Comets are icy bodies that develop spectacular tails when they travel close to the Sun. The intense solar radiation heats the nucleus, causing volatile ices to sublimate and release gas and dust into space.
The ion (or plasma) tail forms when the solar windβa stream of charged particles emitted by the Sunβionizes the released gases. These newlyβcreated ions are then swept away by the solar wind, creating a straight, bluish tail that points directly away from the Sun.
A firstβorder estimate of the ionβtail length can be obtained by multiplying the solarβwind speed by the typical lifetime of an ion before it recombines or is lost. This simple model captures the dominant physics and is useful for quick calculations.
What factors affect the length of a comet’s tail?
How do you estimate the length of a comet’s tail?
What causes the ion tail of a comet to form?
Why is the comet’s tail bluish in color?
Can a comet have more than one tail?
How does the comet’s speed affect its tail?
What happens to a comet’s tail when it moves away from the Sun?
Results are for informational purposes only and do not constitute professional advice.
