73 642 G8III
HD 6676 6676 5361  01h 08m 33.45s +58° 15′ 48.5″ 5.77 −0.43 567 B8V
HD 3283 3283 2876  00h 36m 27.34s +60° 19′ 34.4″ 5.78 −4.29 3361 A4III
44 Cas 44 10425 8046  01h 43m 19.74s +60° 33′ 04.9″ 5.78 −1.46 913 B8IIIn
HD 225289 V567 225289 418  00h 05m 06.13s +61° 18′ 50.3″ 5.80 −0.93 724 B8MNp... α2 CVn variable, Vmax = 5.71m, Vmin = 5.81m, P = 6.43 d
HD 16024 16024 12239  02h 37m 36.01s +65° 44′ 43.3″ 5.80 −1.19 815 K5III
38 Cas 38 9021 7078  01h 31m 13.52s +70° 15′ 53.2″ 5.82 3.49 95 F6V
HD 3856 3856 3299  00h 42m 03.44s +66° 08′ 51.4″ 5.83 −0.11 503 G9III-IV
HR 297 6210 5021  01h 04m 19.55s +61° 34′ 48.9″ 5.83 1.31 261 F6V
HD 1279 1279 1372  00h 17m 09.04s +47° 56′ 50.7″ 5.86 −1.47 953 B7III
HD 4440 4440 3750  00h 48m 08.88s +72° 40′ 28.0″ 5.86 1.69 223 K0IV
HD 225009 225009 207  00h 02m 36.08s +66° 05′ 56.3″ 5.87 −3.15 2076 G8III
V762 Cas V762 7389 5926  01h 16m 11.90s +71° 44′ 37.8″ 5.87 −7.42 2760 M3 BY Draconis variable
HD 19065 19065 14502  03h 07m 19.02s +64° 03′ 27.4″ 5.89 −0.27 557 B9V
9 Cas 9 225180 330  00h 04m 13.66s +62° 17′ 15.6″ 5.90 −4.35 3663 A1III suspected variable
HD 6130 6130 4962  01h 03m 37.01s +61° 04′ 29.4″ 5.92 −2.41 1509 F0II
HD 2952 2952 2611  00h 33m 10.32s +54° 53′ 42.3″ 5.93 0.62 376 K0III has a planet (b)
HD 2626 2626 2377  00h 30m 19.91s +59° 58′ 39.2″ 5.94 −0.77 718 B9IIIn
SU Cas SU 17463 13367  02h 51m 58.75s +68° 53′ 18.7″ 5.94 −2.24 1411 F5:Ib-II classical Cepheid, Vmax = 5.7m, Vmin = 6.18m, P = 1.95 d
HD 16769 16769 12821  02h 44m 49.67s +67° 49′ 29.0″ 5.95 0.47 406 A5III variable star
HD 5550 5550 4572  00h 58m 31.00s +66° 21′ 06.6″ 5.97 0.66 376 A0III
HR 5 V640 123 518  00h 06m 15.54s +58° 26′ 12.1″ 5.98 4.44 70 G5V eclipsing binary, ΔV = 0.066m, P = 1.03 d
HD 6211 6211 4998  01h 04m 02.39s +52° 30′ 08.3″ 5.99 −1.42 991 K2
52 Cas 52 12279 9564  02h 02m 52.49s +64° 54′ 05.4″ 6.00 1.30 284 A1Vn
HD 11857 11857 9220  01h 58m 33.22s +61° 41′ 52.1″ 6.02 −0.70 721 B5III suspected variable
V373 Cas V373 224151 117957  23h 55m 33.84s +57° 24′ 43.8″ 6.03 B0.5IIv SB spectroscopic binary; eclipsing binary, Vmax = 5.9m, Vmin = 6.3m, P = 13.41 d
HD 4817 4817 3988  00h 51m 16.39s +61° 48′ 19.8″ 6.04 −3.37 2489 K5Ib variable star, ΔV = 0.009m, P = 4.32 d
55 Cas 55 13474 10438  02h 14m 29.10s +66° 31′ 28.0″ 6.05 −0.72 738 B9V+... suspected variable
AO Cas AO 1337 1415  00h 17m 43.07s +51° 25′ 59.1″ 6.11 −5.11 5719 O9IIInn Pearce's Star; rotating ellipsoidal variable, Vmax = 6.07m, Vmin = 6.24m, P = 3.52 d
HD 12173 12173 9586  02h 03m 10.51s +73° 51′ 02.0″ 6.12 0.89 363 A5III
HD 9030 9030 7050  01h 30m 52.01s +66° 05′ 53.2″ 6.15 1.46 282 A2Vs
HD 17958 17958 13700  02h 56m 24.66s +64° 19′ 56.8″ 6.17 −1.80 1278 K3Ibvar
HD 224784 224784 43  00h 00m 30.98s +59° 33′ 35.1″ 6.18 0.59 427 G9III-IV suspected variable
HD 2589 2589 2422  00h 30m 54.20s +77° 01′ 10.2″ 6.18 3.20 128 K0IV
13 Cas 13 2729 2474  00h 31m 25.20s +66° 31′ 10.7″ 6.18 −0.53 716 B6V variable star, ΔV = 0.007m, P = 1.08 d
HD 3924 3924 3334  00h 42m 31.01s +58° 45′ 12.4″ 6.18 −1.29 1016 B9.5III
V773 Cas V773 10543 8115  01h 44m 17.91s +57° 32′ 12.0″ 6.18 1.69 258 A3V Algol variable
HD 5343 5343 4383  00h 56m 12.93s +57° 59′ 47.7″ 6.20 0.28 497 K3III
HD 224870 224870 106  00h 01m 19.24s +49° 58′ 53.7″ 6.22 −0.51 724 G7II-III
HD 4881 4881 4023  00h 51m 33.79s +51° 34′ 17.2″ 6.22 −1.51 1148 B9.5V
HD 225094 V639 225094 274  00h 03m 25.72s +63° 38′ 25.9″ 6.24 −3.92 3505 B3Ia α Cyg variable, Vmax = 6.19m, Vmin = 6.28m, P = 2.88 d
HD 217673 217673 113684  23h 01m 30.72s +57° 06′ 19.7″ 6.24 −1.56 1181 K2II suspected variable
HD 222618 222618 116912  23h 41m 54.56s +57° 15′ 35.9″ 6.24 −0.93 886 G8III
HD 10587 10587 8148  01h 44m 46.15s +57° 05′ 21.2″ 6.25 0.07 560 A2V
HD 13222 13222 10350  02h 13m 21.05s +74° 01′ 40.1″ 6.25 0.61 438 G8III
HD 21970 21970 17056  03h 39m 25.10s +75° 44′ 22.6″ 6.25 0.65 429 G9III-IV
RZ Cas RZ 17138 13133  02h 48m 55.51s +69° 38′ 03.1″ 6.26 2.28 204 A3V Algol variable, Vmax = 6.18m, Vmin = 7.72m, P = 1.20 d
HD 222570 222570 116876  23h 41m 26.80s +49° 30′ 44.9″ 6.26 −0.63 778 A4V
HD 5128 5128 4212  00h 53m 47.53s +52° 41′ 21.6″ 6.27 1.61 278 A5m
HD 5273 5273 4298  00h 55m 05.22s +48° 40′ 42.8″ 6.28 −0.68 803 M2.5IIIa variable star, ΔV = 0.012m, P = 21.89 d
HD 6540 6540 5251  01h 07m 09.44s +53° 29′ 53.5″ 6.31 −1.79 1358 K0
HD 7732 7732 6261  01h 20m 19.45s +77° 34′ 13.7″ 6.31 0.98 379 G5III...
35 Cas 35 8003 6312  01h 21m 05.19s +64° 39′ 29.5″ 6.33 2.01 238 A2Vnn
HD 10362 10362 8020  01h 42m 58.32s +61° 25′ 15.9″ 6.33 −1.15 1022 B7II
HD 223386 223386 117450  23h 48m 53.91s +59° 58′ 44.2″ 6.33 1.22 344 A0V
HD 8424 8424 6685  01h 25m 46.30s +70° 58′ 47.7″ 6.34 0.35 514 A0Vnn
HD 10293 10293 7963  01h 42m 17.69s +58° 37′ 39.9″ 6.35 −1.90 1455 B8III suspected variable
HD 8272 8272 6486  01h 23m 21.27s +58° 08′ 35.6″ 6.36 2.56 188 F4V
HD 223421 223421 117472  23h 49m 11.89s +58° 57′ 47.6″ 6.36 1.94 250 F2IV
HD 7925 7925 6378  01h 21m 58.94s +76° 14′ 20.0″ 6.37 1.95 250 F0IVn
V805 Cas V805 21179 16319  03h 30m 19.39s +71° 51′ 50.0″ 6.37 −0.73 856 M2III semiregular variable
HD 4818 V526 4818 3965  00h 50m 57.27s +51° 30′ 28.9″ 6.38 2.26 217 F2IV δ Sct variable, ΔV = 0.03m
HD 4295 4295 3641  00h 46m 38.23s +69° 19′ 31.3″ 6.39 3.35 132 F3V
HD 5357 5357 4446  00h 56m 54.99s +68° 46′ 32.7″ 6.39 2.51 195 F0m
V465 Cas V465 7733 6093  01h 18m 13.89s +57° 48′ 11.4″ 6.39 −0.75 874 M5 semiregular variable, Vmax = 6.1m, Vmin = 7.2m, P = 60 d
HD 220074 220074 115218  23h 20m 14.37s +61° 58′ 12.5″ 6.39 −0.91 942 K1V suspected variable; has a planet
HD 5715 5715 4709  01h 00m 30.87s +70° 58′ 58.8″ 6.40 1.21 355 A4IV
V761 Cas V761 7157 5688  01h 13m 09.82s +61° 42′ 22.3″ 6.40 −0.11 652 B9V α2 CVn variable
