Ann.
Acad.
Rom.
Sci.
Ser.
Math.
Appl.
ISSN
2066-6594
Vol.
18,
No.
3/2026
DYNAMICS
OF
QUANTUM
ENTANGLEMENT
IN
RELATIVISTIC
OPEN
SYSTEMS
∗
M˘
ad˘
alin
Calamanciuc
†
Aurelian
Isar
‡
Dedicated
to
the
memory
of
Professor
Mihail
Megan
DOI
10.56082/annalsarscimath.2026.3.205
Abstract
We
review
the
results
obtained
by
investigating,
in
the
framework
of
the
theory
of
open
systems
based
on
completely
positive
quantum
dynamical
semigroups,
the
time
evolution
of
quantum
entanglement
of
two
different
bimodal
systems,
each
one
interacting
with
a
thermal
environment.
The
first
system
is
formed
of
the
free
massless
bosonic
mode
of
a
stationary
observer
in
a
region
that
is
asymptotically
flat
(Kruskal
observer)
or
freely
falling
in
Schwarzschild
black
hole,
and
the
mode
of
a
uniformly
accelerated
observer
hovering
outside
the
event
horizon
of
black
hole.
For
initial
bimodal
Gaussian
squeezed
thermal
states
of
the
system,
we
show
that
under
the
influence
of
Hawking
ra-
diation
the
quantum
entanglement
of
the
two
modes
is
destroyed
in
a
finite
time,
for
non-zero
values
of
the
temperature
of
the
thermal
en-
vironment,
i.e.
the
phenomenon
of
entanglement
sudden
death
takes
place.
The
second
system
consists
of
two
bosonic
modes
associated
with
a
scalar
quantum
field
in
de
Sitter
space,
characterized
by
two
re-
gions
that
are
causally
disconnected
and
described
using
open
universe
coordinates
on
two
open
charts.
The
survival
time
of
the
entanglement
of
this
bimodal
system
strongly
depends
on
the
competition
between
the
contrary
effects
provided
by
the
squeezing
of
the
initial
bimodal
state,
the
curvature
of
de
Sitter
space,
the
mass
parameter
and
the
∗
Accepted
for
publication
on
July
30,
2026
†
calamanciuc.madalin@theory.nipne.ro
,
Faculty
of
Physics,
University
of
Bucharest;
National
Institute
of
Physics
and
Nuclear
Engineering,
Magurele,
Romania
‡
isar@theory.nipne.ro
,
Faculty
of
Physics,
University
of
Bucharest;
National
Insti-
tute
of
Physics
and
Nuclear
Engineering,
Magurele,
Romania;
Academy
of
Romanian
Scientists
205
On
quantum
entanglement
206
thermal
environment.
It
is
shown
that
the
entanglement
is
minimized
for
values
1/2
and
3/2
of
the
mass
parameter,
corresponding
to
the
conformally
coupled
scalar
field
and,
respectively,
minimally
coupled
massless
field.
Keywords:
quantum
entanglement,
Schwarzschild
black
hole,
de
Sitter
space,
Gaussian
states,
open
systems.
MSC:
81P42,
81V73,
81T20.
1
Introduction
Entanglement
is
a
quantum
correlation
of
major
importance
in
the
theory
of
quantum
information,
being
a
fundamental
resource
for
tasks
of
quan-
tum
information
processing
and
communications,
like
quantum
teleporta-
tion,
quantum
computing,
quantum
cryptography
[
22
].
The
research
on
quantum
correlations
has
traditionally
focused
on
continuous
variable
sys-
tems
within
inertial
frames
of
reference.
However,
the
realistic
quantum
systems
are
essentially
non-inertial
and
they
manifest
relativistic
and
grav-
itational
characteristics,
therefore
relativistic
quantum
investigations
are
of
basic
importance,
both
for
applications
in
quantum
information
proto-
cols
[
3
,
5
,
16
,
20
,
23
,
29
],
and
for
understanding
better
the
features
of
the
uni-
verse.
In
recent
years,
extensive
studies
on
quantum
correlations
in
various
scenarios,
such
as
non-inertial
frames,
curved
spacetime,
and
an
expanding
universe
have
been
performed
[
4
,
6
,
9
,
13
,
24
,
30
].
In
the
present
work
we
review
the
results
obtained
in
Refs.
[
11
,
12
]
by
investigating,
in
the
framework
of
the
theory
of
open
systems
based
on
completely
positive
quantum
dynamical
semigroups,
the
time
evolution
of
quantum
entanglement
of
two
different
bimodal
systems,
each
one
inter-
acting
with
a
thermal
environment.
