查看“︁雷乔杜里方程”︁的源代码

在[[广义相对论]]中，'''雷乔杜里方程'''（{{lang-en|'''Raychaudhuri equation'''}}），或'''朗道–雷乔杜里方程'''（{{lang-en|'''Landau–Raychaudhuri equation'''}}）<ref>Spacetime as a deformable solid, M. O. Tahim, R. R. Landim, and C. A. S. Almeida, {{arXiv|0705.4120v1}}.</ref>是描述邻近物质运动的基本方程。

它不仅是[[彭罗斯-霍金奇点定理]]和[[广义相对论的精确解]]研究的基本引理，还具有独特之处，即它指出[[引力]]应该是广义相对论中任意[[质能等价|质量-能量]]之间的普遍存在的吸引力，正如在[[万有引力定律|牛顿引力理论]]中那样。

这一方程由印度物理学家{{le|阿马尔·库马尔·雷乔杜里|Amal Kumar Raychaudhuri}}<ref>{{cite journal|title=Amal Kumar Raychaudhuri (1923–2005)|author=Dadhich, Naresh|url=http://www.ias.ac.in/currsci/aug102005/569.pdf|date=August 2005|journal=Current Science|volume=89|pages=569–570|access-date=2018-10-29|archive-date=2020-01-03|archive-url=https://web.archive.org/web/20200103170801/https://www.ias.ac.in/currsci/aug102005/569.pdf|dead-url=no}}</ref>和苏联物理学家[[列夫·朗道]]各自独立发现。<ref>''[[The large scale structure of space-time]]'' by [[Stephen W. Hawking]] and [[G. F. R. Ellis]], Cambridge University Press, 1973, p. 84, {{ISBN|0-521-09906-4}}.</ref>

== 数学表述 ==
考虑一个[[类时]]的单位[[矢量场]] <math>\vec{X}</math>（可理解为不相交的[[世界线]]的{{le|汇 (广义相对论)|Congruence (general relativity)|汇}}）, 雷乔杜里方程可写为

: <math>\dot{\theta} = - \frac{\theta^2}{3} - 2 \sigma^2 + 2 \omega^2 - {E[\vec{X}]^a}_a + {{\dot{X}^a}}_{;a}</math>

式中

: <math>\sigma^2 = \frac{1}{2} \sigma_{mn} \, \sigma^{mn}, \; \omega^2 = \frac{1}{2} \omega_{mn} \, \omega^{mn}</math>

是'''剪切张量'''

: <math>\sigma_{ab} = \theta_{ab} - \frac{1}{3} \, \theta \, h_{ab}</math>

和'''涡度张量'''

: <math>\omega_{ab} = {h^m}_a \, {h^n}_b X_{[m;n]}</math>

的二次不变量。这里

: <math>\theta_{ab} = {h^m}_a \, {h^n}_b X_{(m;n)}</math>

是'''扩张张量'''，<math>\theta</math>是它的[[迹 (线性代数)|迹]]，称为'''扩张标量'''。

: <math>h_{ab} = g_{ab} + X_a \, X_b</math>

是正交于<math>\vec{X}</math>的超平面上的'''投影张量'''。另外，圆点表示对[[固有时]]的微分。{{le|电引力张量|Electrogravitic tensor|潮汐张量}}<math>E[\vec{X}]_{ab}</math>的迹可写为

: <math>{E[\vec{X}]^a}_{a} = R_{mn} \, X^m \, X^n</math> +1

这个量有时也称为'''雷乔杜里标量'''。

<!-- == Intuitive significance ==

The expansion scalar measures the fractional rate at which the volume of a small ball of matter changes with respect to time as measured by a central comoving observer (and so it may take negative values). In other words, the above equation gives us the evolution equation for the expansion of the timelike congruence.  If the derivative (with respect to proper time) of this quantity turns out to be ''negative'' along some world line (after a certain event), then any expansion of a small ball of matter (whose center of mass follows the world line in question) must be followed by recollapse.  If not, continued expansion is possible.

