AstroNuclPhysics ® Nuclear Physics - Astrophysics - Cosmology - Philosophy | Gravity, black holes and physics |
Chapter 4
B L A C K H O L E S
4.1. The
role of gravity in the formation and evolution of stars
4.2. The
final stages of stellar evolution. Gravitational
collapse
4.3. Schwarzschild
static black holes
4.4. Rotating and electrically charged Kerr-Newman black holes
4.5. The
"black hole has no hair" theorem
4.6. Laws
of black hole dynamics
4.7. Quantum
radiation and thermodynamics of black holes
4.8. Astrophysical
significance of black holes
4.9. Total
gravitational collapse - the biggest catastrophe in nature
4.4. Rotating and electrically charged Kerr-Newman black holes
In the previous chapters, it was briefly outlined how the complete gravitational collapse of a spherically symmetric star (spherical non-rotating and electrically uncharged) creates a Schwarzschild black hole. However, the conditions of exact spherical symmetry are almost never actually met, with most stars rotating in the first place . The question arises whether a black hole can also be caused by the collapse of a rotating star, or whether the accelerating rotation (centrifugal force) is able to prevent collapse? In Newtonian physics, even the initially slow rotation of the star would eventually prevail and stop the collapse. However, in the general theory of relativity, it is shown that even with the collapse of a rotating star, a black hole can eventually form, albeit in a more complex way [222], [215] , [227].
Collapse of a rotating star
A rotating star,
which is always "flattened" due to centrifugal force,
compresses into a disk-shaped formation (Fig.4.14a), a rapidly
rotating "pancake", during collapse (due to constantly
accelerating rotation due to maintaining angular
momentum), whose
diameter may exceed its thickness several times. If the angular momentum
is not too great (compared to the mass of the star), the collapse
can continue also in the equatorial plane and a black hole
is formed without further complications. A more complex situation
occurs when the angular momentum is large, eg greater
than the critical value J = M ^{2} (see §3.6). In such a case, the
constantly accelerating rotation can tear the disc-shaped
"pancake" into several parts *) - see Fig.4.14c. Some parts that receive a high angular momentum will fly
away (and accordingly reduces the remaining
angular momentum of the system) , but most will be gravitationally bound
and orbit around a common center of
gravity. During their circulation, these fragments will emit
gravitational waves (the system
has a large quadrupole moment rapidly changing with time) carrying away the rotational
energy and thus they will brake and converge (Fig.4.14c, d), until they
gradually merge (Fig.4.14 e) and creates the resulting rotating black hole with angular
momentum J <M ^{2}
. First, large fragments are slowed down and merged ,
because they (according to formula (2.82) ) emit the most intense
gravitational radiation.
*) Theoretically, there is
also the possibility of forming a rotating structure having the
shape of a toroid, in which the collapse would take place first
along a smaller radius and then (if the "longitudinal"
density of mass ~ energy is sufficient) or collapse along a
larger radius. In reality, however, it can be expected that in
such a toroid, immediately upon its formation, there will be
certain inhomogeneities and deformations, which will then grow
with time - the toroidal formation will disintegrate into several
fragments and further evolution will then proceed as
described above. in the text (and the lower part of Fig.4.14).
Fig.4.14. Gravitational collapse of a rotating star.
a) When a rotating
star collapses, it compresses into a sharply rotating disk-like
formation. If the rotation is not fast enough to stop the
equatorial plane collapse, Kerr's black hole will form.
b) With a
large angular momentum due to
the constantly accelerating rotation, instabilities may be
transported and the disk-shaped structure may be torn into
several parts.
c , d) The individual
fragments then revolve around a
common center of gravity, brake by the emission of gravitational
waves, gradually converge and connect.
e) Eventually,
this fragments are absorbed
and a rotating black hole is formed with a correspondingly
reduced rotational angular momentum.
Kerr-Newman geometry
However, a black hole created by the collapse of a
rotating star will no longer be spherically symmetric due to
rotation, but can only be axially
symmetric .
The so-called Kerr-Newman
space-time geometry is considered to be
a general solution for an axially symmetric rotating and
electrically charged black hole (for the
reason see the following §4.5), which we
described from a geometric point of view in §3.6 "Kerr
and Kerr-Newman geometry".
Kerr-Newman geometry
is a generalization of Schwarzschild geometry roughly in the
sense that Schwarzschild geometry is spherical, while Kerr-Newman
geometry is generally elliptical. Some aspects of Kerr-Newman
geometry have been discussed in the aforementioned §3.6; here we
will continue this analysis in order to study the properties of rotating and electrically charged black holes,
whose spacetime is described by this geometry.
^{ }The element of the space-time
interval of Kerr-Newman geometry (3.41) in Boyer-Lindquist
coordinates was given in §3.6; we will
write it again here :^{ }
(4.25) |
where M is the total mass , Q is the electric charge , J is the rotational angular momentum of the axially symmetric source of this geometry; a = J / M is the specific rotational angular momentum per unit mass of the black hole. The event horizon r = r_{g}^{+} has a radius
(4.26) |
The radius of the
horizon is thus smaller than that of an uncharged
non-rotating black hole of the same mass (for
this case of the Schwarzschild black hole, relation (4.26) passes
into relation (3.14), ie r _{g} = 2M) . In conventional spherical coordinates a horizon of a
rotating black hole flattened ellipsoid shape (like the rotation centrifugal force deforms the Earth
into a slightly flattened shape with a diameter of about 20km
difference between the equator and poles; see also notice on
obr.4.16) and thus significantly, the
faster the black hole rotates, the higher the angular momentum J
. The question arises as to whether a rotation too fast could
tear the horizon by "centrifugal force" (similar to what would happen
with an excessively fast spin, such as a grinding wheel or a
circular saw) . In §4.6 " Laws
of black hole dynamics "
it will be shown that a black hole cannot be rotated
above a certain maximum "allowed" or
"insurmountable" speed of the so-called extreme
Kerr black hole, when M ^{2} = J ^{2} / M ^{2} . If we try to throw a body into
a black hole rotating at almost extreme speed, which would spin
it even more, centrifugal forces will prevent this body from
penetrating close enough to the horizon, fly out and not be
absorbed; see also the commentary on inequality below (4.36) .
^{ }^{ }For
the physics of black holes are interesting area compartment r ³ r _{g}^{+
}above the outer horizon - event horizon *). Everything
that takes place below the horizon r = r _{g}^{+} is causally
separated
from the rest of the universe and has no effect. This applies to
the inner horizon r = r _{g
}^{-} = M - Ö (M ^{2}
-a ^{2} -Q ^{2} ) as well as the annular singularity around r = 0, described in §3.6 "Kerr
and Kerr-Newman geometry".
*) In §3.5 and 3.6, the analytical extension inside r = r _{g }^{+} was
discussed . However,
this internal solution below the horizon does not
seem to have physical significance . On the one
hand, this area is filled with the interior of the collapsing
body. In addition, the analogy of Birkhoff's theorem does not
apply to collapse with rotation (§3.4, theorem 3.3); Kerr's
metric does not describe the outer spacetime during the collapse,
but the asymptotic shape of the metric after the end of all
dynamic processes. Other reasons why the complex internal
geometric-topological structure of spacetime inside a rotating
black hole is not realized are discussed below in the section
" Black holes
- bridges to other universes? Time machines? ", Fig.4.19.
Influence
of black hole rotation. Ergosphere.
To clarify the nature of the physical
phenomena that can take place around the Kerr-Newman black hole
(and we will see that very interesting effects can be expected
here), we will first look at the motion properties of the test
particles. The properties of the orbits
of the test particles in the field of the Kerr-Newman geometry
of a general black hole are considerably more complex than in the
case of the Schwarzschild geometry of a non-rotating uncharged
black hole. However, for qualitative knowledge of some basic
aspects of motion it is not necessary to solve complicated Carter equations (3.44), we will suffice with metric
coefficients in the space-time element (4. 25).
