The Rayleigh scattering and the blue sky

Why is the daytime sky blue?
We need to examine a type of scattering that affects photons from solar radiation when they interact with the molecules that make up the atmosphere, namely nitrogen and oxygen (99% of the components).
This is Rayleigh scattering (named after Nobel Prize winner John William Strutt Rayleigh, 1842-1919), which affects particles smaller than the wavelength of the incident radiation. It is an elastic scattering, so the wavelength of the same radiation is not changed.
We are dealing with photons, but the formula was developed on the basis of classical electromagnetic theory, not quantum theory (which was created after Rayleigh’s death).


Figure 1 – Angular dependence of Rayleigh Scattering
(copyright MLisandra, CC BY-SA 4.0, via Wikimedia Commons, here without the formula inscription)


For the explanation we are looking for, the Rayleigh scattering formula can be simplified as follows (see also Figure 1):
[1]    I ~ I₀ (1+cos²γ) / λ⁴
where  I  is the intensity of the scattered radiation,  I₀  is the intensity of the incident radiation with wavelength  λ ,  γ  is the scattering angle of the incident radiation.

We can immediately see that the angle where the intensity  [1]  is lowest is the right angle ( π/2 ), where the cosine is zero (see Figure 2), meaning that the sky is darkest (the blue is most intense) at an angle of 90° to the direction of the Sun.
Furthermore, the dependence on the inverse of the fourth power of  λ suggests that the effects for different wavelengths are significantly different. In fact, blue light is scattered much more than red light, which has a longer wavelength (see Figure 3), making the sky blue. Even shorter wavelengths, such as those of violet, are less intense at source and do not contribute significantly.
At dawn and dusk, blue light is highly scattered by the greater layer of atmosphere it passes through, together with yellow and green light, so red/orange light dominates.

In the case of smaller particles, the cross section and refractive index of the particle are considered, but even if atmospheric gas molecules are treated as point sources, in this case the effects depend on their polarizability due to incident radiation. Those who take photographs using a polarizing filter are familiar with this phenomenon: in fact, by adjusting the filter effect and therefore the polarization, the sky can even become completely black at 90° to the Sun, which can be creative but not very realistic!


Figure 2 – cosine function behaviour

cosine function

Figure 3 – visible band of radiation

visible band of radiation


See also Mie scattering and white clouds.

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Eddington luminosity and limits to stellar growth

The Eddington luminosity (Lₑ) (named after Arthur Stanley Eddington, 1882-1944), also known as the Eddington limit, is the growth limit of a structure that is in hydrostatic equilibrium (see Figure 1), balancing the outward radiation pressure with the inward gravitational pull.


Figure 1 – Hydrostatic equilibrium


The relationship for the luminosity limit can be easily derived, obtaining:
[1]    L ≤ 4π c G M / k = Lₑ
where  G  is the universal gravitational constant,  M  is the mass of the object,  c  is the speed of light, and  k  is the opacity (ability to absorb radiation) of the material that makes up the object.
As a function of solar parameters, in the case of the model consisting of ionized hydrogen, [1] can be expressed as:
[2]    Lₑ ≈ 3.2 * 10⁴ (M/M๏) L๏
where   M๏   and   L๏   are the mass and luminosity of the Sun.

In the very hot core of massive stars (or in accretion disks of black holes), opacity is independent of frequency and temperature, is related to Thomson scattering (see Thomson scattering on Wikipedia for more informations) of free electrons, and can be expressed as:
[3]    kₑₛ = σₜ nₑ / ρ
where σₜ is the Thomson cross section for electrons, nₑ is the number density of electrons, and  ρ  is the density of the medium.
To consider the more general case of models also consisting of helium and metals, the general relationship is expressed as a function of the mass fraction (X) of hydrogen, and the  [3] becomes:
[4]    kₑₛ = σₜ (1+X) / 2 mₚ ≈ 0.2 (1+X)    cm² / gr
where  mₚ  is the mass of the proton.
Therefore, in the case of a model consisting only of helium, Eddington luminosity would double (with   X=0 ,  [4]  is halved and  [1]  is doubled).
Relationships can also be derived for cases of models that are not fully ionized or colder (for less massive stars), or for highly energetic radiation (e.g., gamma rays as in black hole accretion disks), but these are beyond the scope of this note.

What is notable is that this physical limit explains why we do not observe infinitely large stars; beyond a certain mass limit, the luminosity is such that it disrupts the star.
The Eddington luminosity also defines the maximum rate at which a black hole can grow: if matter falls too quickly, the light emitted repels it back.

