Black Hole
A massive astrophysical object that is theorized to be created from the collapse of a neutron star. The gravitational forces are so strong in a black hole that they overcome neutron degeneracy pressure and, roughly speaking, collapse to a point (known as a singularity). Even light cannot escape the gravitational pull of a black hole within the black hole’s socalled Schwarzschild radius.
Uncharged, zero angular momentum black holes are called Schwarzschild black holes. Uncharged nonzero angular momentum black holes are called Kerr black holes. Nonspinning charged black holes are called ReissnerNordström black holes. Charged, spinning black holes are called KerrNewman black holes. The black hole no hair theorem shows that mass, charge, and angular momentum are the only properties which a black hole can possess.
Features of a Black Hole
A black hole forms when an object collapses to a small size (perhaps to a singularity) and the escape velocity in its neighborhood is so great that light cannot escape. The boundary of this region is called the event horizon because any event that occurs inside is invisible to outside observers. The radius of the region is RS, the Schwarzschild radius.
Strange Stuff Explained: Black Holes
A massive star starts to collapse when it exhausts its nuclear fuel and can no longer counteract the inward pull of gravity.
The crushing weight of the star’s overlying layers implodes the core, and the star digs deeper into the fabric of spacetime.
Although the star remains barely visible, its light now has a difficult time climbing out of the enormous gravity of the stillcollapsing core.
The star passes through its event horizon and disappears from our universe, forming a singularity of infinite density.
Pile enough matter into a small enough volume and its gravitational pull will grow so strong that nothing can escape from it. That includes light, which travels at the absolute cosmic speed limit of 186,000 miles per second. In a stroke of descriptive genius, physicist John Wheeler named these objects “black holes.” The radius of a black hole is called the event horizon because it marks the edge beyond which light cannot escape, so any event taking place inside the event horizon can never be glimpsed from outside—in effect, the inside of the black hole is cut off from our universe. It has even been speculated that black holes could be pathways into other universes. Gravity is so strong at the center of a black hole, that even Einstein’s gravitational laws must break down. The theory that governs the incredibly dense matter and strong gravitational fields at the center of a black hole is not yet known.
How Black Holes Might Appear in Nature
 MicroBlack Holes
 Formation: Possibly formed in small regions of high density during the first few seconds of the Big Bang.
 Unusual Features: Microblack holes aren’t so black! Quantum mechanics and thermodynamics tell us that they should radiate all forms of energy due to the strongly varying gravitational fields just outside their event horizon. These black holes slowly radiate themselves away, finally disappearing in a flash of highenergy radiation.
 Size: If a microblack hole is created with a mass of greater than 10^17 grams, it would still be around today. This mass corresponds to about a cubic kilometer of water. In terms of size, it would be smaller than an electron!
 Observations: Once believed to be a possible source of gammaray bursts, there is no current observational evidence for their existence.
 StellarMass Black Holes
 Formation: When a star with a mass of greater than 10 times the mass of the Sun explodes in a supernova, the central core left behind will collapse into a black hole.
 Unusual Features: When this type of black hole is part of a binary system, matter can sometimes stream from the other star into a disk surrounding the black hole. This is called an accretion disk.
 Size: These black holes would range from about 5 to 100 times the mass of the Sun, giving them diameters of 20 to 400 miles.
 Observations: At present, there are over 25 objects astronomers suspect may be black holes near or in our own galaxy. A partial list: Cygnus X1, A062000, V404 Cygni, LMC X1, LMC X3.
What does an XRay binary star look like?
Where is Cygnus X1?
 SuperMassive Black Holes
 Formation: Formed via accretion from smaller bodies in the centers of many galaxies.
 Unusual Features: On this scale, some of the infalling matter may become redirected into jets and ejected over the poles of the black holes. This phenomenon may explain the radio jets observed from the centers of some galaxies.
 Size: HUGE! One million to one billion times the mass of the Sun. They would be about the size of our solar system.
 Observations: Active Galactic Nuclei (AGN), Seyfert Galaxies, Quasars.
HST’s View fo the Jet in Galaxy M87
HST’s view of the accretion Disk in Galaxy NGC 4261
The Black Hole Next Door
Some theorists believe black holes are part of every day life and are even formed by nature right here on Earth. In Science News Online you can find the article The Black Hole Next Door by Peter Weiss about micro black holes. It also explains why the CERN Large Hadron Collider (which will be online in the spring or summer 2007) is important for current theories about multiple dimensions.