HD 222682 222682 116962  23h 42m 31.41s +61° 40′ 45.8″ 6.40 0.66 459 K2III
HD 371 371 695  00h 08m 32.87s +63° 12′ 14.6″ 6.41 −1.91 1502 G3II
HD 2904 2904 2628  00h 33m 19.20s +70° 58′ 54.7″ 6.41 0.36 528 A0Vn
HD 4362 4362 3649  00h 46m 42.47s +59° 34′ 28.3″ 6.41 G0Ib
HD 6497 6497 5240  01h 07m 00.07s +56° 56′ 06.9″ 6.41 1.47 318 K2III...
HD 218440 218440 114163  23h 07m 10.45s +59° 43′ 38.6″ 6.41 −1.65 1336 B2.5IV
HD 220130 220130 115245  23h 20m 34.54s +62° 12′ 47.8″ 6.41 −2.24 1753 K2III
HR 9017 V650 223358 117430  23h 48m 39.03s +64° 52′ 35.3″ 6.41 −0.30 718 A0sp... α2 CVn variable, ΔV = 0.02m
HD 1142 1142 1269  00h 15m 54.87s +61° 00′ 00.7″ 6.43 0.23 566 G8III...
HD 217944 217944 113852  23h 03m 21.33s +58° 33′ 50.0″ 6.43 1.71 286 G8IV
HD 5459 5459 4475  00h 57m 19.53s +61° 25′ 19.0″ 6.44 0.21 575 G8IV
HD 222748 222748 116991  23h 43m 05.03s +51° 56′ 21.6″ 6.44 0.27 559 K0
HD 1601 1601 1639  00h 20m 30.92s +48° 58′ 07.1″ 6.46 −0.86 950 G0
HD 17581 17581 13347  02h 51m 45.92s +58° 18′ 51.5″ 6.46 1.75 285 A1m
HD 222932 222932 117133  23h 44m 48.37s +55° 47′ 58.9″ 6.46 0.65 473 G4III:
16 Cas 16 3038 2707  00h 34m 24.89s +66° 45′ 01.3″ 6.47 0.28 565 B9III
V801 Cas V801 19243 14626  03h 08m 54.18s +62° 23′ 04.5″ 6.47 −2.48 2012 B1V:e Be star
HD 223552 223552 117551  23h 50m 22.12s +51° 37′ 18.1″ 6.47 3.43 132 F3V
HD 224404 224404 118116  23h 57m 33.52s +60° 01′ 25.0″ 6.47 −1.26 1144 B9III-IV
HD 5927 5927 4786  01h 01m 27.04s +49° 32′ 39.2″ 6.48 −0.77 921 G5
HD 6028 6028 4844  01h 02m 18.47s +51° 02′ 05.9″ 6.48 0.04 632 A3V
HD 9811 9811 7593  01h 37m 47.20s +64° 44′ 21.7″ 6.49 −3.30 2964 A6Iab
HR 8770 V638 217833 113797  23h 02m 43.80s +55° 14′ 11.0″ 6.50 723 B9IIIwe... α2 CVn variable
HD 19439 19439 14791  03h 11m 00.80s +64° 53′ 46.7″ 6.50 2.03 256 A4V
V649 Cas V649 219634 114904  23h 16m 27.05s +61° 57′ 46.6″ 6.53 3500 B0Vn Algol variable, ΔV = 0.1m, P = 2.39 d
54 Cas 54 12800 10031  02h 09m 07.69s +71° 33′ 09.3″ 6.57 4.39 89 F8
V816 Cas V816 222670 116948  23h 42m 20.95s +64° 30′ 55.4″ 6.58 942 M2III slow irregular variable
V764 Cas V764 7636 6027  01h 17m 26.69s +57° 37′ 55.5″ 6.61 1900 B2IIIne Be star
V784 Cas V784 13122 10141  02h 10m 25.5s +59° 58′ 47.3″ 6.64 335 F5II δ Sct variable
V772 Cas V772 10260 7939  01h 42m 02.91s +61° 02′ 17.7″ 6.69 1220 B8IIIsp... Algol variable
V809 Cas V809 219978 115141  23h 19m 23.77s +62° 44′ 23.2″ 6.74 1960 K4.5Ib slow irregular variable
V779 Cas V779 12013 9494  02h 02m 09.31s +75° 30′ 07.8″ 6.78 626 A0 Algol variable
HD 11755 11755 9242  01h 58m 50.0s +73° 09′ 09″ 6.87 755 G5 has a planet (b)
TU Cas TU 2207 2085  00h 26m 19.45s +51° 16′ 49.3″ 6.88 F3II... double-mode Cepheid, Vmax = 6.88m, Vmin = 8.18m, P = 2.14 d
HD 18391 18391 13962  02h 59m 48.72s +57° 39′ 47.7″ 6.89 −7.8 8000 G5Ia-Ib Semiregular variable
HD 223960 V819 223960 117830  23h 53m 49.98s +60° 51′ 12.2″ 6.90 A0.1Ia α Cyg variable
V Cas V 218997 114515  23h 11m 40.72s +59° 41′ 59.0″ 6.90 1520 M5-7.5e Mira variable, Vmax = 6.9m, Vmin = 13.4m, P = 229 d
V486 Cas V486 3950 3346  00h 42m 37.99s +52° 20′ 13.7″ 6.95 B1III eclipsing binary, ΔV = 0.04m, P = 5.56 d
HD 14817 V559 14817 11318  02h 25m 40.11s +61° 32′ 58.8″ 7.02 695 B8V Algol variable, Vmax = 7.01m, Vmin = 7.23m, P = 1.58 d
V777 Cas V777 11606 8980  01h 55m 42.85s +59° 16′ 24.4″ 7.02 959 B2Vne Be star
HD 17505 17505 13296  02h 51m 07.98s +60° 25′ 03.9″ 7.08 2860 O7V((f))+O9I associated with a bow shock
CC Cas CC 19820 15063  03h 14m 05.33s +59° 33′ 48.5″ 7.08 1860 O8.5III β Lyr variable, Vmax = 7.06m, Vmin = 7.3m, P = 3.37 d
HD 698 V742 698 940  00h 11m 37.15s +58° 12′ 42.6″ 7.08 3500 B7:Ib-IIe Be star
V989 Cas V989 13579 10531  02h 15m 42.56s +67° 40′ 20.3″ 7.13 60.6 K2V BY Dra variable, ΔV = 0.03m, P = 6.79 d
V636 Cas V636 9250 7192  01h 32m 43.23s +63° 35′ 37.7″ 7.19 1640 G0Ib classical Cepheid, Vmax = 7.09m, Vmin = 7.26m, P = 8.38 d
HD 7924 7924 6379  01h 21m 59.12s +76° 42′ 37.0″ 7.19 6.06 55 K0V has three planets (b, c & d)
TV Cas TV 1486 1550  00h 19m 18.74s +59° 08′ 20.6″ 7.22 516 B9V Algol variable, Vmax = 7.22m, Vmin = 8.22m, P = 1.81 d
V755 Cas V755 3940 3367  00h 42m 50.06s +64° 17′ 28.6″ 7.29 3700 A1Ia α Cyg variable, Vmax = 7.25m, Vmin = 7.31m, P = 5.67 d
RV Cas RV 5016  00h 52m 42.76s +47° 24′ 56.1″ 7.3 M5-6.5Se Mira variable, Vmax = 7.3m, Vmin = 16.1m, P = 332 d
HD 108 108 505  00h 06m 03.39s +63° 40′ 46.8″ 7.40 3800 O4-8f?p binary star; runaway star; variable spectrum
HD 221585 221585 116221  23h 32m 54.0s +63° 09′ 20″ 7.47 G8IV has a planet (b)
HD 13908 13908 10743  02h 18m 15.0s +65° 35′ 40″ 7.51 232 F8V has two planets (b & c)
Gliese 83.3 V598 12208 9481  02h 01m 59.06s +61° 54′ 18.2″ 7.52 906 K5III slow irregular variable, Vmax = 7.38m, Vmin = 7.54m
HD 221568 V436 221568 116210  23h 32m 47.65s +57° 54′ 20.1″ 7.55 709 A0p Osawa's Star; α2 CVn variable, Vmax = 7.55m, Vmin = 7.62m, P = 159 d
HD 19557 V623 19557 14827  03h 11m 25.33s +57° 54′ 11.2″ 7.57 1590 C4,5J slow irregular variable, Vmax = 7.34m, Vmin = 7.96m
V487 Cas V487 6474 5239  01h 06m 59.74s +63° 46′ 23.4″ 7.60 G4Ia UU Her variable, Vmax = 7.44m, Vmin = 7.74m, P = 99.6 d
HD 16429 V482 16429 12495  02h 40m 44.94s +61° 16′ 56.1″ 7.65 O9.5III+F4V triple star; β Cep variable
WZ Cas WZ 224855 99  00h 01m 15.85s +60° 21′ 19.0″ 7.70 2860 C9,2JLi semiregular variable, Vmax = 6.8m, Vmin = 7.7m, P = 186 d
HD 12288 V540 12288 9604  02h 03m 30.51s +69° 34′ 56.4″ 7.74 1010 A2 α2 CVn variable, Vmax = 7.73m, Vmin = 7.75m, P = 34.9 d
W Cas W 5235 4284  00h 54m 53.85s +58° 33′ 49.1″ 7.80 C9,1e Mira variable, Vmax = 7.8m, Vmin = 12.5m, P = 406 d
HD 15558 15558 11832  02h 32m 42.54s +61° 27′ 21.6″ 7.87 O4.5III in IC 1805; binary star; extremely luminous
S Cas S 7769  01h 19m 41.99s +72° 36′ 40.8″ 7.9 S3-5/4-8 Mira variable, Vmax = 7.9m, Vmin = 16.1m, P = 612 d