^{ }Therefore, according to Fig.4.15a, let us
have a test particle (uncharged) in a place with specified
coordinates r,J , which moves only in the j direction ; such a motion is called stationary because the space-time geometry around
the particle does not change . We will be
interested in the angular velocity with respect to the asymptotically rest
frame of reference W º d j / dt
= (d j / d t ) / (dt / d t ) =
u ^{j} / u ^{t} , where u^{j} and u^{t} are the respective components of
the four-velocity ( we investigate the stationary motion, ie only
in the direction j , so u ^{J} = u ^{r} = 0). This
angular velocity cannot be arbitrary, only values of W are permissible for which the 4-velocity u lies inside the light cone of the future :
u ^{2} = g _{tt} u ^{t} u ^{t} + 2 g _{t }_{j} u ^{t} u ^{j} + g _{jj} u ^{j} u ^{j} <0,
which, expressed by W, gives: g _{tt} (u ^{t} ) ^{2} + 2 g _{t }_{j} W (u ^{t} ) ^{2} + g _{jj} W ^{2} (u ^{t} ) ^{2} <0, i.e.
g _{tt} + 2 W g _{t }_{j} + W ^{2} g _{jj} < 0 . | (4.27) |
Thus, the geometry of spacetime "dictates" to a body located at a location with given r and J a permissible angular velocity in the range
(4.28) |
where W ^{- }_{max} is the maximum angular velocity of circulation against the direction of rotation and W ^{+ }_{max} is the maximum velocity of circulation in the direction of rotation of the black hole. For large distances r from a black hole (or at its small angular momentum J ® 0) W^{- }_{max }» - 1 / r, W^{+ }_{max} » 1 / r, so the particle velocity u = W .r Î <-1, + 1> can be at most equal to the speed of light, both in the direction of rotation and against it, as is the case in the plane space-time STR (movement allowed inside the light cone). With the approach to the black hole, the W ^{- }_{max} increases, so the body must move more slowly against the direction of rotation of the black hole, than if the rotation of the black hole were not (Fig.4.15a).
Fig.4.15. Tearing down
the motion of bodies near a rotating black hole. a) The effect of entrainment of local inertial systems (tilting of light cones in the direction of rotation of a black hole) leads to a gradual limitation of the maximum possible speed u ^{-} movement of bodies against the direction of rotation of a black hole when approaching a black hole. Far from the black hole (for r ® ¥ ) is u ^{+} = c, u ^{-} = -c, in finite distances outside the ergosphere it is u ^{+} > 0, u ^{-} <0, | u ^{-} | <| u ^{+} |. On the static limit, however, u ^{-} = 0, in the ergosphere even u^{-} > 0 Þ the body must necessarily move in the direction of rotation of the black hole. b) Free-falling particles on a rotating black hole first move in the radial direction, but as they approach the horizon, the movement rotates in the direction of rotation around the black hole; on the horizon the particle "falls" in the tangential direction and remains rotated along with the horizon. c) A particle thrown at a black hole in the opposite direction to the rotation of the black hole, when approached the horizon, is forced by the entrainment effect to change the direction of orbit and land on the black hole as co-rotating - just like the particle in Fig. b). In Fig. b), c) the particle trajectories for the case of non-rotating (Schwarzschild) black holes ( W _{H} = 0) are plotted in dashed lines for comparison . |
Rotation black hole with
the outer geometry of space exhibits dragging
(entrainment) local inertial system, who free body forces perform a rotational movement about a black hole, and the more
so the nearer they are to the rotating black hole *). This is similar to a ball rotating in a viscous liquid
entraining the liquid near its surface.
*) The effect of entrainment of inertial systems in the
gravitational field of a rotating body (not just black holes)
leads to a kind of "spin-orbital interaction" between
the rotation ("spin") of the central gravitational body
and the angular momentum of orbiting bodies: motion of bodies, eg
their energy (see relation (4.39)), depends on the mutual
orientation of the angular momentum of the black hole and the
orbital moment of the body.
In the gravitational field of rotating bodies, there is also a
"spin-spin interaction" with bodies that have their own
rotation. For example, a gyroscope in the gravitational field of
a body rotating at an angular velocity W will perform a precessional
motion with respect to an asymptotically inertial system - its
axis of rotation having an angle j will rotate at an angular
velocity w º d j / dt » W .r _{g }^{+} / r. This phenomenon is called the Lense-Thirring
effect according to the authors who first studied it
[248], see §2.5, passage " Rotating
gravity ".
^{ }It can be said that Kerr-Newman
geometry in a sense rotates together with a black hole *) -
spacetime light cones are tilted in the direction of rotation
of the black hole. An observer located at a location with
coordinates r, J is at rest with respect to local
geometry, and the directions + j and - j are equivalent for it only when it rotates (orbits) around a black hole at an
angular velocity.
(4.29) |
such an observer is
called locally non-rotating .
*) For common rotating bodies (macroscopic objects, planets,
ordinary stars), the Lense-Thirring gravitational-rotational
effects are negligible, mostly at the limits of measurability (it
is discussed in §2.5, section " Rotating
gravity ", passage " Possibilities
of verifying the effect of rotation ") . However, an
intense gravitational vortex similar to a
massive tornado is created in the vicinity of a
rapidly rotating black hole ! The rotation of the black hole
carries the surrounding space with it and forces it to rotate in
a "vortex" depending on the speed of rotation of the
black hole and the distance from it. At a distance from the
rotating black hole, the space rotates very slowly, the observer
does not even feel it(similar to far from a
tornado, air flows only slowly) . As you
approach the horizon, the space rotates faster,
"pulling" the observer in the direction of rotation (similar to increasing wind speed near a tornado) . At the horizon, space rotates at the same speed as the
horizon itself, each observer is relentlessly drawn into the
vortex of rotation.
^{ }The effect of
entraining the motion of bodies near a rotating black hole has a
significant effect on the motion of particles and bodies falling
into a black hole. In Fig. 4.15b, c the trajectories of two test
bodies falling into a rotating black hole (from the point of view
of the coordinate system of an external static observer) are
schematically drawn. The particle in Fig. 4.15b moves in a free
fall in the radial direction towards the black hole. If only the
black hole did not rotate(static
Schwarzschild black hole) , the particle
would move in a straight line to the horizon (initially faster and faster, close to the horizon it
would stop its fall from the point of view of an external
observer and would remain permanently "frozen" at a
given place on the horizon - discussed in § 4.2, passage " Two different views of gravitational collapse
- external and internal ") . However, the rotation of the black hole causes the
particle's motion to turns in the direction of rotation around
the black hole as it approaches the horizon. The particle
"hits" the horizon in an almost tangential direction
and remains rotated with the horizon(From
the point of view of an external observer, the particle again
"freezes" on the rotating horizon forever; from the
point of view of the particle itself, it reaches the horizon in a
short time of its own time, flies through it and heads towards
the center of a black hole ...) . The
second particle in Fig. 4.15c is thrown at the black hole in the
opposite direction to the rotation of the black hole. As you
approach the horizon, the effect of entrainment gradually forces
you to reverse the direction of orbit and lands on the black hole
as a co-rotating - it ends up in the same way as the particles in
case b).