Final ‘Proof’ Provided for Milky Way’s Central Black Hole
“We could not believe our eyes.”
– Astronomer Thomas Ott on the surprising discovery of a star swinging around the very heart of the Milky Way.
Surprising observations of a star swiftly orbiting the cloudy heart of the Milky Way Galaxy have verified with near certainty the existence of a central black hole, a theoretical object that still eludes direct detection.
Astronomers watched the star for a decade, tracking twothirds of its path around the galactic center. No object has ever before been seen so close to the center of any galaxy, nor has any other object previously been observed making more than a small fraction of its orbital trek around a galaxy.
“Our work proves that there is indeed a supermassive black hole in our own galaxy,” said Rainer Schoedel, a PhD student at the MaxPlanck Institute for Extraterrestrial Physics (MPE) in Germany.
An international team of astronomers photographed the star as it zoomed around the galactic center at speeds ultimately exceeding 11 million mph (5,000 kilometers per second). Early this year, the star flitted precariously close to the black hole, coming within 17 lighthours, or just three times the distance from the Sun to Pluto.
The observations rule out nearly all other possible explanations for the tremendous amount of matter – equal to some 2.6 million suns – packed into a tight spot at the center of our galaxy.
“If one accepts the universal validity of the laws of physics,” Schoedel told SPACE.com, “it is extremely hard to avoid the conclusion that the supermassive black hole in the Milky Way does indeed exist.”
Chandra Catches Milky Way Monster Snacking
Einstein’s Relativity Theory predicted Black Holes. Black holes are formed by the gravitational collapse of solar masses. Astronomical observations suggest a supermassive black hole containing millions to billions of solar masses in the center of most galaxies. As it turns out our Milky Way is no exception.
Also see Animations & Video and The Chandra Spacecraft.
New Twists on the Milky Way’s Big Black Hole
The supermassive black hole at the center of our Milky Way Galaxy is heftier than thought and rotates at an amazing clip, new research shows.
For years scientists said the black hole contained about 2.6 million times the mass of the Sun. They now believe the figure is somewhere between 3.2 million and 4 million solar masses.
And a new study suggests all that mass, confined to an area about 10 times smaller than Earth’s orbit around the Sun, spins around about once every 11 minutes. The Sun, for comparison, takes about a month to make a revolution on its axis. Earth spins once every 24 hours.
Black holes can’t be seen or measured directly, because light passing near them gets trapped. So astronomers measure a black hole’s mass by observing the orbital speed of nearby stars.
The new mass estimate was made by two separate groups, one at the University of California, Berkeley, and another at the University of California, Los Angeles, UC Berkeley physicist Reinhard Genzel told SPACE.com.
Astronomers Watch a Black Hole Eat a Meal
Astronomers from the Institute of Astronomy (IoA) in Cambridge, England have watched a bundle of matter at the heart of a galaxy 100 million lightyears away as it orbited a supermassive black hole four times on its way to being destroyed. The material was approximately the same distance as our Earth is from the Sun, but instead of taking a year, it only took a quarter of a day, because of the massive gravity of the black hole. By tracking the matter’s doomed orbit, astronomers were then able to calculate the mass of the black hole: between 10 and 50 million solar masses.
Static, Uncharged  Schwarzschild Black Holes.
The first kind of black holes hypothesized, and hence, the “simplest”. In 1916, Karl Schwarzschild hypothesized the existence of black holes from Einstein’s theory of relativity. However, Schwarzschild only considered mass as a factor.
The Schwarzschild black hole nonmoving, and does not have any charge. Put simply, it is brought about by the collapse of a stationary star. Light bends around the edge of the black hole, an observation that involves the theory of a photon sphere. A photon sphere occurs at a distance of 1.5 times the Schwarzschild radius. At this distance, light rays orbit unstably around the black hole. Photons orbit in a sphere around the gravity pull (assuming that the pull is equal in all directions).
Moving closer into the cosmic phenomena, we eventually reach the mathematical construct: an event horizon. It marks the distance where the gravity pull of the black hole is so strong that even light cannot escape it, and occurs at the Schwarzschild radius.
When an object is compressed below its Schwarzschild radius (RS), it becomes a black hole.
Static, Charged  ReissnerNordström Black Holes
Unlike the simpler Schwarzschild black hole, the ReissnerNordström black hole contains charge. It has more than one event horizon. A second, inner horizon forms just above the singularity. It is termed the Cauchy horizon. Electrons appear to “hover” around this second horizon. In other words, a charged black hole has two radii where time seems to stop.
