论文标题
重新分析K2-106b的组成：超短期的超级候选者
A Reanalysis of the Composition of K2-106b: an Ultra-short Period Super-Mercury Candidate
论文作者
论文摘要
我们介绍了K2-106过境行星系统的重新分析，重点是K2-106b的组成，即超短时期，超级候选者。我们在全球范围内模拟现有的光度和径向速度数据，并得出K2-106b的行星质量和半径为$ m_ {p} = 8.53 \ pm1.02〜m _ {\ oplus} $和$ r_ {p}导致$ρ_{p} = 9.4^{+1.6} _ { - 1.5} $ $ $ \ rm g〜cm^{ - 3} $的密度，其值明显低于文献中报道的值。我们使用行星内部模型，假设由液体，纯Fe芯和无铁组成的两层行星，$ \ rm mgsio_ {3} $ santle，我们确定与观察到的质量和半径一致的核心质量分数范围。我们使用宿主星的现有高分辨率光谱来得出Fe/mg/si丰度（[[fe/h] $ = -0.03 \ pm 0.01 $，[mg/h] $ = 0.04 \ pm 0.02 $，[si/h] $ = 0.03 $ = 0.03 \ pm 0.06 $）来推断k2-106b的组成。我们发现，尽管与地球相比，K2-106b具有高密度和核心质量分数（$ 44^{+12} _ { - 15} \％$）（$ 33 \％$），但其组成与预期的是它反映其宿主星的相对耐磨丰度的预期。因此，正如先前文献所建议的那样，K2-106b不太可能成为超级储备。
We present a reanalysis of the K2-106 transiting planetary system, with a focus on the composition of K2-106b, an ultra-short period, super-Mercury candidate. We globally model existing photometric and radial velocity data and derive a planetary mass and radius for K2-106b of $M_{p} = 8.53\pm1.02~M_{\oplus}$ and $R_{p} = 1.71^{+0.069}_{-0.057}~R_{\oplus}$, which leads to a density of $ρ_{p} = 9.4^{+1.6}_{-1.5}$ $\rm g~cm^{-3}$, a significantly lower value than previously reported in the literature. We use planet interior models that assume a two-layer planet comprised of a liquid, pure Fe core and iron-free, $\rm MgSiO_{3}$ mantle, and we determine the range of core mass fractions that are consistent with the observed mass and radius. We use existing high-resolution spectra of the host star to derive Fe/Mg/Si abundances ([Fe/H]$=-0.03 \pm 0.01$, [Mg/H]$= 0.04 \pm 0.02$, [Si/H]$=0.03 \pm 0.06$) to infer the composition of K2-106b. We find that although K2-106b has a high density and core mass fraction ($44^{+12}_{-15}\%$) compared to the Earth ($33\%$), its composition is consistent with what is expected assuming that it reflects the relative refractory abundances of its host star. K2-106b is therefore unlikely to be a super-Mercury, as has been suggested in previous literature.
