Day to Sidereal Day Converter

Convert days to sidereal days with our free online time converter.

Quick Answer

1 Day = 1.002738 sidereal days

Formula: Day × conversion factor = Sidereal Day

Use the calculator below for instant, accurate conversions.

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All conversion formulas on UnitsConverter.io have been verified against NIST (National Institute of Standards and Technology) guidelines and international SI standards. Our calculations are accurate to 10 decimal places for standard conversions and use arbitrary precision arithmetic for astronomical units.

Last verified: December 2025Reviewed by: Sam Mathew, Software Engineer

Day to Sidereal Day Calculator

How to Use the Day to Sidereal Day Calculator:

  1. Enter the value you want to convert in the 'From' field (Day).
  2. The converted value in Sidereal Day will appear automatically in the 'To' field.
  3. Use the dropdown menus to select different units within the Time category.
  4. Click the swap button (⇌) to reverse the conversion direction.
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How to Convert Day to Sidereal Day: Step-by-Step Guide

Converting Day to Sidereal Day involves multiplying the value by a specific conversion factor, as shown in the formula below.

Formula:

1 Day = 1.002738 sidereal days

Example Calculation:

Convert 60 days: 60 × 1.002738 = 60.16427 sidereal days

Disclaimer: For Reference Only

These conversion results are provided for informational purposes only. While we strive for accuracy, we make no guarantees regarding the precision of these results, especially for conversions involving extremely large or small numbers which may be subject to the inherent limitations of standard computer floating-point arithmetic.

Not for professional use. Results should be verified before use in any critical application. View our Terms of Service for more information.

What is a Day and a Sidereal Day?

The day (symbol: d) is a unit of time equal to 24 hours, 1,440 minutes, or 86,400 seconds.

Official civil definition: Since 1967, one day is defined as exactly 86,400 SI seconds, where each second equals 9,192,631,770 periods of caesium-133 radiation. Therefore:

  • 1 day = 86,400 × 9,192,631,770 = 793,927,920,332,800,000 caesium-133 oscillations
  • This equals approximately 794 quadrillion atomic oscillations

Astronomical definitions:

  1. Solar day (apparent solar day):

    • Time between two successive transits of the Sun across the local meridian (noon to noon)
    • Varies throughout year: ±16 minutes due to Earth's elliptical orbit and axial tilt
    • Mean solar day: Average of all solar days = 24 hours exactly (86,400 seconds)
    • This is the basis for civil timekeeping
  2. Sidereal day:

    • Time for Earth to rotate 360° relative to distant stars
    • 23 hours, 56 minutes, 4.09 seconds (86,164.09 seconds)
    • ~4 minutes shorter than solar day
    • Used in astronomy for telescope tracking and star charts
  3. Synodic day (planetary science):

    • Time for same position of sun in sky on other planets
    • Mars sol: 24 hours, 39 minutes, 35 seconds
    • Venus day: 116.75 Earth days (very slow rotation)

Why the difference?

  • Earth rotates 360° in one sidereal day
  • But Earth also orbits the Sun (~1° per day along orbit)
  • Must rotate an additional ~1° (4 minutes) for sun to return to same position
  • Result: Solar day = sidereal day + ~4 minutes
  • Over one year: 365 solar days, but 366 sidereal days (one extra rotation)

What Is a Sidereal Day?

A sidereal day is the time required for Earth to complete one full rotation (360 degrees) on its axis relative to the fixed background stars.

Precise value: 1 sidereal day = 86,164.0905 seconds (mean sidereal day) = 23 hours, 56 minutes, 4.0905 seconds

Sidereal vs. Solar Day

Sidereal day (stellar reference):

  • Earth's rotation relative to distant stars
  • Duration: 23h 56m 4.091s
  • Used by astronomers for telescope pointing

Solar day (Sun reference):

  • Earth's rotation relative to the Sun
  • Duration: 24h 00m 00s (mean solar day)
  • Used for civil timekeeping (clocks, calendars)

The difference: ~3 minutes 56 seconds

Why Are They Different?

The sidereal-solar day difference arises from Earth's orbital motion around the Sun:

  1. Start position: Earth completes one full 360° rotation relative to stars (1 sidereal day)
  2. Orbital motion: During that rotation, Earth has moved ~1° along its orbit around the Sun
  3. Extra rotation needed: Earth must rotate an additional ~1° (~4 minutes) to bring the Sun back to the same position in the sky
  4. Result: Solar day = sidereal day + ~4 minutes

Analogy: Imagine walking around a merry-go-round while it spins. If you walk one full circle relative to the surrounding park (sidereal), you'll need to walk a bit farther to return to the same position relative to the merry-go-round center (solar).

