Space Radiation

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Space is trying to kill you. It tries to kill you in many different ways. One of those ways is to flood itself with dangerous radiation that can kill biological organisms, damage or disable electronics, and degrade some kinds of materials.

Galactic Cosmic Rays

Cosmic flux versus particle energy at the top of Earth's atmosphere.

Space is filled with energetic charged particles – primarily protons (~90%) and alpha particles (~9%) but also including other light and medium ions. These are not associated with any immediate stellar environment but instead are thought to come from outside of our solar system, originating in supernovas, neutron stars, active galactic nuclei, quasars, and gamma ray bursts.

These cosmic rays generally have much higher energies than other forms of space radiation. A typical energy common to one of these particles would be around several hundred MeV to a GeV. Some have lower energies; these are often shielded from solar systems or planets by the sun's magnetic field, the solar wind, or planetary magnetospheres. More notorious, however, are those with higher energies. Often much higher. The most energetic cosmic ray ever measured (as of 2024) had an energy of $3.2\times 10^{20}$ eV, or around 50 joules – the energy of a major league baseball pitch in a single particle.

High energy massive particles, such as these cosmic rays, will have a high gyroradius, so they will not be strongly deflected by magnetic fields. Consequently, more energetic cosmic rays can pierce a planets magnetosphere to deliver radiation dose to those in orbit. Lower energy cosmic rays can be deflected by either magnetic fields that cover a very large amount of space (such as those around planets) or magnetic fields with a very high field strength.

Cosmic rays come through at a steady sleet, delivering on the order of 1 – 2.5 mSv/day. This dose is not delivered fast enough to cause acute radiation sickness, but is roughly two orders of magnitude higher than the natural background radiation dose on Earth. This can cause issues with chronic radiation exposure. The main concern is an increased risk of cancer. However, experiments on rodents exposed to radiation from a particle beam simulating long duration exposure to cosmic radiation also suggests the possibility of reduced cognitive function after several months in deep space. The cosmic ray dose rate is lower in times of high solar activity as the increased solar wind prevents more cosmic rays from entering our solar system. A planetary magnetosphere like that of Earth can deflect enough of the lower energy cosmic rays to make a noticeable difference in the dose rate, often in the 0.2 – 1 mSv/day range in low orbits below the main radiation belts, although this depends strongly on the latitudes through which the satellite passes. Equatorial orbits offer the best protection, and polar orbits pass through the radiation belts where the cosmic rays are deflected to. A significant amount of this shielding is also afforded by the planet itself, which will block cosmic rays from close to half the sky for close orbits.

Cosmic rays passing through a computer chip can cause transient errors that can result in a glitch in operations or a corrupted bit of memory. High doses of radiation can also cause permanent damage to elctronics.

Shielding Against Cosmic Rays

Because they can have such a high energy, cosmic rays can be difficult to shield against. A typical cosmic ray will pass through several tens of centimeters of solid or liquid matter before striking an atomic nucleus. The cosmic ray has so much energy that this shatters the nucleus, sending nuclear fragments spraying through the material and possibly (depending on the cosmic ray's energy) creating exotic particles such as pions or kaons as well as energetic electrons and positrons (and possibly the odd anti-proton or anti-neutron as well). The nuclear fragments that come out at lower energy slow down and stop inside the material before colliding with another nucleus, producing a very high ionization density near the end of their track that can cause significant radiation damage. Higher energy fragments, along with the pions and kaons, are likely to continue the radiation cascade by slamming into more nuclei every few tens of centimeters or so and making more showers of nuclear particles until the energy of the primary cosmic ray is distributed among so many secondary particles that there is not enough energy left to shatter additional nuclei. Meanwhile, the high energy electrons and positrons make extensive electron-gamma showers.