The
first
system
is
formed
of
the
free
massless
bosonic
mode
of
a
stationary
observer
in
a
region
that
is
asymptoti-
cally
flat
(Kruskal
observer)
or
freely
falling
in
Schwarzschild
black
hole
[
13
],
and
the
mode
of
a
uniformly
accelerated
observer
hovering
outside
the
event
horizon
of
black
hole.
For
initial
bimodal
Gaussian
squeezed
thermal
states
of
the
system,
we
show
that
under
the
influence
of
Hawking
radiation
the
quantum
entanglement
of
the
two
modes
is
destroyed
in
a
finite
time,
for
non-zero
values
of
the
temperature
of
the
thermal
environment,
i.e.
the
phenomenon
of
entanglement
sudden
death
takes
place.
For
a
zero
temper-
ature
of
the
thermal
bath
the
initial
existing
entanglement
is
decreasing
over
time,
but
it
keeps
for
all
finite
times
a
non-zero
value,
and
the
logarithmic
negativity
tends
to
zero
only
in
the
limit
of
infinite
time.
The
second
sys-
M.
Calamanciuc,
A.
Isar
207
tem
consists
of
two
bosonic
modes
associated
with
a
scalar
quantum
field
in
de
Sitter
space,
characterized
by
two
regions
that
are
causally
disconnected
and
described
using
open
universe
coordinates
on
two
open
charts
[
21
,
26
].
The
positive
frequency
mode
functions
of
a
free
scalar
field
correspond
to
the
Bunch-Davies
vacuum
[
10
],
also
known
as
the
Euclidean
vacuum,
which
has
support
on
both
regions.
The
survival
time
of
the
entanglement
of
this
bimodal
system
strongly
depends
on
the
competition
between
the
contrary
effects
provided
by
the
squeezing
of
the
initial
bimodal
state,
the
curvature
of
de
Sitter
space,
the
mass
parameter
and
the
thermal
environment.
It
is
shown
that
the
entanglement
is
minimized
for
values
1/2
and
3/2
of
the
mass
parameter,
corresponding
to
the
conformally
coupled
scalar
field
and,
respectively,
minimally
coupled
massless
field.
The
work
is
structured
in
the
following
way.
In
Sec.
2
it
is
described
the
dynamics
of
the
scalar
field
for
massless
modes.
There
are
quantized
the
fields
in
the
region
of
the
event
horizon
of
Schwarzschild
black
hole
and
it
is
shown
that
Unruh-Hawking
effect
is
described
by
a
Gaussian
bosonic
amplification
channel
acting
on
a
bipartite
system
[
3
,
7
].
We
also
introduce
the
formalism
for
describing
the
curvature
effects
associated
with
de
Sitter
space.
In
Sec.
3
we
present
the
framework
of
the
theory
of
open
quantum
systems
and
introduce
the
logarithmic
negativity
as
a
measure
of
quantum
entanglement,
by
using
the
symplectic
formalism.
Then
we
analyze
the
time
evolution
of
the
entanglement
of
the
systems
under
scrutiny,
in
interaction
with
the
thermal
environment.
In
Sec.
5
we
give
a
summary
and
the
con-
clusions.
2
Dynamics
of
the
quantum
scalar
field
2.1
Schwarzschild
event
horizon
The
radiation
produced
by
the
black
hole
through
the
Unruh-Hawking
effect
can
be
formulated
in
terms
of
an
amplification
Gaussian
bosonic
channel
[
7
,
27
].
We
take
a
metric
characterizing
the
background
of
the
spacetime
in
the
region
of
an
asymptotically
flat
and
static
Schwarzschild
black
hole
of
the
form
(we
set
the
natural
units
(
=
G
=
c
=
k
B
=
1):
ds
2
=
−
1
−
2
M
r
dt
2
+
1
−
2
M
r
−
1
dr
2
+
r
2
dθ
2
+
sin
2
θdϕ
2
,
(1)
where
r
is
the
radial
coordinate,
t
denotes
the
time,
angles
(
θ,
ϕ
)
define
the
metric
on
the
two-sphere
and
M
denotes
the
black
hole
mass.
On
quantum
entanglement
208
The
massless
bosonic
field
φ
satisfies
in
the
background
of
the
black
hole
the
following
Klein-Gordon
equation
[
8
]:
1
√
−
g
∂
∂x
µ
√
−
gg
µν
∂φ
∂x
ν
=
0
,
(2)
where
x
µ
=
(
t,
r,
θ,
ϕ
)
denotes
the
general
coordinate
and
g
=
det
g
µν
.