HD 220842 220842 115714  23h 26m 37.0s +56° 53′ 12″ 7.99 204 F8 has a planet (b)
U Cas U 4350  00h 46m 21.37s +48° 14′ 38.7″ 8.0 S4.5-6/3-5e Mira variable, Vmax = 8m, Vmin = 15.7m, P = 277 d
HD 15570 15570 11837  02h 32m 49.42s +61° 22′ 42.1″ 8.11 2100 O4If+ in IC 1805
V745 Cas V745 1810 1805  00h 22m 53.32s +62° 14′ 29.1″ 8.11 B0V+B1.5III β Lyr variable
HD 220147 V812 220147 115267  23h 20m 48.92s +62° 24′ 45.2″ 8.12 1060 B9p α2 CVn variable
HD 17156 17156 13192  02h 49m 44.49s +71° 45′ 11.6″ 8.17 3.70 255 G0IV Nushagak,[3] has a confirmed transiting planet (b)
HD 240237 240237 114840  23h 15m 42.22s +58° 02′ 35.7″ 8.17 K2 has a planet (b)
HD 17520 17520 13308  02h 51m 14.46s +60° 23′ 09.8″ 8.24 O8V+O9:V transitioned to a Be star in the 1980s
V641 Cas V641  00h 09m 26.34s +63° 57′ 14.1″ 8.30 M0 semiregular variable
V368 Cas V368 19644 14936  03h 12m 35.54s +59° 55′ 10.9″ 8.32 B8II-III Algol variable
HD 240210 240210  23h 10m 29.23s +57° 01′ 46.0″ 8.33 2.55 468 K3III has a planet
V605 Cas V605 14242 10904  02h 20m 22.47s +59° 40′ 16.9″ 8.36 1570 M2Iab slow irregular variable, Vmax = 8.22m, Vmin = 8.48m
TW Cas TW 16907 12906  02h 45m 54.82s +65° 43′ 35.1″ 8.38 849 A0V Algol variable, Vmax = 8.32m, Vmin = 8.98m, P = 1.43 d
HD 15629 15629 11891  02h 33m 20.59s +61° 31′ 18.2″ 8.42 1330 O4.5V in IC 1805
HD 5797 V551 5797 4717  01h 00m 33.43s +60° 26′ 40.9″ 8.47 1490 Am α2 CVn variable, Vmax = 8.43m, Vmin = 8.77m, P = 69 d
Z Cas Z 222914  23h 44m 31.59s +56° 34′ 52.7″ 8.5 M7e Mira variable, Vmax = 8.5m, Vmin = 15.4m, P = 496 d
HD 217850 217850 113789  23h 02m 37.0s +58° 52′ 34″ 8.5 199 G8V has a companion star (B)
DO Cas DO 16506 12543  02h 41m 24.16s +60° 33′ 11.8″ 8.54 533 A2II β Lyr variable, Vmax = 8.39m, Vmin = 9.01m, P = 0.68 d
HD 12098 V988 12098  02h 00m 40.18s +58° 31′ 37.1″ F0 rapidly oscillating Ap star
RW Cas RW 7548  01h 37m 14.02s +57° 45′ 33.2″ 8.58 G2 classical Cepheid, Vmax = 8.62m, Vmin = 9.67m, P = 14.79 d
DL Cas DL 236429 2347  00h 29m 58.59s +60° 12′ 43.1″ 8.63 1480 G1Ib-II_Hdel-1 in NGC 129; classical Cepheid, Vmax = 8.63m, Vmin = 9.26m, P = 8.00 d
RX Cas RX 14542  03h 05m 45.75s +67° 34′ 38.6″ 8.64 K1III+A5eIII β Lyr variable, Vmax = 8.64m, Vmin = 9.49m, P = 32.31 d
Y Cas Y 225082  00h 03m 21.47s +55° 40′ 51.8″ 8.70 M7.5e Mira variable, Vmax = 8.7m, Vmin = 15.3m, P = 413 d
BD+60 2522  23h 20m 44.52s +61° 11′ 40.6″ 8.7 300 O6.5III source of nebula NGC 7635
T Cas T 1845 1834  00h 23m 14.27s +55° 47′ 33.2″ 8.87 M7-9e Mira variable, Vmax = 6.9m, Vmin = 13m, P = 445 d
PZ Cas PZ 117078  23h 44m 03.28s +61° 47′ 22.2″ 8.90 M3Iab: semiregular variable
BM Cas BM 4279  00h 54m 45.95s +64° 05′ 06.2″ 8.91 1850 F0Ia β Lyr variable, Vmax = 8.78m, Vmin = 9.31m, P = 197 d
HD 219415 219415  23h 14m 54.0s +56° 43′ 49″ 8.94 K0III has a planet
SX Cas SX 232121 871  00h 10m 42.08s +54° 53′ 29.4″ 8.87 771 B5+K3III Algol variable, Vmax = 8.96m, Vmin = 9.83m, P = 36.56 d
WW Cas WW 7260  01h 33m 32.69s +57° 45′ 05.4″ 9.10 C5,5 slow irregular variable, Vmax = 9.1m, Vmin = 11.7m
FM Cas FM 236349 1162  00h 14m 28.24s +56° 15′ 10.6″ 9.16 F7.5Ib classical Cepheid, Vmax = 8.82m, Vmin = 9.47m, P = 5.81 d
TZ Cas TZ 117763  23h 52m 56.24s +61° 00′ 08.4″ 9.18 M3Iab slow irregular variable, Vmax = 8.86m, Vmin = 10.5m
AZ Cas AZ  01h 42m 16.51s +61° 25′ 16.3″ 9.22 M0Ib:ep+B Algol variable, Vmax = 9.22m, Vmin = 9.52m, P = 3402 d
TX Cas TX  02h 52m 16.19s +62° 46′ 57.5″ 9.33 B1V β Lyr variable, Vmax = 9.16m, Vmin = 9.8m, P = 2.93 d
X Cas X 9057  01h 56m 38.09s +59° 15′ 33.7″ 9.45 942 C5,4e Mira variable, Vmax = 9.45m, Vmin = 13.2m, P = 423 d
XX Cas XX  01h 29m 34.61s +60° 58′ 04.7″ 9.57 B4Vn Algol variable
SZ Cas SZ 11420  02h 27m 13.77s +59° 27′ 38.2″ 9.60 1210 G5III classical Cepheid, Vmax = 9.6m, Vmin = 10.02m, P = 13.63 d
SW Cas SW 114160  23h 07m 10.08s +58° 33′ 15.1″ 9.74 1520 K0 classical Cepheid, Vmax = 9.32m, Vmin = 10.01m, P = 5.44 d
UU Cas UU 117576  23h 50m 39.52s +60° 54′ 39.1″ 9.74 B1Iab: β Lyr variable
DD Cas DD 118122  23h 57m 34.96s +62° 43′ 05.7″ 9.84 F7 classical Cepheid, Vmax = 9.56m, Vmin = 10.18m, P = 9.81 d
PV Cas PV 240208  23h 10m 02.58s +59° 12′ 06.1″ 9.86 B6V Algol variable, Vmax = 9.71m, Vmin = 10.36m, P = 1.75 d
SY Cas SY 1213  00h 15m 09.81s +58° 25′ 27.4″ 9.92 1210 F5 classical Cepheid, Vmax = 9.4m, Vmin = 10.24m, P = 4.07 d
DN Cas DN  02h 23m 11.53s +60° 49′ 50.1″ 9.93 O8Vv Algol variable, Vmax = 9.81m, Vmin = 10.24m, P = 2.31 d
RY Cas RY 117690  23h 52m 07.03s +58° 44′ 30.2″ 9.95 F9Ib classical Cepheid, Vmax = 9.38m, Vmin = 10.39m, P = 12.14 d
XY Cas XY 236542 3886  00h 49m 53.26s +60° 07′ 38.6″ 9.97 1190 F6Iab-b:... classical Cepheid, Vmax = 9.61m, Vmin = 10.26m, P = 4.50 d
OX Cas OX 5391  01h 09m 00.10s +61° 28′ 14.8″ 10.06 1230 B1V Algol variable, Vmax = 9.9m, Vmin = 10.35m, P = 2.49 d
RS Cas RS 116556  23h 37m 16.06s +62° 25′ 44.4″ 10.06 F7-G1Ib classical Cepheid, Vmax = 9.53m, Vmin = 10.36m, P = 6.39 d
QQ Cas QQ  23h 45m 36.75s +59° 54′ 21.6″ 10.20 B2 β Lyr variable
V381 Cas V381  00h 32m 51.61s +49° 19′ 39.3″ 10.22 B Algol variable
QX Cas QX  23h 58m 43.15s +61° 09′ 39.5″ 10.25 B1V+B1V Algol variable, Vmax = 10.19m, Vmin = 10.7m, P = 6.00 d
V547 Cas V547 2552  00h 32m 29.43s +67° 14′ 08.4″ 10.29 32.8 M2V+M3V triple star; flare star
AQ Cas AQ 6174  01h 19m 10.35s +62° 23′ 48.4″ 10.31 B3 Algol variable, Vmax = 10.06m, Vmin = 11m, P = 11.72 d
AB Cas AB 12235  02h 37m 31.51s +71° 18′ 16.3″ 10.32 888 A3Vv+... Algol and δ Sct variable, Vmax = 10.1m, Vmin = 11.85m, P = 1.37 d
V459 Cas V459  01h 11m 29.92s +61° 08′ 48.0″ 10.36 B9 Algol variable
BY Cas BY 8312  01h 47m 11.92s +61° 25′ 21.0″ 10.41 F5 classical Cepheid, Vmax = 10.06m, Vmin = 10.58m, P = 3.22 d
