 This article possibly contains original research. Please improve it by verifying the claims made and adding inline citations. Statements consisting only of original research may be removed. (May 2013) 
Hubble's law is the name for the observation in physical cosmology that: (1) objects observed in deep space (extragalactic space, ~10 megaparsecs or more) are found to have a Doppler shift interpretable as relative velocity away from the Earth; and (2) that this Dopplershiftmeasured velocity, of various galaxies receding from the Earth, is approximately proportional to their distance from the Earth for galaxies up to a few hundred megaparsecs away.
^{[1]}^{[2]} This is normally interpreted as a direct, physical observation of the expansion of the spatial volume of the observable universe.^{[3]}
The motion of astronomical objects due solely to this expansion is known as the Hubble flow.^{[4]} Hubble's law is considered the first observational basis for the expanding space paradigm and today serves as one of the pieces of evidence most often cited in support of the Big Bang model.
Although widely attributed to Edwin Hubble, the law was first derived from the General Relativity equations by Georges Lemaître in a 1927 article where he proposed that the Universe is expanding and suggested an estimated value of the rate of expansion, now called the Hubble constant.^{[5]}^{[6]}^{[7]}^{[8]}^{[9]}^{[10]} Two years later Edwin Hubble confirmed the existence of that law and determined a more accurate value for the constant that now bears his name.^{[11]} The recession velocity of the objects was inferred from their redshifts, many measured earlier by Vesto Slipher (1917) and related to velocity by him.^{[12]}
The law is often expressed by the equation v = H_{0}D, with H_{0} the constant of proportionality (the Hubble constant) between the "proper distance" D to a galaxy (which can change over time, unlike the comoving distance) and its velocity v (i.e. the derivative of proper distance with respect to cosmological time coordinate; see Uses of the proper distance for some discussion of the subtleties of this definition of 'velocity'). The SI unit of H_{0} is s^{−1} but it is most frequently quoted in (km/s)/Mpc, thus giving the speed in km/s of a galaxy 1 megaparsec (3.09×10^{19} km) away. The reciprocal of H_{0} is the Hubble time.
Observed values
Date published

Hubble constant (km/s)/Mpc

Observer

Citation

Remarks / methodology

20130321

67.80±0.77

Planck Mission

^{[13]}^{[14]}^{[15]}^{[16]}^{[17]}

The ESA Planck Surveyor was launched in May 2009. Over a fouryear period, it performed a significantly more detailed investigation of cosmic microwave radiation than earlier investigations using HEMT radiometers and bolometer technology to measure the CMB at a smaller scale than WMAP. On 21 March 2013, the Europeanled research team behind the Planck cosmology probe released the mission's data including a new CMB allsky map and their determination of the Hubble constant.

20121220

69.32±0.80

WMAP (9years)

^{[18]}


2010

70.4+1.3

WMAP (7years), combined with other measurements.

^{[19]}

These values arise from fitting a combination of WMAP and other cosmological data to the simplest version of the ΛCDM model. If the data are fit with more general versions, H_{0} tends to be smaller and more uncertain: typically around 67±4 (km/s)/Mpc although some models allow values near 63 (km/s)/Mpc.^{[20]}

2010

71.0±2.5

WMAP only (7years).

^{[19]}


200902

70.1±1.3

WMAP (5years). combined with other measurements.

^{[21]}


200902

71.9+2.6

WMAP only (5years)

^{[21]}


200608

77.6+14.9

Chandra Xray Observatory

^{[22]}


2007

70.4+1.5

WMAP (3years)

^{[23]}


200105

72±8

Hubble Space Telescope

^{[24]}

This project established the most precise optical determination, consistent with a measurement of H_{0} based upon SunyaevZel'dovich effect observations of many galaxy clusters having a similar accuracy.

prior to 1996

50–90 (est.)


^{[25]}


1958

75 (est.)

Allan Sandage

^{[26]}

This was the first good estimate of H_{0}, but it would be decades before a consensus was achieved.

