260:
833:
857:
26:
787:
809:
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821:
598:
Navascués, D. Barrado y; Bayo, A.; Morales-Calderón, M.; Huélamo, N.; Stauffer, J. R.; Bouy, H. (2007-06-01). "The young, wide and very low mass visual binary Lambda
Orionis 167".
465:
Navascués, D. Barrado y; Stauffer, J. R.; Bouvier, J.; Jayawardhana, R.; Cuillandre, Jean-Charles (August 2004). "The
Substellar Population of the Young Cluster λ Orionis".
310:
that exploded one million years ago. The supernova blast encountered the clouds and gas in the region and the blast dispersed the parent core, creating the molecular ring.
365:
716:
Dolan, Christopher J.; Mathieu, Robert D. (January 2002). "A Photometric Study of the Young
Stellar Population throughout the λ Orionis Star-forming Region".
298:
away were unaffected by this and represent the current population of low-mass stars with a circumstellar disk. The cluster is surrounded by a large
176:. With the rest of Orion, it is visible from the middle of August in the morning sky, to late April before Orion becomes too close to the
268:
208:, and as close as 25 kly (7.7 kpc). The inclination of the orbit carries it up to 260 light-years (80 parsecs) away from the
877:
799:
529:
Navascués, David
Barrado y; Stauffer, John R.; Morales-Calderón, María; Bayo, Amelia; Fazzio, Giovanni; Megeath, Tom;
274:
The cluster might have formed in the central region of an elongated cloud, which is supported by the distribution of
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formed in the central regions of these clouds. The low-mass stars closest to the massive stars likely lost their
259:
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161:
132:
120:
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candidates, which are concentrated in the cluster and nearby regions in an elongated shape. Massive
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661:"Photoevaporation of Two Proplyds in the Star Cluster Collinder 69 Discovered with Spitzer MIPS"
537:(July 2007). "Spitzer: Accretion in Low-Mass Stars and Brown Dwarfs in the λ Orionis Cluster*".
751:
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34:
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164:. It is about five million years old and roughly 1,300 ly (400 pc) away from the
451:
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232:
205:
42:
739:
676:
560:
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Wu, Zhen-Yu; et al. (November 2009), "The orbits of open clusters in the Galaxy",
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216:
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25:
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Thévenot, Melina; Doll, Katharina; Luca, Hugo A. Durantini (July 2019).
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of 0.06, carrying it as far as 28 kly (8.6 kpc) from the
612:
551:
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and a brown dwarf. Observations of the star cluster with the
318:
Other celestial bodies included in the constellation Orion:
212:. On average it crosses the plane every 33.3 million years.
239:
have shown that 25% of the low-mass stars and 40% of the
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The star cluster is young and contains a large number of
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231:, which is a wide binary consisting of a potential
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366:Monthly Notices of the Royal Astronomical Society
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200:that has a period of 227.4 million years with an
196:The cluster is following an orbit through the
180:to be seen well. It can be seen from both the
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306:. This was interpreted as a remnant of a
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152:cluster located north-west of the star
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255:Molecular ring and cluster evolution
168:. Included within the cluster is a
14:
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398:10.1111/j.1365-2966.2009.15416.x
775:Sky Atlas 2000.0 Second Edition
247:. Two of these being actively
1:
600:Astronomy & Astrophysics
69:1,300 ly (400 pc)
899:
630:10.1051/0004-6361:20077258
59:+09° 56.0′
665:Research Notes of the AAS
539:The Astrophysical Journal
467:The Astrophysical Journal
126:
23:
718:The Astronomical Journal
686:10.3847/2515-5172/ab30c5
227:. One notable member is
101:Lambda Ori Association,
85:Physical characteristics
33:Observation data (J2000
622:2007A&A...468L...5B
237:Spitzer Space Telescope
294:. Many low-mass stars
276:pre-main-sequence star
271:
142:Lambda Orionis Cluster
19:Lambda Orionis Cluster
878:Orion (constellation)
262:
233:planetary-mass object
133:List of open clusters
794:at Wikimedia Commons
533:; Hartmann, Lee W.;
243:are surrounded by a
43:Right ascension
740:2002AJ....123..387D
677:2019RNAAS...3...95T
561:2007ApJ...664..481B
489:2004ApJ...610.1064B
389:2009MNRAS.399.2146W
304:Lambda Orionis ring
288:circumstellar disks
186:southern hemisphere
182:northern hemisphere
144:(also known as the
272:
263:Molecular Ring in
245:circumstellar disk
241:substellar objects
98:Other designations
90:Estimated age
75:Apparent magnitude
790:Media related to
421:"cl Collinder 69"
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731:astro-ph/0110160
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480:astro-ph/0404072
473:(2): 1064–1078.
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373:(4): 2146–2164,
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328:Horsehead Nebula
292:photoevaporation
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206:Galactic Center
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748:10.1086/324631
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569:10.1086/518816
545:(1): 481–500.
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497:10.1086/421762
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300:molecular ring
284:low-mass stars
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217:low-mass stars
210:galactic plane
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221:T Tauri stars
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158:constellation
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116:Constellation
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862:Solar System
792:Collinder 69
721:
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664:
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606:(1): L5–L8.
603:
599:
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470:
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428:. Retrieved
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415:
370:
364:
323:Orion Nebula
317:
273:
225:brown dwarfs
214:
195:
146:Collinder 69
145:
141:
139:
129:Open cluster
110:Associations
850:Outer space
838:Spaceflight
531:Allen, Lori
267:as seen by
251:by Meissa.
202:ellipticity
192:Description
170:double star
55:Declination
872:Categories
724:(1): 387.
448:|url=
430:2020-06-07
339:References
333:Barnard 30
154:Betelgeuse
127:See also:
814:Astronomy
756:1538-3881
703:199137075
695:2515-5172
671:(7): 95.
646:119579493
638:0004-6361
613:0704.2469
577:0004-637X
552:0704.1963
505:0004-637X
380:0909.3737
308:supernova
198:Milky Way
103:Collinder
77: (V)
764:16622572
585:55846043
513:17152013
439:cite web
314:See also
280:OB stars
265:infrared
184:and the
65:Distance
48:05 35 06
800:Portals
736:Bibcode
673:Bibcode
618:Bibcode
557:Bibcode
485:Bibcode
450:value (
407:6066790
385:Bibcode
296:parsecs
290:due to
229:LOri167
219:, some
156:in the
93:5.0 Myr
762:
754:
701:
693:
644:
636:
583:
575:
511:
503:
446:Check
425:sim-id
405:
174:Meissa
172:named
826:Stars
760:S2CID
726:arXiv
699:S2CID
642:S2CID
608:arXiv
581:S2CID
547:arXiv
509:S2CID
475:arXiv
403:S2CID
375:arXiv
162:Orion
121:Orion
35:epoch
752:ISSN
691:ISSN
634:ISSN
573:ISSN
501:ISSN
452:help
282:and
269:WISE
223:and
150:star
140:The
80:2.8
744:doi
722:123
681:doi
626:doi
604:468
565:doi
543:664
493:doi
471:610
393:doi
371:399
178:Sun
166:Sun
160:of
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758:.
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742:.
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579:.
571:.
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541:.
521:^
507:.
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483:.
469:.
443::
441:}}
437:{{
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377::
37:)
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