One Extra Day Per Year

A surprising consequence: There is one more sidereal day than solar day in a year!

  • Solar year: 365.242199 solar days
  • Sidereal year: 365.256363 sidereal days
  • Extra sidereal days: 366.256363 - 365.242199 ≈ 1 extra day

Why? Earth makes 366.25 full rotations relative to the stars during one orbit, but we only experience 365.25 sunrises because we're moving around the Sun.


Note: The Day is part of the imperial/US customary system, primarily used in the US, UK, and Canada for everyday measurements. The Sidereal Day belongs to the imperial/US customary system.

History of the Day and Sidereal Day

of the Day

Prehistoric Recognition (Before 3000 BCE)

The day-night cycle is the most fundamental observable pattern in nature, recognized by all human cultures and even animals:

Biological origins:

  • Circadian rhythms: Internal ~24-hour biological clock evolved in response to Earth's rotation
  • Found in bacteria, plants, animals, humans
  • Regulated by light/dark cycle
  • Predates human civilization by billions of years

Early human observation:

  • Stone Age: Organized activities by sun position (hunting at dawn, gathering by day)
  • Neolithic era: Agricultural cycles tied to day length (planting, harvesting)
  • Megalithic monuments: Stonehenge (c. 3000 BCE) aligned with solstice sunrise
  • Earliest "clocks": Shadows cast by objects (proto-sundials)

Ancient Egyptian Timekeeping (c. 3000 BCE)

Egyptians formalized day measurement:

  1. Shadow clocks and sundials (c. 1500 BCE):

    • Obelisks cast shadows indicating time of day
    • Divided daylight into 12 parts (seasonal hours)
    • Used horizontal bars with markings
  2. Water clocks (clepsydrae):

    • Used at night when sundials didn't work
    • Water dripped at constant rate through calibrated container
    • Divided night into 12 parts
  3. Decans (star clocks):

    • 36 groups of stars rising throughout year
    • Each decan rose ~40 minutes apart
    • Used to tell time at night

Egyptian day structure:

  • Day began at sunrise (variable time)
  • 12 hours daylight + 12 hours darkness = 24 hours
  • But "hours" varied by season (longer daytime hours in summer)

Babylonian Contributions (c. 2000 BCE)

Babylonians established key concepts:

  1. Seven-day week:

    • Based on seven visible celestial bodies (Sun, Moon, Mercury, Venus, Mars, Jupiter, Saturn)
    • Each day named after a planet/god
    • This system spread globally
  2. Day began at sunset:

    • Still used in Hebrew and Islamic calendars
    • Genesis 1:5: "And there was evening, and there was morning—the first day"
  3. Base-60 mathematics:

    • Eventually led to 24 hours, 60 minutes, 60 seconds
    • 360° circle (from ~360 days in year)

Greek and Roman Systems (500 BCE - 400 CE)

Greek astronomers:

  • Hipparchus (c. 150 BCE): Studied equation of time (variation in solar day length)
  • Recognized need for "mean solar day" as average

Roman timekeeping:

  • Day began at midnight (adopted by modern civil timekeeping)
  • Divided into:
    • Dies (daytime): Sunrise to sunset, 12 horae (hours)
    • Nox (nighttime): Sunset to sunrise, 4 vigiliae (watches) of ~3 hours each
  • Market day cycle: Nundinae (8-day week, superseded by 7-day week)

Roman calendar influence:

  • Julian Calendar (45 BCE): 365.25-day year, leap years
  • Day names from planets (still used): Sunday (Sun), Monday (Moon), Saturday (Saturn)

Medieval and Islamic Developments (600-1300 CE)

Islamic timekeeping:

  • Day begins at sunset (following Hebrew tradition)
  • Five daily prayers (salat) structured the day:
    • Fajr (dawn), Dhuhr (noon), Asr (afternoon), Maghrib (sunset), Isha (night)
  • Sophisticated astronomical tables calculated prayer times
  • "Islamic day" vs. "civil day" distinction in Muslim countries

Medieval Christian hours:

  • Canonical hours: Structured monastic life
    • Matins (midnight), Lauds (dawn), Prime (6 AM), Terce (9 AM)
    • Sext (noon), None (3 PM), Vespers (sunset), Compline (bedtime)
  • Church bells marked these hours, organizing community life