Discovery
A decade before Hubble made his observations, a number of physicists and mathematicians had established a consistent theory of the relationship between space and time by using Einstein's field equations of general relativity. Applying the most general principles to the nature of the universe yielded a dynamic solution that conflicted with the thenprevailing notion of a static universe.
FLRW equations
In 1922, Alexander Friedmann derived his Friedmann equations from Einstein's field equations, showing that the universe might expand at a rate calculable by the equations.^{[27]} The parameter used by Friedmann is known today as the scale factor which can be considered as a scale invariant form of the proportionality constant of Hubble's law. Georges Lemaître independently found a similar solution in 1927. The Friedmann equations are derived by inserting the metric for a homogeneous and isotropic universe into Einstein's field equations for a fluid with a given density and pressure. This idea of an expanding spacetime would eventually lead to the Big Bang and Steady State theories of cosmology.
Shape of the universe
Before the advent of modern cosmology, there was considerable talk about the size and shape of the universe. In 1920, the famous ShapleyCurtis debate took place between Harlow Shapley and Heber D. Curtis over this issue. Shapley argued for a small universe the size of the Milky Way galaxy and Curtis argued that the universe was much larger. The issue was resolved in the coming decade with Hubble's improved observations.
Cepheid variable stars outside of the Milky Way
Edwin Hubble did most of his professional astronomical observing work at Mount Wilson Observatory, the world's most powerful telescope at the time. His observations of Cepheid variable stars in spiral nebulae enabled him to calculate the distances to these objects. Surprisingly, these objects were discovered to be at distances which placed them well outside the Milky Way. They continued to be called "nebulae" and it was only gradually that the term "galaxies" took over.
Combining redshifts with distance measurements
The parameters that appear in Hubble’s law: velocities and distances, are not directly measured. In reality we determine, say, a supernova brightness, which provides information about its distance, and the redshift z = ∆λ/λ of its spectrum of radiation. Hubble correlated brightness and parameter z.
Combining his measurements of galaxy distances with Vesto Slipher and Milton Humason's measurements of the redshifts associated with the galaxies, Hubble discovered a rough proportionality between redshift of an object and its distance. Though there was considerable scatter (now known to be caused by peculiar velocities – the 'Hubble flow' is used to refer to the region of space far enough out that the recession velocity is larger than local peculiar velocities), Hubble was able to plot a trend line from the 46 galaxies he studied and obtain a value for the Hubble constant of 500 km/s/Mpc (much higher than the currently accepted value due to errors in his distance calibrations). (See cosmic distance ladder for details.)
At the time of discovery and development of Hubble's law it was acceptable to explain redshift phenomenon as a Doppler shift in the context of special relativity, and use the Doppler formula to associate redshift z with velocity. Today the velocitydistance relationship of Hubble's law is viewed as a theoretical result with velocity to be connected with observed redshift not by the Doppler effect, but by a cosmological model relating recessional velocity to the expansion of the universe. Even for small z the velocity entering the Hubble law is no longer interpreted as a Doppler effect, although at small z the velocityredshift relation for both interpretations is the same.
Hubble Diagram
Hubble's law can be easily depicted in a "Hubble Diagram" in which the velocity (assumed approximately proportional to the redshift) of an object is plotted with respect to its distance from the observer.^{[30]} A straight line of positive slope on this diagram is the visual depiction of Hubble's law.
Cosmological constant abandoned
