2002A&A...387..890M

Query : 2002A&A...387..890M

2002A&A...387..890M - Astronomy and Astrophysics, volume 387, 890-902 (2002/6-1)

Light element abundances in the young open clusters NGC 3293, NGC 4755 and NGC 6231: Tracers of stellar evolution.

MATHYS G., ANDRIEVSKY S.M., BARBUY B., CUNHA K. and KOROTIN S.A.

Abstract (from CDS):

The abundances of He (LTE), C, N, and O (NLTE) were derived for 21 B stars in three young open clusters. Almost all the stars show subsolar CNO abundances. However, the mean oxygen abundance for each programme cluster appears to be in marginal agreement with the most recent revisions of the solar value. After consideration of the CN abundances in this sample, there is no clear evidence of internal mixing. Only three stars among the non-supergiants seem to show a nitrogen enhancement. Two of them have a fairly low projected equatorial velocity (admittedly, they may be rapid rotators seen pole-on); the third one is a definite fast rotator. In the lower gravity stars (three stars in this sample with logg<3.0) some kind of mixing has apparently occurred. The supergiants do not differ significantly from the other programme stars in their respective helium contents. The mean helium abundance for each cluster is close to the standard value, (He/H) ≃11.0.

Abstract Copyright: ∼

Journal keyword(s): open clusters and associations: individual: NGC 3293, NGC 4755, NGC 6231 - stars: abundances - stars: early type

CDS comments: In reflist, Arp, 1958, AJ : 431 misprint for 341 (1958AJ.63.341A).

Simbad objects: 24

Full paper

View the references in ADS

Number of rows : 24

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2023	#notes
1	V* V403 Car	bC*	10 35 40.7035044864	-58 12 44.280907776	7.93	8.75	8.73	9.48	8.65	OB	49	1
2	CD-57 3348	*	10 35 46.5644077488	-58 14 12.034964904	6.93	7.70	7.75	7.49	7.38	B1II	50	0
3	NGC 3293	OpC	10 35 53	-58 13.9						~	304	0
4	CPD-57 3522	*	10 35 56.5884258456	-58 11 31.603843788	9.31	10.11	10.13	10.10	10.10	B2III	30	0
5	CPD-57 3523	*	10 35 57.7156652832	-58 13 20.816447556	7.19	8.05	8.03	7.92	7.85	B1III	41	0
6	V* V406 Car	bC*	10 35 57.8106305760	-58 12 21.308777280	8.39	9.22	9.26	9.24	9.20	B1V	38	0
7	HD 92044	*	10 36 16.0790202360	-58 16 38.162765820	7.72	8.40	8.25	8.10	7.91	B1II	67	0
8	CD-59 4454	EB*	12 53 20.6734801416	-60 23 16.843450812	9.26	9.90	9.74	10.03		B1V	53	0
9	CPD-59 4535	*	12 53 24.00	-60 23 00.0	9.83	10.370	10.222			~	22	0
10	V* BU Cru	EB*	12 53 37.6193092848	-60 21 25.425832356	6.49	7.04	6.84	7.55		B2Ib	112	0
11	NGC 4755	OpC	12 53 40	-60 22.3						~	286	0
12	CPD-59 4552	*	12 53 46.4935086912	-60 24 12.419407044	7.79	8.337	8.24	9.13		B1III	50	0
13	CPD-59 4553	*	12 53 46.5460448304	-60 22 18.370370064	9.16	9.75	9.58			B1.5V	21	0
14	* kap Cru	SB*	12 53 48.9198156672	-60 22 34.469837436	5.62	6.12	5.94	7.12		B5I	127	0
15	CPD-59 4564	bC*	12 53 57.5386794336	-60 24 58.092625152	8.45	9.12	9.06	9.64		B2III	62	0
16	HD 111990	s*b	12 53 59.7993033672	-60 20 07.510329996	6.46	6.95	6.78	7.68		B1.5I+	85	0
17	NGC 6231	OpC	16 54 08.51	-41 49 36.0		2.83	2.6			~	524	0
18	2MASS J16540927-4148410	Y*?	16 54 09.2737061088	-41 48 41.072216580	8.964	9.564	9.424		9.134	B1V	36	0
19	CD-41 11034	Y*?	16 54 11.3119116264	-41 48 53.965557072	8.878	9.546	9.335	9.744	8.943	B1V	41	0
20	HD 152249	s*b	16 54 11.6395658856	-41 50 57.295111524	5.91	6.65	6.45			OC9Iab	230	0
21	CD-41 11037	SB*	16 54 13.2253067352	-41 50 32.518100184	7.21	8.08	7.90			O9IV	74	0
22	HD 326329	Y*?	16 54 14.1033282720	-41 50 08.503512720	8.141	9.183	9.013	9.477	8.460	O9.7V	69	0
23	V* V1208 Sco	EB*	16 54 21.3090092232	-41 51 41.766233904	9.293	9.91	9.708	9.96	9.344	B0-2V	45	0
24	HD 152314	Y*?	16 54 32.0048577720	-41 48 18.848961036	7.256	7.974	7.749	9.01	7.446	O9IV	107	0

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