VX Cas VX  00h 31m 30.68s +61° 58′ 51.0″ 10.50 A0Vep UX Ori star, Vmax = 10.5m, Vmin = 13.3m
WR 1 V863 4004 3415  00h 43m 28.40s +64° 45′ 35.4″ 10.54 WN4-s
MWC 419 V594 3401  00h 43m 18.26s +61° 54′ 40.1″ 10.60 657 B8eq Orion variable
CE Cas CE  23h 58m 09.31s +61° 12′ 49.3″ 10.63 10800 F9Ib+F8Ib in NGC 7790; binary classical Cepheid, Vmax = 10.63m, Vmin = 11.15m, P = 5.14 d and Vmax = 10.62m, Vmin = 11.30m, P = 4.48 d
CD Cas CD
V405		 117154  23h 45m 02.63s +63° 00′ 13.9″ 10.64 1230 F6-G5 classical Cepheid, Vmax = 10.37m, Vmin = 11.15m, P = 7.80 d
VW Cas VW 5138  01h 05m 48.22s +61° 45′ 17.8″ 10.67 K0 classical Cepheid, Vmax = 10.36m, Vmin = 11.07m, P = 5.99 d
WR 3 9974 7681  01h 38m 55.63s +58° 09′ 22.7″ 10.69 WN3h-w surrounded by a unique stellar-wind bubble
VV Cas VV 8614  01h 51m 07.03s +59° 53′ 17.5″ 10.73 F6 classical Cepheid, Vmax = 10.26m, Vmin = 11.2m, P = 6.21 d
DF Cas DF 12817  02h 44m 43.31s +61° 27′ 52.9″ 10.74 F8 classical Cepheid, Vmax = 10.53m, Vmin = 11.13m, P = 3.83 d
V364 Cas V364  00h 52m 43.01s +50° 28′ 10.2″ 10.75 A7 Algol variable, Vmax = 10.53m, Vmin = 11.22m, P = 1.54 d
WY Cas WY  23h 58m 01.30s +56° 29′ 13.5″ 10.76 S6-6.5/6-e Mira variable
ZZ Cas ZZ 2644  00h 33m 30.38s +62° 30′ 40.2″ 10.79 1290 B3 β Lyr variable
CH Cas CH 115390  23h 22m 28.44s +62° 45′ 25.7″ 10.79 F3Ibp classical Cepheid, Vmax = 10.47m, Vmin = 11.56m, P = 15.09 d
CF Cas CF 118174  23h 58m 17.98s +61° 13′ 15.8″ 10.80 10800 B3 in NGC 7790; classical Cepheid, Vmax = 10.8m, Vmin = 11.47m, P = 4.88 d
BP Cas BP 5846  01h 15m 01.09s +65° 35′ 57.9″ 10.80 F6 classical Cepheid, Vmax = 10.55m, Vmin = 11.33m, P = 6.27 d
LS I +61 303 V615 12469  02h 40m 31.67s +61° 13′ 45.6″ 10.8 B0Ve microquasar, Vmax = 10.4m, Vmin = 11.1m, P = 26.50 d
V523 Cas V523  00h 40m 06.26s +50° 14′ 15.5″ 10.87 K4V W UMa variable, Vmax = 10.62m, Vmin = 11.45m, P = 0.23 d
WASP-93  00h 37m 50.0s +51° 17′ 20″ 10.97 815 F4 has a transiting planet (b)
CW Cas CW  00h 45m 52.69s +63° 05′ 08.4″ 11.08 1340 G8V W UMa variable, Vmax = 11.02m, Vmin = 11.62m, P = 0.32 d
2S 0114+650 V662 6081  01h 18m 02.70s +65° 17′ 29.9″ 11.09 B1Iae X-ray pulsar, Vmax = 10.97m, Vmin = 11.09m, P = 11.60 d
IR Cas IR  23h 06m 52.37s +54° 04′ 52.2″ 11.14 F4... β Lyr variable
IT Cas IT  23h 42m 01.40s +51° 44′ 36.8″ 11.23 F6 Algol variable
WR 2 6327 5100  01h 05m 23.01s +60° 25′ 19.0″ 11.33 WN2-w The only WN2 star known, GRB candidate
CG Cas CG  00h 00m 59.25s +60° 57′ 32.2″ 11.28 F5 classical Cepheid, Vmax = 10.89m, Vmin = 11.73m, P = 4.35 d
RX J0146.9+6121 V831  01h 47m 00.21s +61° 31′ 23.7″ 11.34 B1III-Ve in NGC 663; X-ray pulsar, Vmax = 11.3m, Vmin = 11.5m
IV Cas IV  23h 49m 31.53s +53° 08′ 04.8″ 11.34 A2 Algol and δ Sct variable
IX Cas IX 390  00h 04m 50.82s +50° 14′ 05.5″ 11.36 637 F7 W Vir variable, Vmax = 11.19m, Vmin = 11.77m, P = 9.15 d
UZ Cas UZ 5658  01h 12m 41.16s +61° 12′ 48.1″ 11.45 1840 G2 classical Cepheid, Vmax = 10.93m, Vmin = 11.73m, P = 4.26 d
GP Cas GP 12416  02h 39m 50.44s +59° 35′ 51.3″ 11.50 M2Iab slow irregular variable
MWC 1080 V628 114995  23h 17m 25.58s +60° 50′ 43.4″ 11.58 B0eq Orion variable, Vmax = 10.88m, Vmin = 11.84m
CY Cas CY 115925  23h 29m 12.77s +63° 22′ 27.5″ 11.67 G1-2Ib classical Cepheid, Vmax = 11.07m, Vmin = 12.21m, P = 14.38 d
UV Cas UV  23h 02m 14.66s +59° 36′ 36.7″ 11.80 F0/5Ib R CrB variable
BS Cas BS  01h 21m 38.57s +59° 10′ 27.1″ 11.84 A-F W UMa variable, Vmax = 11.50m, Vmin = 12.16m, P = 0.44 d
Gliese 82 V596 9291  01h 59m 23.51s +58° 31′ 16.1″ 12.04 39.9 M4Ve flare star
V627 Cas V627 113373  22h 57m 40.99s +58° 09′ 12.5″ 12.4 M2eII-III semiregular variable, Vmax = 12.4m, Vmin = 13.24m
TY Cas TY  00h 36m 59.42s +63° 08′ 01.7″ M6 Mira variable
V592 Cas V592  00h 20m 52.22s +55° 42′ 16.3″ 12.79 OB nova-like star, ΔV = 0.4m, P = 0.12 d
HV Cas HV  01h 11m 03.48s +53° 43′ 40.2″ 12.9 Ce Mira variable
BH Cas BH  00h 21m 21.38s +59° 09′ 05.4″ 13 B3 W UMa variable, Vmax = 12.51m, Vmin = 13.10m, P = 0.41 d
IRAS 23304+6147  23h 32m 44.79s +62° 03′ 49.1″ 13.1 G2Ia post-AGB star, ΔV = 0.20m, P = 85 d
LkHα 198 V633  00h 11m 25.83s +58° 49′ 28.6″ 13.79 B9e Herbig Ae/Be star; Orion variable
V664 Cas V664  03h 03m 47.01s +64° 54′ 35.7″ 14.56 central star of HFG 1, re-radiating binary system
V425 Cas V425  23h 03m 46.66s +53° 17′ 14.9″ VY Scl variable
V709 Cas V709  00h 28m 48.84s +59° 17′ 22.0″ DQ Her variable
4U 0115+634 V635  01h 18m 31.90s +63° 44′ 24.0″ 15.19 B0.2Ve X-ray pulsar, Vmax = 14.5m, Vmin = 16.3m, P = 24.3 d
V376 Cas V376  00h 11m 26.52s +58° 50′ 03.7″ A3/F2e Orion variable
IGR J00234+6141 V1033  00h 22m 57.64s +61° 41′ 07.6″ 16.1 DQ Her variable, Vmax = 16.1m, Vmin = 16.9m, P = 0.17 d
V705 Cas V705  23h 41m 47.19s +57° 30′ 59.5″ 16.4 nova, Vmax = 5.7m, Vmin = 16.4m
Tycho G  00h 25m 19.9s +64° 08′ 18″ 17 G2IV former companion of progenitor of SN 1572
V723 Cas V723  01h 05m 05.36s +54° 00′ 40.3″ 18.0 A7 nova, Vmax = 7.08m, Vmin = <18.0m
RNO 1B V710  00h 36m 46.30s +63° 28′ 54.1″ 18.6 F8II FU Ori star, Vmax = 18.6m, Vmin = 21.6m
HT Cas HT  01h 10m 13.13s +60° 04′ 35.4″ 19.32 M5.5e SU UMa variable and eclipsing binary, Vmax = 12.6m, Vmin = 19.32m
4U 0142+61  01h 46m 22.21s +61° 45′ 03.8″ 25.62 magnetar
IGR J00291+5934 V1037  00h 29m 13.06s +59° 34′ 19.0″ X-ray pulsar with millisecond pulsar
1E 2259+586  23h 01m 08.14s +58° 52′ 44.5″ magnetar
PSR B2319+60  23h 21m 55.21s +60° 24′ 30.7″ pulsar
PSR B2334+61  23h 37m 05.78s +61° 51′ 01.7″ pulsar
PSR J0205+6449  02h 05m 37.92s +64° 49′ 42.8″ central pulsar of 3C 58
OH 127.8+0.0 V669  01h 33m 51.21s +62° 26′ 53.2″ M9III Mira variable
W3 IRS 5  02h 25m 40.54s +62° 05′ 51.4″ B1 protostar; possibly similar to a proto-Trapezium
IRAS 00338+6312  00h 36m 47.5s +63° 29′ 02″ protostar
Table legend:

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 IAU-Catalog of Star Names
  2. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 9 日
  3. ↑ "United States of America" (in en). http://www.nameexoworlds.iau.org/united-states-america. 
Short description: Constellation in the northern celestial hemisphere
Cassiopeia
Constellation
Cassiopeia
AbbreviationCas
GenitiveCassiopeiae
Symbolismthe Seated Queen
Right ascension 22h 57m 04.5897s– 03h 41m 14.0997s[1]
Declination77.6923447°–48.6632690°[1]
Area598 sq. deg. (25th)
Main stars5
Bayer/Flamsteed
stars		53
Stars with planets14
Stars brighter than 3.00m4
Stars within 10.00 pc (32.62 ly)7
Brightest starα Cas (Schedar)[lower-alpha 1] (2.24m)
Messier objects2
Meteor showersPerseids
Bordering
constellations		Camelopardalis
Cepheus
Lacerta
Andromeda
Perseus
Visible at latitudes between +90° and −20°.
Best visible at 21:00 (9 p.m.) during the month of November.

Cassiopeia (About this soundlisten) is a constellation and asterism in the northern sky named after the vain queen Cassiopeia, mother of Andromeda, in Greek mythology, who boasted about her unrivaled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'W' shape, formed by five bright stars.

Cassiopeia is located in the northern sky and from latitudes above 34°N it is visible year-round. In the (sub)tropics it can be seen at its clearest from September to early November, and at low southern, tropical, latitudes of less than 25°S it can be seen, seasonally, low in the North.

