Abstract
Abstract
A thin dust shell contracting from infinity to near its gravitational radius r
+, in a spacetime AdS
3 is analyzed; its equation of motion is determined and the solution R(t) as seen by a FIDO observer is estimated. It is concluded that this Shell's exterior looks like a BTZ black hole with similar properties. Based on the Thermo Field Dynamics technique, a scalar field Φ in the proximity of a non-rotating BTZ (2 + 1) black hole is studied. From the corresponding Killing-Boulware
0
KB
*
and Hartle-Hawking
0
HH
*
vacuum states, the associated Wightman function
W
x
,
x
′
HH
*
−
W
x
,
x
′
KB
*
is determined and based on it, the time component of the momentum-energy tensor of the system
∂
0
∂
0
′
W
HH
*
−
W
KB
*
(
x
,
x
′
)
≈
T
00
(
x
,
x
′
)
=
σ
(
r
)
is calculated. Which allows establishing the origin and location of the degrees of freedom responsible for the entropy that describes a source for the Bekenstein-Hawking S
BH
entropy. The thermal environment described by this model manifests itself with a well-defined and concentrated energy density near the event horizon, according to a FIDO observer.