On Earth, we have the benefit of ten tons of air over every square meter of ground to help intercept and stop this space radiation. This is enough to stop almost all of the radiation showers, although the occasional particle does reach the ground. One additional complication is that in air, the pions can fly far enough that they decay into muons before smacking another nucleus. Muons do not strongly interact with nuclei and don't ionize stuff too much, so they make up a lot of the stuff that reaches the ground. However, cosmic rays initially interact with the atmosphere at altitudes of several tens of kilometers. The great distance that the particles have to travel to reach the ground means that even most of the muons decay before reaching us, and the electrons the muons decay into are quickly stopped (the pion and muon decays also produce neutrinos, which are not stopped. By anything. Even the ground. They just go right through the Earth without interacting, and consequently are of little interest when considering the effects of radiation).

On airless bodies such as the Moon, the dose will be cut in half because the body will block out half the sky, absorbing any radiation coming from that direction. The thin atmosphere of Mars is found to cut the dose in half again, for only approximately one quarter of the dose in space.

In space, it is expensive to carry this much shielding. Even worse, a moderate amount of shielding might make things worse, by allowing the impacting cosmic rays to produce more secondary particles. For light elements, shielding seems to give some moderate benefit for low thickness but once the thickness reaches on the order of 300 - 500 kg/m² the dose often plateaus or even rises over a considerable range; often only declining again at thicknesses of around 2 tons per square meter or more. The specific details depend on the material and the spectrum of cosmic rays for this part of the solar cycle. Because the way that cosmic radiation damages cells is not known in detail, the model used for radiation damage can significantly impact the conclusions about how much good (or harm) a given amount of shielding does. The best shielding uses hydrogen-rich materials with only light elements to limit the secondary radiation. One of the preferred materials is polyethylene, composed of two hydrogens for each carbon atom and naught else. Water is also good, and liquid hydrogen, if you can store it, provides the best shielding of all. On a planetary or sub-planetary body lacking an atmosphere, native ice or regolith could be used as shielding by piling it over and around any facilities.

Relative effect of radiation on biological tissue behind a given areal density of material. The results of two models are shown. On the left is the standard risk assessment method using quality factor as a function of linear energy transfer. On the right is a track structure repair kinetic model for mouse cells.	Dose rates for atmospheric shielding. This is the dose an astronaut would take if surrounded by this areal density of air as measured in Earth's atmosphere at different altitudes.	Relative effect of radiation (compared to no shielding) behind different thicknesses of water, aluminum, and lunar regolith.

Comparison of aluminum, lunar regolith, and polyethyene shielding as a function of thickness at both solar maximum and solar minimum galactic cosmic ray conditions.

Solar Radiation

Proton energy spectra at 1 AU, showing the increase in solar energetic particles during solar particle events.

Solar Energetic Particles and Solar Particle Events

The sun is an erratic source of high energy particles, ranging from keV to GeV energies. These solar energetic particles or SEPs, as they are called, are often produced in solar flare or coronal mass ejection events (see below). Such an event that produces SEPs is called a solar particle event. SEPs are primarily protons, with some alpha particles and a small amount of light and medium ions. As protons below about 30 to 50 MeV energy can't penetrate even thin spacecraft hulls, we are mostly concerned about those SEPs in the 100 MeV to GeV range. When the sun is quiescent, SEPs in this energy range are negligible compared to cosmic rays. However, in a solar particle event the flux of SEPs can jump by two, four, even six orders of magnitude, posing a significant radiation hazard to anyone in space and not protected by a planetary magnetosphere. The Earth's magnetosphere does a good job stopping SEPs from reaching close orbits at low latitudes, but funnels the deflected particles to the poles where they produce auroras. SEPs do not penetrate Earth's atmosphere; the atmosphere on Mars has been shown to reduce the dose of a solar particle event by a factor of 30.

Because SEPs have generally lower energies than galactic cosmic rays, less material is required to shield against them. Further, because solar particle events are transitory, it is feasible to shield a small portion of a spacecraft in which the crew can huddle for the duration of an event without requiring shielding over the entire spacecraft.

Relative dose of solar energetic particles as a function of thickness of aluminum and polyethylene shielding.

Solar Wind

The solar wind is an outflowing plasma streaming from the Sun's outer layer called the corona. These are low energy particles, generally ranging from sub-keV to several keV, and quite incapable of penetrating spacecraft hulls or space suits. This solar wind is of little concern from a radiological perspective.

