  Tidal dissipation in a celestial body can be used to probe its internal
structure. Tides govern the orbital evolution of binary systems and therefore
constraints on the interior of binary system members can be derived by knowing
the age and tidal state of the binary system. For asteroids, age estimates are
challenging due to a lack of direct observation of their surface. However, the
age of asteroid pairs formed by rotational fission of a parent body can be
derived from dynamical modeling, and as such can be used to constrain the age
of binary systems existing within asteroid pairs.We study 13 binary asteroid
systems existing in asteroid pairs by modeling their tidal locking and
eccentricity damping timescales from tidal dissipation in the primaries and
secondaries. We consider the impact of thermal torques on these timescales from
the YORP and BYORP effects. The resulting constraints on the tidal dissipation
ratio Q/k2 are compared to monolithic and rubble pile asteroid theories,
showing that all secondaries are consistent with rubble piles with regolith
layers greater than 3m and suggest that Q/k2 for rubble piles increases with
radius. A particular case is the first bound secondary of asteroid (3749)
Balam, whose Q/k2 is constrained to be between 2.7x10^4 and 1.4x10^6,
consistent with a rubble-pile with a regolith thickness between 30m and 100m.