We
consider
a
bipartite
system,
with
a
stationary
observer
in
asymptot-
ically
flat
region
and
a
Schwarzschild
observer
who
hovers
uniformly
accel-
erated
near
the
event
horizon
of
the
black
hole.
The
Unruh
vacuum
state
in
single-mode
approximation,
when
only
bosons
exist
outside
the
event
hori-
zon
(only
particles
can
be
detected
as
Hawking
radiation)
and
antibosons
are
living
inside
event
horizon,
reduces
to
a
two-mode
squeezing
state
|
0
Ω
>
H
=
1
cosh
r
Ω
∞
n
=0
(tanh
r
Ω
)
n
|
n
>
out
|
n
>
in
,
(3)
where
|
n
>
out
and
|
n
>
in
denote
the
bosonic
and
antibosonic
states,
outside
and
inside
of
the
event
horizon.
Here
sinh
r
Ω
=
e
Ω
T
H
−
1
−
1
2
and
T
H
denotes
the
Hawking
temperature.
Hawking
temperature
parameter
r
Ω
is
a
function
that
monotonically
increases
with
T
H
.
The
expression
in
Eq.
(
3
)
can
be
written
as
the
action
of
a
bimodal
squeezing
operator
on
associated
vacuum
states
|
n
>
in
and
|
n
>
out
,
inside
and
outside
regions
of
event
horizon,
therefore,
from
Eq.
(
3
)
it
follows
that
the
Unruh-Hawking
radiation
can
be
expressed
as
an
amplification
bosonic
channel
[
15
,
30
,
31
].
The
Gaussian
operation
expressed
by
this
squeezing
operator
and
preserving
the
Gaussianity
of
the
input
states
has
the
following
symplectic
phase-space
representation
(we
abbreviate
r
Ω
≡
r
for
simplicity):
S
(
r
)
=
cosh
r
0
sinh
r
0
0
cosh
r
0
−
sinh
r
sinh
r
0
cosh
r
0
0
−
sinh
r
0
cosh
r
.
(4)
We
consider
that
the
scalar
massless
field
φ
has
two
Unruh
modes
A
and
B
,
which
share
in
the
inertial
frame
a
bimodal
Gaussian
state
ρ
AB
.
We
denote
by
R
=
{
x,
p
x
,
y,
p
y
}
T
the
operators
of
canonical
quadratures
of
two
bosonic
modes
and
by
σ
AB
the
two-mode
covariance
matrix,
whose
elements
are
given
by
the
statistical
moments
of
second
order
of
quadrature
operators,
which
completely
characterize
the
two-mode
Gaussian
states:
σ
ij
=
Tr[(
R
i
R
j
+
R
j
R
i
)
ρ
AB
]
,
i,
j
=
1
,
.
.
.
,
4
.
(5)
M.
Calamanciuc,
A.
Isar
209
We
neglect
the
moments
of
the
first
order,
since
they
can
be
made
zero
by
performing
local
displacements
in
the
phase
space.
The
covariance
matrix
fulfills
the
uncertainty
relation
σ
AB
+iΩ
AB
≥
0,
where
Ω
AB
=
⊕
2
1
0
1
−
1
0
is
the
symplectic
form.
The
previously
introduced
amplification
channel
is
expressed
by
the
bi-
modal
squeezing
operation
associated
with
symplectic
transformation
(
4
).
The
amplification
maps
the
mode
B
of
the
Schwarzschild
observer
into
the
modes
B
and
¯
B
situated
outside
and
inside
of
event
horizon,
respectively.
Therefore,
from
inertial
point
of
view
the
considered
system
has
two
par-
ties,
while,
from
the
point
of
view
of
a
Schwarzschild
observer,
becomes
relevant
an
additional
mode
¯
B
.
Consequently,
the
initial
bipartite
state
is
transformed
into
a
three-partite
state,
with
the
mode
A
of
the
stationary
ob-
server
in
asymptotically
flat
region,
mode
B
of
the
Schwarzschild
observer,
and
mode
¯
B
of
a
hypothetical
observer,
situated
inside
event
horizon
of
Scharzschild
black
hole.
Then
the
three-mode
system
can
be
described
by
the
following
covariance
matrix
[
3
]:
σ
AB
¯
B
(
s,
r
)
=
I
A
⊕
S
B,
¯
B
(
r
)
σ
0
AB
(
s
)
⊕
I
¯
B
I
A
⊕
S
B,
¯
B
(
r
)
T
.
