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Rotation of Late-type Stars in Praesepe with K2

  • Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, J. Bouvier, D. R. Soderblom, M. Pinsonneault, and L. Hebb

2017 The Astrophysical Journal 839 92.

  • Provider: AAS Journals

Caption: Figure 13.

Plot of P vs. ﹩(V-{K}_{{\rm{s}}})﹩ (top row) and ﹩{K}_{{\rm{s}}}﹩ vs. ﹩(V-{K}_{{\rm{s}}})﹩ (bottom row) highlighting the single-period (left) and multi-period (right) populations. The vertical lines are at ﹩(V-{K}_{{\rm{s}}})﹩ = 1.3 and 4.5, the divisions are from Figure 7 above, for reference. The multi-period stars dominate for ﹩(V-{K}_{{\rm{s}}})﹩ ≲ 1.5–2. The M stars that are multi-periodic are more likely to be photometric binaries, as in the Pleiades.

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