We show that
slow rotators develop a high degree of differential rotation between the radiative core and the convective envelope, while fast rotators evolve with little core - envelope decoupling.
We conclude that lithium - depleted exoplanet host stars were
slow rotators on the zero - age main sequence (ZAMS) and argue that slow rotation results from a long lasting star - disk interaction during the PMS.
We suggest that strong differential rotation at the base of the convective envelope is responsible for enhanced lithium depletion in
slow rotators.
And there are many hypervelocity impactors straying out there and looking for targets to hit — be it a fast or
slow rotator,» Drahus said.
Not exact matches
We have developed rotational evolution models for
slow, median and fast
rotators with initial periods of 10, 7, and 1.4 d, respectively.
We find the model parameters accounting for the
slow and median
rotators are very similar to each other, with a disk lifetime of 5 Myr and a core - envelope coupling timescale of 28 - 30 Myr.