^{ }Because real bodies can only move inside
the light cone, it limits this tilting of the space-time light cones
the maximum possible speed of movement of the body against the
direction of rotation of the black hole from the original value
equal to the speed of light to a value the lower the closer it is
to the black hole (as shown above). On the surface given by
the equation
r = r _{S} = M + Ö (M ^{2} - a ^{2} cos ^{2} J - Q ^{2} ) | (4.30) |
the maximum possible speed of the stationary observer against the direction of rotation of the black hole is already zero . This surface (in the shape of a rotating ellipsoid, Fig. 4.16), on which no object can move against the direction of rotation of the black hole (g _{t }_{j} = 0), is called the static limit ; outside this limit there may be static (immobile with respect to infinity) bodies, inside not. The area spread between the static boundary and the horizon is called the ergosphere . Inside the ergosphere, the entrainment is already so strong that no body can remain still here; it is inevitably drawn into rotationand its rotation around the black hole is not prevented by any force - the light cones are completely turned in the direction of rotation of the black hole. The ergosphere (which only rotating black holes have) is the largest in the "equatorial" region and narrows towards the poles, where the static limit r = r _{S} touches the horizon r = r _{g }^{+} (Fig.4.16).
Fig.4.16.
Schematic representation of the horizon, static limits
and region of the ergosphere of a rotating Kerr-Newman
black hole with a rotational angular momentum J in the direction of the Z axis. This is a "
side" view - from the equator side; the
"top" view (from the pole side) is in Fig.4.17.
Note: The r, J coordinates marked in the figure for better orientation are not common spherical coordinates! Near a rotating black hole, the coordinates r, J differ from the spherical coordinates because they are "elliptical" (spheroidal) Boyer-Lindquist coordinates (§3.6). In common spherical coordinates, the horizon of a rotating black hole has a flattened ellipsoidal shape. |
In the ergosphere, there are orbits on which
the particles have a negative total energy
with respect to infinity - the binding energy exceeds the proper
mass of the particle *). When passing over the static limit r = r
_{S} , the
time component of the metric tensor g _{oo} changes sign and becomes negative. Therefore, the
energy E = m g _{ik} u ^{k} = m (g _{oo} u ° + g _{o }_{a} u ^{a} ) a
particle of mass m moving at the velocity u ^{a} may become negative for some orbits of the test
particle. Such a particle with negative energy cannot leave the
ergosphere and, when absorbed by a black hole, brings negative
energy below the horizon with respect to infinity - it reduces
the weight of the black hole. Negative energy geodesics are
completely enclosed within the ergosphere, so that no free-moving
particles from the outer region can enter the negative energy
orbit; to achieve a negative energy orbit, the body inside the
ergosphere must be given additional (non-gravitational)
acceleration - see the Penrose process below.
*) From the analysis of the relation (4.34 ") energy
particles in the Kerr-Newman field implies that the E <0 it is
necessary to counter the movement orbit (L _{j} <0), the
parameters r,^{.}r,L_{j} meet a certain (generally relatively complicated)
inequality [8]; it follows from this inequality that the boundary
of the region containing negative energy orbits is precisely the
static limit given by equation (4.30).
Penrose
process ;
Superradiation; The Blandford-Znajek process
The ergosphere has the interesting property (and hence its name - Greek ergos = work ) that it is possible to obtain
from the black hole the part of energy (~ matter) that is related
to rotation. Penrose [205] investigated the following effect
(Fig.4.17): if body A enters the ergosphere and decays
into two parts B , C so that one part, such as B ,
gets n and the opposite orbit with negative
energy and is absorbed by a black hole, the second part C
can recoil and fly out of the ergosphere with more energy than the original body, while reducing the
rotational angular momentum of the black hole. This
phenomenon, which makes it possible to extract rotational energy
and angular momentum from a black hole, is now called
the Penrose process .
Fig.4.17. Penrose's process of obtaining energy from the
ergosphere of a rotating black hole. Body A flies into the
ergosphere and there, at the appropriate time, splits into two
bodies B and C so that body B enters an
orbit with negative energy (with respect to infinity) and is
absorbed by a black hole. The second part C then flips
from Ergosphere with more energy than the original body A
.
If the body A had (with respect to infinity) the total energy E _{A} and the absorbed body B the energy E _{B} <0 (got into orbit with negative energy), the change in the mass of the black hole when absorbed D M = E _{B} <0. Total energy balance then it will look like this:
E _{C} = E _{A} - D M > E _{A} ; | (4.31) |
therefore, the total energy obtained in this process is
D E = E _{C} - E _{A} = - D M > 0 . | (4.31 ') |
The balance of kinetic energy is also interesting; for this purpose, we divide the total energy of the body into the kinetic energy E ^{kin} and the rest mass: E _{A} = E _{A }^{kin} + m _{A} .c ^{2} , E _{C} = E _{C }^{kin} + m _{C} c ^{2} . The obtained kinetic energy D E ^{kin }= E _{C }^{kin} - E _{A }^{kin} = E _{C} - m _{C} c ^{2} - E _{A} + m _{A} c ^{2} then after substituting from (4.31) am_{A} = m _{B} + m _{C} is based
D E ^{kin} = m _{B} . c ^{2} - D M ; | (4.32) |
in other words, all the
rest mass of the absorbed body B and, in addition, part of the
mass of the black hole were converted into the kinetic energy of
the flying body C.
^{ }A black hole, if it has a maximum
(extreme) rotational speed, can theoretically store up to 42% (of
mc ^{2} ) of its mass in the form of rotational energy . This energy is contained in a rotating
gravitational field outside the horizon, so it can in principle be drawn .
^{ }Regarding the practical
(astrophysical) significance of the Penrose process, various
mechanisms and arrangements have been proposed for obtaining
energy from rotating black holes [204],
[205] *) .
*) Penrose even designed a curious
sci-fi project "black hole power plant" using energy
obtained by throwing waste into a rotating black hole. Waste
containers are thrown into a black hole, the lid opens inside the
ergosphere and the waste is "poured" into a path with
negative energy. The containers thus gain considerable kinetic
energy through the Penrose process, they fly out of the
ergosphere quickly and can impact the turbine blades connected to
the electric generator ..
^{ }However, a more detailed analysis of the
motion of bodies in the Penrose process by Bardeen, Press and
Teukolský [8] showed, that the decay of a body within the
ergosphere would have to take place with a very
high mutual speed of both fragments - at least c/2. Therefore,
for macroscopic bodies, the Penrose process is unlikely to be
astrophysically significant; we do not know the physical
processes that could give such great mutual velocities to
macroscopic material objects. For charged particles, however,
such a mechanism may be a strong magnetic field around a black
hole - the so-called Blandford-Znajek
process
outlined below.
^{ }Another
possibility would be to inject unstable particles (eg
mesons m, p or K, see "Elementary particles and their properties") into the ergosphere, which
would decay into muons, electrons and neutrinos inside the
ergosphere. These secondary particles would fly from each other
at relativistic velocities (> c/2), so that they could be
accelerated by the Penrose process due to the rotation of the
black hole. However, the "practical use" of the kinetic
energy of these accelerated particles flying out of the
ergosphere would be very difficult (cf.
"Antiparticles - antiatoms -
antimatter - antiworlds").
