Photoevaporation is the process where energetic radiation ionises gas and causes it to disperse away from the ionising source. The term is typically used in an astrophysical context where ultraviolet radiation from hot stars acts on clouds of material such as molecular clouds, protoplanetary disks, or planetary atmospheres.^[1][2][3]

One of the most obvious manifestations of astrophysical photoevaporation is seen in the eroding structures of molecular clouds that luminous stars are born within.^[4]

Evaporating Gaseous Globules or EGGs were first discovered in the Eagle Nebula. These small cometary globules are being photoevaporated by the stars in the nearby cluster. EGGs are places of ongoing star-formation.^[5]

A planet can be stripped of its atmosphere (or parts of the atmosphere) due to high energy photons and other electromagnetic radiation. If a photon interacts with an atmospheric molecule, the molecule is accelerated and its temperature increased. If sufficient energy is provided, the molecule or atom may reach the escape velocity of the planet and "evaporate" into space. The lower the mass number of the gas, the higher the velocity obtained by interaction with a photon. Thus hydrogen is the gas which is most prone to photoevaporation.

Photoevaporation is the likely cause of the small planet radius gap.^[6]

Examples of exoplanets with an evaporating atmosphere are HD 209458 b, HD 189733 b and Gliese 3470 b. Material from a possible evaporating planet around WD J0914+1914 might be responsible for the gaseous disk around this white dwarf.

Protoplanetary disks can be dispersed by stellar wind and heating due to incident electromagnetic radiation. The radiation interacts with matter and thus accelerates it outwards. This effect is only noticeable when there is sufficient radiation strength, such as coming from nearby O and B type stars or when the central protostar commences nuclear fusion.

The disk is composed of gas and dust. The gas, consisting mostly of light elements such as hydrogen and helium, is mainly affected by the effect, causing the ratio between dust and gas to increase.

Radiation from the central star excites particles in the accretion disk. The irradiation of the disk gives rise to a stability length scale known as the gravitational radius (${\displaystyle r_{g}}$). Outside of the gravitational radius, particles can become sufficiently excited to escape the gravity of the disk, and evaporate. After 10⁶ – 10⁷ years, the viscous accretion rates fall below the photoevaporation rates at ${\displaystyle r_{g}}$. A gap then opens around ${\displaystyle r_{g}}$, the inner disk drains onto the central star, or spreads to ${\displaystyle r_{g}}$ and evaporates. An inner hole extending to ${\displaystyle r_{g}}$ is produced. Once an inner hole forms, the outer disk is very rapidly cleared.

The formula for the gravitational radius of the disk is^[7]

${\displaystyle r_{g}={\frac {\left(\gamma -1\right)}{2\gamma }}{\frac {GM\mu }{k_{B}T}}\approx 2.15{\frac {\left(M/M_{\odot }\right)}{\left(T/10^{4}\ {\rm {K}}\right)}}\ {\rm {AU}},\!}$

where ${\displaystyle \gamma }$ is the ratio of specific heats (= 5/3 for a monatomic gas), ${\displaystyle G}$ the universal gravitational constant, ${\displaystyle M}$ the mass of the central star, ${\displaystyle M_{\odot }}$ the mass of the Sun, ${\displaystyle \mu }$ the mean weight of the gas, ${\displaystyle k_{B}}$ Boltzmann constant, ${\displaystyle T}$ is the temperature of the gas and AU the Astronomical Unit.

If we denote the coefficient in the above equation by the Greek letter ${\textstyle \kappa }$ then

         ${\displaystyle \kappa ={\frac {(\gamma -1)}{2\gamma }}={\frac {1}{(2+f)}}}$  ,                                           .                                                                    

where ${\textstyle f}$ is the number of degrees of freedom and we have used the formula: ${\textstyle \gamma =1+{\frac {2}{f}}}$.

For an atom, such as a hydrogen atom, then ${\textstyle f=3}$, because an atom can move in three different, orthogonal directions. Consequently, ${\textstyle \kappa =0.2}$. If the hydrogen atom is ionized, i.e., it is a proton, and is in a strong magnetic field then ${\textstyle f=2}$, because the proton can move along the magnetic field and rotate around the field lines. In this case, ${\textstyle \kappa =0.25}$. A diatomic molecule, e.g., a hydrogen molecule, has ${\textstyle f=5}$ and ${\textstyle \kappa =1/7\approx 0.143}$. For a non-linear triatomic molecule, such as water, ${\textstyle f=6}$ and ${\textstyle \kappa =0.125}$. If ${\textstyle f}$ becomes very large, then ${\textstyle \kappa }$ approaches zero. This is summarised in the Table 1 , where we see that different gases may have different gravitational radii.

Particle	${\textstyle f}$	${\textstyle \kappa }$
H+ in a B field	2	0.25
H	3	0.2
H2	5	~ 0.143
H2O	6	0.125
Limiting case	∞	0

Table 1: Gravitational radius coefficient as a function of the degrees of freedom.

Because of this effect, the presence of massive stars in a star-forming region is thought to have a great effect on planet formation from the disk around a young stellar object, though it is not yet clear if this effect decelerates or accelerates it.