Ursa Major Moving Group

The Ursa Major Moving Group, also known as Collinder 285 and the Ursa Major association, is a nearby stellar moving group – a set of stars with common velocities in space and thought to have a common origin in space and time. In the case of the Ursa Major group, all the stars formed about 300 million years ago.^[1] Its core is located roughly 80 light years away. It is rich in bright stars including most of the stars of the Big Dipper.

Discovery and constituents

All stars in the Ursa Major Moving Group are moving in roughly the same direction at similar velocities, and also have similar chemical compositions and estimated ages. This evidence suggests to astronomers that the stars in the group share a common origin.

Based on the numbers of its constituent stars, the Ursa Major Moving Group is believed to have once been an open cluster, having formed from a protostellar nebula approximately 500 million years ago. Since then, the sparse group has scattered over a region about 30 by 18 light-years, whose center is currently about 80 light-years away, making it the closest cluster-like object to Earth.

The Ursa Major Moving Group was discovered in 1869 by Richard A. Proctor, who noticed that, except for Dubhe and Alkaid (Eta Ursae Majoris), the stars of the Big Dipper asterism all have proper motions heading towards a common point in Sagittarius. Thus, the Big Dipper, unlike most constellations or asterisms, is largely composed of related stars.

Some of the brighter stream members include Alpha Coronae Borealis (α CrB or Alphecca or Gemma), Beta Aurigae (β Aur), Delta Aquarii (δ Aqr), Gamma Leporis (γ Lep) and Beta Serpentis (β Ser). More bright and moderately bright stars which are currently believed to be members of the group are listed below.

Group members

Current criteria for membership in the moving group is based on the stars' motion in space. This motion can be determined from the proper motions and parallax (or distance) to the stars and radial velocities. A study published in 2003 using data gathered by the Hipparcos satellite (1989-1993) greatly improved both the proper motion and parallax estimates of nearby bright stars, refining the study of this and other moving groups.^[1]

Based on their distances (measured with Hipparcos) and apparent magnitude, the absolute magnitude can be used to estimate the age of the stars. The stars in the moving group appear to have a common age of about 500 million years.

Core stars

The core of the moving group consists of 14 stars, of which 13 are in the Ursa Major constellation and the other is in the neighboring constellation of Canes Venatici.

The following are members of the moving group closest to its center.^[1] These stars are all in Ursa Major except where indicated.

Name	Constellation	B	F	HD	HIP	vis. mag.	Dist. (ly)	Sp. class	Notes
ε UMa	Ursa Major	ε	77	112185	62956	1.76	81	A0p	Alioth
ζ UMa A	Ursa Major	ζ	79	116656	65378	2.23	78	A2V	Mizar, Mizat, Mirza, Mitsar, Vasistha (quadruple system)
β UMa	Ursa Major	β	48	95418	53910	2.34	79	A1V	Merak, Mirak
γ UMa	Ursa Major	γ	64	103287	58001	2.41	84	A0V SB	Phad, Phecda, Phegda, Phekha, Phacd
δ UMa	Ursa Major	δ	69	106591	59774	3.32	81	A3V	Megrez, Kaffa
ζ UMa B	Ursa Major	ζ	79	116657		3.95			Part of Mizar quadruple system
80 UMa	Ursa Major	g	80	116842	65477	3.99	81	A5V SB	Alcor, Saidak, Suha, Arundhati (binary system)
78 UMa	Ursa Major		78	113139	63503	4.93	81	F2V
37 UMa	Ursa Major		37	91480	51814	5.16	86	F1V
HD 115043	Ursa Major			115043	64532	6.82	84	G1V	Gliese 503.2
HD 109011	Ursa Major			109011	61100	8.10	77	K2V	NO UMa
HD 110463	Ursa Major			110463	61946	8.28	76	K3V	NP UMa
HD 109647	Canes Venatici			109647	61481	8.53	86	K0	DO CVn

Stream stars

There is also a "stream" of stars which are likely members of the Ursa Major Moving Group, scattered more widely across the sky (from Cepheus to Triangulum Australe).