Solar Flares

Solar plasma is a soup of free charged particles, and charged particles do not cross magnetic field lines. If the plasma is dense enough and moving swiftly enough, it will drag the magnetic fields with it rather than being deflected by the fields. In the turbulent plasma of the sun's upper layers, this results in the magnetic fields getting all twisted up and looping back on themselves. While this turbulence helps to create a strong solar magnetic field by this churning action (called the solar dynamo), twisted up fields can sometimes snap and smooth out in a process called magnetic reconnection. A magnetic reconnection will release considerable amount of energy as the fields re-arrange themselves into a more relaxed state over a period of usually five to ten minutes, but ranging from tens of seconds to hours. This energy takes the form of a burst of highly energetic particles and x-rays – a solar flare.

The x-rays from a solar flare can pose a radiation risk. The total dose varies considerably, but at 1 AU a dose of 0.05 to 0.2 of a Gy to unprotected people is not uncommon, and doses as high as 2 Gy are possible with a suggested occurance of perhaps once every ten years. When the x-rays hit the Earth's upper atmosphere they are absorbed. This can cause temporary interference with shortwave radio communication and expand the outer layers of the atmosphere to cause additional drag on satellites in low orbit. Unlike SEPs or other charged particles, these x-rays are not affected by magnetic fields and are unhindered by the Earth's magnetosphere. They are, however, swiftly absorbed by air and are rapidly blocked by our planet's atmosphere.

It is estimated that solar flares which deliver a dangerous dose of SEPs are roughly 50 times less frequent than those which deliver a dangerous x-ray dose. Still, the dose from flare SEPs can still be dangerous.

Solar flares occur more frequently during the solar maximum of the 11-year sunspot cycle. Sunspots happen with strong bundles of trapped magnetic fields emerge from the sun's atmosphere. Consequently, solar flares often occur near sunspots.

The x-rays from solar flares are best shielded using heavy elements. This is the opposite of shielding against particle radiation (such as galactic cosmic rays, SEPs, or radiation belt particles) where heavy elements can end up making things worse. If you are going to shield against x-rays you might consider putting a thin layer of heavy metal on the inside of your particle shielding, where the particle shower has hopefully already attenuated into low enough energy particles to not significantly multiply within your x-ray shield.

Relative dose of solar flare x-rays for a given thickness of polymer or aluminum shielding. Different curves show different flare spectral distributions of x-rays.

Coronal Mass Ejections

The churning magnetic field of the sun will occasionally launch large loops of detached magnetic fields and solar plasma out into space, called a coronal mass ejection. This is often accompanied by solar flares as the detachment of the field lines requires magnetic reconnection. The launched plasma from a fast coronal mass ejection can move faster than the speed of sound in the solar wind. This leads to a shock wave at the front which can accelerate ions to high speeds and create a solar particle event. However, not all coronal mass ejections are spat out quickly enough to do this. The solar particle events associated with coronal mass ejections often last for a few days, although the period of maximum radiation intensity might be over in several hours. The dose over the entire event can vary considerably, from a fraction of a cGy up to ten or more Gy, with an equivalent dose in Sv roughly double the physical dose in Gy.

It takes a few days for the plasma in a coronal mass ejection to reach Earth. When the mass of plasma impacts the Earth's magnetosphere, it compresses the magnetic field. The ramping magnetic flux at ground level can induce strong currents in long conductors, such as power lines, and this can lead to blackouts and damage to power grid infrastructure. The resulting geomagnetic storms can also mess with the ionosphere, causing radio blackouts. Not all coronal mass ejections are aimed at Earth – if the plasma blob is not aimed at you it will pass you by and you won't be affected.

Coronal mass ejections are most common during solar maxima – the phase of the sun's 11 year sunspot cycle when it is most active.

Solar Ultraviolet Light

The sun puts out a steady glow of light. Most of this is in the visible and infrared part of the spectrum, but some is ultraviolet. The energetic particles of ultraviolet light can break apart many kinds of molecules. Over time, anything organic which is exposed to ultraviolet light will be degraded. Rubber will lose its elasticity and crack, plastics will yellow and crumble, dyes will lose their luster and fade, fabrics will weaken and become fragile. Direct exposure to the full glare of the sun, unshielded by any intervening material or atmosphere, can cause sunburns more rapidly than you would expect – but if you find yourself in this situation, sunburn is probably the least of your concerns.

