1393:
28:
402:, around 10,000 light years away. The primary is a hydrogen-free weak-lined WN7 star, the secondary is a hydrogen-free WN3 or 4 star, and the system is a possible member of the cluster Dolidze 33. From our point of view, WR 120 is reddened by 4.82 magnitudes, and it has the variable designation of V462 Scuti.
484:
In 2021, WR 120 was revealed to be a binary star. Previously, it was thought to be a single WR star, but it is in fact a rare double Wolf-Rayet star. The companion (a WN3/4 WR star) is located approximately 1700 AU from the primary WN7 WR, and is about 2.1 magnitudes fainter than WR 120.
611:
Hamann, W.-R.; Gräfener, G.; Liermann, A.; Hainich, R.; Sander, A. A. C.; Shenar, T.; Ramachandran, V.; Todt, H.; Oskinova, L. M. (2019-05-01). "The
Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters".
421:/year, or 1 solar mass every 80,000 years, which is being carried away from the surface at a speed of 1,225 kilometres per second. Taking its close distance into account, WR 120 A's luminosity turns out to be a mere 83,200
1420:
994:
673:
Shara, Michael M.; Howell, Steve B.; Furlan, Elise; Gnilka, Crystal L.; Moffat, Anthony F. J.; Scott, Nicholas J.; Zurek, David (2022-01-01).
987:
410:
Analysis of the primary's spectrum with PoWR shows that it has a temperature of around 50,000 Kelvins, and is losing mass at a rate of
1425:
1396:
980:
446:
is derived, and a "transformed" radius at an optical depth of 2/3, more comparable to other types of stars, is at about 6
48:
1415:
430:, which would make it one of the dimmest WN stars known, and one of the only WN stars with a luminosity below 100,000
1155:
1019:
780:
735:
Ducati, J. R. (2002). "VizieR Online Data
Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system".
1086:
767:
358:
838:
1014:
675:"A speckle-imaging search for close and very faint companions to the nearest and brightest Wolf-Rayet stars"
1003:
122:
1281:
328:
36:
for V462 Scuti, adapted from Chené and St-Louis (2007). The left-most point shows the 3 sigma error bar.
940:
881:
799:
744:
696:
631:
578:
547:
217:
538:
Gaia
Collaboration (2018-04-01). "VizieR Online Data Catalog: Gaia DR2 (Gaia Collaboration, 2018)".
1215:
1170:
1195:
958:
930:
871:
817:
789:
686:
655:
621:
238:
93:
1350:
1038:
899:
714:
647:
110:
44:
1165:
1160:
948:
889:
860:"Unlocking Galactic Wolf-Rayet stars with Gaia DR2 - II. Cluster and association membership"
828:
807:
803:
704:
639:
635:
555:
515:
461:
431:
422:
315:
201:
383:
1210:
919:"Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – I. Distances and absolute magnitudes"
395:
354:
115:
69:
1150:
944:
885:
748:
700:
582:
573:
Zacharias, N. (2012). "The fourth US Naval
Observatory CCD Astrograph Catalog (UCAC4)".
551:
346:
209:
189:
177:
460:, one of the lowest masses of any WR star. WR 120 A’s visual luminosity is 2,858
1409:
1066:
962:
821:
659:
166:
56:
1345:
1270:
1246:
1241:
832:
473:
295:
268:
812:
771:
643:
1320:
1061:
1056:
1046:
144:
133:
82:
33:
27:
559:
1330:
1315:
1310:
1135:
1109:
1071:
1051:
520:
503:
308:
275:
224:
154:
903:
894:
859:
718:
709:
674:
651:
1256:
1251:
1233:
1205:
1200:
1190:
1076:
953:
918:
453:. Using the WR Luminosity-Mass ratio, WR 120 may have a mass of just 7
972:
1325:
1294:
1289:
1145:
1140:
1104:
1376:
1119:
1099:
1094:
1368:
1180:
1175:
1114:
842:
399:
377:
335:
288:
229:
61:
776:
Early Data
Release 3: Summary of the contents and survey properties"
935:
876:
794:
691:
626:
504:"The First Determination of the Rotation Rates of Wolf-Rayet Stars"
1340:
1335:
362:
858:
Rate, Gemma; Crowther, Paul A.; Parker, Richard J. (2020-06-01).
1029:
193:
181:
976:
469:, which is also on the lower end of WR visual luminosities.
