Carbon monoxide occurs in many environments, usually in trace levels. Photochemical degradation of plant matter, for example, generates an estimated 60 million tons/year. Typical concentrations in
parts per million are as follows:
Atmospheric presence ,
Africa, and the
Atlantic Ocean in this animation points to high levels of carbon monoxide on September 30, 2005. Carbon monoxide (CO) is present in small amounts (about 80
ppb) in the
Earth's atmosphere. Most comes from chemical reactions with
organic compounds emitted by human activities and natural origins due to
photochemical reactions in the
troposphere that generate about 5 × 1012 kilograms per year. Other natural sources of CO include volcanoes,
forest and
bushfires, and other miscellaneous forms of combustion such as
fossil fuels. Small amounts are also emitted from the ocean, and from geological activity because carbon monoxide occurs dissolved in molten volcanic rock at high pressures in the Earth's
mantle. Because natural sources of carbon monoxide vary from year to year, it is difficult to accurately measure natural emissions of the gas. Carbon monoxide has an indirect effect on
radiative forcing by elevating concentrations of direct
greenhouse gases, including
methane and
tropospheric ozone. CO can react chemically with other atmospheric constituents (primarily the
hydroxyl radical, •OH) that would otherwise destroy methane. Through natural processes in the atmosphere, it is oxidized to
carbon dioxide and ozone. Carbon monoxide is short-lived in the atmosphere (with an average lifetime of about one to two months), and spatially variable in concentration. Due to its long lifetime in the mid-troposphere, carbon monoxide is also used as a tracer for pollutant plumes.
Astronomy Beyond Earth, carbon monoxide is the second-most common diatomic molecule in the
interstellar medium, after
molecular hydrogen. Because of its asymmetry, this
polar molecule produces far brighter
spectral lines than the hydrogen molecule, making CO much easier to detect. Interstellar CO was first detected with
radio telescopes in 1970. It is now the most commonly used tracer of molecular gas in general in the interstellar medium of galaxies, as molecular hydrogen can only be detected using ultraviolet light, which requires
space telescopes. Carbon monoxide observations provide much of the information about the
molecular clouds in which most
stars form.
Beta Pictoris, the second brightest star in the constellation
Pictor, shows an
excess of infrared emission compared to normal stars of its type, which is caused by large quantities of dust and gas (including carbon monoxide) near the star. In the
atmosphere of Venus carbon monoxide occurs as a result of the photodissociation of carbon dioxide by electromagnetic radiation of wavelengths shorter than 169
nm. It has also been identified spectroscopically on the surface of Neptune's moon
Triton. Solid carbon monoxide is a component of
comets. The
volatile or "ice" component of
Halley's Comet is about 15% CO. At room temperature and at atmospheric pressure, carbon monoxide is actually only metastable (see
Boudouard reaction) and the same is true at low temperatures where CO and are solid, but nevertheless it can exist for billions of years in comets. There is very little CO in the atmosphere of
Pluto, which seems to have been formed from comets. This may be because there is (or was) liquid water inside Pluto. Carbon monoxide can react with water to form carbon dioxide and hydrogen: : This is called the
water-gas shift reaction when occurring in the gas phase, but it can also take place (very slowly) in an aqueous solution. If the hydrogen partial pressure is high enough (for instance in an underground sea),
formic acid will be formed: : These reactions can take place in a few million years even at temperatures such as found on Pluto. == Pollution and health effects ==