(6)
We
denote
by
σ
0
AB
(
s
)
the
covariance
matrix
of
the
bimodal
Gaussian
thermal
squeezed
state
of
bosonic
fields:
σ
0
AB
(
s
)
=
a
0
0
c
0
0
0
a
0
0
−
c
0
c
0
0
b
0
0
0
−
c
0
0
b
0
,
(7)
where
a
0
=
2
n
1
cosh
2
s
+
2
n
2
sinh
2
s
+
cosh
2
s,
b
0
=
2
n
2
cosh
2
s
+
2
n
1
sinh
2
s
+
cosh
2
s,
c
0
=
(
n
1
+
n
2
+
1)
sinh
2
s.
(8)
Here
s
denotes
the
squeezing
parameter
of
the
state
and
n
1
,
n
2
denote
the
associated
average
thermal
photon
numbers.
The
covariance
matrix
for
the
outside
region
can
be
obtained
by
per-
forming
trace
over
mode
¯
B
situated
inside
black
hole,
associated
with
the
hypothetical
observer.
Then
we
obtain
from
Eq.
(
6
)
the
following
covariance
matrix
of
modes
A
and
B
[
3
]:
σ
AB
(
s,
r
)
=
A
C
C
T
B
,
(9)
On
quantum
entanglement
210
where:
A
=
a
0
I,
B
=
b
0
cosh
2
r
+
sinh
2
r
I,
C
=
c
0
cosh
rZ,
(10)
I
is
the
identity
matrix
and
Z
is
Z
-Pauli
matrix.
2.2
Euclidean
de
Sitter
space
The
4D
Euclidean
de
Sitter
space
can
be
embedded
in
the
5D
Euclidean
space.
Therefore,
the
open
charts
in
de
Sitter
space,
defined
by
the
Hubble
radius
H
−
1
,
have
coordinate
frames
that
can
be
derived
through
analytic
continuation
of
the
Euclidean
metric.
These
frames
can
be
separated
into
three
regions
(R,C,L),
each
one
with
its
own
individual
metric:
ds
2
R
=
H
−
2
−
dt
2
R
+
sinh
2
t
R
dr
2
R
+
sinh
2
r
R
d
Ω
2

,
ds
2
C
=
H
−
2
dt
2
C
+
cos
2
t
C
−
dr
2
C
+
cosh
2
r
C
d
Ω
2

,
ds
2
L
=
H
−
2
−
dt
2
L
+
sinh
2
t
L
dr
2
L
+
sinh
2
r
L
d
Ω
2

,
(11)
where
d
Ω
2
is
the
metric
on
the
two-sphere.
The
regions
R
and
L
,
described
by
the
coordinates
(
t
R
,
r
R
)
and
(
t
L
,
r
L
),
respectively,
are
causally
discon-
nected.
The
region
C
is
described
by
the
coordinates
(
r
C
,
t
C
).
The
Bunch-Davies
vacuum
[
10
]
for
a
global
observer
in
de
Sitter
space
connects
R
vacuum
and
L
vacuum
through
the
Bogoliubov
transformation
and
can
be
expressed
as
a
two-mode
squeezed
state
of
the
R
and
L
vacua
in
the
Fock
space:
|
0
BD
=
U
R,L
(
γ
p
)
|
0
R
|
0
L
=
1
−
|
γ
p
|
2
∞
n
=0
γ
n
p
|
n
R
|
n
L
,
(12)
where
U
R,L
(
γ
p
)
is
the
two-mode
squeezing
operator
corresponding
to
a
Gaussian
channel
and
the
squeezing
parameter
is
given
by
γ
p
=
i
√
2
√
cosh
2
πp
+
cos
2
πν
+
√
cosh
2
πp
+
cos
2
πν
+
2
.
(13)
Here
ν
is
the
mass
parameter
(
m
is
the
mass
of
the
scalar
field):
ν
=
9
4
−
m
2
H
2
.
(14)
For
ν
=
1
/
2
and
ν
=
3
/
2
this
parameter
simplifies
to
|
γ
p
|
=
e
−
πp
,
which
tends
to
1
in
the
limit
of
small
p
(large
curvature)
and
takes
small
values
in
M.
Calamanciuc,
A.
Isar
211
the
limit
of
large
p
.
The
value
ν
=
1
/
2
corresponds
to
the
conformal
coupled
scalar
field
and
ν
=
3
/
2
to
the
minimally
coupled
massless
scalar
field.
The
parameter
p
is
normalized
by
H
and
it
represents
the
curvature
parameter
of
de
Sitter
space,
namely
the
effect
of
the
curvature
of
the
3D
hyperbolic
space
appears
when
p
approaches
to
1,
and
gets
stronger
by
decreasing
p
,
so
that
the
limit
of
infinite
curvature
is
reached
for
p
→
0.