The more charge the black hole has, the smaller the outer event horizon is, and the larger the inner event horizon. If enough charge is amassed to equal the mass of a black hole, then both the outer and the inner horizon would merge. However, this would be near impossible as the minimum mass that a black hole is calculated to have is 10^30 times the speed of light. If charge becomes greater than the mass of the black hole, then both horizons would vanish, revealing the singularity (“naked singularity”). When this happens, we may actually be free to move around the singularity and resist being sucked into it without having to go faster than the speed of light. However, in order for this to occur, we have to generate charge equal to or more than the value of at least 3 solar masses, or 6 x 10^30. This would be near impossible to do.
Kerr Black Holes
The Schwarzschild reference frame is static outside the Black Hole, so even though space is curved, and time is slowed down close to the Black Hole, it is much like the absolute space of Newton. But we will need a generalized reference frame in the case of rotating Black Holes. Roy Kerr generalized the Schwarzschild geometry to include rotating stars, and especially rotating Black Holes. Most stars are rotating, so it is natural to expect newly formed Black Holes to process significant rotation too.
Features of a Kerr Black Hole
The Kerr black hole consists of a rotating mass at the center, surrounded by two event horizons. The outer event horizon marks the boundary within which an observer cannot resist being dragged around the black hole with spacetime. The inner event horizon marks the boundary from within which an observer cannot escape. The volume between the event horizons is known as the ergosphere.
What is a Kerr black hole?
The usual idealised “static” black hole is stationary, unaccelerated, at an arbitarilylarge distance from the observer, is perfectly spherical, and has a pointsingularity at its centre.
When one of these idealised black holes rotates, it gets an extra property. It’s no longer spherically symmetrical , the receding and approaching edges have different pulling strengths and spectral shifts, and the central singularity is no longer supposed to be a dimensionless point.
The equatorial bulge in the event horizon can be deduced in several ways

… as a sort of centrifugal forces effect. Since it’s possible to model the (distantlyobserved) hole as having all its mass existing as an infinitelythin film at the event horizon itself (i.e. where the mass is “seen” to be), you’d expect this virtual film to have a conventionallooking equatorial bulge, through centrifugal forces.

… as a sort of massdilation effect. Viewed from the background frame, the “moving film” of matter ought to appear massdilated, and therefore ought to have a greater gravitational effect, producing an increase in the extent of the event horizon. Since the background universe sees the bh equator to be moving faster than the region near the bh poles, the equator should appear more massdilated, and should have a horizon that extends further.

… as a shift effect. This tidy ellipsoidal shape isn’t necessarily what people actually see  it’s an idealised shape that’s designed to illustrate an aspect of the hole’s deduced geometry independent of the observer’s viewing angle. In fact, the receding and approaching sides of the hole (viewed from the equator) might appear to have different radii, because it’s easier for light to reach the observer from the approaching (blueshifted) side than the receding (redshifted) side (these shifts are superimposed on top of the normal Schwarzchild redshift).
If we calculate these motion shifts using either the SR shift assumptions f’/f = (flat spacetime propagation shift) × root[1  v²/c²] or the plain fixedemitter shift law f’/f = (cv)/c, and then treat them as “gravitational”, then by multiplying the two opposing shifts together and rooting the result, we can get the same averaged dilation factor of f’/f=root(1  v²/c²) in each case, and by applying the averaged value, we recreate the same sort of equatoriallydilated shape that we got in the other two arguments.
Of course, none of these “film” arguments work for a rotating point, which immediately tells us that the distribution of matter within a rotating black hole is important, and that the usual method of treating the actual extent of a body within the horizon as irrelevant (allowing the use of a pointsingularity) no longer works when the hole is rotating (a rotating hole can’t be said to contain a pointsingularity).
In the case of a rotating hole, the simplest state that we can claim is equivalent to the rotating film of matter for a distant observer is a ringsingularity.
Notes

The idea of being able to treat a nonrotating black hole as either a pointsingularity or a hollow infinitelythin film is a consequence of the result that the actual massdistribution is a “null” property for a black hole, as long as it is spherically symmetrical. If the mass fits into a Schwarzchild sphere, the usual static model of a black hole allows the hole’s mass to be pointsized, golfballsized, or of any size up to the size of the event horizon.
