Astrophysics (Index)About

rotation period

(time it takes an astronomical body to revolve)

A rotating body's rotation period is the time it takes to revolve once, e.g., about a day or 24 hours for Earth. The body's rotation rate is the reciprocal of the rotation period, e.g., about 1 rotation per day or 1/24 of a rotation per hour for Earth. Its rotation speed is the speed of movement at the body's equator, on the order of 1,000 miles per hour for Earth. For a non-solid body such as a star, the rotation period is not a single time period since portions rotate faster than other portions, termed differential rotation.

Regarding planetary rotation (or planet rotation), a planet's day consists of a rotation plus or minus a fraction of a rotation to the point where the same side faces the host star given their new positions in the course of their orbit (synodic rotation period). Thus the Earth's day is 86400 seconds, but its rotation period is about 86164 seconds (sidereal rotation period). Venus, which rotates in the opposite direction to its orbit (retrograde rotation), has a day is shorter than its rotation period. Determining the rotation of extra-solar planets is a challenge, so the number of planets for which rotation is known is limited. Rotation of rocky planets may be of interest in determining their habitability.

Pulsars are neutron stars, which are sufficiently compact to rotate rapidly, some have rotation periods of small fractions of a second (millisecond pulsars). Relativity places a limit on a rotation period of an object because rotation cannot be so rapid that any part of the object (e.g., its equator) moves faster than the speed of light in a vacuum, which places a limit on the possible rotation rate and period based upon the size of the object. The clock-like steadiness of the repeating pulses suggested a rotating source, and the implied rotation periods were far too small for a main sequence star, important clues toward concluding pulsars are neutron stars.

If the rotation period matches the orbital period and is prograde (i.e., not retrograde), the same side of the object constantly faces its host (if the orbit is circular: to the degree that it is eccentric, there is some variation in exactly which side faces the host) which is termed a synchronous rotation, a sign of tidal locking. This is true of the Moon, facing Earth, and is true of most moons in the solar system. Some rotation periods:

Sun 25-to-35 (Earth) days (differential).
Mercury 59 days.
Venus 243 days (retrograde).
Moon 27.3 days (synchronous).
Mars 1 day.
Jupiter 0.41 days (interior).
Saturn 0.44 days (interior).
Uranus 0.72 days.
Neptune 0.67 days.
Pluto 6.39 days.
51 Pegasi b 4.2 days (synchronous).
Hulse-Taylor Binary 59 milliseconds.
J1713+0747 4.57 ms.
Black Widow Pulsar 1.61 ms.

(kinematics,objects,period,rotation)
Further reading:
https://en.wikipedia.org/wiki/Rotation_period

Referenced by pages:
Achernar
Ap star
Beta Pictoris b (β Pic b)
brown dwarf (BD)
color-period diagram
gravitational potential model
gyrochronology
Hadley cell
Haumea
J2
Meier paradox
millisecond pulsar (MSP)
period derivative
planet formation
P-Pdot diagram
Hulse-Taylor Binary (PSR B1913+16)
pulsar (PSR)
pulsar characteristic age (τ)
rotating radio transient (RRAT)
sidereal
stellar age determination
stellar parameter determination
Sun
synchronous orbit
tidal locking
tidal migration
T-Tauri star (TTS)
Venus

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