At magnitude 2.2, Alpha Cassiopeiae, or Schedar, is generally the brightest star in Cassiopeia, though it is occasionally outshone by the variable Gamma Cassiopeiae, which has reached magnitude 1.6. The constellation hosts some of the most luminous stars known, including the yellow hypergiants Rho Cassiopeiae and V509 Cassiopeiae and white hypergiant 6 Cassiopeiae. In 1572, Tycho Brahe's supernova flared brightly in Cassiopeia.[2] Cassiopeia A is a supernova remnant and the brightest extrasolar radio source in the sky at frequencies above 1 GHz. Fourteen star systems have been found to have exoplanets, one of which—HD 219134—is thought to host six planets. A rich section of the Milky Way runs through Cassiopeia, containing a number of open clusters, young luminous galactic disc stars, and nebulae. IC 10 is an irregular galaxy that is the closest known starburst galaxy and the only one in the Local Group of galaxies.

Mythology

Cassiopeia in her chair, as depicted in Urania's Mirror

The constellation is named after Cassiopeia, the queen of Aethiopia. Cassiopeia was the wife of King Cepheus of Aethiopia[2] and mother of Princess Andromeda. Cepheus and Cassiopeia were placed next to each other among the stars, along with Andromeda. She was placed in the sky as a punishment after enraging Poseidon with the boast that her daughter Andromeda was more beautiful than the Nereids or, alternatively, that she herself was more beautiful than the sea nymphs.[3] She was forced to wheel around the north celestial pole on her throne, spending half of her time clinging to it so she does not fall off, and Poseidon decreed that Andromeda should be bound to a rock as prey for the monster Cetus. Andromeda was then rescued by the hero Perseus, whom she later married.[4][5]

Cassiopeia has been variously portrayed throughout her history as a constellation. In Persia, she was drawn by al-Sufi as a queen holding a staff with a crescent moon in her right hand, wearing a crown, as well as a two-humped camel. In France, she was portrayed as having a marble throne and a palm leaf in her left hand, holding her robe in her right hand. This depiction is from Augustin Royer's 1679 atlas.[4]

In Chinese astronomy, the stars forming the constellation Cassiopeia are found among three areas: the Purple Forbidden enclosure (紫微垣, Zǐ Wēi Yuán), the Black Tortoise of the North (北方玄武, Běi Fāng Xuán Wǔ), and the White Tiger of the West (西方白虎, Xī Fāng Bái Hǔ).

The Chinese astronomers saw several figures in what is modern-day Cassiopeia. Kappa, Eta, and Mu Cassiopeiae formed a constellation called the Bridge of the Kings; when seen along with Alpha and Beta Cassiopeiae, they formed the great chariot Wang-Liang. The charioteer's whip was represented by Gamma Cassiopeiae, sometimes called "Tsih", the Chinese word for "whip".[4]

In Hindu Mythology, Cassiopeia was associated with the mythological figure Sharmishtha – the daughter of the great Devil (Daitya) King Vrishparva and a friend to Devayani (Andromeda).

In Welsh Mythology Llys Dôn (literally "The Court of Dôn") is the traditional Welsh name for the constellation. At least three of Dôn's children also have astronomical associations: Caer Gwydion ("The fortress of Gwydion") is the traditional Welsh name for the Milky Way, and Caer Arianrhod ("The Fortress of Arianrhod") being the constellation of Corona Borealis.[6]

In the 17th century, various Biblical figures were depicted in the stars of Cassiopeia. These included Bathsheba, Solomon's mother; Deborah, an Old Testament prophet; and Mary Magdalene, a follower of Jesus.[4]

A figure called the "Tinted Hand" also appeared in the stars of Cassiopeia in some Arab atlases. This is variously said to represent a woman's hand dyed red with henna, as well as the bloodied hand of Muhammad's daughter Fatima. The hand is made up of the stars α Cas, β Cas, γ Cas, δ Cas, ε Cas, and η Cas. The arm is made up of the stars α Per, γ Per, δ Per, ε Per, η Per, and ν Per.[4]

Another Arab constellation that incorporated the stars of Cassiopeia was the Camel. Its head was composed of Lambda, Kappa, Iota, and Phi Andromedae; its hump was Beta Cassiopeiae; its body was the rest of Cassiopeia, and the legs were composed of stars in Perseus and Andromeda.[4]

Other cultures see a hand or moose antlers in the pattern.[7] These include the Sámi, for whom the W of Cassiopeia forms an elk antler. The Chukchi of Siberia similarly saw the five main stars as five reindeer stags.[4]

The people of the Marshall Islands saw Cassiopeia as part of a great porpoise constellation. The main stars of Cassiopeia make its tail, Andromeda and Triangulum form its body, and Aries makes its head.[4] In Hawaii, Alpha, Beta, and Gamma Cassiopeiae were named. Alpha Cassiopeiae was called Poloahilani, Beta Cassiopeiae was called Polula, and Gamma Cassiopeiae was called Mulehu. The people of Pukapuka saw the figure of Cassiopeia as a distinct constellation called Na Taki-tolu-a-Mataliki.[8]

Characteristics

Cassiopeia in the night sky

File:Cassiopeia.4m-10m.webm Cassiopeia had a supernova, Cassiopeia A, SN 1572.

Covering 598.4 square degrees and hence 1.451% of the sky, Cassiopeia ranks 25th of the 88 constellations in area.[9] It is bordered by Cepheus to the north and west, Andromeda to the south and west, Perseus to the southeast and Camelopardalis to the east, and also shares a short border with Lacerta to the west.

The three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is "Cas".[10] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930,[lower-alpha 2] are defined by a polygon of 30 segments. In the equatorial coordinate system, the right ascension coordinates of these borders lie between  00h 27m 03s and  23h 41m 06s, while the declination coordinates are between 77.69° and 46.68°.[1] Its position in the Northern Celestial Hemisphere means that the whole constellation is visible to observers north of 12°S.[9][lower-alpha 3] High in the northern sky, it is circumpolar (that is, it never sets in the night sky) to viewers in the British Isles, Canada and the northern United States.[12]

Features

Stars

Main article: Astronomy:List of stars in Cassiopeia
The constellation Cassiopeia as it can be seen by the naked eye from a northern location

The German cartographer Johann Bayer used the Greek letters Alpha through Omega, and then A and B, to label the most prominent 26 stars in the constellation. Upsilon was later found to be two stars and labelled Upsilon1 and Upsilon2 by John Flamsteed. B Cassiopeiae was in fact the supernova known as Tycho's Supernova.[13] Within the constellation's borders, there are 157 stars brighter than or equal to apparent magnitude 6.5.[lower-alpha 4][9]

'W' asterism

The five brightest stars of Cassiopeia – Alpha, Beta, Gamma, Delta, and Epsilon Cassiopeiae – form the characteristic W-shaped asterism.[12] All five are prominent naked eye stars, three are noticeably variable, and a fourth is a suspected low amplitude variable. The asterism is oriented as a W when below Polaris during northern spring and summer nights. In northern winter, and when seen from southern latitudes, it is "above" Polaris (i.e. closer to the zenith) and the W appears inverted.

Alpha Cassiopeiae, traditionally called Schedar (from the Arabic Al Sadr, "the breast"), is a four-star system. The primary dominates, an orange-hued giant of magnitude 2.2, 228 ± 2 light-years from Earth.[15] With a luminosity of around 771 times that of the Sun, it has swollen and cooled after exhausting its core hydrogen over its 100 to 200 million-year lifespan, spending much of it as a blue-white B-type main-sequence star.[16] Magnitude 8.9 yellow dwarf companion (B) is widely separated; companions (C and D) are closer and magnitudes 13 and 14 respectively.[17]

Beta Cassiopeiae, or Caph (meaning "hand"), is a white-hued star of magnitude 2.3, 54.7 ± 0.3 light-years from Earth.[15] Around 1.2 billion years old, it has used up its core hydrogen and begun expanding and cooling off the main sequence. It is around 1.9 times as massive as the Sun, and around 21.3 times as luminous. Rotating at about 92% of its critical speed, Caph completes a full rotation every 1.12 days. This is giving the star an oblate spheroid shape with an equatorial bulge that is 24% larger than the polar radius.[18] It is a Delta Scuti variable with a small amplitude and period of 2.5 hours.[19]

Gamma Cassiopeiae is the prototype Gamma Cassiopeiae variable star, a type of variable star that has a variable disc of material flung off by the high rotation rate of the star. Gamma Cassiopeiae has a minimum magnitude of 3.0 and a maximum magnitude of 1.6, but is generally near magnitude 2.2, with unpredictable fades and brightenings. It is a spectroscopic binary, with an orbital period of 203.59 days and a companion with a calculated mass about the same as the Sun. However, no direct evidence of this companion has been found, leading to speculation that it might be a white dwarf or other degenerate star.[20] It is 550 ± 10 light-years from Earth.