After Hubble's discovery was published, Albert Einstein abandoned his work on the cosmological constant, which he had designed to modify his equations of general relativity, to allow them to produce a static solution which, in their simplest form, model either an expanding or contracting universe.^{[31]} After Hubble's discovery that the Universe was, in fact, expanding, Einstein called his faulty assumption that the Universe is static his "biggest mistake".^{[31]} On its own, general relativity could predict the expansion of the universe, which (through observations such as the bending of light by large masses, or the precession of the orbit of Mercury) could be experimentally observed and compared to his theoretical calculations using particular solutions of the equations he had originally formulated.
In 1931, Einstein made a trip to Mount Wilson to thank Hubble for providing the observational basis for modern cosmology.^{[32]}
The cosmological constant has regained attention in recent decades as a hypothesis for dark energy.^{[33]}
Interpretation
The discovery of the linear relationship between redshift and distance, coupled with a supposed linear relation between recessional velocity and redshift, yields a straightforward mathematical expression for Hubble's Law as follows:
 $v\; =\; H\_0\; \backslash ,\; D$
where
 $v$ is the recessional velocity, typically expressed in km/s.
 H_{0} is Hubble's constant and corresponds to the value of $H$ (often termed the Hubble parameter which is a value that is time dependent and which can be expressed in terms of the scale factor) in the Friedmann equations taken at the time of observation denoted by the subscript 0. This value is the same throughout the universe for a given comoving time.
 $D$ is the proper distance (which can change over time, unlike the comoving distance which is constant) from the galaxy to the observer, measured in mega parsecs (Mpc), in the 3space defined by given cosmological time. (Recession velocity is just v = dD/dt).
Hubble's law is considered a fundamental relation between recessional velocity and distance. However, the relation between recessional velocity and redshift depends on the cosmological model adopted, and is not established except for small redshifts.
For distances D larger than the radius of the Hubble sphere r_{HS} , objects recede at a rate faster than the speed of light (See Uses of the proper distance for a discussion of the significance of this):
 $r\_\{HS\}\; =\; \backslash frac\{c\}\{H\_0\}\; \backslash \; .$
Since the Hubble "constant" is a constant only in space, not in time, the radius of the Hubble sphere may increase or decrease over various time intervals. The subscript '0' indicates the value of the Hubble constant today.^{[28]} Current evidence suggests the expansion of the universe is accelerating (see Accelerating universe), meaning that for any given galaxy, the recession velocity dD/dt is increasing over time as the galaxy moves to greater and greater distances; however, the Hubble parameter is actually thought to be decreasing with time, meaning that if we were to look at some fixed distance D and watch a series of different galaxies pass that distance, later galaxies would pass that distance at a smaller velocity than earlier ones.^{[35]}
Redshift velocity and recessional velocity
Redshift can be measured by determining the wavelength of a known transition, such as hydrogen αlines for distant quasars, and finding the fractional shift compared to a stationary reference. Thus redshift is a quantity unambiguous for experimental observation. The relation of redshift to recessional velocity is another matter. For an extensive discussion, see Harrison.^{[36]}
Redshift velocity
The redshift z often is described as a redshift velocity, which is the recessional velocity that would produce the same redshift if it were caused by a linear Doppler effect (which, however, is not the case, as the shift is caused in part by a cosmological expansion of space, and because the velocities involved are too large to use a nonrelativistic formula for Doppler shift). This redshift velocity can easily exceed the speed of light.^{[37]} In other words, to determine the redshift velocity v_{rs}, the relation:
 $v\_\{rs\}\; \backslash equiv\; cz\; \backslash \; ,$
is used.^{[38]}^{[39]} That is, there is no fundamental difference between redshift velocity and redshift: they are rigidly proportional, and not related by any theoretical reasoning. The motivation behind the "redshift velocity" terminology is that the redshift velocity agrees with the velocity from a lowvelocity simplification of the socalled FizeauDoppler formula^{[40]}