Superradiation
The wave (radiation) similar to Penrose's
process is the effect of so-called superradiation
[287], [8] ,
when a wave incident on a rotating black hole is - if it has a
suitable wavelength - amplified by
a black
hole at the expense of the rotational energy of a black hole. Let
us have a (monochromatic) wave of a classical field with
frequency w , angular momentum (axial quantum number) l and possibly an electric charge q, which
hits (from infinity) on a black hole. In a stationary axially
symmetric Kerr-Newman field, such a wave will be described by the
function (solving the wave equation of the respective field) y (t, r, J
, j ) = F (r, J ) e ^{-i }^{w }^{t} e ^{i }^{l }^{j} ; for scalar and electromagnetic fields
it is possible to separate variables, ie F (r, J ) can be written in the form of the
product of two functions: F (r, J ) =
R (r). S ( J ) [43], [246]. Because the
Kerr-Newman black hole is stationary and axisymmetrically ý will
variables w and l integrals of motion. Part of the wave will
be absorbed and after interacting with the black hole, the
"scattered" wave, which will have the same frequency w , will continue to move ,but
generally a different amplitude. Changes in the mass, charge, angular momentum,
and area of a black hole during this interaction are bound by the
1st law of Black Hole Mechanics (see §4.6, equation (4.50)) :
d M = ( k / 8 p ) d A + W d J + F d Q.
The ratio of energy flow, angular momentum and charge (generally admit that the wave can also carry an electric charge q) in the incident and scattered wave is equal to w : l : q, so thanks to the conservation of energy and angular momentum, changes in the relevant parameters will be black in the same ratio holes d M : d J : d Q = w : l : q . The first law of black hole dynamics then gives
d M ( 1 - W l / w - F q / w ) = ( k / 8 p ) d A.
Because according to the 2nd law of black hole dynamics (see §4.6; we assume that the considered wave satisfies the energy condition (2.60) of non-negative local energy density for each observer) is d A> 0, the inequality will apply
d M ( w - l W - q F ) ³ 0 .
If it is
w < l W + q F
(sufficiently low wave
frequency), the change in the mass of the black hole d M <0 will be negative, so that the
black hole will give energy to the
waves .
Thus, as such a wave interacts with a black hole, its amplitude
increases: even if the wave is partially absorbed, the scattered
portion may receive more energy from the black hole than the
incident wave had - the wave amplifies at the expense of the black
hole's rotational energy. It can be compared to a gravitational
"maser". The effect of superradiation could have some
astrophysical significance *); for black holes of stellar masses
of frequency w satisfying the condition of
superradiation fall into the field of radio waves. Superradiation
can also lead to one interesting effect for black hole physics.
At the end of the last paragraph, it was shown that the orbits of
the particles around the Schwarzschild black hole are always
unstable due to losses by gravitational radiation. However, the
effect of superradiation amplification of gravitational waves
allows the existence of some " floating
orbits
" near the rotating black hole , on which the losses by
radiating gravitational waves are compensated by the energy
obtained from the black hole by the superradiation scattering of
these radiated gravitational waves [210] .
*) Based on the effect of
superradiation, some thought projects [210] have also been
proposed to allow highly developed civilizations to draw large
amounts of energy from rotating black holes, as well as the
"black hole bomb" mechanism: when a black hole is
surrounded by a spherical mirror, the electromagnetic waves will
be reflected many times to the black hole and amplified by
superradiation ("positive feedback" will be created),
so that their intensity (energy) will increase avalanche until
the explosion.
^{ }This is how the process of
superradiation for "boson" classical arrays with
integer spin takes place. In the case of "fermion"
classical fields, it turns out that superradiation does not
occur. This is caused by the fact that the energy-momentum tensor
of the classical field does not meet the half-integer spin energy
conditions (2.60), and therefore can not be applied mechanics 2.law black
holes, and from a quantum viewpoint, Pauli principle allows the
presence of only one particle at a time for a given frequency of scattering
wave, so that the scattered wave cannot be stronger than
the incident wave. Quantum aspects of superradiation and the
related effect of quantum evaporation of black holes will be
discussed in §4.7, section " Mechanism of quantum radiation ".
Electromagnetic extraction of
rotational energy - Blandford-Znajek mechanism
Another interesting modification of the Penrose process with the
participation of a strong magnetic field was discussed by R. Blandford and
R. Znajek in an extensive work [20]. It
turns out that an external very strong magnetic field
around a rotating black hole can force fast-moving charged
particles into negative energy orbits
in the ergosphere of a rotating Kerr black hole, which could lead
to the extraction of rotational energy (and
angular momentum) from black hole by the Penrose process. The
extracted energy in the ergosphere would be transmitted to an
electromagnetic field, which could then accelerate other charged
particles. Such the Blandford-Znajek mechanism
could be applied inside accretion disks around black holes, where
it could contribute to the energy of relativistic jets from
quasars and active galactic nuclei, see §4.8 " Astrophysical
significance of black holes
".
^{ }When a plasma of charged particles orbits
a rotating black hole, it creates a strong poloidal magnetic
field by rotating toroidal currents flowing in the equatorial
plane. The entrainment of space and magnetic field lines by the
rotation of a black hole then induces a powerful electric
generatorin the form of a stream of charged particles.
Some of them enter orbits with negative energy in the ergosphere
and fall into a black hole, while the extracted energy
strengthens the electromagnetic field. Other charged particles
are then electromagnetically accelerated by the extracted
rotational energy and transfer this energy to the plasma in the
jets by magnetohydrodynamic effects. Such a " gravito-magnetic
dynamo ", driven by the rotation of a black hole,
could supply a considerable amount of energy to the jets from the
accretion disk.
^{ }Thus, the above mechanisms show
that rotating black holes are "alive" unlike
"dead" Schwarzschild black holes, from which no energy
can be obtained (if we do not take into
account quantum phenomena) . This "liveliness" of rotating black holes can have considerable astrophysical
significance (in
§4.8., section " Accretion
disks around black holes
" - " Thick accretion disks. Quasars
" will be discussed ) .
The
motion of particles in the field of a rotating black hole
The motion
of test particles in the Kerr-Newman field of a general black
hole is given by equations (3.44). From equations (3.44a) and
(3.44b) we get for a particle with rest mass m _{o}
, electric charge q, energy (with respect to infinity) E
and axial component of the angular momentum L_{j} (with respect to the axis of rotation of
a black hole) the relation
(4.33) |
For the coefficients at individual powers of energy E (which are functions of the place and parameters of the test particle and the black hole), we introduce the notation [43]
(4.33a) (4.33b) (4.33c) |
The above equation then has the form
(r^{2} + a^{2} cos^{2} J) [ (dr/dl)^{2} + (dJ/dl)^{2} ] = a E^{2} - 2 b E + g . | (4.34) |
If we express energy from here
(4.34 ') |
is seen (given that a > 0 everywhere outside of the horizon) that satisfies the energy inequality
E ³ | . | (4.35) |
On the horizon r = r _{g }^{+} is a = (r _{g }^{+ 2} + a ^{2} ) ^{2} , b = (L _{j} a + q Q r _{g }^{+} ) (r _{g }^{+ 2} + a ^{2} ), g = (L _{j} a + q Q r _{g }^{+} ) ^{2} , so the relation (4.35) is simplified here to :
(4.36) |
only if this condition is met can the particle reach the horizon and be absorbed. Inequality (4.36), which from below limits the amount of energy brought below the horizon when absorbing a body with charge q and angular momentum L_{j} , plays an important role in the dynamics of black holes - see §4.6 " Laws of black hole dynamics ", where it directly derives the relation (4.51 ).
The analysis of the
motion of test particles in Kerr-Newman geometry according to
Carter's equations (3.44) is generally quite complicated [228],
[48] , [237]. We achieve a certain simplification if we
investigate only the motion of particles in the
"equatorial" plane of a rotating black hole. Equatorial orbits in the Kerr-Newman black hole field are
at the same time the most interesting, the most characteristic
and the most important for practice. Due to the effect of
entrainment of local inertial systems, for example, the accretion
disk around the rotating black hole (§4.8) is rotated into the
equatorial plane and the actual accretion takes place mainly from
the equatorial orbits. At great distances from the black hole, the effect of its rotation is small again and the trajectory of the particles here
does not depend too much on in which plane and
in which direction with respect to the axis of rotation of the
black hole the particle moves (the motion of the particle at
great distances is similar to that in the Schwarzschild field of
a non-rotating black hole).