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Snell’s law and the causes of refraction

Let us recall Snell’s well-known law, which describes the phenomenon of refraction:
– a ray of light undergoes a deviation when it passes from one transparent medium to another with a different refractive index (see Figure 2).


Figure 1 – Snell law

 

Figure 2 – Refraction example


Mathematically (see Figure 1):
[1]    n’ sin(θ’) = n” sin(θ”)
where  n’ ,  n”  are the refractive indices of the two transparent media,  θ’ ,  θ”  are the angles of incidence and refraction (measured relative to normal at the interface between the media).
In other words, given two media, the ratio between the respective sines of the angles of incidence and refraction is constant.
A first proof can be obtained by applying Pierre de Fermat’s (1601-1665) principle of least time, namely that light follows the path that requires the least time to travel from one point to another. Attached below is the simple geometric-analytical proof (in italian):

pdf  Fermat_Snell_geometric-analytical demonstration

Okay, this relationship (perhaps already studied in the 10th century by the Persian mathematician Ibn Sahl) is certainly interesting, but what is the physical motivation for this constant quantity? It is necessary to identify where this regularity lies.
The reasons derive directly from Maxwell’s equations, the fundamental laws describing the interaction between electric and magnetic fields.
From these, it follows that the boundary conditions require that the tangential components of the electric field and magnetic field be continuous across the separation surface. Therefore, the phase of the incident, (reflected,) and transmitted wave must be the same along this boundary.

The assumption that the frequency ( ν ) of the incident light remains constant (i.e., that it is independent of the medium in which it propagates) can also be understood by considering that if this were not the case, it would lose coherence as it crossed the surface between the two media, probably transforming the image observed through the separation surface into a uniform grey color, which is not observed.
Furthermore, since the energy associated with incident photons is  E = h ν , where  h  is the Planck constant, the same conservation of energy tells us that the frequency cannot change.
Quantistic note: this consideration refers to a single photon, which would change color (towards red) if it lost energy (phenomenon that does not occur for all observed refracted photons). Considering a beam of photons, however, it may be that the second medium causes absorption of the incident light, thus a decrease in total energy, but this concerns the entire beam that absorbs some photons completely and not the individual photons.

Considering the wave vectors  k’  (incident) and  k”  (refracted) associated with their respective phases, and equating their projections on the separation interface, we obtain:
[2]     k’ sin(θ’) = k” sin(θ”)
but  k = ω / v  , where  ω  is the angular frequency of the electromagnetic wave of the incident light,  v  is the velocity in the medium, and defining the refractive index  n = c / v  (derived from the constants  ε₀  and  μ₀  of the medium using Maxwell’s equations, where  c =  1/√(ε₀ μ₀)  ), from  [2]  we finally obtain  [1] .

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An easy note on the chain rule in differential equations

The chain rule in differential equations is a small but powerful trick often used to derive composite functions by finding the derivative of the outer function while keeping the inner function unchanged.
For example, the expression  dy/dx  can be rewritten as:
[1]    dy/dx = dy/du * du/dx  .
In this way, we can obtain a derivative with respect to a variable that is more useful, for example because we know its value (possibly in a simpler formal expression, or already known), or is easier to integrate.
In simple terms, this means transforming the rate of change of  x  with respect to  y  into the product of the rate of change of  u  with respect to  y  and the rate of change of  x  with respect to  u .
Regarding rules for deriving functions, the chain rule leads to the proof that if  F(x) = f(g(x)) , its derivative is:
[2]    F'(x) = f'(g(x) * g'(x)  .

But while this rule for deriving functions is used every day without thinking about it, the chain rule can be a useful trick in solving many physics problems when we don’t know the direct rate of change between two variables.
A simple example of its use in astrophysics is in the study of star formation and Jeans’ Mass (the critical threshold required for a cloud of interstellar gas and dust to collapse under its own gravity to form stars). The chain rule is used to convert acceleration into a form that depends on position rather than time, making the differential equation integrable. In formal terms, as in  [1] , we can write:
[3]    d²R/dt² = dv/dt = dv/dR * dR/dt = v * dv/dR  ,
where  v = dR/dt  .
In this case, this substitution allows us to integrate the equation of motion with respect to radius  R  to determine the free-fall time of a collapsing gas cloud (off-topic calculation omitted).


collapsing gas cloud
Collapsing gas cloud(source accademiadellestelle.org)

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References for laymen: Archimedes’ hydrostatic principle

Archimedes of Syracuse (287-212) was perhaps one of humanity’s greatest mathematical geniuses. He is remembered for the principle of hydrostatic thrust, the screw pump, and war machines, but his most advanced studies were on conics and mathematical methods for calculating surfaces and volumes (e.g., of sphere). These are considered among the highest achievements of ancient science and, although they lack modern formal rigor, they represent the direct precursors of the concept of limits and integral calculus (independently developed by Sir Isaac Newton and Gottfried Wilhelm Leibniz in the late 17th century). See, for example, Lucio Russo, Archimedes: A Great Ancient Scientist (Carocci Editore, 2019).