It’s usual to treat all the matter as being compacted to a dimensionless point, but sometimes it’s useful to go to the other extreme and treat the matter as being at its “observed” position  as an infinitelythin film at the event horizon (see Thorne’s membrane paradigm). 
The idea of being able to treat all shifts as being propagation effects is something that probably ought to be part of GR  in the context of black holes, the timedilation effect comes out as a curvedspace propagation effect due the enhanced gravitation due to kinetic energy. However, there’s a slight “political” problem here, in that GR is supposed to reduce to SR, and SR is usually interpreted as having Lorentz shifts which are supposed to be nongravitational (because allowing the possibility of gravitational effects upsets the usual SR derivations). A GRcentred physicist might not have a problem with this approach of treating all shift effects as being equivalent, a SRcentred one probably would.

The “bulginess” of a Kerr black hole is illustrated on p.293 of the Thorne book (fig 7.9). Thorne says that the effect of the spin on the horizon shape was discovered Larry Smarr in 1973.
Overview of Kerr Spacetime
Kerr spacetime is the unique explicitly defined model of the gravitational field of a rotating star. The spacetime is fully revealed only when the star collapses, leaving a black hole – otherwise the bulk of the star blocks exploration. The qualitative character of Kerr spacetime depends on its mass and its rate of rotation, the most interesting case being when the rotation is slow. (If the rotation stops completely, Kerr spacetime reduces to Schwarzschild spacetime.)
The existence of black holes in our universe is generally accepted – by now it would be hard for astronomers to run the universe without them. Everyone knows that no light can escape from a black hole, but convincing evidence for their existence is provided their effect on their visible neighbors, as when an observable star behaves like one of a binary pair but no companion is visible.
Suppose that, travelling our spacecraft, we approach an isolated, slowly rotating black hole. It can then be observed as a black disk against the stars of the background sky. Explorers familiar with the Schwarzschild black holes will refuse to cross its boundary horizon. First of all, return trips through a horizon are never possible, and in the Schwarzschild case, there is a more immediate objection: after the passage, any material object will, in a fraction of a second, be devoured by a singularity in spacetime.
If we dare to penetrate the horizon of this Kerr black hole we will find … another horizon. Behind this, the singularity in spacetime now appears, not as a central focus, but as a ring – a circle of infinite gravitational forces. Fortunately, this ring singularity is not quite as dangerous as the Schwarzschild one – it is possible to avoid it and enter a new region of spacetime, by passing through either of two “throats” bounded by the ring (see The Big Picture).
In the new region, escape from the ring singularity is easy because the gravitational effect of the black hole is reversed – it now repels rather than attracts. As distance increases, this negative gravity weakens, just as on the positive side, until its effect becomes negligible.
A quick departure may be prudent, but will prevent discovery of something strange: the ring singularity is the outer equator of a spatial solid torus that is, quite simply, a time machine. Travelling within it, one can reach arbitrarily far back into the past of any entity inside the double horizons. In principle you can arrange a bridge game, with all four players being you yourself, at different ages. But there is no way to meet Julius Caesar or your (predeparture) childhood self since these lie on the other side of two impassable horizons.
This rough description is reasonably accurate within its limits, but its apparent completeness is deceptive. Kerr spacetime is vaster – and more symmetrical. Outside the horizons, it turns out that the model described above lacks a distant past, and, on the negative gravity side, a distant future. Harder to imagine are the deficiencies of the spacetime region between the two horizons. This region definitely does not resemble the Newtonian 3spacebetween two bounding spheres, furnished with a clock to tell time. In it, space and time are turbulently mixed. Pebbles dropped experimentally there can simply vanish in finite time – and new objects can magically appear.
The complete model of Kerr spacetime built in Chapter 3 adds two more horizons to each such interhorizon region (there will be many regions) – and shows that Kerr spacetime is organized symmetrically around the spatial 2spheres at which these horizons intersect.
KerrNewman Black Hole
A rotating charged black hole. An exact, unique, and complete solution to the Einstein field equations in the exterior of such a black hole was found by Newman et al. (1965), although its connection to black holes was not realized until later (Shapiro and Teukolsky 1983, p. 338).
Rotating (Kerr) Black Holes, Charged and Uncharged
Most stars spin on an axis. In 1963, Roy Kerr reasoned that when rotating stars shrink, they would continue to rotate. Kip Thorne calculated that most black holes would rotate at a speed 99.8% of their mass. Unlike the static black holes, rotating black holes are oblate and spheroidal. The lines of constant distance here are ellipses, and lines of constant angle are hyperbolas.