 $z\; =\; \backslash frac\{\backslash lambda\_o\}\{\backslash lambda\_e\}1\; =\; \backslash sqrt\{\backslash frac\{1+v/c\}\{1v/c\}\}1\; \backslash approx\; \backslash frac\{v\}\{c\}\; \backslash \; .$
Here, λ_{o}, λ_{e} are the observed and emitted wavelengths respectively. The "redshift velocity" v_{rs} is not so simply related to real velocity at larger velocities, however, and this terminology leads to confusion if interpreted as a real velocity. Next, the connection between redshift or redshift velocity and recessional velocity is discussed. This discussion is based on Sartori.^{[41]}
Recessional velocity
Suppose R(t) is called the scale factor of the universe, and increases as the universe expands in a manner that depends upon the cosmological model selected. Its meaning is that all measured distances D(t) between comoving points increase proportionally to R. (The comoving points are not moving relative to each other except as a result of the expansion of space.) In other words:
 $\backslash frac\; \{D(t)\}\{D(t\_0)\}\; =\; \backslash frac\; \{R(t)\}\{R(t\_0)\}\; \backslash \; ,$
where t_{0} is some reference time. If light is emitted from a galaxy at time t_{e} and received by us at t_{0}, it is red shifted due to the expansion of space, and this redshift z is simply:
 $z\; =\; \backslash frac\; \{R(t\_0)\}\{R(t\_e)\}\; \; 1\; \backslash \; .$
Suppose a galaxy is at distance D, and this distance changes with time at a rate d_{t}D . We call this rate of recession the "recession velocity" v_{r}:
 $v\_r\; =\; d\_tD\; =\; \backslash frac\; \{d\_tR\}\{R\}\; D\; \backslash \; .$
We now define the Hubble constant as
 $H\; \backslash equiv\; \backslash frac\; \{d\_tR\}\{R\}\; \backslash \; ,$
and discover the Hubble law:
 $v\_r\; =\; H\; D\; \backslash \; .$
From this perspective, Hubble's law is a fundamental relation between (i) the recessional velocity contributed by the expansion of space and (ii) the distance to an object; the connection between redshift and distance is a crutch used to connect Hubble's law with observations. This law can be related to redshift z approximately by making a Taylor series expansion:
 $z\; =\; \backslash frac\; \{R(t\_0)\}\{R(t\_e)\}\; \; 1\; \backslash approx\; \backslash frac\; \{R(t\_0)\}\; \{R(t\_0)\backslash left(1+(t\_et\_0)H(t\_0)\backslash right)\}1\; \backslash approx\; (t\_0t\_e)H(t\_0)\; \backslash \; ,$
If the distance is not too large, all other complications of the model become small corrections and the time interval is simply the distance divided by the speed of light:
 $z\; \backslash approx\; (t\_0t\_e)H(t\_0)\; \backslash approx\; \backslash frac\; \{D\}\{c\}\; H(t\_0)\; \backslash \; ,$ or $cz\; \backslash approx\; D\; H(t\_0)\; =\; v\_r\; \backslash \; .$
According to this approach, the relation cz = v_{r} is an approximation valid at low redshifts, to be replaced by a relation at large redshifts that is modeldependent. See velocityredshift figure.
Observability of parameters
Strictly speaking, neither v nor D in the formula are directly observable, because they are properties now of a galaxy, whereas our observations refer to the galaxy in the past, at the time that the light we currently see left it.
For relatively nearby galaxies (redshift z much less than unity), v and D will not have changed much, and v can be estimated using the formula $v\; =\; zc$ where c is the speed of light. This gives the empirical relation found by Hubble.
For distant galaxies, v (or D) cannot be calculated from z without specifying a detailed model for how H changes with time. The redshift is not even directly related to the recession velocity at the time the light set out, but it does have a simple interpretation: (1+z) is the factor by which the universe has expanded while the photon was travelling towards the observer.
Expansion velocity vs relative velocity
In using Hubble's law to determine distances, only the velocity due to the expansion of the universe can be used. Since gravitationally interacting galaxies move relative to each other independent of the expansion of the universe, these relative velocities, called peculiar velocities, need to be accounted for in the application of Hubble's law.
The Finger of God effect is one result of this phenomenon. In systems that are gravitationally bound, such as galaxies or our planetary system, the expansion of space is a much weaker effect than the attractive force of gravity.
Idealized Hubble's Law