Name	Constellation	B	F	HD	HIP	vis. mag.	Dist. (ly)	Sp. class	Notes
β Aur	Auriga	β	34	40183	28360	1.90	82	A2V	Menkalinan, Menkalina
α CrB	Corona Borealis	α	5	139006	76267	2.22	75	A0V	Alphecca, Alphacca, Alphekka, Gemma, Gnosia, Gnosia Stella Coronae, Asteroth, Ashtaroth
δ Aqr	Aquarius	δ	76	216627	113136	3.27	159	A3V	Skat, Scheat, Seat, Sheat
ζ Leo	Leo	ζ	36	89025	50335	3.43	260	F0III	Adhafera, Aldhafera, Aldhafara
γ Lep A	Lepus	γ	13	38393	27072	3.59	29	F7V
β Ser	Serpens	β	28	141003	77233	3.65	153	A3V	Chow
ζ Boo A	Boötes	ζ	30	129246	71795	3.78	180	A3IVn
χ¹ Ori	Orion	χ¹	54	39587	27913	4.39	28	G0V
ζ Boo B	Boötes	ζ	30	129247		4.43	180	A2III
21 LMi	Leo Minor		21	87696	49593	4.49	91	A7V
χ Cet A	Cetus	χ	53	11171	8497	4.66	77	F3III
γ Mic	Microscopium	γ	39	199951	103738	4.67	223	G8III
ζ Crt	Crater	ζ	27	102070	57283	4.71	350	G8III
ζ TrA	Triangulum Australe	ζ	31	147584	80686	4.90	39	F9V
16 Lyr	Lyra		16	177196	93408	5.00	128	A7V
66 Tau	Taurus	r	66	27820	20522	5.10	396	A3V
59 Dra	Draco		59	180777	94083	5.11	89	A9V
89 Psc	Pisces	f	89	7804	6061	5.13	220	A3V
HD 75605	Pyxis			75605	43352	5.19	229	G8III
18 Boo	Boötes		18	125451	69989	5.41	85	F5IV
HD 109799	Hydra			109799	61621	5.41	113	F0V
π¹ UMa	Ursa Major	π¹	3	72905	42438	5.63	47	G1.5Vb	Muscida
HD 220096	Sculptor			220096	115312	5.65	329	G5IV
29 Com	Coma Berenices		29	111397	62541	5.71	402	A1V
HD 18778	Cepheus			18778	14844	5.92	202	A7III-IV
HD 165185	Sagittarius			165185	88694	5.94	57	G3V	Gliese 702.1
6 Sex	Sextans		6	85364	48341	6.01	200	A8III
HD 171746	Hercules			171746	91159	6.21	112	G2Vv comp
HD 26932	Taurus			26932		6.23	69	G0IV
HD 129798	Draco			129798	71876	6.24	139	F2V	DL Dra
41 Vir	Virgo		41	112097	62933	6.25	199	A7III
χ Cet B	Cetus	χ	53	11131	8486	6.72	78	G0	EZ Cet
HD 71974 A	Lynx			71974	41820	7.51	94	G5
HD 59747	Lynx			59747	36704	7.70	64	G5	DX Lyn
HD 28495	Camelopardalis			28495	21276	7.76	90	G0	MS Cam
HD 173950	Lyra			173950	92122	8.08	121	G5	V595 Lyr
HIP 66459	Canes Venatici				66459	9.06	36	K5	Gliese 519
HD 71974 B	Lynx			71974	41820	9.09	94
HD 95650	Leo			95650	53985	9.68	38	M0	DS Leo, Gliese 410
HD 238224	Ursa Major			238224	65327	9.72	82	K5	Gliese 509.1
HD 13959	Cetus			13959	10552	9.76	124	K2	Gliese 91.1
HD 156498	Ophiuchus			156498	84595	9.98	271		V2369 Oph

Non-members

The bright, nearby star Sirius was long believed to be a member of the group, but may not be, according to research in 2003 by Jeremy King et al. at Clemson University. This research seems to indicate that it is too young to be a member.

Our Solar System is in the outskirts of this stream, but is not a member, being about 10 times older. Our Sun merely drifted in along its 250-million-year galactic orbit, and 40 million years ago was nowhere near the Ursa Major group.

References

1 2 3 King, Jeremy R.; et al. (April 2003), "Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group", The Astronomical Journal, 125 (4): 1980–2017, Bibcode:2003AJ....125.1980K, doi:10.1086/368241

External links

University of Arizona website
Ken Croswell's astronomy website.
LeDrew, Glenn (1998). "AstroNotes: The Ursa Major Moving Cluster". Retrieved July 28, 2005.
Stellar kinematic groups, Superclusters, Moving Groups - D. Montes, UCM
J.R.King et al. 2003 Astronomical Journal paper classifying group members based on Hipparcos data.

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[aj125_4_1980-1] 1 2 3 King, Jeremy R.; et al. (April 2003), "Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group", The Astronomical Journal, 125 (4): 1980–2017, Bibcode:2003AJ....125.1980K, doi:10.1086/368241