Ozone in the Earth's atmosphere absorbs much of the ultraviolet light headed our way, including the more dangerous shorter wavelengths. This helps to make our world more livable.

Flare Stars

Our sun is not the only star in space. If you find yourself around another star, many of the same phenomena can occur to produce space radiation. Hotter stars make more ultraviolet light. However, hotter stars have a thinner convective layer at their surface. As you might remember from previous sections, it is the convective boiling of the solar plasma that makes solar magnetic fields from the dynamo effect, and which twists up the magnetic fields in ways that produce solar flares and coronal mass ejections. Cool stars such as red dwarfs can be convective everywhere, with strong magnetic fields and frequent, powerful flares. Such stars can produce powerful but erratic bursts of space radiation from their various solar particle events and x-ray flashes. Meanwhile, hotter stars starting at mid-range spectral class F main sequence stars are not convective anywhere and will likely lack significant flares and solar particle events.

Planetary Radiation Belts

Planetary magnetic field (black) with trapped radiation belts (green) and the trajectory of an individual charged particle in the belt (red).

Many planets have planetary magnetic fields. Usually, these have a simple magnetic north pole and magnetic south pole on opposite sides of the planet. (The magnetic north and south poles do not necessarily align with the rotational north and south poles – in fact, on Earth, it is the magnetic south pole that is closest to the rotational north pole.) In the field line approximation, "lines" of magnetic field (each representing a certain amount of magnetic flux) emerge from the magnetic north pole to go out into space, spread out, then curve around and come back in through the south magnetic pole.

Charged particles spiral around magnetic field lines. Where the lines become more concentrated and the field gets stronger, the particle will spiral around faster and the energy for that increased spiraling speed will come from the energy of its speed along the field line. If the field gets strong enough, the particle will stop drifting along the field line when all its kinetic energy ends up in the spiraling motion after which the particle will start drifting the other way along the field line. In this way, charged particles can be reflected from areas of strong fields.

When you combine these facts, you get particles stuck in the magnetic field of the planet that drift back and forth along the field lines and get reflected from the stronger fields at the poles. When you get many particles trapped in this way, you get a radiation belt.

A charged particle that comes into a planet's magnetic field from the outside will always get bent back so that it flies away, as long as the field itself doesn't change. This means that any planetary radiation belts are either made up of radiation that was produced inside the planet's magnetic field, or that the incoming radiation distorted the field enough to become captured. The former kind can happen deep inside the planet's field, the latter are generally out near the edges. Particles in the field with enough energy to go deep into the polar region fields and encounter the atmosphere will be stopped by all that air they hit, and produce colorful auroras in the process. This puts an upper limit on the energies of particles you will encounter in a radiation belt.

Planetary radiation belts often have changing radiation conditions, both fluctuating with time and varying across space as you go in and out across magnetic field lines. A given "shell" of field lines that reach the same altitude generally have close to the same intensity and spectrum of radiation within them, however.

Earth

Typical proton energy spectra for the inner Van Allen belt for magnetic shells extending to various distances as measured in Earth radii from Earth's center.

Earth has two radiation belts, known as Van Allen belts after their discoverer. The inner belt consists mainly of protons with energies ranging up to 400 MeV. These are created by cosmic rays – when a cosmic ray collides with the upper atmosphere, it can produce neutrons which can scatter out of the air and into space. Being uncharged, neutrons pass unhindered through the Earth's magnetic field. Free neutrons are unstable, however, and decay into protons and electrons with a 15 minute half life. If this happens within magnetic field lines that loop out to about 0.2 to 2 Earth radii in altitude from the planet (or 1.2 to 3 Earth radii from Earth's center, using the standard method of measurement), the protons can become trapped. This is what forms the inner belt.

The outer belt forms from electrons leaking in from the solar wind and accelerated by waves in the space plasma. The outer belt is much more variable, and can change quickly based on space weather conditions. It extends across field lines that loop out to about 3 to 10 Earth radii altitude (4 to 11 Earth radii from the Earth's center).