The mathematical derivation of an idealized Hubble's Law for a uniformly expanding universe is a fairly elementary theorem of geometry in 3dimensional Cartesian/Newtonian coordinate space, which, considered as a metric space, is entirely homogeneous and isotropic (properties do not vary with location or direction). Simply stated the theorem is this:
 Any two points which are moving away from the origin, each along straight lines and with speed proportional to distance from the origin, will be moving away from each other with a speed proportional to their distance apart.
In fact this applies to nonCartesian spaces as long as they are locally homogeneous and isotropic; specifically to the negatively and positivelycurved spaces frequently considered as cosmological models (see shape of the universe).
An observation stemming from this theorem is that seeing objects recede from us on Earth is not an indication that Earth is near to a center from which the expansion is occurring, but rather that every observer in an expanding universe will see objects receding from them.
Ultimate fate and age of the universe
The value of the Hubble parameter changes over time either increasing or decreasing depending on the sign of the socalled deceleration parameter $q$ which is defined by
 $q\; =\; \backslash left(1+\backslash frac\{\backslash dot\; H\}\{H^2\}\backslash right).$
In a universe with a deceleration parameter equal to zero, it follows that H = 1/t, where t is the time since the Big Bang. A nonzero, timedependent value of $q$ simply requires integration of the Friedmann equations backwards from the present time to the time when the comoving horizon size was zero.
It was long thought that q was positive, indicating that the expansion is slowing down due to gravitational attraction. This would imply an age of the universe less than 1/H (which is about 14 billion years). For instance, a value for q of 1/2 (once favoured by most theorists) would give the age of the universe as 2/(3H). The discovery in 1998 that q is apparently negative means that the universe could actually be older than 1/H. However, estimates of the age of the universe are very close to 1/H.
Olbers' paradox
The expansion of space summarized by the Big Bang interpretation of Hubble's Law is relevant to the old conundrum known as Olbers' paradox: if the universe were infinite, static, and filled with a uniform distribution of stars, then every line of sight in the sky would end on a star, and the sky would be as bright as the surface of a star. However, the night sky is largely dark. Since the 17th century, astronomers and other thinkers have proposed many possible ways to resolve this paradox, but the currently accepted resolution depends in part upon the Big Bang theory and in part upon the Hubble expansion. In a universe that exists for a finite amount of time, only the light of finitely many stars has had a chance to reach us yet, and the paradox is resolved. Additionally, in an expanding universe distant objects recede from us, which causes the light emanating from them to be redshifted and diminished in brightness.^{[42]}
Dimensionless Hubble parameter
Instead of working with Hubble's constant, a common practice is to introduce the dimensionless Hubble parameter, usually denoted by h, and to write the Hubble's parameter H_{0} as 100 h km s ^{−1} Mpc^{−1}, all the uncertainty relative of the value of H_{0} being then relegated on h.^{[43]}
Determining the Hubble constant
The value of the Hubble constant is estimated by measuring the redshift of distant galaxies and then determining the distances to the same galaxies (by some other method than Hubble's law). Uncertainties in the physical assumptions used to determine these distances have caused varying estimates of the Hubble constant.
Earlier measurement and discussion approaches
For most of the second half of the 20th century the value of $H\_0$ was estimated to be between 50 and 90 (km/s)/Mpc.
The value of the Hubble constant was the topic of a long and rather bitter controversy between Gérard de Vaucouleurs who claimed the value was around 100 and Allan Sandage who claimed the value was near 50.^{[25]} In 1996, a debate moderated by John Bahcall between Gustav Tammann and Sidney van den Bergh was held in similar fashion to the earlier ShapleyCurtis debate over these two competing values.
