scholarly journals Pre-main sequence candidates in the very young open cluster NGC 6611

1997 ◽  
Vol 121 (2) ◽  
pp. 223-242 ◽  
Author(s):  
D. de Winter ◽  
C. Koulis ◽  
P. S. Thé ◽  
M. E. van den Ancker ◽  
M. R. Pérez ◽  
...  
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Young Open Cluster

scholarly journals Pre-main-sequence variable stars in young open cluster NGC 1893

2012 ◽  
Vol 427 (2) ◽  
pp. 1449-1462 ◽  
Author(s):  
Sneh Lata ◽  
A. K. Pandey ◽  
W. P. Chen ◽  
G. Maheswar ◽  
Neelam Chauhan
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Variable Stars ◽  
Young Open Cluster

scholarly journals Interstellar polarization and extinction towards the young open cluster NGC 1502

2018 ◽  
Vol 615 ◽  
pp. A166 ◽  
Author(s):  
G. A. Topasna ◽  
N. T. Kaltcheva ◽  
E. Paunzen
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Extinction Ratio ◽  
Color Excess ◽  
Young Open Cluster ◽  
Multi Wavelength ◽  
Solar Metallicity ◽  
The Individual ◽  
Photometric Distance ◽  
Selective Extinction

Aims. NGC 1502 is located at the periphery of the Cam OB1 association and probably within the Orion Spur, with published distance estimates varying between 0.7 and 1.5 kpc. We combine new polarimetric observations and existing uvbyβ and UBV photometries to provide new estimates of the cluster’s parameters. Methods. We present new multi-wavelength polarization observations of 22 stars in the direction of the cluster and, using the wavelength of maximum polarization, calculate the total-to-selective extinction ratio for each of these stars. These are combined with homogenized uvbyβ and UBV photometries to obtain the individual stellar distances and study the structure of the field. Results. We found no evidence of significant extinction variation across the cluster and obtained an average color excess E(b − y) = 0.56 ± 0.02 mag, corresponding to E(B − V) = 0.76 mag. Given the uniformity of both pmax and λmax toward the cluster and the distribution of the color excess with distance, it seems likely that the polarization in this region arises from aligned dust grains in the foreground of the cluster, not farther than 500–600 pc. Based on 20 stars located beyond 500 pc within the studied field of view, we obtained an average polarization-based total-to-selective extinction ratio R = 2.83 ± 0.14 yielding visual absorption AV = 2.14 ± 0.16 mag. Using 11 stars with uvbyβ data that represent the main sequence of the cluster, we calculated a photometric distance of 1117−89+96 pc. This estimate is fully supported by the UBV -based analysis and the new individual membership probabilities that we derive. Assuming a solar metallicity yields an age of 5 Myr. Our analysis yields controversial results regarding the membership of the stars associated with the SZ Cam system (HD 25638 and HD 25639) to the cluster.

scholarly journals From the Top to the Bottom of the Main Sequence: A Complete Mass Function of the Young Open Cluster M35

2001 ◽  
Vol 546 (2) ◽  
pp. 1006-1018 ◽  
Author(s):  
David Barrado y Navascues ◽  
John R. Stauffer ◽  
Jerome Bouvier ◽  
Eduardo L. Martin
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Mass Function ◽  
Young Open Cluster

scholarly journals Main-sequence variable stars in young open cluster NGC 1893

2014 ◽  
Vol 442 (1) ◽  
pp. 273-284 ◽  
Author(s):  
Sneh Lata ◽  
Ram Kesh Yadav ◽  
A. K. Pandey ◽  
Andrea Richichi ◽  
C. Eswaraiah ◽  
...  
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Variable Stars ◽  
Young Open Cluster

scholarly journals Triggered massive star formation in the open cluster NGC 1893

2003 ◽  
Vol 212 ◽  
pp. 562-563
Author(s):  
Amparo Marco ◽  
Ignacio Negueruela
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Massive Star ◽  
Main Sequence ◽  
Open Cluster ◽  
Star Forming ◽  
Young Open Cluster ◽  
H Ii Region ◽  
Pms Stars ◽  
Bright Emission

We have carried out a search for emission line pre-main sequence (PMS) stars in the area of the star-forming young open cluster NGC 1893 by means of slitless spectroscopy. We find 19 emission line stars with spectral types spanning the range from early B-type to G-type. All the PMS stars are confined to two small regions: the outer rim of the molecular cloud associated with the H ii region IC 410 and the vicinity of the bright emission cometary nebulae Sim 129 and Sim 130. The overall spatial distribution of PMS stars strongly suggests, that present day star formation in NGC 1893 is triggered by the O-type stars in the cluster.

scholarly journals Pre-main-sequence stars in the young open cluster NGC 1893

2007 ◽  
Vol 471 (2) ◽  
pp. 485-497 ◽  
Author(s):  
I. Negueruela ◽  
A. Marco ◽  
G. L. Israel ◽  
G. Bernabeu
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Main Sequence Stars ◽  
Young Open Cluster

scholarly journals Stellar Content of the Young Open Cluster NGC 6823

2000 ◽  
Vol 176 ◽  
pp. 499-500
Author(s):  
A. Pigulski ◽  
Z. Kolaczkowski ◽  
G. Kopacki
Keyword(s):  
Main Sequence ◽  
Evolutionary Rate ◽  
Open Cluster ◽  
Variable Stars ◽  
Period Change ◽  
Stellar Content ◽  
Preliminary Results ◽  
The Future ◽  
Young Open Cluster

AbstractThe preliminary results of the CCD search for variable stars in the very young open cluster NGC 6823 are presented. About ten new variable stars were discovered. The most interesting finding is that of the two pre-main sequence (PMS) δ Scuti-type variables. Because the evolutionary rate of period change is large at the PMS stage, these stars could be used in the future for testing it observationally.

scholarly journals He I 5876 Å Line in the Study of Chromospheric Activity in F-type MS Stars

1991 ◽  
Vol 130 ◽  
pp. 477-479
Author(s):  
R. J. García López ◽  
R. Rebolo ◽  
J. E. Beckman ◽  
C. D. McKeith
Keyword(s):  
Energy Source ◽  
Magnetic Fields ◽  
Main Sequence ◽  
Open Cluster ◽  
X Rays ◽  
Chromospheric Activity ◽  
Heating Mechanism ◽  
Young Open Cluster ◽  
Activity Indices

AbstractWe have measured the He I D3 line, λ5876 Å, in 32 F-type young open cluster stars and in 4 field stars. Combining our results with previous observations of D3 we strengthen the following conclusions: (a) Sub-surface convective zones appear, on the main sequence, around F0 (B – V ~ 0.3). (b) The stars between F0 and F5 (0.3 ≲ B – V ≲ 0.42) are chromospherically “active” irrespective of age, which implies a heating mechanism not affected by evolutionary effects. In this range the activity in D3 and X-rays are uncorrelated. (c) For stars later than F5 the correlation among all the activity indices, chromospheric and coronal, shows a common energy source. Convective zones here should be deep enough to generate magnetic fields capable of supplying this energy, and also for braking the rotation.

scholarly journals NGC 146: a young open cluster with a Herbig Be star and intermediate mass pre-main sequence stars

2005 ◽  
Vol 440 (2) ◽  
pp. 511-522 ◽  
Author(s):  
A. Subramaniam ◽  
D. K. Sahu ◽  
R. Sagar ◽  
P. Vijitha
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Main Sequence Stars ◽  
Intermediate Mass ◽  
Young Open Cluster ◽  
Be Star
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