The
Bunch-Davies
vacuum
observed
by
the
global
observer
of
the
mode
A
can
be
expressed
as
a
two-mode
squeezed
state
of
the
R
vacuum
observed
by
the
observer
of
the
mode
B
and
the
L
vacuum
observed
by
the
observer
of
the
mode
¯
B
.
The
squeezing
operator
U
R,L
(
γ
p
)
is
a
Gaussian
operation
that
preserves
the
Gaussianity
of
the
state,
and
in
the
phase
space
it
is
represented
by
the
following
curvature-induced
symplectic
operator
acting
on
the
modes
B
and
¯
B
:
S
B,
¯
B
(
γ
p
)
=
1
1
−
|
γ
p
|
2
I
|
γ
p
|
Z
|
γ
p
|
Z
I
,
(15)
with
I
being
the
unity
matrix
in
2
×
2
space
and
Z
the
Z
-Pauli
matrix.
Therefore,
under
the
transformation
(
15
)
the
single
mode
B
is
converted
to
two
modes
in
two
open
charts.
We
consider
an
initial
entangled
Gaussian
two-mode
squeezed
vacuum
state
of
the
free
scalar
field
shared
by
the
modes
A
and
B
.
In
the
Bunch-
Davies
vacuum,
this
state,
with
the
squeezing
parameter
s
,
is
described
by
the
following
covariance
matrix:
σ
0
AB
(
s
)
=
cosh
2
s
I
sinh
2
s
Z
sinh
2
s
Z
cosh
2
s
I
.
(16)
Considering
that
there
are
no
initial
correlations
between
the
state
de-
scribed
by
the
covariance
matrix
(
16
)
and
the
subsystem
observed
by
¯
B
,
the
initial
covariance
matrix
of
the
entire
system
is
σ
0
AB
(
s
)
⊕
I
¯
B
.
Consequently,
a
full
description
of
the
system
involves
three
modes:
the
mode
A
observed
by
a
global
observer,
the
mode
B
observed
by
observer
in
the
region
of
open
charts
R
and
the
mode
¯
B
observed
in
the
region
L
of
open
charts.
The
covariance
matrix
of
the
three-mode
Gaussian
state
describing
the
complete
system
has
the
following
form
[
3
]:
σ
AB
¯
B
(
s,
γ
p
)
=
I
A
⊕
S
B,
¯
B
(
γ
p
)
σ
0
AB
(
s
)
⊕
I
¯
B
I
A
⊕
S
B,
¯
B
(
γ
p
)
T
.
(17)
Since
an
observer
living
in
region
L
is
causally
disconnected
from
region
R
,
the
physically
accessible
information
is
encoded
in
the
mode
A
and
the
On
quantum
entanglement
212
mode
B
.
By
performing
partial
trace
over
¯
B
in
the
tripartite
covariance
matrix
(
17
)
we
will
get
rid
of
the
mode
¯
B
,
obtaining
the
initial
covariance
matrix
for
the
modes
A
and
B
,
associated
with
region
R
:
σ
AB
(
s,
γ
p
)
=
A
C
C
T
B
,
(18)
with
A
=
cosh
2
s
I,
B
=
|
γ
p
|
2
+
cosh
2
s
1
−
|
γ
p
|
2
I,
C
=
sinh
2
s
1
−
|
γ
p
|
2
Z.
(19)
3
Time
evolution
of
quantum
entanglement
In
this
Section
we
will
investigate
the
time
evolution
of
the
entanglement
be-
tween
the
two
bosonic
modes
of
the
considered
systems,
each
one
immersed
in
its
common
thermal
bath.
To
study
the
dynamics
of
the
bimodal
sys-
tems
we
use
the
axiomatic
formalism
of
open
systems,
based
on
completely
positive
quantum
dynamical
semigroups.
In
this
framework
the
Markovian
irreversible
time
evolution
of
an
open
system
is
described
by
the
following
Gorini-Kossakowski-Sudarshan-Lindblad
master
equation
for
the
density
op-
erator
ρ
(
t
)
(we
set
=
1)
[
17
–
19
]
dρ
(
t
)
dt
=
−
i[
H
,
ρ
(
t
)]
+
1
2
k
2
L
k
ρ
(
t
)
L
†
k
−
ρ
(
t
)
,
L
†
k
L
k
+
,
(20)
where
H
=
1
2
(
x
2
+
p
2
x
+
y
2
+
p
2
y
)
(21)
is
the
Hamiltonian
of
the
two
bosonic
modes
(we
take
identical
frequencies
ω
=
1
for
the
two
modes)
and
the
operators
L
k
,
L
†
k
describe
the
interaction
of
the
system
with
a
general
environment.
