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• W2077962146 abstract "We have applied the image subtraction method of Alard and Lupton to the extensive M3 data set previously analyzed by Corwin and Carney using DAOPHOT and ALLSTAR. This new analysis has produced light curves and periods for 15 variables not found in the previous study but already known to be variables, and it has also resulted in improved periods for several other variables. The additional variables recovered with the image subtraction analysis are in the very central region of M3, where crowding is severe and the photometry was not of sufficient quality that it could be put on the standard system. The present study brings to 222 the total number of RR Lyrae variables in Corwin and Carney's M3 data set for which light curves and periods are available. Among them we have identified three new candidate double-mode pulsating variables (V13, V200, and V251), reported here for the first time. This brings to eight the total number of double-mode RR Lyrae (RRd's) identified in M3. Of the newly discovered RRd's V13 is unusual in that it has the fundamental as the dominant pulsation mode. M3 is unique among the globular clusters in having RRd variables with a dominant fundamental mode. Two of the new candidate RRd's (V13 and V200) have period ratios as low as 0.738–0.739. They lie well separated from all previously known double-mode variable stars in the Petersen diagram in positions implying a large spread in mass and/or, less likely, in heavy element mass fraction, among the M3 horizontal-branch (HB) stars. We explore mass transfer and helium enhancement as possible explanations for the apparent spread in HB masses. We also note that the masses derived from the double-mode analyses now favor little mass loss on the red giant branch. We find that V200 has changed its dominant pulsation mode from fundamental to first overtone, while V251 has changed its dominant mode from first overtone to fundamental in the interval 1992 to 1993. Together with M3-V166 this is the first time that double-mode variables are observed to switch their dominant pulsation modes while remaining RRd's. The phenomenon is found to occur in a 1 yr time span, thus suggesting that these stars are undergoing a rapid evolutionary phase and that both redward and blueward evolution may take place among the HB stars in the Oosterhoff type I cluster M3. The unusual behavior of the M3 RRd's is discussed in detail and compared with that of the double-mode RR Lyrae identified so far in globular clusters and in the field of our and other Local Group galaxies. We find a lack of correlation between the presence of RRd variables and any of the cluster structural parameters." @default.
• W2077962146 created "2016-06-24" @default.
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• W2077962146 date "2004-02-01" @default.
• W2077962146 modified "2023-09-27" @default.
• W2077962146 title "Image-Subtraction Photometry of the Globular Cluster M3: Identification of New Double-Mode RR Lyrae Stars" @default.
• W2077962146 cites W1543514612 @default.
• W2077962146 cites W1659264257 @default.
• W2077962146 cites W1768987830 @default.
• W2077962146 cites W1852203787 @default.
• W2077962146 cites W188478295 @default.
• W2077962146 cites W1966590499 @default.
• W2077962146 cites W1966714030 @default.
• W2077962146 cites W1970306442 @default.
• W2077962146 cites W1970473639 @default.
• W2077962146 cites W1974474208 @default.
• W2077962146 cites W1974618482 @default.
• W2077962146 cites W1974632500 @default.
• W2077962146 cites W1974872442 @default.
• W2077962146 cites W1976968164 @default.
• W2077962146 cites W1977220861 @default.
• W2077962146 cites W1979886222 @default.
• W2077962146 cites W1982250812 @default.
• W2077962146 cites W1982798438 @default.
• W2077962146 cites W1983881558 @default.
• W2077962146 cites W1984417655 @default.
• W2077962146 cites W1986316936 @default.
• W2077962146 cites W1988147641 @default.
• W2077962146 cites W1989763959 @default.
• W2077962146 cites W1990566336 @default.
• W2077962146 cites W1992962624 @default.
• W2077962146 cites W1993821528 @default.
• W2077962146 cites W1998686452 @default.
• W2077962146 cites W1999920716 @default.
• W2077962146 cites W2010808245 @default.
• W2077962146 cites W2020291889 @default.
• W2077962146 cites W2021321914 @default.
• W2077962146 cites W2022340092 @default.
• W2077962146 cites W2022347699 @default.
• W2077962146 cites W2023016496 @default.
• W2077962146 cites W2024450031 @default.
• W2077962146 cites W2024599398 @default.
• W2077962146 cites W2026280496 @default.
• W2077962146 cites W2026294585 @default.
• W2077962146 cites W2027415228 @default.
• W2077962146 cites W2029990369 @default.
• W2077962146 cites W2035747200 @default.
• W2077962146 cites W2035819620 @default.
• W2077962146 cites W2048399053 @default.
• W2077962146 cites W2054757488 @default.
• W2077962146 cites W2062100494 @default.
• W2077962146 cites W2063770063 @default.
• W2077962146 cites W2064249025 @default.
• W2077962146 cites W2066406099 @default.
• W2077962146 cites W2067076144 @default.
• W2077962146 cites W2068043666 @default.
• W2077962146 cites W2071666852 @default.
• W2077962146 cites W2073842175 @default.
• W2077962146 cites W2075667030 @default.
• W2077962146 cites W2081394709 @default.
• W2077962146 cites W2083272039 @default.
• W2077962146 cites W2085420866 @default.
• W2077962146 cites W2085557516 @default.
• W2077962146 cites W2085739302 @default.
• W2077962146 cites W2087572450 @default.
• W2077962146 cites W2088285361 @default.
• W2077962146 cites W2089285061 @default.
• W2077962146 cites W2092528015 @default.
• W2077962146 cites W2093547946 @default.
• W2077962146 cites W2095176036 @default.
• W2077962146 cites W2109127561 @default.
• W2077962146 cites W2110253451 @default.
• W2077962146 cites W2115783648 @default.
• W2077962146 cites W2122500744 @default.
• W2077962146 cites W2126393356 @default.
• W2077962146 cites W2131462302 @default.
• W2077962146 cites W2131495488 @default.
• W2077962146 cites W2145618994 @default.
• W2077962146 cites W2478105191 @default.
• W2077962146 cites W2757218774 @default.
• W2077962146 cites W2800816723 @default.
• W2077962146 cites W3099665156 @default.
• W2077962146 cites W3100682716 @default.
• W2077962146 cites W3101001548 @default.
• W2077962146 cites W3101303784 @default.
• W2077962146 cites W3104685924 @default.
• W2077962146 cites W3105440368 @default.
• W2077962146 cites W3105441361 @default.
• W2077962146 cites W4299584246 @default.
• W2077962146 cites W4301672288 @default.
• W2077962146 doi "https://doi.org/10.1086/380938" @default.
• W2077962146 hasPublicationYear "2004" @default.
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