This previously wide variance in estimates was partially resolved with the introduction of the ΛCDM model of the universe in the late 1990s. With the ΛCDM model observations of highredshift clusters at Xray and microwave wavelengths using the SunyaevZel'dovich effect, measurements of anisotropies in the cosmic microwave background radiation, and optical surveys all gave a value of around 70 for the constant.
The consistency of the measurements from all these methods lends support to both the measured value of $H\_0$ and the ΛCDM model.
See table of measurements above for many recent and older measurements.
Acceleration of the expansion
A value for $q$ measured from standard candle observations of Type Ia supernovae, which was determined in 1998 to be negative, surprised many astronomers with the implication that the expansion of the universe is currently "accelerating"^{[44]} (although the Hubble factor is still decreasing with time, as mentioned above in the Interpretation section; see the articles on dark energy and the ΛCDM model).
Derivation of the Hubble parameter
Start with the Friedmann equation:
 $H^2\; \backslash equiv\; \backslash left(\backslash frac\{\backslash dot\{a\}\}\{a\}\backslash right)^2\; =\; \backslash frac\{8\; \backslash pi\; G\}\{3\}\backslash rho\; \; \backslash frac\{kc^2\}\{a^2\}+\; \backslash frac\{\backslash Lambda\; c^2\}\{3\},$
where $H$ is the Hubble parameter, $a$ is the scale factor, G is the gravitational constant, $k$ is the normalised spatial curvature of the universe and equal to −1, 0, or +1, and $\backslash Lambda$ is the cosmological constant.
Matterdominated universe (with a cosmological constant)
If the universe is matterdominated, then the mass density of the universe $\backslash rho$ can just be taken to include matter so
 $\backslash rho\; =\; \backslash rho\_m(a)\; =\; \backslash frac\{\backslash rho\_\{m\_\{0\}\}\}\{a^3\},$
where $\backslash rho\_\{m\_\{0\}\}$ is the density of matter today. We know for nonrelativistic particles that their mass density decreases proportional to the inverse volume of the universe so the equation above must be true. We can also define (see density parameter for $\backslash Omega\_m$)
 $\backslash rho\_c\; =\; \backslash frac\{3\; H^2\}\{8\; \backslash pi\; G\};$
 $\backslash Omega\_m\; \backslash equiv\; \backslash frac\{\backslash rho\_\{m\_\{0\}\}\}\{\backslash rho\_c\}\; =\; \backslash frac\{8\; \backslash pi\; G\}\{3\; H\_0^2\}\backslash rho\_\{m\_\{0\}\};$
so $\backslash rho=\backslash rho\_c\; \backslash Omega\_m\; /a^3.$ Also, by definition,
 $\backslash Omega\_k\; \backslash equiv\; \backslash frac\{kc^2\}\{(a\_0H\_0)^2\}$
and
 $\backslash Omega\_\{\backslash Lambda\}\; \backslash equiv\; \backslash frac\{\backslash Lambda\; c^2\}\{3H\_0^2\},$
where the subscript nought refers to the values today, and $a\_0=1$. Substituting all of this in into the Friedmann equation at the start of this section and replacing $a$ with $a=1/(1+z)$ gives
 $H^2(z)=\; H\_0^2\; \backslash left(\; \backslash Omega\_M\; (1+z)^\{3\}\; +\; \backslash Omega\_k\; (1+z)^\{2\}\; +\; \backslash Omega\_\{\backslash Lambda\}\; \backslash right).$
Matter and dark energydominated universe
If the universe is both matterdominated and dark energy dominated, then the above equation for the Hubble parameter will also be a function of the equation of state of dark energy. So now:
 $\backslash rho\; =\; \backslash rho\_m\; (a)+\backslash rho\_\{de\}(a),$
where $\backslash rho\_\{de\}$ is the mass density of the dark energy. By definition an equation of state in cosmology is $P=w\backslash rho\; c^2$, and if we substitute this into the fluid equation, which describes how the mass density of the universe evolves with time,
 $\backslash dot\{\backslash rho\}+3\backslash frac\{\backslash dot\{a\}\}\{a\}\backslash left(\backslash rho+\backslash frac\{P\}\{c^2\}\backslash right)=0;$
 $\backslash frac\{d\backslash rho\}\{\backslash rho\}=3\backslash frac\{da\}\{a\}\backslash left(1+w\backslash right).$
If w is constant,
 $\backslash ln\{\backslash rho\}=3\backslash left(1+w\backslash right)\backslash ln\{a\};$
 $\backslash rho=a^\{3\backslash left(1+w\backslash right)\}.$
Therefore for dark energy with a constant equation of state w, $\backslash rho\_\{de\}(a)=\; \backslash rho\_\{de0\}a^\{3\backslash left(1+w\backslash right)\}$. If we substitute this into the Friedman equation in a similar way as before, but this time set $k=0$ which is assuming we live in a spatially flat universe, (see Shape of the Universe)
 $H^2(z)=\; H\_0^2\; \backslash left(\; \backslash Omega\_M\; (1+z)^\{3\}\; +\; \backslash Omega\_\{de\}(1+z)^\{3\backslash left(1+w\; \backslash right)\}\; \backslash right).$
