quantity

flux

The rate of flow of a quantity, such as particles or energy, through a unit area.
21 related articles · 6 formulas

Description

Flux is a measure of how much of a quantity—particles, energy, fluid, or even a field—passes through a given area over time. It is a central concept in physics because it connects the microscopic motion of individual entities to the macroscopic behavior of systems. In the context of the provided titles, flux appears in diverse settings: the flow of blood carrying drugs through porous implants, the movement of cerebrospinal fluid in the brain, the transport of substances in porous media, and even the behavior of quantum vortices. In each case, flux quantifies the rate of transfer, making it essential for understanding how systems change and how materials or energy move from one place to another.

History

The concept of flux has roots in the work of Isaac Newton, who used the term 'fluxion' for derivatives, but the modern integral definition in physics was formalized in the 19th century, particularly through the work of James Clerk Maxwell in electromagnetism and later in fluid dynamics. The specific application to porous media was developed by Henry Darcy in 1856.

How it works

Flux is defined mathematically as the integral of a vector field over a surface. For a simple case, if a fluid flows with velocity v through a flat area A, the flux is the product of the component of velocity perpendicular to the area and the area itself: Φ = v·A·cos(θ), where θ is the angle between the flow direction and the normal to the surface. For more complex situations, such as flow through a porous medium or turbulent mixing, the flux is computed by summing contributions over infinitesimal surface elements, often using differential equations like Darcy's law or the Navier-Stokes equations.

In practice

Flux is used in designing drug delivery systems, such as porous implants that release medication at controlled rates, and in environmental engineering to model groundwater contamination and remediation. It is also fundamental in astrophysics for interpreting observations of radiation and particle flows from cosmic sources.

Fun fact

In the brain, the flux of cerebrospinal fluid is not constant—it pulses with each heartbeat, which helps distribute drugs more effectively through the brain tissue.

Concept graph →

Formulas

$$\Phi(E) = \Phi_0 \left(\frac{E}{E_0}\right)^{-\gamma}$$
Flux scales as a power of energy.
What is in the formula
\PhivariableFlux (e.g., particle or energy flux) — flux varies
EvariableEnergy — energy joule
\Phi_0variableNormalization constant (flux at E = E_0) — flux constant varies
E_0variableReference energy — energy joule
\gammavariableSpectral index (power-law exponent) — spectral index
$$E(B-V) = \frac{2.5}{k(\lambda_2) - k(\lambda_1)} \log_{10}\left( \frac{(F_{\lambda_1}/F_{\lambda_2})_{\text{obs}}}{(F_{\lambda_1}/F_{\lambda_2})_{\text{int}}} \right)$$
Corrects observed flux ratios for interstellar extinction using reddening curve.
What is in the formula
E(B-V)variableColor excess between B and V bands — color excess
k(λ)variableExtinction curve at wavelength λ — extinction curve
F_λvariableFlux at wavelength λ — flux watt per metre squared
λvariableWavelength — wavelength metre
log10operatorBase-10 logarithm — logarithm base 10
$$L = 4\pi D_L^2 F \cdot 10^{0.4 k(\lambda) E(B-V)}$$
Relates observed flux to intrinsic luminosity accounting for distance and extinction.
What is in the formula
LvariableIntrinsic luminosity — luminosity watt
D_LvariableLuminosity distance — photometric distance metre
FvariableObserved flux — flux watt per metre squared
k(λ)variableExtinction curve at wavelength λ — extinction curve
E(B-V)variableColor excess between B and V bands — color excess
πconstantRatio of a circle's circumference to its diameter — pi = 3.14159
$$f'_\lambda = f_\lambda \cdot 10^{-0.4 A_\lambda}$$
Starlight is dimmed by dust, with wavelength-dependent extinction.
What is in the formula
f'_λvariableobserved flux at wavelength λ after extinction — flux watt per square metre
f_λvariableintrinsic flux at wavelength λ before extinction — flux watt per square metre
A_λvariableextinction magnitude at wavelength λ — extinction magnitude
$$\Phi_{\text{eff}} \geq \Phi_{\text{min}}$$
Effective flux must exceed a minimum threshold value.
What is in the formula
Φ_effvariableeffective flux — flux weber
Φ_minvariableminimum threshold flux — flux weber
$$m = -2.5 \log_{10}(F) + \text{ZP}$$
Definition of astronomical magnitude from flux.
What is in the formula
mvariableapparent magnitude — magnitude
Fvariableflux — flux watt per square metre
ZPvariablezero point — zero point
log10operatorbase-10 logarithm — logarithm base 10

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