Papers › On the Evolution of Rotational Modulation Amplitude in Solar-mass Main-sequence Stars
On the Evolution of Rotational Modulation Amplitude in Solar-mass Main-sequence Stars
Kento Masuda
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We investigate the relation between rotation periods Pᵣₒₜ and photometric modulation amplitudes Rₚₑᵣ for ≈4,000 Sun-like main-sequence stars observed by Kepler, using Pᵣₒₜ and Rₚₑᵣ from McQuillan et al. (2014), effective temperature T_(eff) from LAMOST DR6, and parallax data from Gaia EDR3. As has been suggested in previous works, we find that Pᵣₒₜ scaled by the convective turnover time τ_c, or the Rossby number Ro=Pᵣₒₜ/τ_c, serves as a good predictor of Rₚₑᵣ: Rₚₑᵣ plateaus around 1% in relative flux for 0.2 ≲Ro/Ro_⊙ ≲0.4, and decays steeply with increasing Ro for 0.4 ≲Ro/Ro_⊙ ≲0.8, where Ro_⊙ denotes Ro of the Sun. In the latter regime we find dlnRₚₑᵣ/dlnRo ∼-4.5 to -2.5, although the value is sensitive to detection bias against weak modulation and may depend on other parameters including T_(eff) and surface metallicity. The existing X-ray and Ca II H&K flux data also show transitions at Ro/Ro_⊙∼0.4, suggesting that all these transitions share the same physical origin. We also find that the rapid decrease of Rₚₑᵣ with increasing Ro causes rotational modulation of fainter Kepler stars with Ro/Ro_⊙ ≳0.6 to be buried under the photometric noise. This effect sets the longest Pᵣₒₜ detected in the McQuillan et al. (2014) sample as a function of T_(eff), and obscures the signature of stalled spin down that has been proposed to set in around Ro/Ro_⊙ ∼1.
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