Unlike static black holes, rotating black holes have two photon spheres. In a sense, this results in a more stable orbit of photons. The collapsing star “drags” the space around it into rotating with it, kind of like a whirlpool drags the water around it into rotating. As in the diagram above, there would be two different distances for photons. The outer sphere would be composed of photons orbiting in the opposite direction as the black hole. Photons in this sphere travel slower than the photons in the inner sphere. In a sense, since they are orbiting in the opposite direction, they have to deal with more resistance, hence they are “slowed down”. Similarly, photons in the inner ring travel faster since they are not going against the flow. It is because the photon sphere in agreement with the rotation can travel “faster” that it is on the inside. The closer one gets to the event horizon, the faster one has to travel to avoid falling into the singularity  hence the “slower” moving photons travel on the outer sphere to lessen the gravitational hold the black hole has.
The rotating black hole has an axis of rotation. This, however, is not spherically symmetric. The structure depends on the angle at which one approaches the black hole. If one approaches from the equator, then one would see the crosssection as in the diagram above, with two photon spheres. However, if one approached at angles to the equator, then one would only see a single photon sphere.
The position of the photon spheres also depend on the speed at which the black hole rotates. The faster the black hole rotates, the further apart the two photon spheres would be. For that matter, a black hole with a speed equal to its mass would have the greatest possible distance between the two photon spheres. This is because of greater difference in the speed between the photon spheres. As the speed of rotation increases, the outer sphere of photons would slow down as it meets greater resistance, even as the inner sphere would travel “faster” as it is pushed along by the centripetal forces.
Next, we move on to look at the ergosphere. The ergosphere is unique to the rotating black hole. Unlike the event horizon, the ergosphere is a region, and not a mathematical distance. It is a solid ellipsoid (or a 3dimensional ellipse). The ergosphere billows out from the black hole above the outer event horizon of a charged black hole (a.k.a. KerrNewman), and above the event horizon of an uncharged black hole (a.k.a. Kerr). This distance is known as the static limit of a rotating black hole. At this distance, it is no longer possible to stay still even if one travels at the speed of light. One would inevitably be drawn towards the singularity. The faster the rotation, the further out it billows. When the ergosphere’s radius is half the Schwarzschild radius along the axis of rotation, it experiences the greatest distance it can billow out. At this point, even light rays are dragged along in the direction of rotation. Strangely enough, it is postulated that one can enter and leave as one likes since technically, you have not hit the event horizon yet.
For a rotating black hole, the outer event horizon switches time and space as we know it. The inner event horizon, in turn, returns it to the way we know it. Singularity then becomes a place rather than a time, and can technically be avoided. When angular velocity increases, both the outer and the inner event horizon move closer together.
In the diagram, you would have noticed that the singularity here is drawn as a ring, and not a point, as it was for the static black hole. In the case of a rotating black hole, the gravity around the ringed singularity is repulsive. In other words, it actually pushes one away, allowing you to actually leave the black hole. The only way to approach the ring singularity would be to come in from the equatorial plane. Other trajectories would be repelled with greater strength, proportional to the closer the angle is to the axis of rotation.
In addition, there would be a third photon sphere about the ring singularity. If light is parallel to the axis of rotation, the gravity and the antigravity of the singularity are balanced out. Light then traces out the path of constant distance (which, in the case is an ellipsoid). Technically, this might lead the light into another universe through the singularity, and then back out again. At this point within the black hole, we may see three types of light: the light reflected from our universe behind us; the light from other universes; and the light from the singularity.
Beyond the Event Horizon
Of all a black hole’s bizarre characteristics, none seems stranger than the fact that the solutions to Einstein’s equations tell us that these holes in spacetime can serve as bridges into other universes. As fans of science fiction are well aware, a parallel universe is a universe entirely separate from our own. Among the many speculations as to the nature of these universes, is the idea that there could be parallel versions of ourselves inhabiting these universes; each living out a slightly different version of our lives. This idea doesn’t seem so irrational when viewed in relation to the equally strange world of quantum mechanics [10]. It is important to note, however, that the existence of these other universes is, at present, a purely theoretical construction.
Scientists often use a spacetime diagram to demonstrate graphically the
strange world of General Relativity (figure 5).