Mechanical Clocks and Equal Hours (1300s)

Transformation of daily time:

Before mechanical clocks:

  • "Hours" varied by season
  • Time was task-oriented ("work until sunset")
  • Imprecise coordination

After mechanical clocks (1300s-1400s):

  • 24 equal hours became standard
  • Clocks tick at constant rate regardless of season
  • "Clock time" replaced "sun time" for daily schedules
  • Enabled precise coordination of activities

Social impact:

  • Time discipline: Workers expected at specific times
  • Urban life required synchronization
  • "Punctuality" became a virtue
  • Transition from natural rhythms to mechanical rhythms

Scientific Definition (1800s)

Astronomical measurement:

  • 1832: Second officially defined as 1/86,400 of mean solar day
  • Astronomers recognized Earth's rotation not perfectly uniform
  • Tidal friction slowly increases day length (~1.7 milliseconds per century)

Problem discovered:

  • Earth's rotation varies:
    • Seasonal variations (atmosphere, ice melt)
    • Long-term slowing (tidal friction from Moon)
    • Irregular variations (core-mantle coupling, earthquakes)
  • "Day" based on Earth rotation became unreliable time standard

Atomic Era: Day Decoupled from Rotation (1967)

Atomic second (1967):

  • Second redefined based on caesium-133 atomic transitions
  • Day remains 86,400 seconds (by definition)
  • But now independent of Earth's actual rotation period

Consequence: Leap seconds

  • Earth's rotation gradually slowing
  • Atomic time (TAI) and Earth rotation time (UT1) drift apart
  • Leap seconds added to keep them synchronized:
    • 27 leap seconds added between 1972-2016
    • Last one: December 31, 2016 (23:59:60)
    • Makes that day 86,401 seconds long
  • Controversy: May abolish leap seconds in favor of "leap hours" every few centuries

Current system:

  • UTC (Coordinated Universal Time): Atomic time with leap seconds
  • Keeps within 0.9 seconds of Earth rotation (UT1)
  • Used for civil timekeeping worldwide

Calendar Evolution

Ancient calendars:

  • Lunar calendars: Based on moon phases (~29.5 days per month)
  • Solar calendars: Based on seasonal year (365.25 days)
  • Lunisolar calendars: Combine both (Hebrew, Chinese)

Gregorian Calendar (1582):

  • Reformed Julian calendar
  • Year = 365.2425 days (very close to true solar year: 365.2422 days)
  • Leap year rules:
    • Divisible by 4: Leap year (1600, 2000, 2004, 2024)
    • Divisible by 100: Not leap year (1700, 1800, 1900)
    • Divisible by 400: Leap year anyway (1600, 2000, 2400)
  • Now used in nearly all countries for civil purposes

Ancient Observations (2000-300 BCE)

Babylonian astronomy (circa 2000-1500 BCE):

  • Babylonian astronomers tracked stellar positions for astrological and calendrical purposes
  • Noticed stars rose earlier each night relative to the Sun's position
  • Created star catalogs showing this gradual eastward drift

Greek astronomy (circa 600-300 BCE):

  • Thales of Miletus (624-546 BCE): Used stellar observations for navigation
  • Meton of Athens (432 BCE): Discovered the 19-year Metonic cycle, reconciling lunar months with solar years
  • Recognized that stellar year differed from seasonal year

Hipparchus and Precession (150 BCE)

Hipparchus of Nicaea (circa 190-120 BCE), one of history's greatest astronomers:

Discovery: By comparing ancient Babylonian star catalogs with his own observations, Hipparchus discovered precession of the equinoxes—the slow westward drift of the vernal equinox against the stellar background

Sidereal measurements: To detect this subtle effect (1 degree per 72 years), Hipparchus needed precise sidereal positions, implicitly understanding the sidereal day concept

Legacy: His work established the difference between:

  • Sidereal year: One orbit relative to stars (365.256363 days)
  • Tropical year: One cycle of seasons (365.242199 days)

The ~20-minute difference between these years arises from precession.

Ptolemy's Almagest (150 CE)

Claudius Ptolemy compiled Greek astronomical knowledge in the Almagest, including:

  • Star catalogs with sidereal positions
  • Mathematical models for predicting stellar rising times
  • Understanding that stars complete one full circuit of the sky slightly faster than the Sun

Though Ptolemy's geocentric model was wrong, his sidereal observations were accurate and useful for centuries.