If
the
initial
states
are
Gaussian
and
the
operators
L
k
are
chosen
poly-
nomials
of
first
degree
in
the
canonically
conjugated
quadrature
operators
x,
p
x
,
y,
p
y
of
the
two
bosonic
modes,
then,
due
to
the
linear
character
of
the
dynamics,
the
Gaussianity
is
preserved
in
time
[
14
,
28
].
M.
Calamanciuc,
A.
Isar
213
From
Eq.
(
20
)
it
is
obtained
that
the
time
evolution
of
the
corresponding
bimodal
covariance
matrix
σ
(
t
)
is
given
by
the
following
Lyapunov
equation
of
motion
[
25
]:
dσ
(
t
)
dt
=
Y
σ
(
t
)
+
σ
(
t
)
Y
T
+
2
D,
(22)
where
Y
=
−
λ
1
0
0
−
1
−
λ
0
0
0
0
−
λ
1
0
0
−
1
−
λ
(23)
is
the
drift
matrix,
λ
is
the
dissipation
rate,
and
we
assume
that
the
diffusion
matrix
D
has
the
form
[
25
]
D
=
diag
{
λ
coth
1
2
k
B
T
,
λ
coth
1
2
k
B
T
,
λ
coth
1
2
k
B
T
,
λ
coth
1
2
k
B
T
}
,
(24)
where
k
B
is
the
Boltzmann
constant
and
T
is
the
temperature
of
the
thermal
bath.
The
solution
of
Eq.
(
22
)
is
given
by
[
25
]:
σ
(
t
)
=
Γ(
t
)[
σ
AB
(
s
)
−
σ
T
]Γ
T
(
t
)
+
σ
T
,
(25)
where
σ
AB
(
s
)
is
the
initial
covariance
matrix
(
9
)
or
(
18
)
of
the
two
modes,
Γ(
t
)
=
exp(
Y
t
),
with
Γ(
t
)
→
0
when
t
→
∞
.
We
notice
that
the
evolution
generated
by
the
Gaussian
completely
positive
map
is
determined
by
two
4
x
4
real
matrices
Γ
and
A
=
σ
T
−
Γ
σ
T
Γ
T
,
which
satisfy
A
+iΩ
AB
≥
iΓΩ
AB
Γ
T
.
The
covariance
matrix
corresponding
to
the
asymptotic
Gibbs
state
of
the
system
of
two
bosonic
modes,
interacting
with
the
thermal
reservoir
of
temperature
T
,
is
given
by
(we
set
Boltzmann
constant
k
B
=
1):
σ
T
=
coth
1
2
T
0
0
0
0
coth
1
2
T
0
0
0
0
coth
1
2
T
0
0
0
0
coth
1
2
T
.
To
quantify
the
quantum
entanglement
we
choose
logarithmic
negativity
as
a
measure,
defined
in
terms
of
the
symplectic
invariants
of
the
covariance
matrix
σ
(
t
)
written
in
block
form
σ
(
t
)
=
A
(
t
)
C
(
t
)
C
T
(
t
)
B
(
t
)
,
(26)
On
quantum
entanglement
214
as
follows
[
1
,
2
]:
E
N
=
−
log
2
g
(
σ
(
t
))
,
(27)
g
(
σ
(
t
))
=
1
√
2
∆(
t
)
−
∆
2
(
t
)
−
4det
σ
(
t
)
,
(28)
where
we
introduced
the
seralian
∆(
t
)
≡
det
A
(
t
)
+
det
B
(
t
)
−
2det
C
(
t
)
.
(29)
For
E
N
≤
0
the
state
is
separable
and
E
N
>
0
determines
the
strength
of
the
entanglement.
3.1
Time
evolution
of
quantum
entanglement
in
Schwarzschild
background
To
describe
the
time
evolution
of
the
logarithmic
negativity
as
a
measure
of
the
Gaussian
quantum
entanglement
between
the
considered
observers,
we
suppose
that
they
share
initially
a
bimodal
symmetric
thermal
squeezed
state,
with
the
covariance
matrix
given
by
Eq.
(
7
)
in
which
we
denote
n
≡
n
1
=
n
2
=
1
.
From
Figs.
1
and
2
we
notice
that,
due
to
decoherence
and
dissipation
induced
by
the
environment,
the
entanglement
is
destroyed
in
a
finite
time
for
all
values
of
the
Hawking
parameter
r
,
squeezing
parameter
of
the
initial
bimodal
state
s
and
for
non-zero
values
of
the
temperature
T
of
the
thermal
environment.
We
witness
the
phenomenon
of
entanglement
sudden
death,
with
a
single
notable
exception.