If dark energy does not have a constant equationofstate w, then
 $\backslash rho\_\{de\}(a)=\; \backslash rho\_\{de0\}e^\{3\backslash int\backslash frac\{da\}\{a\}\backslash left(1+w(a)\backslash right)\},$
and to solve this we must parametrize $w(a)$, for example if $w(a)=w\_0+w\_a(1a)$, giving
 $H^2(z)=\; H\_0^2\; \backslash left(\; \backslash Omega\_M\; a^\{3\}\; +\; \backslash Omega\_\{de\}a^\{3\backslash left(1+w\_0\; +w\_a\; \backslash right)\}e^\{3w\_a(1a)\}\; \backslash right).$
Other ingredients have been formulated recently.^{[45]}^{[46]}^{[47]} In certain era, where the high energy experiments seem to have a reliable access in analyzing the property of the matter dominating the background geometry, with this era we mean the quarkgluon plasma, the transport properties have been taken into consideration. Therefore, the evolution of the Hubble parameter and of other essential cosmological parameters, in such a background are found to be considerably (nonnegligibly) different than their evolution in an ideal, gaseous, nonviscous background.
Units derived from the Hubble constant
Hubble time
The Hubble constant H_{0} has units of inverse time, i.e. H_{0} ≈ 2.3×10^{} s^{−1}. "Hubble time" is defined as 1/H_{0}. The value of Hubble time in the standard cosmological model is 4.35×10^{17} s or 13.8 billion years. (Liddle 2003, p. 57) The phrase "expansion timescale" means "Hubble time".
The Hubble unit is defined as hH_{0}, where h is around 1, and denotes the uncertainty in H_{0}. H_{0} is 100 km/s / Mpc = 1 dm/s/pc. The unit of time, then has as many seconds as there are decimetres in a parsec.
As mentioned above, H_{0} is the current value of Hubble parameter H. In a model in which speeds are constant, H decreases with time. In the naive model where H is constant the Hubble time would be the time taken for the universe to increase in size by a factor of e (because the solution of dx/dt = xH_{0} is x = s_{0}exp(H_{0}t), where s_{0} is the size of some feature at some arbitrary initial condition t = 0).
Over long periods of time the dynamics are complicated by general relativity, dark energy, inflation, etc., as explained above.
Hubble length
The Hubble length or Hubble distance is a unit of distance in cosmology, defined as cH_{0}^{1}—the speed of light multiplied by the Hubble time. It is equivalent to 4,228 million parsecs or 13.8 billion light years. (The numerical value of the Hubble length in light years is, by definition, equal to that of the Hubble time in years.) The Hubble distance would be the distance at which galaxies are currently receding from us at the speed of light, as can be seen by substituting D = c/H_{0} into the equation for Hubble's law, v = H_{0}D.
Hubble volume
Main article:
Hubble volume
The Hubble volume is sometimes defined as a volume of the universe with a comoving size of cH_{0}. The exact definition varies: it is sometimes defined as the volume of a sphere with radius cH_{0}, or alternatively, a cube of side cH_{0}. Some cosmologists even use the term Hubble volume to refer to the volume of the observable universe, although this has a radius approximately three times larger.
See also
Notes
References
Further reading
External links
 The Hubble Key Project
 The Hubble Diagram Project

 Hubble's quantum law.
This article was sourced from Creative Commons AttributionShareAlike License; additional terms may apply. World Heritage Encyclopedia content is assembled from numerous content providers, Open Access Publishing, and in compliance with The Fair Access to Science and Technology Research Act (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S. National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National Institutes of Health (NIH), U.S. Department of Health & Human Services, and USA.gov, which sources content from all federal, state, local, tribal, and territorial government publication portals (.gov, .mil, .edu). Funding for USA.gov and content contributors is made possible from the U.S. Congress, EGovernment Act of 2002.
Crowd sourced content that is contributed to World Heritage Encyclopedia is peer reviewed and edited by our editorial staff to ensure quality scholarly research articles.
By using this site, you agree to the Terms of Use and Privacy Policy. World Heritage Encyclopedia™ is a registered trademark of the World Public Library Association, a nonprofit organization.