Delta Cassiopeiae, also known as Ruchbah or Rukbat, meaning "knee," is a possible Algol-type eclipsing binary star with a maximum brightness of magnitude 2.7. It has been reported to show eclipses of less than 0.1 magnitudes with a period of 2 years and 1 month.,[21] but this has never been confirmed. It is 99.4 ± 0.4 light-years from Earth.[15]

Epsilon Cassiopeiae has an apparent magnitude of 3.3. Located 410 ± 20 light-years from Earth,[15] it is a hot blue-white star of spectral type B3 III with a surface temperature of 15,680 K. It is 6.5 times as massive and 4.2 times as wide as the Sun, and belongs to a class of stars known as Be stars—rapidly spinning stars that throw off a ring or shell of matter.[22]

Fainter stars

Kappa Cassiopeiae and its bow shock. Spitzer infrared image (NASA/JPL-Caltech)

The next seven brightest stars in Cassiopeia are also all confirmed or suspected variable stars, including 50 Cassiopeiae which was not given a Greek letter by Bayer and is a suspected variable with a very small amplitude. Zeta Cassiopeiae (Fulu[23]) is a suspected slowly pulsating B-type star. Eta Cassiopeiae (Achird[23]) is a spectroscopic binary star with a period of 480 years, and a suspected RS Canum Venaticorum variable. The primary is a yellow-hued star of magnitude 3.5 and the secondary is a red-hued star of magnitude 7.5. The system is 19 light-years from Earth. Kappa Cassiopeiae is a blue supergiant of spectral type BC0.7Ia that is some 302,000 times as luminous as the Sun and has 33 times its diameter.[24] It is a runaway star, moving at around 2.5 million mph relative to its neighbors (1,100 kilometers per second).[25] Its magnetic field and wind of particles creates a visible bow shock 4 light-years ahead of it, colliding with the diffuse, and usually invisible, interstellar gas and dust. The dimensions of the bow shock are vast: around 12 light-years long and 1.8 light-years wide.[26] Theta Cassiopeiae, named Marfak, is a suspected variable star whose brightness changes by less than a tenth of a magnitude. Iota Cassiopeiae is a triple star 142 light-years from Earth. The primary is a white-hued star of magnitude 4.5 and an α2 Canum Venaticorum variable, the secondary is a yellow-hued star of magnitude 6.9, and the tertiary is a star of magnitude 8.4. The primary and secondary are close together but the primary and tertiary are widely separated. Omicron Cassiopeiae is a triple star and the primary is another γ Cassiopeiae variable.

Sigma Cassiopeiae is a binary star 1500 light-years from Earth. It has a green-hued primary of magnitude 5.0 and a blue-hued secondary of magnitude 7.3. Psi Cassiopeiae is a triple star 193 light-years from Earth. The primary is an orange-hued giant star of magnitude 4.7 and the secondary is a close pair of stars that appears to be of magnitude 9.0.[21]

Rho Cassiopeiae is a semi-regular pulsating variable yellow hypergiant, among the most luminous stars in the galaxy at approximately 500,000 L☉.[27] It has a minimum magnitude of 6.2 and a maximum magnitude of 4.1; its period is approximately 320 days. It has around 450 times the Sun's diameter and 17 times its mass, having begun life 45 times as massive as the Sun. Rho Cassiopeiae is about 10,000 light-years from Earth. Cassiopeia includes V509 Cassiopeiae, a second example of the extremely rare yellow hypergiants, which is around 400,000 times as luminous as the Sun and 14 times as massive,[27] as well as 6 Cassiopeiae which is a hotter white hypergiant. It also hosts the red supergiant PZ Cassiopeiae, which is one of the largest known stars with an estimate of 1,190–1,940 R☉ and is also a semiregular variable.[28] Between 240,000 and 270,000 times as luminous as the Sun, it is around 9,160 light-years distant from Earth.[29]

AO Cassiopeiae is a binary system composed of an O8 main sequence star and an O9.2 bright giant that respectively weigh anywhere between 20.30 and 57.75 times and 14.8 and 31.73 times the mass of the Sun.[30] The two massive stars are so close to each other they distort each other into egg-shapes.[31]

Tycho Brahe's supernova was visible within Cassiopeia, and the star Tycho G is suspected of being the donor of the material that triggered that explosion.

Deep-sky objects

File:Potw1327a.tif A rich section of the Milky Way runs through Cassiopeia, stretching from Perseus towards Cygnus, and it contains a number of open clusters, young luminous galactic disc stars, and nebulae.

The Heart Nebula and the Soul Nebula are two neighboring emission nebulae about 7,500 light-years away.

Two Messier objects, M52 (NGC 7654) and M103 (NGC 581), are located in Cassiopeia; both are open clusters. M52, once described as a "kidney-shaped" cluster, contains approximately 100 stars and is 4600 light-years from Earth.[32] Its most prominent member is an orange-hued star of magnitude 8.0 near the cluster's edge. M103 is far poorer than M52, with only about 25 stars included. It is also more distant, between 8000 and 9500 light-years from Earth.[33] Its most prominent member is actually a closer, superimposed double star; it consists of a 7th-magnitude primary and 10th-magnitude secondary.[21]

The other prominent open clusters in Cassiopeia are NGC 457 and NGC 663, both of which have about 80 stars. NGC 457 is looser, and its brightest member is Phi Cassiopeiae, a white-hued supergiant star of magnitude 5.0. However, it is uncertain whether Phi Cassiopeiae is part of the open cluster or not.[34] The stars of NGC 457, arrayed in chains, are approximately 10,000 light-years from Earth. NGC 663 is both closer, at 8200 light-years from Earth, and larger, at 0.25 degrees in diameter.[21]

There are two supernova remnants in Cassiopeia. The first, designated 3C 10 or just Tycho's Supernova Remnant, is the aftermath of the supernova called Tycho's Star. It was observed in 1572 by Tycho Brahe and now exists as a bright object in the radio spectrum.[21] Within the 'W' asterism formed by Cassiopeia's five major stars lies Cassiopeia A (Cas A). It is the remnant of a supernova that took place approximately 300 years ago (as observed now from Earth; it is 10,000 light-years away),[35] and has the distinction of being the strongest radio source observable outside the Solar System. It was perhaps observed as a faint star in 1680 by John Flamsteed. It was also the subject of the first image returned by the Chandra X-Ray Observatory in the late 1990s. The shell of matter expelled from the star is moving at 4,000 kilometres (2,500 mi) per second; it has a temperature of 30,000 kelvins on average.[35]

NGC 457 is another open cluster in Cassiopeia, also called the E.T. Cluster, the Owl Cluster, and Caldwell 13. The cluster was discovered in 1787 by William Herschel. It has an overall magnitude of 6.4 and is approximately 10,000 light-years from Earth, lying in the Perseus arm of the Milky Way. However, its most prominent member, the double star Phi Cassiopeiae, is far closer – between 1000 and 4000 light-years away. NGC 457 is fairly rich; it is a Shapley class e and Trumpler class I 3 r cluster. It is concentrated towards its center and detached from the star field. It contains more than 100 stars, which vary widely in brightness.[36]

Two members of the Local Group of galaxies are in Cassiopeia. NGC 185 is a magnitude 9.2 elliptical galaxy of type E0, 2 million light-years away. Slightly dimmer and more distant NGC 147 is a magnitude 9.3 elliptical galaxy, like NGC 185 it is an elliptical of type E0; it is 2.3 million light-years from Earth. Though they do not appear in Andromeda, both dwarf galaxies are gravitationally bound to the far larger Andromeda Galaxy.[37]

IC 10 is an irregular galaxy that is the closest known starburst galaxy and the only one in the Local Group of galaxies.[38]

Cassiopeia also contains part of the closest galaxy group to our Local Group, the IC 342/Maffei Group. The galaxies Maffei 1 and Maffei 2 are located just to the south of the Heart and Soul nebulae. As a result of this location in the Zone of Avoidance, both are surprisingly faint despite both being within 10 million light-years away (Maffei 2 is below the range of most amateur telescopes).[39]

Meteor shower

The December Phi Cassiopeiids are a recently discovered early December meteor shower that radiates from Cassiopeia. Phi Cassiopeiids are very slow, with an entry velocity of approximately 16.7 kilometers per second. The shower's parent body is a Jupiter family comet, though its specific identity is unknown.[40]

Namesakes

USS Cassiopeia (AK-75) was a United States Navy Crater-class cargo ship named after the constellation.

In Pokémon Scarlet and Violet, the villainous team, Team Star, is divided into five squads named after the brightest stars in the constellation: Segin Squad, Schedar Squad, Ruchbah Squad, Navi Squad, and Caph Squad. In addition, the character Penny's alias, Cassiopeia, is named after the constellation.