Maximum dose estimates for both the inner and outer belt range from a dose of approximately 0.2 Gy/hour to 0.5 Gy/hour to individuals and equipment with 20 kg/m² of shielding, although shielding of 250 kg/m² will reduce this to 0.05 Gy/hour.

Jupiter

Radiation dose rate with distance from Jupiter's center, as measured in Jupiter radii.

Jupiter has one of the largest and strongest magnetic fields of any planet in the solar system. Like that of Earth, it will trap particles from the solar wind and the decay products of cosmic neutrons. However, what really sets Jupiter's radiation belts apart is what happens because of its moon, Io. Io is extremely volcanic, and regularly erupts fountains of sulfur dioxide into space. This gas is then ionized by ultraviolet sunlight, producing positively charged sulfur and oxygen ions. These ions spread out to form the Io plasma torus. Electric currents within the torus, driven by Jupiter's rotation, accelerates ions and electrons to high speeds and can produce dangerous radiation. Jupiter's radiation belts are not as well understood as those of Earth, but data suggests that the particle energies are higher than those of the Van Allen belts and that the doses can be around a thousand times as intense. The radiation is most intense closer to Jupiter, reaching a maximum of over 300 Gy/hour near Amalthea and other inner moons, approximately 20 Gy/hour at Io, 12 Gy/hour at Europa, 10 Gy/day (0.4 Gy/hour) at Ganymede, and 0.4 Gy/day at Callisto (all assuming 10 kg/m² shielding). These doses are for the moon's orbits, presumably if you are on the moon the dose will be approximately halved (on average) because the moon will be shielding half the sky. However, the interaction's of the radiation with the moon's orbits is complicated, and generally one side (often the leading side) gets irradiated more than the other. This suggests that a spacecraft for a Jupiter mission could benefit from directional shielding, pointing its thicker shielded cap in the direction from which more radiation is incident – although you would still probably want substantial shielding from all directions!

Dose rate at Europa and Ganymede orbit for different amounts of shielding.

Other Planets

All the planets in our solar system with a substantial magnetic field have radiation belts to some degree. The best known outside of Earth and Jupiter are the radiation belts of Saturn, which were studied extensively by various probes, particularly the 13 year Cassini mission. Saturn's belts are complex, with gaps due to absorption by its moons and rings and different sources and features in different regions. Like Jupiter, Saturn's radiation belts are largely driven by a plasma torus, this time sources from water vapor escaping from the moon Enceladus although cosmic ray decay protons also have a contribution. Saturn's rings block radiation that passes through them, so that the radiation belts end where the field lines pass through the rings separating the radiation into a belt outside the rings and one inside the rings. Little work appears to have been done on estimating the dose that instruments, equipment, or people would accumulate when passing through the Saturn radiation belts.

Compared to Earth, Saturn, and Jupiter very little is known about the belts of Uranus or Neptune. Mercury, Venus, Mars, and most of the various giant moons have fields far weaker than that of Earth, and lack radiation belts. Ganymede is an exception, having a small magnetosphere within Jupiter's powerful fields that has a modest trapped radiation belt.

Relativistic Travel

Space is not truly empty. It is filled with a very diffuse plasma. In between stars, this is called the interstellar medium (or ISM). Within a star system, it is the solar wind. The density of the plasma varies considerably depending on the environment, but is roughly one proton (and one electron) per cubic centimeter.

if you are traveling between stars at relativistic speeds, from your standpoint you are not moving and the ISM is moving at, past, and through you at those relativistic speeds. In essence, you have managed to turn the entire universe into a particle beam, and the parts in front of you are aimed right at you!

Low relativistic particles are fairly easy to shield against. A thin layer of just about anything will bring them to a stop. And even if they do get to you, their main hazard is radiation burns to your skin because they cannot reach deep organs to cause radiation poisoning. But as your speed increases, the particles will be hitting the front of your spacecraft faster and faster and they will penetrate more and more shielding material ... and more of you. One estimate of the dose and penetration is shown below; at 50% of light speed the ISM particles will be passing all the way through your body and delivering dose to your bone marrow and central nervous system where the really bad radiation exposure stuff happens. As you go faster and faster you need a thicker and thicker radiation shield in front of you to stop these particles.