^{ }The equation of the radial
component of motion in the equatorial plane of the Kerr-Newman
geometry is obtained from equation (4.34) by substituting J = p / 2 and d J / d l = 0:^{ }
r ^{4} ( dr / d t ) ^{2} = a E ^{2} - 2 b E + g .^{ } | (4.37) |
a , b , g are again denoted by quantities according to (4.33a, b, c), where, however, sin ^{2} J = 1 and cos ^{2} J = 0. This equation can also be rewritten in the form
(4.37 ') |
The only factor that can change the sign here is factor II; factors I and III are positive (if energy E is positive). Quantity
V (r) = | (4.38) |
here, therefore, it plays the role of an effective potential for the radial component of the motion. A particle with energy E can only get to places where V (r) £ E in accordance with the general relation (4.35). The places where V (r) = E are the turning points where the radial component of the motion changes its direction. Circular orbits are (together with the condition V (r) = E) given by the condition dV (r) / dr = 0. Thus, circular orbits are at the extremes of the potential V (r), while the minima V (r) correspond to stable circular orbits . The conditions V (r) = E and dV (r) / dr = 0 lead to the relations (for movement in the equatorial plane, L _{j} = L)
(4.39) |
wherein ` E º E / m _{on} a ` L º L / m _{on} the energy and the angular momentum per unit mass of the test particles [8], [81]. The angular and orbital velocities in orbit (from the point of view of a distant observer) are equal
(4.39 ') |
which is a
generalization of 3.Kepler's law for circular equatorial orbits
in the Kerr metric of rotating black holes. Formulas (4.39) are
given for simplicity only for the Kerr black hole, ie for Q = 0
(otherwise the rest mass m _{o} could not be included in E
and L and in addition would depend on the
specific charge q / m _{o }of the test
particles). The upper signs applies to the movement in the
direction of rotation of the black hole (L.a> 0),
the lower signs for orbits against the direction
of rotation (L.a <0).
From relations (4.39) it can be seen that circular orbits can
exist only at such distances from the black hole for which the
condition is met^{ }
r ^{3/2} - 3 M r ^{1/2} ± 2 a .M ^{1/2} > 0 .^{ } | (4.40) |
The photon circular orbit (on which ` E = ¥ ,` L = ± ¥ ) in the equatorial plane of the Kerr black hole r = r _{f} , which is also the innermost (boundary) circular orbit , has a radius r_{f} given by the equation r ^{3/2} - 3 M r ^{1/2} ± 2 a. M ^{1/2} = 0, ie.
r _{f} = 2m [1 + cos ^{2} / _{3} arccos (± a / m)] . | (4.41) |
For a = 0 we get r _{f} = 3M in accordance with the relation (4.5) for the photon
sphere of the Schwarzschild black hole, for the extreme black
hole a = M is r _{f} = M for the co-rotating
orbits and r _{f} = 4M for the opposite photon
paths. As in the Schwarzschild field, not all circular orbits are
bound here: for orbits close enough to the boundary photon orbit,
the energy value (4.39) becomes greater than one ( ` E º E / m _{o} > 1) - particles on such a
circular orbit E in The relationship is not tied
to a black hole and, under the influence of the slightest upward
perturbation, flies out of this orbit into the
infinity.
^{ }Bound
circular orbits exist only for r ³ r _{mv} , where
r _{mv} = 2M + 2M (M ± a) ^{1/2} ± a
is the boundary radius of the bound orbit corresponding to E / m _{o} = 1. This radius r _{mv} is also the minimum "perihelion" of all parabolic orbits (ie orbits with E / m _{o} = 1, eg bodies falling from infinity); every parabolic trajectory of a body that penetrates closer than r _{mv} ends at a black hole. For a = 0 we get r _{mv} = 4M (compare with Fig.4.6 on the left), for a = M it is for the co-rotating circular paths r _{mv} = M, resp. r _{mv} = 5.83 M for opposite orbits. In order for a circular orbit to be stable to radial perturbations (even all bounded circular orbits are not stable!), it must correspond to the minimum effective potential, ie the condition d^{2}V(r)/dr^{2} L 0 must still be met, leading to inequality
r ^{2} - 6 M r ± 8 a Ö (M r) - 3 a ^{2} ³ 0 . | (4.42) |
Only for radii satisfying this inequality can there exist stable circular orbits, where the equation v (4.42) corresponds to the innermost (lowest, limit) stable circular orbit r = r _{ms} [8] :
(4.42 ') |
For a = 0 we again get the radius of the innermost stable circular orbit r _{ms} = 6M in the Schwarzschild geometry, for an extremely rotating black hole a = M the correspondingly co-rotating innermost stable circular orbit has a radius r _{ms} = M, while for the innermost stable opposite circular orbit it is r _{ms} = 9M.
At large distances r
from the rotating black hole, the parameters (binding energy,
specific angular momentum, velocity of circulation) of the
co-rotating and counter-rotating orbits
are almost the same. Approaching the black hole (with decreasing r ),
however, increases the influence of the angular momentum of a
black hole - the binding energy of the
co-rotating orbits increases, while the
binding energy of the opposite orbits
decreased in
comparison with Schwarzschild orbits. The most striking difference
motion of test particles compared to the Schwarzschild geometry
will be near the extreme Kerr black hole (a = M), where the trajectories of particles moving in the
direction and against the direction of rotation of the black hole
will also differ the most. This is markedly reflected in the
parameters of boundary stable circular orbits. The innermost
stable circular orbit around the Schwarzschild black hole had the
following characteristics (see §4.3): radius r = 6M, specific angular momentum` L = 2 Ö(3) M, energy E = m _{o}
.8 / 9 and binding energy of particle E _{bind} = m _{o} - E = 5.72% m _{o}
.
For the extreme Kerr black hole, according to formulas (4.42) and
(4.39), the innermost stable co-rotating orbit will have a radius r = M,
a specific angular momentum` L =
2M / Ö3, energy E = m _{o} / Ö3
and the binding energy of the particle will be E_{bind} = 42.26% m_{o} ; in circulation against the
direction of rotation of the black hole is the innermost
stable circular orbit in the equatorial plane have a radius r = 9M, specific
angular momentum of` L = 22M /Ö27 , energy E
= 5M / Ö27 and the binding energy of the
particle will only E _{bind} = 3.77% from
m_{o} .
^{ }If we compare this with the
results obtained in the previous §4.3 (passage
" Emission of gravitational waves
when moving in the field of a black hole ") ,
specifically with relation (4.21), the most remarkable is that a
body orbiting in a circular orbit (co-rotating) in the equatorial plane
extreme Kerr's black holes glow
out in the form of
gravitational waves more than 40% of its rest weight! This value of the binding energy at the marginal stable
co-rotating orbit is also of great importance for assessing the
potential efficiency of energy release in accretion disks around
black holes - see §4.8, section " Accretion disks " .
Light propagation in
the field of a rotating black hole
Similar to
the trajectories of test particles, the rotation of a black hole
also affects the propagation of light in its field - it affects
photon orbits. The angle of deflection of the photons by a
spherically symmetric Schwarzschild black hole depends only on
the impact parameter, not on the direction from which they come
to the black hole. There is only one photon sphere around
Schwarzschild's black hole, on which photons can move at all
angles depending on the direction from which they came.
^{ }However, if the black hole
rotates, the situation is more complicated - the geometry is not
spherically symmetrical, but only axially symmetrical, so that
for rays coming from different directions, spacetime appears
differently curved. The angle of deflection of the rays (and the
whole character of their trajectory) can significantly depend on
the direction of movement of the photons with respect to the
direction of rotation of the black hole. In general, rays directed against the direction of rotation are deflected
more than photons going in the direction of rotation - Fig.4.18.
