CKS IX: Revisiting the Minimum-Mass Extrasolar Nebula with Precise Stellar Parameters

Abstract

We investigate a possible correlation between the solid surface density $\Sigma$ of the minimum-mass extrasolar nebulae (MMEN) and the host star mass $M_{\star }$ and metallicity [Fe/H]. Leveraging on the precise host star properties from the California-{\it Kepler}-Survey (CKS), we found that $\Sigma =$ 50^{+33}_{-20} \rm{~g~cm}^{-2} $(a/1AU{)}^{-1.75\pm 0.07}$ $(M_{\star }/M_{\odot }{)}^{1.04\pm 0.22}$ $10^{0.22\pm 0.05[Fe/H]}$ for {\it Kepler}-like systems (1-4$R_{\oplus }$; $a<$1AU). The strong $M_{\star }$ dependence is reminiscent of previous dust continuum results that the solid disk mass scales with $M_{\star }$. The weaker [Fe/H] dependence shows that sub-Neptune planets, unlike giant planets, form readily in lower-metallicity environment. The innermost region ($a<$ 0.1AU) of a MMEN maintains a smooth profile despite a steep decline of planet occurrence rate: a result that favors the truncation of disks by co-rotating magnetospheres with a range of rotation periods, rather than the sublimation of dusts. The $\Sigma$ of {\it Kepler} multi-transiting systems shows a much stronger correlation with $M_{\star }$ and [Fe/H] than singles. This suggests that the dynamically hot evolution that produced single systems also partially removed the memory of formation in disks. Radial-velocity planets yielded a MMEN very similar to CKS planets; transit-timing-variation planets' postulated convergent migration history is supported by their poorly constrained MMEN. We found that lower-mass stars have a higher efficiency of forming/retaining planets: for sun-like stars about 20\% of the solid mass within $\sim$1AU are converted/preserved as sub-Neptunes, compared to 70\% for late-K-early-M stars. This may be due to the lower binary fraction, lower giant-planet occurrence or the longer disk lifetime of lower-mass stars.

Accepted to AAS Journals

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