More details on the hazards of relativistic travel can be found in Interstellar_Medium_Shielding.

The rate at which an unshielded individual will take radiation dose as a function of speed $\beta =v/c$ relative to light speed.	Stopping distance of protons in titanium and living tissue as a function of speed $\beta =v/c$ relative to light speed.

Extreme Astrophysical Environments and Phenomena

There's a lot of crazy stuff out there. Stuff that often features extreme conditions and exotic physics that can result in high radiation environments. Because people will not visit any of these sites in the near future, there is little urgency for quantifying the radiation hazards, in terms of dose or shielding. So this section will be fairly high level, giving qualitative descriptions of the kinds of hazards that can be encountered.

White Dwarfs

A young white dwarf will be much less luminous than its parent star. However, it will be much hotter with most of its radiated power in the ultraviolet and soft x-ray regions of the spectrum. Radiation of this nature can be dangerous to unprotected skin, but then so is space so this feature is probably not much of a concern. The shielding of even a space suit or thing spacecraft hull should suffice for protection. As the white dwarf cools, both the luminosity and the proportion of its emitted heat as x-rays and ultraviolet drops.

White dwarfs have magnetic fields ranging from between 0.2 T and 100 kT. This is well above the field of Earth, which raises the possibility of strong radiation belts around these objects.

Infalling matter from an accretion disk – possibly supplied by a closely orbiting companion – can radiate strongly in the ultraviolet and x-ray part of the spectrum as it spirals in. Instabilities in the rate at which the accretion disk is heated can lead to significant changes in brightness and radiation from the disk in a process called a dwarf nova. As material fall on the white dwarf, it leads to a build up of material. If hydrogen or helium from this accretion builds up sufficiently it can ignite as a wave of thermonuclear fusion engulfs the star, producing a classical nova explosion. If enough material builds up that the pressure causes fusion in the carbon and oxygen that makes up the majority of the white dwarf star, the entire star can be consumed in a Type 1a supernova explosion. In either case, intense x-rays and gamma rays will be produced, although in the latter case no star will remain after the explosion. All such white dwarf stars with accretion disks are classified as various kinds of cataclysmic variable stars.

Neutron Stars

Neutron stars are extreme radiation environments.

Newly formed neutron stars are x-ray hot. While they cool down with time, their thermal emissions are but a small part of the radiation in their vicinities.

Neutron stars have magnetic fields on the order of 10 kT to 100 GT. They are usually formed rotating at several Hz, but may spin up to nearly a kHz by accreting material and will eventually slow down over time if not accreting material. Material falling onto a neutron star will hit with enough speed that it will emit x-rays and gamma rays. The extreme fields of the neutron star channel the in-falling material down the magnetic field lines and onto the magnetic poles. This can lead to the x-ray source appearing to flash on and off when the pole is pointed toward or away from an observer. This forms an <i.x-ray pulsar. This effect should not be confused with the radio pulsar that forms as the spinning field accelerates electrons in spiraling paths along its field lines to produce intense jets of radio waves that appear to pulse on an off as the beam spins past the observer.

The neutron star iaccretion disk can also form an astrophysical jet, a beam of intense particle radiation shooting out along the axis of rotation at nearly the speed of light. Interactions among these particles and between the particles and any ambient material can create x-rays and gamma rays as well.

The ejected shell of matter from the outer layers of the star that collapsed to form the neutron star may still be in the vicinity of a young neutron star. As the field spins through this ionized matter, various processes create powerful currents, shock waves, and other plasma interactions that produce a variety of radiation. This includes some of the most intense long-lived x-ray and gamma ray sources that can be observed from Earth. It is likely that these same phenomena will also produce intense particle radiation.

Neutron stars with the most extreme magnetic fields, of about 1 to 100 GT, are known as magnetars. At these magnetic field strengths, the magnetar becomes an extremely strong source of x-rays and gamma rays as its thermal emissions are scattered to higher energies by the field. Some magnetars produce repeating pulses of even more extreme intensity soft gamma rays. When strain builds up in a magnetar's crust, it can suddenly rupture to produce a star quake analogous to the way an earthquake relieves built up stress in the Earth's crust. This produces an even more extreme burst of gamma rays.