These differences are most pronounced for photons passing in close proximity to a black hole. Indeed, from relation (4.41)
it can be seen that there are two photon circular orbits in the
equatorial plane around a rotating black hole: an opposite
circular photon orbit with a larger diameter than Schwarzschild oa photon
sphere, and a co-rotating photon orbit lying lower than for a non-rotating
black hole. The total effective cross-section of the
gravitational capture of photons by a rotating black hole does
not differ much from the corresponding value (4.15) for the
Schwarzschild black hole. However, the capture angle is asymmetric - photons going in the opposite direction
of rotation are captured with a larger effective cross section
than photons coming along the direction of rotation - Fig.
4.18b.
Fig.4.18. Light propagation in the gravitational field of a
rotating black hole.
a) Light
geodesics in the equatorial plane of the Kerr black hole. The
angle of deflection Dj^{- }of
a photon moving against the
direction of rotation is (at the same collision parameter)
greater than the angle Dj ^{+ }of deflection of a photon along the direction of rotation of a black
hole. The co-rotating photon orbit r = r _{f }^{+} has a larger radius than the opposite
photon orbit r = r _{f }^{-} . b) The effective cross-section of capturing
photons (as well as other particles) by a rotating black hole is
asymmetric - counter-moving photons are captured more efficiently
than photons going in the direction of rotation. c
, d) Rotating (Kerr) gravitational lens: c
- asymmetrical beam path in
equatorial plane; d
- deflection of rays in the general
plane.
Parameters of the
Kerr-Newman black hole
In addition
to the expressions (4.26) and (4.30) for the horizon and the
ergosphere, we present other important relationships between the
quantities characterizing a general black hole. The horizon area of the Kerr-Newman black hole is
A
= _{r=2M,}n_{t=const.}|g_{JJ} g_{jj}|^{1/2} dJ dj = 4p (r_{g}^{+}^{2}
+ a^{2}) = = 4p [^{ }2^{ }M^{2} - Q^{2} + 2M^{ }Ö(M^{2}^{ }-^{ }Q^{2}^{ }-^{ }a^{2})^{ }] |
(4.43) |
in geometrodynamic units; in ordinary units, the area of the horizon is given by the formula
A = ^{4}^{p}^{G}/_{c}_{4} [^{ }2^{ }G^{ }M^{2} - Q^{2} + 2^{ }Ö(G^{2}^{ }M^{4}^{ }-^{ }J^{2}^{ }c^{2 }-^{ }G^{ }M^{2}^{ }Q^{2}^{ })^{ }] . | (4.43 ') |
The angular velocity of a black hole horizon (which is the angular velocity with which a locally non-rotating observer orbits on the horizon with respect to infinity) is calculated from (4.29) by placing r = r _{g }^{+} (which can be further adjusted by substituting from (4.26) and (4.43) for r _{g }^{+} and area A ) :
(4.44) |
It can be seen that this
angular velocity is the same at all points on the horizon (the
black hole rotates like a "solid"), so W _{H} is defined as the angular velocity of the black hole .
For completeness, we will also state the electrical
potential of the horizon :
(4.45) |
the four-potential of the electromagnetic field A _{i} (r, J ) around the Kerr-Newman black hole at the location with the coordinates r, J is (in the Lorentz calibration A ^{i }_{; i} = 0) given by
A_{ t} = Q r^{ }/ (r^{2} + a^{2}cos^{2} J) , A_{ j} = - a Q r sin^{2} J^{ }/ (r^{2} + a^{2}cos^{2} J) ; | (4.46) |
(due to stationarity and axial symmetry, the
potential does not depend on time t and on angle j and its other components are equal to
zero).
The surface gravity k on the horizon (see §4.3), which is the
gravitational force acting on the test particle on the horizon
and having the same angular velocity W _{H} as the horizon (ie on the
locally non-rotating particle on the horizon) is equal to
(4.47) |
It can be seen at first
glance, that for an extreme black hole (for which r _{g }^{+} = r _{g }^{-} = M) the surface gravity is zero
(!).
^{ }It is useful to define the
so-called irreducible mass of
a black hole M _{ired} (the meaning of this quantity and its
name will be shown in §4.6 in connection with the laws of
dynamics of black holes), which is the mass that should
Schwarzschild black hole with the same area of the horizon would
have - 16 p M _{ired} = 4 p ( r _{g }^{+ 2} + a ^{2} ) :^{ }
M _{ired} º Ö (A / 16 p ) = ^{1} / _{2} Ö (r _{g }^{+ }^{2} + a ^{2} ) . | (4.48) |
For a black hole of total mass M , the quantity M _{ired} is limited by inequality
M / Ö 2 £ M _{ired} £ M,
where the upper limit corresponds to a Schwarzschild black hole and the lower limit to an extreme black hole. From (4.48), (4.43) and (4.44) the following relations can be easily deduced :
(4.49) |
W _{H} = a / (4 M ^{2 }_{ired} ) = J / (4 M . 4 M ^{2 }_{ired} ). | (4.44 ') |
The physical significance of the important relationship (4.49) will be discussed in §4.6 "Laws of black hole dynamics" in connection with the 2nd law of Black Hole Dynamics .
Classification
of black holes
In general
Kerr-Newman geometry, which in the next paragraph we will show is
probably the most general space-time geometry of a general
stationary black hole, we can distinguish some significant
special cases (we can compare with the
classification of Kerr-Newman geometry in §3.6) :
Kerr-Newman geometry has
a horizon (and thus describes a black hole) only if the condition
M ^{2} ³ Q ^{2}
+ J ^{2} / M ^{2} is met , ie if it "does not
rotate too fast" or is not "too electrically
charged" compared to its total mass M.
^{ }Rotation (intrinsic angular momentum J )
plays an important role for the geometry of spacetime
around a black hole formed by gravitational collapse, because
most stars are rotating and angular momentum of the rotation due
to the law of conservation of angular momentum during the collapse
would not change significantly (unless the case shown in Fig. 4.14 occurs,
where a considerable part of the angular momentum can be carried away by
gravitational waves; however, only the "excess" angular
momentum is carried away, the
remaining rotational momentum is still considerable) . However, it is different with the electric charge of
black holes :
Electrically
charged black holes?^{ }
The electric charge Q is probably not important
for black holes in space. In order for an electric charge to
leave a noticeable mark on the space-time metric, it would have
to have a huge value comparable to the total mass M (in
geometrodynamic units). Because stars are usually electrically
virtually neutral, the creation and maintenance
of such a large charge is very unlikely; in addition, such large
electrical repulsive forces would probably prevent collapse to
dimensions of ~ 2M, because in areas r> 2M these electrical
repulsive forces would be completely dominant. Even if a highly
electrically charged black hole formed, it would soon
"discharge" in a real situation. If there is a material
environment around the black hole (interstellar matter), opposite
charges (particles, ions) will be attracted and captured from the
surroundings by the charged black hole - by this selective
absorption(accretion) of oppositely charged particles with
the charge neutralizes the black hole quickly *). But even when a
heavily charged black hole is in a vacuum, quantum
electron-positron pair formation processes in a strong electric
field will play a neutralizing role, repelling black-hole charges
and attracting and absorbing opposite charges through the black
hole. The electric charge of a stationary black hole is therefore
practically zero . The reason why we dealt with
the influence of charge and Reissner-Nordström geometry here and
in §3.5 was rather theoretical - to show interesting (and at
least physically possible in principle) properties of spacetime.
