The Short-Period Variable Stars in the Magellanic Clouds

Author(s):  
Jorge Landi Dessy ◽  
José R. Laborde
2016 ◽  
Vol 465 (1) ◽  
pp. 434-459 ◽  
Author(s):  
S. A. Macfarlane ◽  
P. A. Woudt ◽  
P. J. Groot ◽  
G. Ramsay ◽  
R. Toma ◽  
...  

1989 ◽  
Vol 111 ◽  
pp. 285-285
Author(s):  
H.A. Smith ◽  
J.R. Kuhn ◽  
J. Curtis

AbstractBVR observations of the relatively metal-rich globular cluster NGC 6388 have been obtained with a CCD on the CTIO 0.9 m telescope. Eighteen possible short period variable stars have been discovered in or near the cluster. At least 10 of these are probable RR Lyrae members of NGC 6388. We confirm the finding of Hazen and Hesser that this cluster is one of the most metal-rich to contain a significant number of RR Lyraes. A program of CCD photometry of field and cluster variable stars has been initiated on the 0.6m telescope of the Michigan State University Observatory.


1993 ◽  
Vol 139 ◽  
pp. 337-337
Author(s):  
Martha L. Hazen

A search for variable stars in the globular cluster NGC 6544 has revealed only one possible short period variable within the tidal radius of the cluster. A search in NGC 6642 yielded 16 new RR Lyrae stars within the tidal radius and 5 new field RRs. The previously discovered (Hoffleit 1972) V1 is a slow variable, and V2 is an RR Lyrae star. Photometry of the variables within the tidal radius gives a mean B for the horizontal branch of < B > = 17.0 mag. With E(B – V) = 0.37 mag and (B – V) = 0.35 mag for RR Lyraes, a value for V(HB) = 16.3 mag is derived. This is about one mag fainter than previous estimates (Webbink 1985), and places NGC 6642 at a distance of approximately 7.9 kpc.


1964 ◽  
Vol 69 ◽  
pp. 251 ◽  
Author(s):  
J. R. McCullough

1984 ◽  
Vol 108 ◽  
pp. 223-224
Author(s):  
Horace A. Smith ◽  
Leo Connolly

The Small Magellanic Cloud is known to contain types of short period Cepheid variable stars not yet discovered in either the Large Magellanic Cloud or, with the exception of a single star, in the Galaxy. These variables can be divided into two categories: anomalous Cepheids and Wesselink-Shuttleworth (WS) stars. The former, which have also been found in dwarf spheroidal systems and in the globular cluster NGC 5466, have periods of 0.4–3 days, but average 0.7–1.0 mag. brighter than RR Lyrae and BL Her stars of equal period. The stars we call WS stars have periods less than about 1.1 day and, at MV = −1 to −2, are brighter than anomalous Cepheids of equal period.


1967 ◽  
Vol 149 ◽  
pp. 55 ◽  
Author(s):  
I. J. Danziger ◽  
R. J. Dickens

New Astronomy ◽  
2012 ◽  
Vol 17 (2) ◽  
pp. 65-72
Author(s):  
L. Fox Machado ◽  
A.S. Baran ◽  
M. Winiarski ◽  
J. Krzesiński ◽  
M. Dróżdz

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