Black Holes

An isolated stellar mass black hole is cold, quiescent, and lacking activity – radioactivity or otherwise. The interesting stuff happens when the black hole is not isolated.

Material attracted by the black hole's gravity will spiral around to form an accretion disk. As the material falls deeper into the disk, it will be heated by the shear flow of the neighboring gas to produce intense thermal x-rays and gamma rays. Up to approximately 5 to 30% of the mass-energy of infalling material can be radiated away, such that an actively eating black hole can be a source of intense radiation. In addition, much as with a neutron star, the accretion disk can produce an astrophysical jet of intense particle radiation and associated x-ray and gamma ray emissions.

The largest black holes known are the supermassive black holes, one of which sits in the hear of every galaxy. These behemoths can have accretion disks made of many stars and their associated solar systems at once, all of which have been torn to pieces and are spinning down the drain of oblivion. The most active supermassive black holes are quasars, which can consume between ten and a thousand suns worth of material a year. These are the brightest known objects in the universe, and are certain to be some of the most extreme persistent radiation environments in existence.

Supernovas

If you are near a supernova, space radiation is probably one of the smaller of your concerns. However, core collapse (or Type II) supernovas are notable in being one of the only phenomena known that can produce dangerous levels of neutrino radiation. Neutrinos are normally so penetrating that they go through everything without significant interactions. However, the core collapse of Type II supernovas makes neutrinos in such prodigious quantities that enough of them can interact and cause radiation sickness and death within approximately the distance of the inner solar system. Core collapse supernovas also often leave behind neutron stars (see above), and the young rapidly rotating neutron star in the nebula formed from the supernova remains will whip up some really nice particle, x-ray, and gamma ray radiation as well.

Supernova shock waves, when the expanding shell of former star plows into the interstellar medium, or into former shells of matter ejected from the star, are thought to be one of the primary sources of galactic cosmic rays. Again, if you are in the shock wave of a supernova you'll have much more immediate concerns than your radiation dose, but that dose is going to be very high anyway.

Artificial Radiation Sources

The main focus of this article is on natural sources of radiation. But if you expect to operate in space you will also need to consider common artificial radiation sources. Many spacecraft and other space infrastructure are expected to be powered by fission or fusion reactors, or to use fission or fusion propulsion. All of these will produce copious amounts of nuclear radiation in the form of energetic neutrons, gamma rays, and the emissions of radioactive isotopes produced through fission or neutron capture. Without an atmosphere to attenuate the radiation produced, high power radiation sources can have an effect over a much larger distance than a similar unshielded source on Earth. This will produce a hostile radiation environment that will require large exclusion zones or shielding.

In addition, space conflict scenarios are likely to use particle beam weapons, x-ray or gamma-ray lasers, and nuclear explosives. All of these produce radiation as a primary effect or side effect of their operation.

Nuclear reactors and explosions in the vicinity of a planet with a magnetic field can make artificial radiation belts that persist for days to years (depending on the altitude), and can severely damage electronics operating within or passing through the belt.

Protection and Mitigation

There are several ways to avoid problems with space radiation. If the thing you are sending into space does not have people or other living things on it, the usual preferred method is to design it to just tough out the radiation. Space rated electronics might not be as fast or capable as normal consumer electronics, but they can tolerate much larger doses. Space rated electronics can continue to operate at doses exceeding several thousand Gy, compared to tens of Gy for the usual things you pick up from Best Buy.

