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| Cl* NGC 2264 HAR 13 , the SIMBAD biblio (10 results) | C.D.S. - SIMBAD4 rel 1.8 - 2026.10.18CEST23:23:41 |
| 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 |
|---|---|---|---|---|---|---|---|---|---|
| 1965VA......8...89H | 190 | ~ | Flare stars in stellar aggregates of different ages. | HARO G. and CHAVIRA E. | |||||
|
1999A&A...345..521F |
523 | 53 | BVRI photometry of the star-forming region NGC 2264: the initial mass function and star-forming rate. | FLACCOMIO E., MICELA G., SCIORTINO S., et al. | |||||
|
2004A&A...417..557L |
2310 | 153 | A rotational and variability study of a large sample of PMS stars in NGC2264. | LAMM M.H., BAILER-JONES C.A.L., MUNDT R., et al. | |||||
|
2013ApJS..209...32B |
15 | D | 1 | 8196 | 71 | Identifying young stars in massive star-forming regions for the MYStIX project. | BROOS P.S., GETMAN K.V., POVICH M.S., et al. | ||
|
2014A&A...570A..82V |
15 | D | 1 | 770 | 103 | Mapping accretion and its variability in the young open cluster NGC 2264: a study based on u-band photometry. | VENUTI L., BOUVIER J., FLACCOMIO E., et al. | ||
|
2015A&A...581A..66V |
16 | D | 1 | 683 | 36 | UV variability and accretion dynamics in the young open cluster NGC 2264. | VENUTI L., BOUVIER J., IRWIN J., et al. | ||
|
2016A&A...586A..47S |
16 | D | 1 | 476 | 27 | CSI 2264: Accretion process in classical T Tauri stars in the young cluster NGC 2264. | SOUSA A.P., ALENCAR S.H.P., BOUVIER J., et al. | ||
|
2016ApJ...821....8K |
16 | D | 1 | 1943 | 23 | Spectroscopic binaries in the Orion nebula cluster and NGC 2264. | KOUNKEL M., HARTMANN L., TOBIN J.J., et al. | ||
|
2017A&A...599A..23V |
16 | D | 1 | 513 | 69 | CSI 2264: Investigating rotation and its connection with disk accretion in the young open cluster NGC 2264. | VENUTI L., BOUVIER J., CODY A.M., et al. | ||
|
2022ApJS..262....7H |
17 | D | 1 | 134735 | 19 | A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun. | HE Z., WANG K., LUO Y., et al. |