Astrophysics (Index)About

black hole

(BH)
(region of such high mass that light cannot escape)

A black hole is a region of space with such high mass that gravity allows nothing to escape, including electromagnetic radiation. General relativity's consequence that gravity bends light suggests that enough mass within a small enough area could bend nearby light to the point where it cannot escape. Such an "object" could have a very small mass if sufficiently concentrated (in which case the volume of from which no escape is possible would also be very small). The surface-shape delineating the volume from which light cannot escape is termed its event horizon. Since black holes lose their ability to interact via EMR, seeing into them is impossible and they can be fully characterized from our point of view by just a few aspects: their mass, rotation (angular momentum) and electric charge. The event horizon forms a sphere if the black hole has no rotation, and forms an ablated sphere according to the amount of rotation. Three types of black holes are generally assumed to exist:

Stellar black holes are thought to form from stars that have burned off sufficient fuel that their fusion no longer keeps them hot enough to maintain the pressure to counteract gravity, allowing the mass to collapse (gravitational collapse). Intermediate-mass black holes (IMBH, between stellar and supermassive, e.g., 100 to a million solar masses, sometimes referred to as a massive black hole or MBH) have also been theorized and observations have suggested their presence. A Planck hole is the smallest possible black hole according to quantum theory. It would be smaller than an atom but would have the mass of "a flea's egg", about 1/50000 gram. Hawking radiation, a theorized quantum phenomenon that would slowly dissolve black holes would instantly dissolve one that small.

Models for the formation of the largest black holes (SMBHs) that have been observed are a challenge, but there is no theoretical upper limit to the size of a black hole ignoring a means of forming it: conceivably the universe is a black hole in the process of formation, though current observations of the universe's expansion complicate such a theory.

Rotating black holes are more complicated, and virtually all black holes manufactured by astronomical events (e.g., core collapse supernovae) would rotate, at least a little. Models suggest a non-rotating black hole includes a point singularity (point where the equations governing normal space and mass reach zeros and infinities) at the center, but some models suggest a rotating black hole would have a disk-shaped singularity. Also, rotating black holes exhibit frame dragging, a rotation of space around them, and with sufficient black hole rotation, a layer of this dragged space can be traveling faster than light as compared to the surrounding space further out. This "faster than light" region is termed the ergosphere. (Such a region has been described as one in which a particle cannot stand still, and as far as I can understand, that's to say it is impossible for it to move fast enough, given the dragged frame it inhabits, to appear to be standing still in relation to the surrounding space further out.) The outer boundary of the ergosphere is termed the static limit or static surface.

The term black hole candidate (BHC) is used for observed astronomical objects under consideration as black holes, often X-ray source sources.


(physics,gravity,object type)
Further reading:
http://en.wikipedia.org/wiki/Black_hole

Referenced by pages:
accretion
accretion disk
accretion rate
advection dominated accretion flow (ADAF)
asymptotic giant branch (AGB)
active galactic nucleus (AGN)
alpha disk
broad emission line region
black hole accretion rate (BHAR)
black hole binary (BHB)
black hole merger
black hole model
binary star
Blandford-Znajek mechanism (BZ process)
Bondi radius
Blandford-Payne mechanism (BP process)
binary SMBH (BSMBH)
Chandra Deep Field South (CDFS)
Chandrasekhar limit
comoving units
compact object (CO)
Compton reflection
Compton scattering
computational astrophysics
cosmic string
direct collapse black hole (DCBH)
Eddington luminosity
Event Horizon Telescope (EHT)
electron degeneracy
extreme mass ratio inspiral (EMRI)
ergosphere
escape velocity (Ve)
event horizon (EH)
final parsec problem
47 Tucanae (47 Tuc)
galactic binary
galactic bulge
gas streamer
globular cluster (GC)
gravitational redshift
GRO J1655-40
gravitational wave (GW)
GW170817
GW detection (GW)
gravitational wave spectrum
hypermassive neutron star (HMNS)
innermost stable circular orbit (ISCO)
jet
jet current
law of cosmic censorship
light cone
LIGO
MACHO
mass ratio (μ)
microquasar
neutron star (NS)
NGC 3201
nova (N)
neutron star merger
Planck constant (h)
post-main-sequence star
relic
retrograde accretion
Salpeter timescale
Schwarzschild radius
Sloan Digital Sky Survey (SDSS)
Spitzer Extended Deep Survey (SEDS)
supermassive black hole (SMBH)
supernova remnant (SNR)
Soltan argument
SS 433
stellar-mass black hole
stellar evolution
stellar rotation
strong-field gravity
subgrid-scale physics
superradiance
transient
ultraluminous X-ray source (ULX)
X-ray burster (XRB)
X-ray source

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