But if you need to have a person on your spacecraft, it is often not possible to choose people that have increased radiation tolerance. Sure, in a post-human setting where everyone is engineered or one where AI are considered people, you could do this. But if you are stuck with normally evolved Homo sapiens you're going to want to limit them to well less than a Gy if you want them to be mission effective and to avoid health problems when they get back home. For the Apollo moon mission, the method used was to go fast. Fly through the Van Allen belts in short enough time that the astronauts didn't pick up too much dose, don't spend so long in space that galactic cosmic rays are a concern, and gamble that in your short time in space a solar particle event doesn't come by and give your crew a fatal dose. This latter was a very real possibility. In August 1972 a massive solar particle event swept past Earth. Fortunately, this was between the April 1972 Apollo 16 mission and the December 1972 Apollo 17 mission and no one was outside of Earth's magnetosphere at the time. Any astronauts who were moonwalking during the event could have received a fatal dose, and even inside of the Apollo capsule they could have been sickened.

Medical techniques could be used to mitigate the damage of radiation exposure, including radical scavenger medication (to be taken immediately before exposure), taking anti-oxidant pills (which should be kept up continuously for as long as the risk persists), cytokenes (which might help with immune and blood disorders due to radiation exposure), and cell transplants to replace quickly dividing cell tissues killed by the radiation.

Passive Shielding

But maybe you want something more sure than trying to avoid or tough out the radiation. Shielding is the usual answer. This usually involves putting layers of stuff around your spacecraft to block the radiation before it gets to you. Or at least around the parts of the spacecraft that have stuff that you want to protect. In the descriptions of the various kinds of space radiation, we have tried to give an idea of how much shielding you need to reduce the dose (or dose rate) to whatever you decide is an acceptable level. Particle radiation is best stopped with hydrogen rich stuff or at least light elements because this reduces the radiation cascades that make showers of secondary particles. X-ray or gamma radiation, on the other hand, is best stopped with heavy elements – so you might want to try to reduce the particle radiation as much as possible with shielding on the outside before it gets to the heavy metal photon shielding layer. The problem with shielding is that it is heavy. With anything like today's technology, that makes it prohibitive to have much shielding beyond a basic spacecraft structural hull. Any shielding can help some by screening out the lower energy particles, and radiation environments with lower energy particles (such as planetary radiation belts or solar particle events) might be feasible to fully shield with reasonable advances in rocketry capability. The high energy cosmic rays, however, are a significant challenge and it may be necessary to tolerate some degree of elevated cosmic ray dose for interplanetary trips if the alternative is so much shielding that you can't go at all.

Active Shielding

There is one other kind of shielding, however. It is called active shielding. It uses electric or magnetic fields or both to reduce the flux of radiation reaching the spacecraft. No active shielding can stop x-rays or gamma rays. These are not affected by electric or magnetic fields.

Electrostatic Shielding

To protect with electric fields, you need to charge your spacecraft up to a high enough positive voltage that the positively charged particle radiation is repelled from the spacecraft and cannot reach it. In the above descriptions of the sources of different kinds of particle radiation, at least some approximation of the energy spectrum of the particles is given, with the energy in electronvolts, or eV. One keV is 1000 eV, one MeV is 1,000,000 eV, and a GeV is one billion eV. A proton can be stopped from getting to the spacecraft if the voltage (in volts) is higher than the particle energy in eV. So if you want to stop a GeV proton, you need to charge your spacecraft up to a billion volts (or a gigavolt, to use SI prefixes). Ions will be stopped by a voltage of their energy in eV divided by their electric charge. So a fully ionized manganese nucleus with charge +25 with an energy of a GeV would be blocked with a spacecraft voltage of 1,000,000,000/25 = 40,000,000 volts.

At a gigavolt, you'll be stopping more than half of the galactic cosmic rays, and nearly all of the radiation from planetary radiation belts and solar particle events.

However, there are difficulties with this option. Now electrons in the solar wind or ISM are attracted to your spacecraft rather than repelled. And they'll gain an energy in eV equal to the voltage on your spacecraft when they hit it. At a GeV, this will create large amounts of penetrating gamma rays that can irradiate you even though you stopped most of the protons and ions. various ways have been proposed to keep the electrons out. Perhaps you could have an outer shell with a potential of minus several thousand volts, and an inner shell of positive a few gigavolts. The outer shell repels the electrons, and the ions that get through are then kept out by the inner shell voltage. Alternately, you could use a magnetic field to deflect the electrons, making a magnetostatic electron shield and an electrostatic ion shield.

Credit

Author: Luke Campbell