One day, my young son asked me, “Why do ships that are heavy and made of iron float?” I couldn’t explain the density of water to him, but I found a good answer for a child: “Because they weigh less than the water they displace.”
This is exactly Archimedes’ principle of hydrostatic thrust, which in more complicated terms is expressed as: “A body immersed in a fluid experiences an upward thrust equal to the weight of the volume of fluid displaced.” So if this is greater than the weight of the body, it floats.

We can express Archimedes’ principle of hydrostatic thrust (force) F(A) using the following formula:
[1]    F(A) = m * g = ρ(fluid) * V(displaced) * g
where  m =  ρ *  V  is the mass,  g  is the acceleration due to gravity,  ρ  represents the density, and  V  represents the volume of fluid displaced by the body.
For this reason, any body also ‘weighs’ according to the density of the fluid in which it is immersed. The greater the density, the greater the hydrostatic thrust and the lower the weight of the body.

As an example, if an iron nail (which, due to its shape, does not seem to be able to float like a ship by displacing a lot of fluid) were placed in a container with liquid mercury, which has a density almost double that of iron, the nail would float at the level of the weight of mercury displaced. Calculations show that it would be immersed just over half its volume (about 58%).


In this video, we can see how an iron anvil floats in mercury because the density of iron (7.87 g/cm³) is almost half that of mercury (13.55 g/cm³) (source: Wonder of science on X channel).


Another famous example of buoyancy is that of hot air balloons: they float exactly like a ship because the volume of fluid (atmospheric air) they displace weighs more (is denser) than that contained in the balloon, which is heated with a burner (and is therefore less dense).


An hot air balloon (source: freedome.it)

mongolfiera

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Brief on Kramers’ Opacity Law in Stellar Astrophysics

In stellar astrophysics, opacity  ( k ) is a measure of a material’s resistance to the flow of radiative energy. One analytical descriptions of this phenomenon is Kramers’ opacity law, a power-law relation derived from atomic physics that characterizes how stellar matter interacts with radiation under specific thermodynamic conditions.

pdf  Brussi 2026_Brief on Kramers’ Opacity Law in Stellar Astrophysics

 

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Note for laymen – what is the dark matter?

Let’s consider a disc galaxy with billions of stars forming the disc, which rotates (the Andromeda galaxy in the photo, to give a well-known example). We can consider for each of these stars that the centripetal acceleration
[1]    a’ = v²/R
is equal to the gravitational acceleration
[2]    a” = G M/R²
therefore from  [1] = [2]  we obtain:
[3]    v = √(G M/R)
where  v  is the local velocity of the source considered,  R  is its distance from the galactic center,  G  is the gravitational constant,  M  is the total mass contained within the radius  R  (which determines the gravitational attraction).
Measuring the rotational velocities of galaxies is relatively easy, if they are not seen face on, and it is generally observed that throughout the disk the rotational velocities of the sources (stars but also gas clouds) are almost constant. Therefore, from relation  [3]  it follows that the mass  M  must increase in proportion to the radius  R , since  G  is a constant. Indeed, the mass contained within the radius  R  increases as  R  increases, but what is observed is not sufficient to justify the constant value of  v . These considerations leads to the hypothesis that there is a substance that is invisible and non-baryonic in nature (i.e., not made up of protons and neutrons, which are not detected) that manifests itself only through gravitational behavior, which is called dark matter.


Processed photograph of M31, Andromeda. It was not possible to obtain the author of this beautiful photograph.


Andromeda

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Ole Rømer and the finite speed of light

The first to observe that the propagation of light was not instantaneous was the astronomer Giovanni Domenico Cassini (1625-1712); the first to estimate its speed, in 1676, was the Danish astronomer Ole Christensen Rømer (1644-1710), both based their observations on the solar system.

pdf  Brussi 2026_Ole Rømer and the finite speed of light

 

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