*) If a rotating black hole is immersed in
an environment with a strong magnetic field, a certain
equilibrium very small value of electric charge, determined by
the speed of rotation and the intensity of the external magnetic
field, may persist even in the steady state.
Black
holes - bridges to other universes? Time machines?
Rotating or electrically charged black holes have a complex
geometric and topological structure of spacetime (as we have shown in §3.5 " Reissner-Nordström
geometry " and §3.6 " Kerr and
Kerr-Newman geometry ") ; there has been speculation that they could serve as bridges
- tunnels or portals - to other universes , or tunnels
between distant places or other times
in the same universe. We will try to critically
assess these possibilities from a physical point of view.
Wormholes^{ }^{ }
Hypothetical "tunnels" in space-time that connect the
shorter route two remote sites in the same space, or two places
in various otherwise separate universes, are called " worm
holes " - according to the similarity with
connecting paths that a worm biting through an apple.
A worm that is located on the
surface of an apple and has to get from one side to the other can
do this in two ways. If it considers its space to be
two-dimensional (the surface of the apple), it must crawl over
the entire circumference of the apple. However, if he perceives
the apple as a three-dimensional object, he can choose the path
through it and bite through the desired opposite place along a
much shorter path (or also longer in the case of a crooked
corridor ...). It does not travel two-dimensionally on the
surface of the apple, but uses the three-dimensional abbreviation
"wormhole".
The wormhole in the apple allows only a slight shortening of the
path between the two places on the surface-peel. However, with a
suitable geometric-topological structure in space, a wormhole
could represent an absolutely fundamental shortening of the path
between very distant places in space (eg from many light-years to
hundreds of meters or kilometers)!
^{ }According to this analogy with the worm, we intuitively
imagine that the abbreviated path between different places or
universes takes place through another, higher dimension
, through hyperspace . In mathematical topology
(§3.1 " Geometric-topological properties of spacetime "), however, a space (manifold) can be multiply
connected by its internal structure, so there
is no need to use additional dimensions to "travel"
between different parts.
^{ }Something that could be a forerunner of
the worm hole model, was first sent in 1935 by A. Einstein and N.
Rosen as the so-called Einstein -Rosen bridge (see §3.4
" Schwarzschild geometry ",
Fig. 3.18) in Schwarzschild's solution of the centrally symmetric
gravitational field.
Fig.3.18. a) Schematic
representation of the
geometric structure of the section (spatial hyperplanes)
v = t = 0, J = p / 2
Schwarzschild spacetime in the form of nesting into auxiliary three-dimensional
Euclidean space. This auxiliary three-dimensional space
has no physical significance (it is only a means of
representation); only the internal geometry of the nested
surface, which shows the two asymptotically planar
regions A and A ' connected by the
Einstein-Rosen bridge, is relevant. b) A topological tunnel between two places in the same universe. c) "Wormhole" between two places in the same universe. |
The name " worm hole
" was proposed in 1957 by J.A.Wheeler. The mouth or gullet
of a wormhole would look like a two-dimensional sphere. Unlike
the spherical horizon of a black hole, which allows only a
"one-way path without return", mostly to perdition,
however, the estuary of a wormhole is a bidirectional through
surface (at least in principle) . The wormhole has an entrance and an exit
, we can pass them both inside the wormhole and out into the
outer universe. If a hypothetical astronaut penetrates a
wormhole, he could find himself in another place in
space and at a different time , in the future or
in the past (depending on the values of the
metric tensor in both mouths).. Possibly,
even in another causally separated universe (according
to the global topology of spacetime)..?..
The wormhole has no direct connection with the black hole, but in
many mathematical models of black holes there is also a wormhole
inside.
^{ }From a geometrical-topological point of view, a wormhole
can be defined as a compact region of spacetime, whose spatial
boundary is topologically equivalent to a simple sphere S ^{3} , but whose interior
is topologically connected to places outside
this initial region. It is thus a compact region W in asymptotically
flat spacetime, whose topology has the form W ~ R ´S , where R is the
Riemann space and S is a 3-dimensional tube whose boundary has a topology
of the shape ¶S ~ S ^{2} and the hyper-area S
described in space-time has a spatial
(space-like) character. From a geometric point of view, we have
two types of wormholes:
a) Tunnels connecting different separate
universes ; b) Connections between different distant places of the same
universe (ours).
^{ }In terms of "throughput", we also recognize
two types of wormholes:
- Traversible - stable, allowing movement
across space (spacetime), wormholes connecting two different and
distant places in our universe or different universes. To stabilize
these wormholes need matter with a negative energy density
(see the discussion below " Can wormholes really exist? ") .
- Non -
traversible -
very short-lived, vanishing so fast that no real object can fly
through them without being absorbed by singularity. Such are the
characteristics of wormholes inside black holes (such as the
Einstein-Rosen bridge), connecting various separate universes. Of
course, all virtual worm micro-holes in quantum topological foam
are non-digestible (again discussed below
in the section " Can
Worm Holes Really Exist ? ") .
^{ }Ordinary tunnel (such
as railway)connects two places in space, a
wormhole connects two places in space-time. If there were a
wormhole, it would theoretically make it possible to bridge two
very distant places in space in a much shorter path
. An observer (astronaut) through a wormhole - even if it does
not exceed the speed of light anywhere - could cover the distance
between the two places much faster than a light beam flying in
the usual straight path (through the space outside the wormhole).
He would reach a distant place before the light. Due to the fact
that the observer "precedes" light with this
abbreviation, from the point of view of the theory of relativity
he can "overcome time" - he can travel in time
to the future and back to the past. The possibilities of
fictitious or real time travel are discussed in §3.3, part
"Closed
worldlines and time travel ",
then systematically in the syllabus" Time Travel: Fantasy or
Physical Reality? "
Can there really be
wormholes ?^{ }
Large" wormholes "could occur in space as remnants of
turbulent processes with matter and space-time during the Big
Bang, which cosmic inflation has expanded to macroscopic or even
astronomical sizes. Microscopic wormholes measuring about 10 ^{-33} cm everywhere and
constantly created and destroyed as a result of quantum gravity
fluctuations of spacetime metric and topology (see §B.4 " quantum
geometrodynamika ") - in quantum topological foam .
^{ }Wormholes inside black holes^{ }
they have a "mayfly" life. In addition to
gravitationally dynamic effects, quantum radiation effects also
contribute to this. A random quantum of radiation falling on a
black hole from the outside will accelerate to high energies due
to gravity and will "bomb" even the esophagus of a
wormhole, which will shrink and close quickly as a result. Any
object that would attempt to pass through such a wormhole during
its short life will disappear at the moment of the wormhole's
rupture, along with it, in the resulting singularity. Due to this
extremely short duration of topological tunnel is problematic
even speak of the existence of wormhole ...
^{ }To macroscopic wormhole could maintain
stable "through" must be present or mass field inducing
antigravity effects (material with negative
energy density), Which would avoid the tendency of gravity
to "necking" in singularities and the formation of a
black hole - by Raychaudhuryho equation (2.59) deviation
geodesics ( §2.6 " deviation and
focusing of geodesics ") energy condition opposite to (2.60) causes expansion of
geodesics after passage through the wormhole . The only
hypothetical possibility of stable wormholes is to " reinforce
" them with a specific type of substance that would have antigravity
effects and thus effectively "push" the walls of
the wormhole apart; in terms of energy-momentum tensor
components, this substance must have a large stress in the radial
direction, exceeding the energy density.*) (violating the weak
energy condition (2.60)), which K. Thorne called " exotic
matter ".
*) The exotic substance must have a
negative energy from the point of view of the observer or the
light beam passing through the wormhole, not necessarily
from the point of view of the observer who is at rest inside the
wormhole. In the theory of relativity, the energy density can be
negative in one frame of reference, positive in another.
