Variable stars in the Ursa Minor dwarf galaxy

Details Variable stars in the Ursa Minor dwarf galaxy Variable stars in the Ursa Minor dwarf galaxy

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988aj.....96..528n&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 96, Aug. 1988, p. 528-559, 793-795. Research supported by Palomar Observatory and Ki

Astronomy and Astrophysics

Astronomy

64

Blue Stars, Cepheid Variables, Dwarf Galaxies, Elliptical Galaxies, Giant Stars, Abundance, Astronomical Photometry, Charge Coupled Devices, Color-Magnitude Diagram, Light Curve, Photographic Plates, Stellar Color, Stellar Mass

Scientific paper

The system of ≡95 variable stars in the Ursa Minor (UMi) dwarf galaxy has been studied using two new sets of photometry (derived from 22 photographic plates and 38 CCD frames taken in 1984), combined with van Agt's (1967, 1968) photometry of Baade's photographic plates. Accurate pulsation periods are derived for 88 variable stars, three of which were discovered near the outer edge of the galaxy. Despite the existence of many relatively long-period c type RR Lyrae stars, an extensive search revealed no double-mode RR Lyrae stars. Period-amplitude and period-rise-time diagrams are plotted and discussed. A c-m diagram for UMi, which is based on CCD photometry and includes the RR Lyrae stars, shows that the blue and red edges of the instability strip occur at B-V = 0.16±0.03 mag and 0.40±0.05 mag, respectively. The distance modulus for UMi is (m-M)0 = 19.24±0.24 mag, corresponding to a distance of 70±9 kpc. In addition to the three previously known anomalous Cepheids in UMi four new anomalous Cepheids have been identified. By using the P-L diagram to establish the true pulsation modes for anomalous Cepheids, much more reliable mass estimates can now be made.

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