The shear tensor measures any tendency of an initially spherical ball of matter to become distorted into an ellipsoidal shape.  The vorticity tensor measures any tendency of nearby world lines to twist about one another (if this happens, our small blob of matter is rotating, as happens to fluid elements in an ordinary fluid flow which exhibits nonzero vorticity).

The right hand side of Raychaudhuri's equation consists of two types of terms:

# terms which promote (re)-collapse
#* initially nonzero expansion scalar,
#* nonzero shearing,
#* positive trace of the tidal tensor; this is precisely the condition guaranteed by assuming the ''strong energy condition'', which holds for the most important types of solutions, such as physically reasonable [[fluid solution]]s),
# terms which oppose (re)-collapse
#* nonzero vorticity, corresponding to Newtonian [[centrifugal force]]s,
#* positive divergence of the acceleration vector (e.g., outward pointing acceleration due to a spherically symmetric explosion, or more prosaically, due to body forces on fluid elements in a ball of fluid held together by its own self-gravitation).

Usually one term will win out.  However, there are situations in which a balance can be achieved.  This balance may be:

* ''stable'': in the case of [[hydrostatic equilibrium]] of a ball of perfect fluid (e.g. in a model of a stellar interior), the expansion, shear, and vorticity all vanish, and a radial divergence in the acceleration vector (the necessary [[body force]] on each blob of fluid being provided by the pressure of surrounding fluid) counteracts the Raychaudhuri scalar, which for a perfect fluid is <math>E[\vec{X}]_{ab} = 4 \pi ( \mu + 3 p )</math>.  In Newtonian gravitation, the trace of the tidal tensor is <math>4 \pi \mu</math>; in general relativity, the tendency of pressure to oppose gravity is partially offset by this term, which under certain circumstances can become important.
* ''unstable'': for example, the world lines of the dust particles in the [[Gödel metric|Gödel solution]] have vanishing shear, expansion, and acceleration, but constant vorticity just balancing a constant Raychuadhuri scalar due to nonzero vacuum energy ("cosmological constant").

== Focusing theorem ==

Suppose the strong [[Energy conditions|energy condition]] holds in some region of our spacetime, and let <math>\vec{X}</math> be a timelike ''geodesic'' unit vector field with ''vanishing vorticity'', or equivalently, which is hypersurface orthogonal.  For example, this situation can arise in studying the world lines of the dust particles in cosmological models which are exact dust solutions of the Einstein field equation (provided that these world lines are not twisting about one another, in which case the congruence would have nonzero vorticity).

Then Raychaudhuri's equation becomes

: <math>\dot{\theta} = - \frac{\theta^2}{3} - 2 \sigma^2 - {E[\vec{X}]^a}_a</math>

Now the right hand side is always ''negative'', so even if the expansion scalar is initially positive (if our small ball of dust is initially increasing in volume), eventually it must become negative (our ball of dust must recollapse).

Indeed,  in this situation we have

: <math>\dot{\theta} \leq - \frac{\theta^2}{3}</math>

Integrating this inequality with respect to proper time <math>\tau</math> gives

: <math>\frac{1}{\theta} \geq \frac{1}{\theta_0} + \frac{\tau}{3}</math>

If the initial value <math>\theta_0</math> of the expansion scalar is negative, this means that our geodesics must converge in a [[Caustic (mathematics)|caustic]] (<math>\theta</math> goes to minus infinity) within a proper time of at most <math>-3/\theta_0</math> after the measurement of the initial value <math>\theta_0</math> of the expansion scalar.  This need not signal an encounter with a curvature singularity, but it does signal a breakdown in our mathematical description of the motion of the dust.

== Optical equations ==

There is also an optical (or null) version of Raychaudhuri's equation for null geodesic congruences.

: <math>\dot{\widehat{\theta}} = - \frac{1}{2}\widehat{\theta}^2 - 2 \widehat{\sigma}^2 + 2 \widehat{\omega}^2 - T_{\mu\nu} U^\mu U^\nu</math>.

Here, the hats indicate that the expansion, shear and vorticity are only with respect to the transverse directions.
When the vorticity is zero, then assuming the [[null energy condition]], caustics will form before the [[affine parameter]] reaches <math>2/\widehat{\theta}_0</math>.