^{ }Black holes are (at least at the level of
current astrophysical knowledge) a legitimate
physical consequence of stellar evolution (§4.1.
" The role of gravity in the
formation and evolution of stars " and §4.2, section " Complete gravitational collapse. Black hole. ")and their existence is
evidenced by strong astronomical observational data. However,
wormholes are still a mere hypothesis - we do
not know of any natural way in which wormholes in the universe
could form outside the interiors of black holes.
^{ }So far there are no observational indications
for wormholes !
Topological
tunnels inside black holes
The complete analytical extension of the Kerr-Newman geometry
shown in Figs. 3.21 to 3.25 and the resulting
geometric-topological consequences are essentially the same as
the extension of the Schwarzschild geometry (see end of §4.3).
Let us first notice Schwarzschild's geometry, for which a Kruskal
diagram was constructed in §3.4 (Fig. 3.17) showing the presence
of two mirror-inverted universes - Fig . 3.18a . However, in a gravitational
collapse, Schwarzschild's solution describes the geometry of
spacetime only above the surface of a collapsing star. Therefore, most part of the idealized (an extended)
Schwarzschild solution on the Kruskal diagram is therefore not realized - is "cut off" by the inside of
a collapsing star (Fig. 4.19a).
^{ }In §3.5 "
Reissner-Nordström
geometry " and §3.6
" Kerr and Kerr-Newman geometry " we
have shown, that an observer who, during his motion
in Reissner-Nordström or Kerr-Newman spacetime, intersects the
inner (Cauchy) horizon r = r _{g }^{-} , can get into another
"universe". Accordingly, in the event of a
gravitational collapse (of an electrically charged or rotating
mass), there would be a possibility that after crossing the
Cauchy horizon r = r _{g }^{-} the shrinking mass may avoid singularity and begin to expand
again into another region of spacetime ("another universe") -
Fig.4.19b.
^{ }The Einstein-Rosen bridge and
analogous structures of Kerr-Newman geometry can be understood as
a "bridges" connecting two different asymptotically planar universes (assuming the usual Euclidean global
topology of each). With a suitable topology, such a bridge could
connect two different places of
the same (multiple conected) universe - Fig.3.18b, c. Such a " worm hole " (as defined
above) could create
a "topological abbreviation" between two distant
regions of spacetime. There is even speculation about the
possibility that a certain movement of both ends of the wormhole
could form a closed time curve. From here, it is only a step
towards the sci-fi idea of how a technically advanced
civilization, with technology that allows it to manipulate
(through gravity) a wormhole, triggers a " time machine " (" Time Travel: Fantasy or
Physical Reality? ") ...
^{ }Such travel
between different universes , or between different distant places in
the same universe, or even time travel, may be an exciting topic
for science fiction, but the reality is probably more prosaic.
The exact Schwarzschild, Reissner-Nordström or Kerr solution
containing "tunnels" between different universes is
valid only under the conditions for which it was derived, ie for
an otherwise completely empty
asymptotically planar universe .^{ }
^{ }At the end of §3.5, it was noted
that an observer moving so that it intersects the inner horizon r
= r _{g }^{-}, will see during the final
interval of his own time the whole further history of the
"universe" he is leaving. Any body from this universe
would be seen by an observer approaching r _{g}^{-} with a purple shift increasing to
infinity. In connection with this, it has been shown [114], [192]
that the Cauchy horizon r = r _{g }^{-} inside a black hole is unstable to electromagnetic and gravitational
perturbations occurring outside the black hole (classical
instability) *). Analysis of quantum processes of particle
formation in strong fields inside a black hole further shows [192
] (see also §4.7) that there is also a quantum instability of the inner horizon **), which
manifests itself even in the case when the space is empty from
the classical point of view.
*) Figuratively speaking, a
particle that would fly through such a black hole into another
universe would "demolish"
this theoretical tunnel into other universes.
**) In addition, the existence of closed time worldlines would
allow particles to interfere with their own past through a time
loop. Quantum considerations suggest that the disturbances
resulting from such phenomena would intensify spontaneously and,
with their high energy, would eventually destroy the topological
tunnel...
Fig.4.19. The space-time structure of a real black hole.
a) In
Schwarzschild's spacetime of a static black hole created by the
collapse of a (non-rotating) star, a large part of the structure
of the Kruskal's diagram is cut off by interior of
collapsing star.
b) The collapse of a rotating star into a black
hole could theoretically create a space-time structure allowing
it to travel to another universe. The collapsing matter could
then emerge in the second universe in the form of a "white
hole".
c) However,
due to the diverging intensity of the incoming radiation at the
inner horizon and the quantum production of particles around the
singularity, much of the theoretical structure of Kerrr-Newman
geometry (including inner horizons and other universes on the
Penrose diagram) cannot actually be realized. The collapse
creates a singularity that is in the future and takes on a
spatial character, which does not allow any travel to other
universes.
These instabilities (to
perturbations and quantum processes) lead in practice to the destruction and disappearance
of the Cauchy horizon and the emergence of a singularity of the
spatial type - Fig.4.19c. Therefore, it can be expected that in
the real situation the structure of spacetime within the event
horizon r = r _{g }^{+} will be qualitatively similar to
Schwarzschild's black hole and the complex topological
construction according
to Fig.3.25 will not apply (matter would have to pass
through the singular region before).
^{ }Again, we come to the conclusion
that the "exotic" possibilities of traveling between
different universes, or time travel, could work at most within
elementary particles (or only a single elementary particle !^{ }) - cf. with a discussion of closed time
curves in §3.3., passage " Closed worldlines and time travel ". The individual
mechanisms are described in more detail in the work (syllabus) "
Journeys
through time: fantasy or physical reality? ". At
the end of §3.4, the note " Dual
solutions in analytic extension - reality or fiction? ", doubts are discussed about the
very physical meaning of the full extensions of Schwarzschild and
Kerr-Newman geometry of spacetime, on which all ideas about
traveling between different universes or in time are
ideologically based..?..
Some related considerations about the direction of time flow are
further outlined in §5.6, section " Time arrow
".
Black
holes - "hatcheries"
of new universes ?
In addition to the idea that black holes are portals to other
worlds (universes), an even bolder sci-fi hypothesis has emerged
(recently revived and supplemented by Lee Smolin): that new
universes are being born in black holes
. Our entire universe could have been born of a black hole from
another universe; big-bang would really just be a widening of a
black hole in another universe. The idea also emerged that these
emerging universes also carried away the physical laws of the
original ("mother") universe - as if there was a kind
of "cosmic inheritance". This speculative " evolutionary
cosmology of natural selection"would then be
similar in some sense to Darwinian evolutionary biology, as it
said that the most common types of universes would be the ones
that make the most "copies of themselves"; universes
with a large number arer formed would have a certain
"reproductive advantage" passing on to the next
"generations" of universes...
From the point of view of the sober physical approach of general
relativity and quantum theory, however, these speculative
concepts appear to be unfounded :
1. Black holes do not produce new universes
- from a classical (non-quantum) point of view they do not arise
inside black holes at all (as discussed above ), from a quantum
point of view, spontaneous fluctuations in space-time, which can
potentially lead to the emergence of new universes, are taking
place everywhere.and constantly, not just inside
black holes.
2. There is no mechanism by which any particular physical
information can be transferred from one universe to another.
Within classical GTR, this is forbidden by Hawking's and
Penrose's theorems on singularities. In the approach of quantum
cosmology, chaotic quantum field fluctuations and metrics in the
"topological foam" of space-time effectively erase
and randomize any macroscopic physical structure and information
from another (previous) universe..!..
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