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The Classificiation of Kepler B star Variables
Solar and Stellar Astrophysics · Submitted 10 Feb 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We increase the number of candidate B-star variables found in the Kepler data base by Balona et al. (2011) in the following fashion: $\beta$ Cep stars from 0 to 10, slowly pulsating B stars from 8 to 54, hybrid pulsators from 7 to 21, and Bin/Rot stars from 23 to 82.
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The abstract, sentence by sentence
The light curves of 252 B-star candidates in the Kepler data base are analyzed in a similar fashion to that done by Balona et al. (2011) to further characterize B star variability, increase the sample of variable B stars for future study, and to identify stars whose power spectra include particularly interesting features such as frequency groupings. Stars are classified as either constant light emitters, $\beta$ Cep stars, slowly pulsating B stars, hybrid pulsators, binaries or stars whose light curves are dominated by rotation (Bin/Rot), hot subdwarfs, or white dwarfs. One-hundred stars in our sample were found to be either light contants or to be variable at a level of less than 0.02 mmag. We increase the number of candidate B-star variables found in the Kepler data base by Balona et al. (2011) in the following fashion: $\beta$ Cep stars from 0 to 10, slowly pulsating B stars from 8 to 54, hybrid pulsators from 7 to 21, and Bin/Rot stars from 23 to 82. For comparison purposes, approximately 51 SPBs and 6 hybrids had been known prior to 2007. The number of $\beta$ Cep stars known prior to 2004 was 93. A secondary result of this study is the identification of an additional 11 pulsating white dwarf candidates, four of which possess frequency groupings.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The light curves of 252 B-star candidates in the Kepler data base are analyzed in a similar fashion to that done by Balona et al. (2011) to further characterize B star variability, increase the sample of variable B stars for future study, and to identify stars whose power spectra include particularly interesting features such as frequency groupings. | contribution 0.69 | 0.88 | 0.07 | asserted 0.94 |
| s1 | Stars are classified as either constant light emitters, $\beta$ Cep stars, slowly pulsating B stars, hybrid pulsators, binaries or stars whose light curves are dominated by rotation (Bin/Rot), hot subdwarfs, or white dwarfs. | method 0.72 | 0.69 | 0.14 | asserted 1.00 |
| s2 | One-hundred stars in our sample were found to be either light contants or to be variable at a level of less than 0.02 mmag. | result 1.00 | 0.97 | 0.08 | asserted 1.00 |
| s3 | We increase the number of candidate B-star variables found in the Kepler data base by Balona et al. (2011) in the following fashion: $\beta$ Cep stars from 0 to 10, slowly pulsating B stars from 8 to 54, hybrid pulsators from 7 to 21, and Bin/Rot stars from 23 to 82. | result 0.93 | 0.95 | 0.48 | asserted 1.00 |
| s4 | For comparison purposes, approximately 51 SPBs and 6 hybrids had been known prior to 2007. | background 0.97 | 0.05 | 0.04 | asserted 0.95 |
| s5 | The number of $\beta$ Cep stars known prior to 2004 was 93. | background 1.00 | 0.04 | 0.02 | asserted 1.00 |
| s6 | A secondary result of this study is the identification of an additional 11 pulsating white dwarf candidates, four of which possess frequency groupings. | result 0.99 | 0.96 | 0.07 | asserted 0.94 |
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Original abstract
The light curves of 252 B-star candidates in the Kepler data base are analyzed in a similar fashion to that done by Balona et al. (2011) to further characterize B star variability, increase the sample of variable B stars for future study, and to identify stars whose power spectra include particularly interesting features such as frequency groupings. Stars are classified as either constant light emitters, $\beta$ Cep stars, slowly pulsating B stars, hybrid pulsators, binaries or stars whose light curves are dominated by rotation (Bin/Rot), hot subdwarfs, or white dwarfs. One-hundred stars in our sample were found to be either light contants or to be variable at a level of less than 0.02 mmag. We increase the number of candidate B-star variables found in the Kepler data base by Balona et al. (2011) in the following fashion: $\beta$ Cep stars from 0 to 10, slowly pulsating B stars from 8 to 54, hybrid pulsators from 7 to 21, and Bin/Rot stars from 23 to 82. For comparison purposes, approximately 51 SPBs and 6 hybrids had been known prior to 2007. The number of $\beta$ Cep stars known prior to 2004 was 93. A secondary result of this study is the identification of an additional 11 pulsating white dwarf candidates, four of which possess frequency groupings.
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