Degrees per minute to Degrees per hour

A full circle is 360° and the minute hand completes it in 60 minutes: 360 ÷ 60 = 6°/min. It is one of those satisfying integer results in everyday physics. The hour hand, by contrast, moves at 0.5°/min (360° ÷ 720 minutes). At any given time, the angle between them changes at 5.5°/min — which is the key to solving those "when do the hands overlap?" puzzles.

The Sun crosses the sky at 15°/hr (360° ÷ 24 h), or 0.25°/min. A single-axis solar tracker matches this rate, adjusting continuously or in small steps throughout the day. Dual-axis trackers also compensate for the Sun's seasonal altitude change — a much slower adjustment of roughly 0.5–1° per week. The daily tracking rate of 0.25°/min is slow enough that you cannot see the panel moving.

Large rotary cement kilns typically rotate at 1–5°/min (roughly 0.003–0.014 RPM). That glacial pace is intentional: raw material needs 30–60 minutes to travel the kiln's 50–100 meter length, slowly heating to 1,450°C. Faster rotation would push material through before it fully reacts. Industrial drum dryers and composting drums operate in a similar 2–10°/min range.

Divide by 360. One full revolution is 360°, so degrees per minute ÷ 360 = RPM. The clock minute hand at 6°/min is 6/360 = 0.01667 RPM — one revolution per hour. A turntable at 33⅓ RPM is 33.33 × 360 = 12,000°/min. For rad/min, multiply °/min by π/180 ≈ 0.01745.

Most revolving restaurants complete one full rotation in 45–90 minutes, which translates to 4–8°/min. The slow rate is deliberate — fast enough that diners get a complete panoramic view during a meal, but slow enough that you do not notice the motion or feel any inertia. The famous revolving restaurant atop the BT Tower in London took about 22 minutes per revolution (16.4°/min) when it operated.

The ISS completes one orbit (360°) in about 92 minutes, giving roughly 235°/hr — almost 16 times faster than Earth's rotation. That is why astronauts see 16 sunrises every 24 hours. At an altitude of ~408 km, the station covers about 7.66 km/s of ground track. If you could watch it from a fixed point in space, it would visibly sweep through the sky at a rate where one degree takes only about 15 seconds.

Because even tiny drift accumulates into serious navigation errors over a flight or voyage. A navigation-grade ring-laser gyroscope drifts less than 0.01°/hr; over a 10-hour flight that is only 0.1° of heading error. A cheap MEMS gyro drifting 10°/hr would accumulate 100° of error in the same time — useless for navigation. Expressing drift in °/hr makes the operational impact immediately obvious to a pilot or engineer.

Equatorial telescope mounts have a motorised right-ascension axis aligned with Earth's rotation axis. By driving that axis at exactly 15°/hr (one sidereal rate), the telescope counter-rotates against Earth's spin, keeping a star fixed in the eyepiece. Without this drive, stars would drift out of view in seconds at high magnification. Astrophotographers rely on it for long exposures without star trails.

The Moon's apparent motion has two components. It shares the sky's overall 15°/hr westward motion due to Earth's rotation. But it also orbits Earth, moving about 0.55°/hr eastward relative to the stars (360° ÷ 27.32 days ÷ 24 hr). The net effect: the Moon moves westward across the sky at roughly 14.5°/hr, which is why moonrise occurs about 50 minutes later each day.

A Foucault pendulum's swing plane rotates relative to the floor at 15° × sin(latitude) per hour. At the North Pole (90°) that is the full 15°/hr; at 45° latitude it is about 10.6°/hr; at the equator it is zero. The pendulum always swings in a fixed plane in inertial space — it is the Earth rotating underneath it. The sine factor comes from the fact that only the vertical component of Earth's angular velocity vector projects into the pendulum's swing plane. Paris (48.9°N) sees about 11.3°/hr, which is why Foucault's original 1851 demonstration took most of a day to complete a visible rotation.