Cassiopeia is also the name of a song by London-based band Bears in Trees. Although the lyrics of the song mainly refer to the ancient Greek woman, the album cover shows the constellation.[41]

See also

  • Cassiopeia (Chinese astronomy)

References

Explanatory notes

  1. ↑ γ Cas is variable and occasionally brighter than α.
  2. ↑ Delporte had proposed standardising the constellation boundaries to the International Astronomical Union, who had agreed and gave him the lead role[11]
  3. ↑ While parts of the constellation technically rise above the horizon to observers between the latitudes of 12°S and 43°S, stars within a few degrees of the horizon are to all intents and purposes unobservable.[9]
  4. ↑ Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.[14]

Citations

  1. ↑ 1.0 1.1 1.2 "Cassiopeia, Constellation Boundary". The Constellations (International Astronomical Union). https://www.iau.org/public/themes/constellations/#cas. Retrieved 2 December 2016. 
  2. ↑ 2.0 2.1 Chisholm, Hugh, ed (1911). "Cassiopeia". Encyclopædia Britannica. 5 (11th ed.). Cambridge University Press. p. 460. 
  3. ↑ Chen, P.K. (2007). A Constellation Album: Stars and Mythology of the Night Sky. p. 82. ISBN 9781931559386. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Staal 1988, pp. 14–18
  5. ↑ Chen 2007, pp. 82–83
  6. ↑ Squire, Charles (2013). Celtic Myth and Legend. Courier Corporation. ISBN 978-0-486-12209-0. https://books.google.com/books?id=nyjDAgAAQBAJ&pg=PT169. 
  7. ↑ Ptak, Robert (1998). Sky Stories Ancient and Modern. New York: Nova Science Publishers. p. 104. 
  8. ↑ Makemson, Maud Worcester (1941). The Morning Star Rises: an account of Polynesian astronomy. Yale University Press. p. 281. Bibcode: 1941msra.book.....M. 
  9. ↑ 9.0 9.1 9.2 9.3 Ian Ridpath. "Constellations: Andromeda–Indus". Star Tales. self-published. http://www.ianridpath.com/constellations1.html. 
  10. ↑ Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy 30: 469. Bibcode: 1922PA.....30..469R. 
  11. ↑ Ridpath, Ian. "Constellation boundaries: How the modern constellation outlines came to be". Star Tales. self-published. http://www.ianridpath.com/boundaries.html. 
  12. ↑ 12.0 12.1 Arnold, H.J.P; Doherty, Paul; Moore, Patrick (1999). The Photographic Atlas of the Stars. Boca Raton, Florida: CRC Press. p. 20. ISBN 978-0-7503-0654-6. https://books.google.com/books?id=YjcvJUfnWBAC&pg=PA20. 
  13. ↑ Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, Virginia: The McDonald & Woodward Publishing Company. pp. 91–92. ISBN 978-0-939923-78-6. 
  14. ↑ Bortle, John E. (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Sky Publishing Corporation. http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y. 
  15. ↑ 15.0 15.1 15.2 15.3 van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics 474 (2): 653–64. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  16. ↑ Professor James B. (Jim) Kaler. "SHEDAR (Alpha Cassiopeiae)". University of Illinois. http://stars.astro.illinois.edu/sow/shedar.html. 
  17. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M. 
  18. ↑ Che, X.; Monnier, J. D.; Zhao, M.; Pedretti, E.; Thureau, N.; Mérand, A.; ten Brummelaar, T.; McAlister, H. et al. (2011). "Colder and Hotter: Interferometric Imaging of β Cassiopeiae and α Leonis". The Astrophysical Journal 732 (2): 68. doi:10.1088/0004-637X/732/2/68. Bibcode: 2011ApJ...732...68C. 
  19. ↑ Kaler, James B. (Jim). "Caph". Stars. University of Illinois. http://stars.astro.illinois.edu/sow/caph.html. 
  20. ↑ Harmanec, P.; Habuda, P.; Štefl, S.; Hadrava, P.; Korčáková, D.; Koubský, P.; Krtička, J.; Kubát, J. et al. (2000). "Properties and nature of Be stars. XX. Binary nature and orbital elements of gamma Cas". Astronomy and Astrophysics 364: L85–L88. Bibcode: 2000A&A...364L..85H. 
  21. ↑ 21.0 21.1 21.2 21.3 21.4 Ridpath & Tirion 2001, pp. 106–108.
  22. ↑ Catanzaro, G. (2013). "Spectroscopic atlas of Hα and Hβ in a sample of northern Be stars". Astronomy & Astrophysics 550 (A79): 18. doi:10.1051/0004-6361/201220357. Bibcode: 2013A&A...550A..79C. 
  23. ↑ 23.0 23.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. 
  24. ↑ Searle, S. C.; Prinja, R. K.; Massa, D.; Ryans, R. (2008). "Quantitative studies of the optical and UV spectra of Galactic early B supergiants. I. Fundamental parameters". Astronomy and Astrophysics 481 (3): 777. doi:10.1051/0004-6361:20077125. Bibcode: 2008A&A...481..777S. 
  25. ↑ Clavin, Whitney (21 February 2014). "The bow shock of Kappa Cassiopeiae, a massive, hot supergiant". Phys.org. http://phys.org/news/2014-02-kappa-cassiopeiae-massive-hot-supergiant.html. 
  26. ↑ Peri, C. S.; Benaglia, P.; Brookes, D. P.; Stevens, I. R.; Isequilla, N. L. (2012). "E-BOSS: An Extensive stellar BOw Shock Survey. I. Methods and first catalogue". Astronomy & Astrophysics 538: A108. doi:10.1051/0004-6361/201118116. Bibcode: 2012A&A...538A.108P. 
  27. ↑ 27.0 27.1 Stothers, Richard B. (2012). "Yellow Hypergiants Show Long Secondary Periods?". The Astrophysical Journal 751 (2): 151. doi:10.1088/0004-637X/751/2/151. Bibcode: 2012ApJ...751..151S. 
  28. ↑ Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal 628 (2): 973–985. doi:10.1086/430901. Bibcode: 2005ApJ...628..973L. 
  29. ↑ Kusuno, K.; Asaki, Y.; Imai, H.; Oyama, T. (2013). "Distance and Proper Motion Measurement of the Red Supergiant, Pz Cas, in Very Long Baseline Interferometry H2O Maser Astrometry". The Astrophysical Journal 774 (2): 107. doi:10.1088/0004-637X/774/2/107. Bibcode: 2013ApJ...774..107K. 
  30. ↑ Hohle, M.M.; Neuhäuser, R.; Schutz, B.F. (2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten 331 (4): 349. doi:10.1002/asna.200911355. Bibcode: 2010AN....331..349H. 
  31. ↑ Astronomy and Cosmogony. CUP Archive. 1928. pp. 125–. GGKEY:KFJRG3PWW14. https://books.google.com/books?id=M988AAAAIAAJ&pg=PA125. 
  32. ↑ Wu, Zhen-Yu et al. (November 2009), "The orbits of open clusters in the Galaxy", Monthly Notices of the Royal Astronomical Society 399 (4): 2146–2164, doi:10.1111/j.1365-2966.2009.15416.x, Bibcode: 2009MNRAS.399.2146W. 
  33. ↑ Sanner, J.; Geffert, M.; Brunzendorf, J.; Schmoll, J. (1999). "Photometric and kinematic studies of open star clusters. I. NGC 581 (M 103)". Astronomy and Astrophysics 349: 448–456. Bibcode: 1999A&A...349..448S. 
  34. ↑ Zhang, X. B.; Luo, C. Q.; Fu, J. N. (2012). "B-Type Variables in the Young Open Cluster Ngc 457". The Astronomical Journal 144 (3): 86. doi:10.1088/0004-6256/144/3/86. Bibcode: 2012AJ....144...86Z. 
  35. ↑ 35.0 35.1 Wilkins, Jamie; Dunn, Robert (2006). 300 Astronomical Objects: A Visual Reference to the Universe (1st ed.). Buffalo, New York: Firefly Books. ISBN 978-1-55407-175-3. 
  36. ↑ Levy 2005, pp. 92–93.
  37. ↑ Levy 2005, pp. 180–181.
  38. ↑ Nidever, David L.; Ashley, Trisha; Slater, Colin T.; Ott, Jürgen; Johnson, Megan; Bell, Eric F.; Stanimirović, Snežana; Putman, Mary et al. (2013). "Evidence for an interaction in the nearest starbursting dwarf irregular galaxy IC 10". The Astrophysical Journal Letters 779 (2): L15. doi:10.1088/2041-8205/779/2/L15. Bibcode: 2013ApJ...779L..15N. 
  39. ↑ I. D. Karachentsev (2005). "The Local Group and Other Neighboring Galaxy Groups". Astronomical Journal 129 (1): 178–188. doi:10.1086/426368. Bibcode: 2005AJ....129..178K. 
  40. ↑ Jenniskens, Peter (September 2012). "Mapping Meteoroid Orbits: New Meteor Showers Discovered". Sky & Telescope: 25. 
  41. ↑ "Cassiopeia". https://bearsintreesofficial.bandcamp.com/track/cassiopeia. 

General and cited sources

Template loop detected: Template:Stars of Cassiopeia

Coordinates: Sky map 01h 00m 00s, +60° 00′ 00″




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