Namely,
for
a
zero
temperature
of
the
ther-
mal
bath,
the
initial
existing
entanglement
is
decreasing
over
time,
but
it
keeps
for
all
finite
times
a
non-zero
value
and
the
logarithmic
negativity
asymptotically
tends
to
zero
only
in
the
limit
of
infinite
time.
In
Figs.
1
and
2
it
is
also
illustrated
that,
as
expected,
the
logarithmic
negativity
is
decreasing
by
increasing
the
temperature
of
the
environment
and
that
the
survival
time
of
the
entanglement
is
decreasing
by
increasing
the
temper-
ature
and
the
Hawking
parameter
r.
Conversely,
we
see
that
the
survival
time
of
the
entanglement
increases
with
the
squeezing
parameter
s.
We
can
also
see
that
the
logarithmic
negativity
decreases
by
increasing
the
Hawk-
ing
parameter
r
,
which
is
a
function
that
monotonically
increases
with
the
Hawking
temperature
T
H
,
so
that
for
a
relatively
large
values
of
the
Hawk-
ing
parameter
the
entanglement
is
destroyed.
It
is
also
illustrated
that
the
logarithmic
negativity
increases
with
the
squeezing
parameter
s
of
the
initial
state
[
11
].
M.
Calamanciuc,
A.
Isar
215
s
=
n
=
1,
r
=
0
.
2
,
λ
=
0
.
1
s
=
n
=
T
=
0
.
5
,
λ
=
0
.
1
Figure
1:
Logarithmic
negativity
E
N
versus
bath
temperature
T
and
time
t
(left),
and
versus
Hawking
parameter
r
and
time
t
(right).
r
=
n
=
1,
T
=
0
.
5
,
λ
=
0
.
1
s
=
n
=
t
=
1
,
λ
=
0
.
1
Figure
2:
Logarithmic
negativity
E
N
versus
squeezing
parameter
s
and
time
t
(left),
and
versus
bath
temperature
T
and
Hawking
parameter
r
at
a
given
moment
of
time
(right).
3.2
Time
evolution
of
quantum
entanglement
in
de
Sitter
space
The
time
evolution
of
Gaussian
quantum
entanglement
as
a
function
of
cur-
vature
parameter
p
is
plotted
in
Fig.
3,
for
a
given
value
of
the
mass
parame-
ter
ν
.
We
see
that
the
entanglement
increases
with
the
curvature
parameter
p
,
and,
due
to
the
interaction
with
the
thermal
bath,
the
entanglement
On
quantum
entanglement
216
vanishes
at
a
finite
moment
of
time.
The
survival
time
of
entanglement
in-
creases
by
increasing
the
curvature
parameter
p.
The
same
phenomenon
of
entanglement
sudden
death
can
be
observed
for
the
logarithmic
negativity
plotted
as
a
function
of
the
mass
parameter
ν
and
time,
for
a
fixed
value
of
the
curvature
parameter
p
.
We
notice
that
entanglement
has
an
oscillatory
behavior
with
respect
to
the
mass
parameter
ν
,
with
period
1,
which
comes
from
cos
2
πν
.
We
can
also
see
that
the
entanglement
is
minimized
when
ν
=
1
/
2
and
ν
=
3
/
2,
corresponding
to
the
conformal
coupled
scalar
field,
respectively
minimally
coupled
massless
field.
Therefore,
we
can
assert
that
a
massive
field
preserves
more
entanglement
than
a
massless
field,
i.e.
the
entanglement
of
a
massive
scalar
field
is
more
robust
than
that
of
a
massless
field
in
de
Sitter
space.
We
notice
that
the
entanglement
decreases
over
time
and
for
a
nonzero
time
the
entanglement
vanishes
for
definite
values
of
the
curvature
parameter
p
.
The
entanglement
can
survive
for
definite
values
of
times
and
in
the
presence
of
the
curvature
of
the
space,
even
in
the
limit
of
infinite
curvature
with
p
→
0
,
but
only
for
a
mass
parameter
of
a
scalar
field
other
than
ν
=
1
/
2
and
ν
=
3
/
2
.
In
Fig.
4
we
notice
that
the
amount
of
entanglement
decreases
as
T
is
increasing,
while
it
increases
with
p
and
there
is
a
critical
value
of
p
beyond
which
the
amount
of
entanglement
saturates.
At
a
given
moment
of
time
and
for
a
given
temperature
of
the
thermal
environment,
the
Gaussian
quantum
entanglement
can
survive
only
for
a
sufficiently
large
value
of
the
parameter
p,
that
is
for
a
sufficiently
small
curvature.
