The rubble pile spin barrier is an upper limit on the rotation rate of
asteroids larger than \~200-300 m. Among thousands of asteroids with diameters
larger than \~300 m, only a handful of asteroids are known to rotate faster than
2.0 h, all are in the sub-km range (<=0.6 km). Here we present photometric
measurements suggesting that (60716) 2000 GD65, an S-complex, inner-main belt
asteroid with a relatively large diameter of 2.3 +0.6-0.7 km, completes one
rotation in 1.9529+-0.0002 h. Its unique diameter and rotation period allow us
to examine scenarios about asteroid internal structure and evolution: a rubble
pile bound only by gravity; a rubble-pile with strong cohesion; a monolithic
structure; an asteroid experiencing mass shedding; an asteroid experiencing
YORP spin-up/down; and an asteroid with a unique octahedron shape results with
a four-peak lightcurve and a 3.9 h period. We find that the most likely
scenario includes a lunar-like cohesion that can prevent (60716) 2000 GD65 from
disrupting without requiring a monolithic structure or a unique shape. Due to
the uniqueness of (60716) 2000 GD65, we suggest that most asteroids typically
have smaller cohesion than that of lunar regolith.
%0 Generic
%1 citeulike:13893598
%A Polishook, D.
%A Moskovitz, N.
%A Binzel, R. P.
%A Burt, B.
%A DeMeo, F. E.
%A Hinkle, M. L.
%A Lockhart, M.
%A Mommert, M.
%A Person, M.
%A Thirouin, A.
%A Thomas, C. A.
%A Trilling, D.
%A Willman, M.
%A Aharonson, O.
%D 2015
%K imported
%T A 2 km-size asteroid challenging the rubble-pile spin barrier - a case for cohesion
%U http://arxiv.org/abs/1512.07088
%X The rubble pile spin barrier is an upper limit on the rotation rate of
asteroids larger than \~200-300 m. Among thousands of asteroids with diameters
larger than \~300 m, only a handful of asteroids are known to rotate faster than
2.0 h, all are in the sub-km range (<=0.6 km). Here we present photometric
measurements suggesting that (60716) 2000 GD65, an S-complex, inner-main belt
asteroid with a relatively large diameter of 2.3 +0.6-0.7 km, completes one
rotation in 1.9529+-0.0002 h. Its unique diameter and rotation period allow us
to examine scenarios about asteroid internal structure and evolution: a rubble
pile bound only by gravity; a rubble-pile with strong cohesion; a monolithic
structure; an asteroid experiencing mass shedding; an asteroid experiencing
YORP spin-up/down; and an asteroid with a unique octahedron shape results with
a four-peak lightcurve and a 3.9 h period. We find that the most likely
scenario includes a lunar-like cohesion that can prevent (60716) 2000 GD65 from
disrupting without requiring a monolithic structure or a unique shape. Due to
the uniqueness of (60716) 2000 GD65, we suggest that most asteroids typically
have smaller cohesion than that of lunar regolith.
@misc{citeulike:13893598,
abstract = {{The rubble pile spin barrier is an upper limit on the rotation rate of
asteroids larger than \~{}200-300 m. Among thousands of asteroids with diameters
larger than \~{}300 m, only a handful of asteroids are known to rotate faster than
2.0 h, all are in the sub-km range (\<=0.6 km). Here we present photometric
measurements suggesting that (60716) 2000 GD65, an S-complex, inner-main belt
asteroid with a relatively large diameter of 2.3 +0.6-0.7 km, completes one
rotation in 1.9529+-0.0002 h. Its unique diameter and rotation period allow us
to examine scenarios about asteroid internal structure and evolution: a rubble
pile bound only by gravity; a rubble-pile with strong cohesion; a monolithic
structure; an asteroid experiencing mass shedding; an asteroid experiencing
YORP spin-up/down; and an asteroid with a unique octahedron shape results with
a four-peak lightcurve and a 3.9 h period. We find that the most likely
scenario includes a lunar-like cohesion that can prevent (60716) 2000 GD65 from
disrupting without requiring a monolithic structure or a unique shape. Due to
the uniqueness of (60716) 2000 GD65, we suggest that most asteroids typically
have smaller cohesion than that of lunar regolith.}},
added-at = {2019-03-25T08:20:55.000+0100},
archiveprefix = {arXiv},
author = {Polishook, D. and Moskovitz, N. and Binzel, R. P. and Burt, B. and DeMeo, F. E. and Hinkle, M. L. and Lockhart, M. and Mommert, M. and Person, M. and Thirouin, A. and Thomas, C. A. and Trilling, D. and Willman, M. and Aharonson, O.},
biburl = {https://www.bibsonomy.org/bibtex/2991b155832a6a8afde764f2e094699ab/ericblackman},
citeulike-article-id = {13893598},
citeulike-linkout-0 = {http://arxiv.org/abs/1512.07088},
citeulike-linkout-1 = {http://arxiv.org/pdf/1512.07088},
day = 22,
eprint = {1512.07088},
interhash = {1c0ccd2779323f09218840b5d5574768},
intrahash = {991b155832a6a8afde764f2e094699ab},
keywords = {imported},
month = dec,
posted-at = {2015-12-24 20:39:34},
priority = {2},
timestamp = {2019-03-25T08:20:55.000+0100},
title = {{A 2 km-size asteroid challenging the rubble-pile spin barrier - a case for cohesion}},
url = {http://arxiv.org/abs/1512.07088},
year = 2015
}