=== Applications ===

The [[event horizon]] is defined as the boundary of the [[causal past]] of null infinity. Such boundaries are generated by null geodesics. The affine parameter goes to infinity as we approach null infinity, and no caustics form until then. So, the expansion of the event horizon has to be nonnegative. As the expansion gives the rate of change of the logarithm of the area density, this means the event horizon area can never go down, at least classically, assuming the null energy condition. -->

== 参见 ==
* {{le|汇 (广义相对论)|Congruence (general relativity)|汇}}
* [[引力奇点]]
* [[彭罗斯-霍金奇点定理]]

== 注释 ==
{{reflist}}

== 参考资料 ==
* {{cite book|title=A Relativist's Toolkit: The Mathematics of Black Hole Mechanics|url=https://archive.org/details/relativiststoolk0000pois|author=Poisson, Eric|publisher=[[Cambridge University Press]]|year=2004|isbn=0-521-83091-5|location=Cambridge}} See ''chapter 2'' for an excellent discussion of Raychaudhuri's equation for both timelike and null ''geodesics'', as well as the focusing theorem.
* {{cite book|title=Spacetime and Geometry: An Introduction to General Relativity|author=Carroll, Sean M.|publisher=[[Addison-Wesley]]|year=2004|isbn=0-8053-8732-3|location=San Francisco}} See ''appendix F''.
* {{cite book|title=Exact Solutions to Einstein's Field Equations (2nd ed.)|author2=Kramer, Dietrich|author3=MacCallum, Malcolm|author4=Hoenselaers, Cornelius|author5=Hertl, Eduard|publisher=Cambridge University Press|year=2003|isbn=0-521-46136-7|location=Cambridge|author1=Stephani, Hans}} See ''chapter 6'' for a very detailed introduction to geodesic congruences, including the general form of Raychaudhuri's equation.
* {{cite book|title=The Large Scale Structure of Space-Time|url=https://archive.org/details/largescalestruct0000hawk|author2=Ellis, G. F. R.|publisher=Cambridge University Press|year=1973|isbn=0-521-09906-4|location=Cambridge|author1=Hawking, Stephen|last-author-amp=yes}}  See ''section 4.1'' for a discussion of the general form of Raychaudhuri's equation.
* {{cite journal|title=Relativistic cosmology I.|author=Raychaudhuri, A. K.|journal=Phys. Rev.|issue=4|doi=10.1103/PhysRev.98.1123|year=1955|volume=98|pages=1123|bibcode=1955PhRv...98.1123R}}  Raychaudhuri's paper introducing his equation.
* {{cite journal|title=Kinematics of geodesic flows in stringy black hole backgrounds|journal=Phys. Rev. D|issue=12|doi=10.1103/PhysRevD.79.124004|year=2009|volume=79|pages=124004|arxiv=0809.3074|bibcode=2009PhRvD..79l4004D|author3=Kar, Sayan|author1=Dasgupta, Anirvan|author2=Nandan, Hemwati|last-author-amp=yes}} See ''section IV '' for derivation of the general form of Raychaudhuri equations for three kinematical quantities (namely expansion scalar, shear and rotation).
* {{cite journal|title=The Raychaudhuri equations: A Brief review|journal=[[Pramana (journal)|Pramana]]|doi=10.1007/s12043-007-0110-9|year=2007|volume=69|pages=49|arxiv=gr-qc/0611123|bibcode=2007Prama..69...49K|author1=Kar, Sayan|author2=SenGupta, Soumitra|last-author-amp=yes}} See for a review on Raychaudhuri equations.

== 外部链接 ==
* [http://math.ucr.edu/home/baez/einstein/ The Meaning of Einstein's Field Equation] {{Wayback|url=http://math.ucr.edu/home/baez/einstein/ |date=20210405021200 }} by John C. Baez and Emory F. Bunn.  Raychaudhuri's equation takes center stage in this well known (and highly recommended) semi-technical exposition of what Einstein's equation says.

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