508:
Massive Stars as Cosmic
Engines, Proceedings IAU Symposium
439:. Using the Stefan-Boltzmann Law, a radius of 3.78
1367:
1303:
1280:
1269:
1232:
1128:
1085:
1037:
1028:
472:WR 120 is thought to be a member of Dolidze 33, an
923:Monthly Notices of the Royal Astronomical Society
864:Monthly Notices of the Royal Astronomical Society
679:Monthly Notices of the Royal Astronomical Society
16:Binary star system in the constellation Scutum
988:
87:−4° 26′ 14.47345″
8:
770:; et al. (Gaia collaboration) (2021).
1364:
1277:
1229:
1034:
995:
981:
973:
952:
934:
893:
875:
811:
793:
708:
690:
625:
519:
47:J2000
730:
728:
606:
604:
602:
600:
598:
596:
594:
592:
1421:Objects with variable star designations
917:Crowther, Paul A.; Rate, Gemma (2020).
494:
173:
762:
760:
758:
533:
531:
18:
7:
853:
851:
185:
14:
1392:
1391:
839:Gaia EDR3 record for this source
26:
208:0.3246 ± 0.0541
32:A near-infrared (2.033 micron)
1:
502:Chené, André-Nicolas (2007).
833:10.1051/0004-6361/202039657e
781:Astronomy & Astrophysics
1020:Scutum in Chinese astronomy
813:10.1051/0004-6361/202039657
644:10.1051/0004-6361/201834850
575:VizieR On-line Data Catalog
394:is a binary containing two
1442:
737:VizieR Online Data Catalog
614:Astronomy and Astrophysics
540:VizieR Online Data Catalog
1389:
1363:
1228:
1010:
521:10.1017/S1743921308020425
370:
352:
345:
341:
262:
257:
253:
160:
153:
104:
41:
24:
560:10.26093/cds/vizier.1345
398:in the constellation of
365: J18410086-0426145
1156:2MASS J18450079–1409036
1015:List of stars in Scutum
1004:Constellation of Scutum
804:2021A&A...649A...1G
636:2019A&A...625A..57H
239:Absolute magnitude
111:Evolutionary stage
94:Apparent magnitude
1426:Scutum (constellation)
895:10.1093/mnras/staa1290
710:10.1093/mnras/stab2666
476:nearly 3,000 pc away.
954:10.1093/mnras/stz3614
228:(approx. 3,100
223:approx. 10,000
1216:Stephenson 2 DFK 49
945:2020MNRAS.493.1512R
886:2020MNRAS.495.1209R
749:2002yCat.2237....0D
701:2022MNRAS.509.2897S
583:2012yCat.1322....0Z
552:2018yCat.1345....0G
371:Database references
21:
1196:Stephenson 2 DFK 1
347:Other designations
188: −2.524
176: −0.489
123:Spectral type
19:
1403:
1402:
1385:
1384:
1359:
1358:
1351:Wild Duck Cluster
1265:
1264:
1224:
1223:
389:
388:
1433:
1416:Wolf–Rayet stars
1395:
1394:
1365:
1278:
1230:
1035:
997:
990:
983:
974:
967:
966:
956:
938:
929:(1): 1512–1529.
914:
908:
907:
897:
879:
870:(1): 1209–1226.
855:
846:
836:
825:
815:
797:
764:
753:
752:
732:
723:
722:
712:
694:
685:(2): 2897–2907.
670:
664:
663:
629:
608:
587:
586:
570:
564:
563:
535:
526:
525:
523:
499:
413:
396:Wolf-Rayet stars
187:
175:
105:Characteristics
97:
77:
72:
42:Observation data
30:
22:
1441:
1440:
1436:
1435:
1434:
1432:
1431:
1430:
1406:
1405:
1404:
1399:
1381:
1355:
1299:
1272:
1261:
1220:
1211:IRAS 18357-0604
1124:
1081:
1024:
1006:
1001:
971:
970:
916:
915:
911:
857:
856:
849:
827:(Erratum:
826:
768:Brown, A. G. A.
