No Sub-Saturn Mass Planet Desert in the CORALIE/HARPS Radial Velocity Sample. (arXiv:2104.05713v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bennett_D/0/1/0/all/0/1">David P. Bennett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ranc_C/0/1/0/all/0/1">Clément Ranc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandes_R/0/1/0/all/0/1">Rachel B. Fernandes</a>
We analyze the CORALIE/HARPS sample of exoplanets (Mayor et al. 2011) found
by the Doppler radial velocity method for signs of the predicted “desert” at
10-$100 M_odot$ caused by runaway gas accretion at semimajor axes of $<
3,$AU. We find that these data are not consistent with this prediction. This
result is similar to the finding by the MOA gravitational microlensing survey
that found no desert in the exoplanet distribution for exoplanets in slightly
longer period orbits and somewhat lower host masses (Suzuki et al. 2018).
Together, these results imply that the runaway accretion scenario of the core
accretion theory does not have a large influence on the final mass and
semimajor axis distribution of exoplanets.
We analyze the CORALIE/HARPS sample of exoplanets (Mayor et al. 2011) found
by the Doppler radial velocity method for signs of the predicted “desert” at
10-$100 M_odot$ caused by runaway gas accretion at semimajor axes of $<
3,$AU. We find that these data are not consistent with this prediction. This
result is similar to the finding by the MOA gravitational microlensing survey
that found no desert in the exoplanet distribution for exoplanets in slightly
longer period orbits and somewhat lower host masses (Suzuki et al. 2018).
Together, these results imply that the runaway accretion scenario of the core
accretion theory does not have a large influence on the final mass and
semimajor axis distribution of exoplanets.
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