The future is located at the top of the diagram. All motion in space must travel within 45º of the vertical time line. Paths that are inclined greater than 45º are spacelike, faster than light trips. Accordingly, the zone below the 45º line is shaded gray and marked “forbidden”. Professor Roger Penrose of Oxford University has developed a special type of spacetime diagram that is very useful for representing the solutions of black hole equations [12]. These diagrams quickly show the black hole’s connection with parallel universes.
Figure 6 is a Penrose diagram of a simple Schwartzchild black hole. Upon first glance, it appears far more complex than the diagram in figure 5, yet it really isn’t. Just as before, all paths through space must be inclined at an angle less than 45º from the vertical axis. The singularity of the black hole, denoted by the row of shark’s teeth at the top, is at a 90º angle, hence it is spacelike. The event horizon’s one way nature is shown by the sharp bend in it’s line. The path of a traveler into the hole is shown by the curved line that passes through the event horizon. Two things stand out as unusual about this diagram: First there is an extra singularity in the past (at the bottom). Secondly, there is the extra universe on the left.
Figure 6: Penrose Diagram of Schwartzchild Black Hole [13].
The additional singularity, marked as past spacelike singularity on the diagram, is what is known as a white hole. Very simply put, a white hole is the opposite of a black hole. Instead of engulfing everything that comes near it, the white hole repels matter. Notice the direction of its event horizon. Some physicists maintain that the singularity of a black hole opens into another universe (figure 7). The idea behind a white hole is that matter that falls into a black hole in our universe is then belched out in another. It is worth noting, however, that astronomers have never observed a white hole, so their existence is doubted.
Figure 7: Black Hole Connected to Another Universe [15].
Figure 8 is a Penrose diagram of a Kerr black hole. It will be remembered that the spinning black hole exhibits several curious features, such as the ring singularity, the region of negative space, and the region through which travels into the past are possible. The ring singularity is denoted by the rounded off sharks teeth to show that it is a bit more forgiving than its nonrotating cousin. It should be obvious that the singularity is vertical (timelike). This means that one could escape from it with slower than light velocities. The area marked negative closed timelike loop is a region just inside the singularity. Very simply put, this is a region in which the normal barriers between past and future lose meaning. A traveler into this region could visit any place in his past or future, were it not for the one way nature of the event horizon. Just beyond the timelike loop region, lies the area of negative space. Unfortunately, this hole has not one, but two one way event horizons that would prevent a traveler from ever reentering our own universe. However, as shown in the diagram, he would have his choice of many other universes to visit. Figure 8 shows four (three parallel universes, in addition to our own), however, this diagram could be extended an infinite number of times in both the past and future directions. Two examples of a travelers path into the Kerr hole are shown in the diagram. Path “A” takes the traveler into the ring singularity, while path “B” shows his path into another universe.
Figure 8: Penrose Diagram of a Kerr Black Hole.
More general indepth information: Black Holes.
Developments in General Relativity: Black Hole Singularity and Beyond
Igor Novikov wrote:
At the 20th Texas Symposium on Relativistic Astrophysics there was a plenary talk devoted to the recent developments in classical Relativity. In that talk the problems of gravitational collapse, collisions of black holes, and of black holes as celestial bodies were discussed. But probably the problems of the internal structure of black holes are a real great challenge. In my talk I want to outline the recent achievements in our understanding of the nature of the singularity (and beyond!) inside a realistic rotating black hole. This presentation also addresses the following questions:
Can we see what happens inside a black hole?
Can a falling observer cross the singularity without being crushed?
An answer to these questions is probably “yes”.
Black Holes & Thermodynamics
RongGen Cai, LiMing Cao and DaWei Pang wrote:
Recently Gibbons et al. in hepth/0408217 defined a set of conserved quantities for KerrAdS black holes with the maximal number of rotation parameters in arbitrary dimension. This set of conserved quantities is defined with respect to a frame which is nonrotating at infinity. On the other hand, there is another set of conserved quantities for KerrAdS black holes, defined by Hawking et al. in hepth/9811056, which is measured relative to a frame rotating at infinity. Gibbons et al. explicitly showed that the quantities defined by them satisfy the first law of black hole thermodynamics, while those quantities defined by Hawking et al. do not obey the first law. In this paper we discuss thermodynamics of dual CFTs to the KerrAdS black holes by mapping the bulk thermodynamic quantities to the boundary of the AdS space. We find that thermodynamic quantities of dual CFTs satisfy the first law of thermodynamics and CardyVerlinde formula only when these thermodynamic quantities result from the set of bulk quantities given by Hawking et al. We discuss the implication of our results.