766:
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756:
734:
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610:
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467:
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428:
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417:
411:
408:
366:
321:
318:
301:
298:
281:
278:
244:
227:
184:
92:
75:
70:Right ascension
68:
43:
37:
31:
17:
12:
11:
5:
1439:
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1171:PSR J1841−0500
1168:
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1125:
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462:
457:
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76:18 41 00.86698
73:
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52:
39:
38:
25:
15:
13:
10:
9:
6:
4:
3:
2:
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1199:
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946:
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823:
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769:
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746:
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623:
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541:
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532:
528:
522:
517:
513:
509:
505:
498:
495:
488:
486:
479:
477:
475:
470:
468:
438:
429:
405:
403:
401:
397:
393:
385:
382:
380:
379:
375:
374:
369:
364:
361: Scuti,
360:
356:
351:
348:
344:
340:
337:
333:
331:
330:
326:
325:
322:
313:
311:
310:
306:
305:
302:
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273:
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207:
205:
203:
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191:
183:
179:
172:
170:
168:
167:Proper motion
164:
163:
159:
156:
152:
148:
146:
142:
141:
137:
135:
131:
130:
127:WN7w + WN3/4
126:
124:
121:
120:
117:
114:
112:
109:
108:
103:
99:
95:
91:
90:
86:
84:
81:
80:
74:
71:
67:
66:
63:
60:
58:
57:Constellation
55:
54:
50:
46:
40:
35:
29:
23:
1346:Stephenson 2
1242:BD-11 4672 b
1185:
1166:PSR B1829−10
1161:PSR B1828−11
926:
922:
912:
867:
863:
785:
779:
773:
740:
736:
682:
678:
668:
617:
613:
574:
568:
543:
539:
511:
507:
497:
483:
474:open cluster
471:
409:
391:
390:
376:
334:50,100
327:
314:83,200
307:
287:
267:
237:
216:
200:
165:
1321:Alicante 10
514:: 139–144.
329:Temperature
145:color index
134:color index
83:Declination
34:light curve
1410:Categories
1331:Messier 26
1316:Alicante 8
1311:Alicante 7
1234:Exoplanets
1151:IRC −10414
1136:BD-11 4672
936:1912.10125
877:2005.02533
795:2012.01533
692:2109.06975
627:1904.04687
489:References
406:Properties
357: 89,
309:Luminosity
294:3.78
155:Astrometry
116:Wolf-Rayet
1257:CoRoT-17b
1252:CoRoT-16b
1206:RSGC1-F02
1201:RSGC1-F01
1191:WR 121-16
963:209444955
904:0035-8711
822:227254300
719:0035-8711
660:104292503
652:0004-6361
96: (V)
1397:Category
1326:Mercer 3
1273:clusters
1146:CoRoT-17
1141:CoRoT-16
1087:Variable
480:Binarity
466:☉
458:☉
451:☉
444:☉
436:☉
427:☉
419:☉
320:☉
300:☉
280:☉
241: (M
218:Distance
202:Parallax
1377:IC 1295
1369:Nebulae
941:Bibcode
882:Bibcode
837:.
800:Bibcode
745:Bibcode
697:Bibcode
632:Bibcode
620:: A57.
579:Bibcode
548:Bibcode
274:7
258:Details
49:Equinox
20:WR 120
1186:WR 120
1181:WR 119
1176:WR 114
961:
902:
843:VizieR
820:
788:: A1.
717:
658:
650:
414:
400:Scutum
392:WR 120
378:SIMBAD
289:Radius
100:11.93
62:Scutum
51:J2000
1341:RSGC3
1336:RSGC1
1304:Other
1129:Other
1039:Bayer
1030:Stars
959:S2CID
931:arXiv
872:arXiv
818:S2CID
790:arXiv
687:arXiv
656:S2CID
622:arXiv
363:2MASS
249:−3.81
186:Dec.:
149:1.04
138:0.13
45:Epoch
1295:6712
1290:6649
1271:Star
1120:V479
1115:V452
1110:V373
900:ISSN
774:Gaia
741:2237
715:ISSN
648:ISSN
544:1345
384:data
359:V462
269:Mass
143:B−V
132:U−B
1282:NGC
949:doi
927:493
890:doi
868:495
841:at
829:doi
808:doi
786:649
705:doi
683:509
640:doi
618:625
556:doi
516:doi
512:250
210:mas
204:(π)
190:mas
178:mas
174:RA:
169:(μ)
1412::
1105:UY
957:.
947:.
939:.
925:.
921:.
898:.
888:.
880:.
866:.
862:.
850:^
816:.
806:.
798:.
784:.
778:.
757:^
743:.
739:.
727:^
713:.
703:.
695:.
681:.
677:.
654:.
646:.
638:.
630:.
616:.
591:^
577:.
554:.
546:.
542:.
530:^
510:.
506:.
412:10
355:MR
230:pc
225:ly
194:yr
182:yr
1247:c
1100:S
1095:R
1077:η
1072:ζ
1067:ε
1062:δ
1057:γ
1052:β
1047:α
996:e
989:t
982:v
965:.
951::
943::
933::
906:.
892::
884::
874::
845:.
835:)
831::
824:.
810::
802::
792::
772:"
751:.
747::
721:.
707::
699::
689::
662:.
642::
634::
624::
585:.
581::
562:.
558::
550::
524:.
518::
463:L
455:M
448:R
441:R
433:L
424:L
416:M
336:K
317:L
297:R
277:M
245:)
243:V
232:)
192:/
180:/
Text is available under the Creative Commons Attribution-ShareAlike License. Additional terms may apply.
