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| 2MASS J19361171+4523009 , the SIMBAD biblio (10 results) | C.D.S. - SIMBAD4 rel 1.8 - 2026.10.18CEST13:55:16 |
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More on score
| Bibcode/DOI | Score |
in Title|Abstract| Keywords |
in a table | in teXt, Caption, ... | Nb occurence | Nb objects in ref |
Citations (from ADS) |
Title | First 3 Authors |
|---|---|---|---|---|---|---|---|---|---|
2014ApJS..211...24M 
|
15 | D | 1 | 34022 | 573 | Rotation periods of 34,030 Kepler main-sequence stars: the full autocorrelation sample. | McQUILLAN A., MAZEH T. and AIGRAIN S. | ||
| 2019MNRAS.482.1757L | 179 | D | C F | 4 | 25 | 13 | Period spacings of γ Doradus pulsators in the Kepler field: detection methods and application to 22 slow rotators. | LI G., BEDDING T.R., MURPHY S.J., et al. | |
|
2019MNRAS.485.2380M
|
16 | D | 1 | 14330 | 108 | Gaia-derived luminosities of Kepler A/F stars and the pulsator fraction across the δ Scuti instability strip. | MURPHY S.J., HEY D., VAN REETH T., et al. | ||
|
2020MNRAS.491.3586L
|
16 | D | 3 | 609 | 75 | Gravity-mode period spacings and near-core rotation rates of 611 γ Doradus stars with Kepler. | LI G., VAN REETH T., BEDDING T.R., et al. | ||
|
2020MNRAS.499.3481A
|
16 | D | 1 | 28505 | 24 | Evidence for metallicity-dependent spin evolution in the Kepler field. | AMARD L., ROQUETTE J. and MATT S.P. | ||
|
2021AJ....161..189L
|
17 | D | 1 | 29956 | 19 | Gyro-kinematic ages for around 30,000 Kepler stars. | LU Y., ANGUS R., CURTIS J.L., et al. | ||
|
2022ApJS..259...63S
|
17 | D | 1 | 10269 | 2 | Objective Separation between CP1 and CP2 Based on Feature Extraction with Machine Learning. | SHANG L.-H., LUO A.-L., WANG L., et al. | ||
|
2023ApJS..266...14T
|
17 | D | 1 | 21501 | ~ | A New Catalog of Am-type Chemically Peculiar Stars Based on LAMOST. | TIAN X.-M., WANG Z.-H., ZHU L.-Y., et al. | ||
| 2023A&A...677A..63M | 17 | D | 1 | 19 | ~ | Calibrating angular momentum transport in intermediate-mass stars from gravity-mode asteroseismology. | MOMBARG J.S.G. | ||
|
2024A&A...684A.112F
|
18 | D | 1 | 491 | ~ | Age uncertainties of red giants due to cumulative rotational mixing of progenitors calibrated by asteroseismology. | FRITZEWSKI D.J., AERTS C., MOMBARG J.S.G., et al. |