Entanglement
is
an
increasing
function
of
the
squeezing
s
and
the
curvature
parameter
p
[
12
].
T
=
0
.
3
,
ν
=
1
,
s
=
0
.
2
,
λ
=
0
.
2
T
=
0
.
3
,
p
=
0
.
1
,
s
=
0
.
2
,
λ
=
0
.
2
Figure
3:
Logarithmic
negativity
E
N
versus
curvature
parameter
p
and
time
t
(left),
and
versus
mass
parameter
ν
and
time
t
(right).
M.
Calamanciuc,
A.
Isar
217
t
=
0
.
1
,
ν
=
1
,
s
=
0
.
5
,
λ
=
0
.
2
t
=
0
.
1
,
T
=
0
.
3
,
ν
=
1
,
λ
=
0
.
2
Figure
4:
Logarithmic
negativity
E
N
versus
curvature
parameter
p
and
temperature
T
at
a
given
moment
of
time
(left),
and
versus
squeezing
s
and
curvature
parameter
p
at
a
given
moment
of
time
(right).
4
Summary
In
the
framework
of
the
theory
of
open
quantum
systems
we
investigated
the
evolution
of
Gaussian
quantum
entanglement,
quantified
by
the
logarithmic
negativity,
for
two
different
systems
in
interaction
with
a
thermal
reservoir:
-
two
bosonic
modes
of
a
massless
scalar
quantum
field
in
the
presence
of
a
Schwarzschild
black
hole,
under
the
influence
of
the
Hawking
effect;
-
two
bosonic
modes
of
a
massive
scalar
quantum
field
in
de
Sitter
space.
For
both
scenarios
of
the
considered
observers,
namely
a
Kruskal
observer
and
an
accelerated
observer
hovering
outside
the
event
horizon
of
black
hole
and,
respectively,
a
global
observer
situated
in
the
Bunch-Davies
vacuum
and
an
observer
who
stays
in
the
region
R
of
open
charts
of
de
Sitter
space,
we
have
obtained
the
following
results:
-
due
to
decoherence
and
dissipation
induced
by
the
thermal
environ-
ment,
for
non-zero
values
of
the
temperature,
the
initially
existing
quantum
entanglement
decreases
over
time
and
is
destroyed
in
a
finite
time
(phe-
nomenon
of
entanglement
sudden
death);
-
logarithmic
negativity
and
the
survival
time
of
entanglement
are
de-
creasing
by
increasing
the
temperature
of
the
environment,
while
they
in-
crease
with
the
squeezing
parameter
of
the
bimodal
state.
Therefore,
the
thermal
environment
has
a
destructive
influence
on
the
entanglement,
whose
survival
time
depends
on
the
competition
between
the
On
quantum
entanglement
218
contrary
effects
provided
by
the
squeezing
of
the
bimodal
state
and
the
thermal
bath.
We
have
also
shown
that:
-
the
survival
time
of
entanglement
decreases
by
increasing
the
Hawking
parameter,
while
it
increases
with
de
Sitter
curvature
parameter;
-
as
de
Sitter
parameter
decreases,
the
amount
of
entanglement
also
de
creases,
which
means
that
the
effect
of
space
curvature
reduces
the
entangle-
ment
of
the
state,
that
is,
the
state
becomes
less
entangled
as
the
curvature
of
the
open
chart
gets
larger;
at
a
given
moment
of
time
and
for
a
given
tem-
perature
of
the
thermal
environment,
the
Gaussian
quantum
entanglement
can
survive
only
for
a
sufficiently
large
value
of
the
curvature
parameter,
that
is
for
a
sufficiently
small
curvature;
-
the
entanglement
is
minimized
for
values
1/2
and
3/2
of
the
mass
pa-
rameter,
corresponding
to
the
conformally
coupled
scalar
field,
respectively,
minimally
coupled
massless
field;
therefore,
the
entanglement
of
a
massive
scalar
field
is
more
robust
than
that
of
a
massless
field
in
de
Sitter
space;
the
entanglement
can
survive
for
definite
values
of
times
and
in
the
presence
of
the
curvature
of
the
space,
even
in
the
limit
of
infinite
curvature,
but
only
for
a
mass
parameter
of
a
scalar
field
different
from
1/2
and
3/2.
The
obtained
results
illustrate
the
role
that
the
Hawking,
mass
and
cur-
vature
of
space
parameters
and
the
parameters
describing
the
state
squeez-
ing
and
thermal
environment
play
in
order
to
ensure
the
preservation
of
the
entanglement
over
time
for
practical
implementation
of
quantum
communi-
cation
protocols
that
rely
on
quantum
entanglement.
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