论文标题
关于太阳质量主序列中旋转调制幅度的演变
On the Evolution of Rotational Modulation Amplitude in Solar-mass Main-sequence Stars
论文作者
论文摘要
我们研究旋转期之间的关系$ p_ \ mathrm {rot} $和光度调制放大$ r_ \ r_ \ mathrm {perrm {per} $ for $ \ for $ \大约4,000 $ $ sun $ po_plm { （2014年），Lamost DR6的有效温度$ T_ \ MATHRM {EFF} $，以及Gaia EDR3的视差数据。正如以前的作品所建议的那样，我们发现$ p_ \ mathrm {rot} $由对流周转时间$τ_\ mathrm {c} $缩放，或者rossby number $ \ mathrm {ro} = p_ \ mathrm {rotrm {rot} $ r_ \ mathrm {per} $：$ r_ \ mathrm {per} $ plapeaus左右$ 1 \％$相对通量的相对通量，$ 0.2 \ sillsim \ simsim \ mathrm \ mathrm {ro}/\ mathrm {ro} \ Mathrm {ro}/\ MathRM {ro} _ \ odot \ sillsim 0.8 $，其中$ \ mathrm {ro} _ \ odot $ nesot $ nesotes $ \ mathrm {ro}的太阳在后一种方案中，我们发现$ \ mathrm {d} \ ln r_ \ mathrm {per}/\ mathrm {d} \ ln \ mathrm {ro} \ sim -4.5 $ to $ -2.5 $金属性。现有的X射线和CA II H＆K通量数据还显示了$ \ Mathrm {Ro}/\ Mathrm {Ro} _ \ odot \ sim 0.4 $的过渡，这表明所有这些过渡都共享相同的物理起源。我们还发现，随着$ \ mathrm {ro} $的增加，$ r_ \ mathrm {per} $的迅速减少导致使用$ \ mathrm {ro}/\ mathrm {ro}/\ mathrm {ro} _ \ odot \ odot \ odot \ gtrsim 0.6 $ 0.6 $ 0.6 $ 0.6 $ bured the Photemement的旋转调制。此效果设置了McQuillan等人检测到的最长$ P_ \ Mathrm {Rot} $。 （2014）示例作为$ t_ \ mathrm {eff} $的函数，并掩盖了停滞的签名，该签名已被提议设置在$ \ mathrm {ro}/\ mathrm {ro} _ \ odot \ odot \ sim 1 $中。
We investigate the relation between rotation periods $P_\mathrm{rot}$ and photometric modulation amplitudes $R_\mathrm{per}$ for $\approx 4,000$ Sun-like main-sequence stars observed by Kepler, using $P_\mathrm{rot}$ and $R_\mathrm{per}$ from McQuillan et al. (2014), effective temperature $T_\mathrm{eff}$ from LAMOST DR6, and parallax data from Gaia EDR3. As has been suggested in previous works, we find that $P_\mathrm{rot}$ scaled by the convective turnover time $τ_\mathrm{c}$, or the Rossby number $\mathrm{Ro}=P_\mathrm{rot}/τ_\mathrm{c}$, serves as a good predictor of $R_\mathrm{per}$: $R_\mathrm{per}$ plateaus around $1\%$ in relative flux for $0.2 \lesssim \mathrm{Ro}/\mathrm{Ro}_\odot \lesssim 0.4$, and decays steeply with increasing $\mathrm{Ro}$ for $0.4 \lesssim \mathrm{Ro}/\mathrm{Ro}_\odot \lesssim 0.8$, where $\mathrm{Ro}_\odot$ denotes $\mathrm{Ro}$ of the Sun. In the latter regime we find $\mathrm{d}\ln R_\mathrm{per}/\mathrm{d}\ln\mathrm{Ro} \sim -4.5$ to $-2.5$, although the value is sensitive to detection bias against weak modulation and may depend on other parameters including $T_\mathrm{eff}$ and surface metallicity. The existing X-ray and Ca II H&K flux data also show transitions at $\mathrm{Ro}/\mathrm{Ro}_\odot\sim 0.4$, suggesting that all these transitions share the same physical origin. We also find that the rapid decrease of $R_\mathrm{per}$ with increasing $\mathrm{Ro}$ causes rotational modulation of fainter Kepler stars with $\mathrm{Ro}/\mathrm{Ro}_\odot \gtrsim 0.6$ to be buried under the photometric noise. This effect sets the longest $P_\mathrm{rot}$ detected in the McQuillan et al. (2014) sample as a function of $T_\mathrm{eff}$, and obscures the signature of stalled spin down that has been proposed to set in around $\mathrm{Ro}/\mathrm{Ro}_\odot \sim 1$.