Islamic Golden Age (800-1400 CE)

Islamic astronomers refined sidereal timekeeping:

Al-Battani (850-929 CE):

  • Measured the tropical year to high precision
  • Created improved star catalogs using sidereal positions

Ulugh Beg (1394-1449 CE):

  • Built the Samarkand Observatory with advanced instruments
  • Produced star catalogs accurate to ~1 arcminute using sidereal measurements

Copernican Revolution (1543)

Nicolaus Copernicus (De revolutionibus orbium coelestium, 1543):

Heliocentric model: Placing the Sun (not Earth) at the center explained the sidereal-solar day difference:

  • Earth rotates on its axis (sidereal day)
  • Earth orbits the Sun (creating solar day difference)
  • The 4-minute discrepancy results from Earth's ~1° daily orbital motion

This was strong evidence for heliocentrism, though it took decades for acceptance.

Kepler's Laws (1609-1619)

Johannes Kepler formulated laws of planetary motion using sidereal periods:

Third Law: The square of a planet's orbital period is proportional to the cube of its orbit's semi-major axis

Application: Calculating planetary positions required precise sidereal reference frames, not solar time

Rise of Telescopic Astronomy (1600s-1700s)

Galileo Galilei (1609):

  • Telescopic observations required tracking celestial objects as they moved across the sky
  • Sidereal time became essential for predicting when objects would be visible

Royal Observatory, Greenwich (1675):

  • Founded by King Charles II with John Flamsteed as first Astronomer Royal
  • Developed accurate sidereal clocks to time stellar transits
  • Greenwich Mean Sidereal Time (GMST) became the astronomical standard

Paris Observatory (1667):

  • French astronomers developed precision pendulum clocks for sidereal timekeeping
  • Cassini family produced detailed planetary observations using sidereal coordinates

Precision Timekeeping (1800s)

19th century: Mechanical sidereal clocks achieved second-level accuracy:

Sidereal clock design: Modified to tick 366.2422/365.2422 times faster than solar clocks (accounting for the extra sidereal day per year)

Observatory operations: Major observatories (Greenwich, Paris, Harvard, Lick, Yerkes) used sidereal clocks as primary timekeeping for scheduling observations

Photography: Long-exposure astrophotography required tracking objects at the sidereal rate to prevent star trailing

IAU Standardization (1900s)

International Astronomical Union (IAU) formalized definitions:

Mean sidereal day: 86,164.0905 seconds (exactly, by definition)

Greenwich Mean Sidereal Time (GMST): Standard sidereal time referenced to Greenwich meridian

Vernal equinox reference: Traditional sidereal time measures Earth's rotation relative to the vernal equinox (intersection of celestial equator and ecliptic)

Modern Era: ICRF (1997-Present)

International Celestial Reference Frame (ICRF):

Problem: The vernal equinox shifts due to precession, making it an imperfect reference

Solution: ICRF uses ~300 distant quasars (billions of light-years away) as fixed reference points

Accuracy: Defines celestial positions to milliarcsecond precision

Atomic time: Sidereal time is now calculated from International Atomic Time (TAI) and Earth orientation parameters measured by Very Long Baseline Interferometry (VLBI)

Modern sidereal clocks: Digital, GPS-synchronized, automatically updated for Earth rotation variations


Common Uses and Applications: days vs sidereal days

Explore the typical applications for both Day (imperial/US) and Sidereal Day (imperial/US) to understand their common contexts.

Common Uses for days

and Applications

1. Age and Lifespan Measurement

Human life measured in days:

  • Age calculation:

    • Newborn: Age in days (first month)
    • Infant: Days and weeks (first 12 months)
    • Adult: Years (365.25 days per year)
  • Life expectancy:

    • Global average: ~73 years = 26,645 days
    • US average: ~78 years = 28,470 days
    • Japan (highest): ~84 years = 30,660 days
  • Milestones:

    • 100 days: Traditional celebration in some cultures
    • 1,000 days: ~2.7 years (toddler milestone)
    • 10,000 days: ~27.4 years (young adult)
    • 20,000 days: ~54.8 years (mid-life)
    • 30,000 days: ~82.2 years (if reached, long life)
  • Historical figures:

    • "Lived 90 years" = 32,850 days
    • Queen Elizabeth II: 35,065 days (96 years, 140 days)
    • Oldest verified person: Jeanne Calment, 44,724 days (122 years, 164 days)

2. Project Management and Planning

Projects measured in days:

  • Timeline terminology:

    • "Day 0": Project start
    • "Elapsed days": Total calendar days
    • "Working days": Excluding weekends/holidays
    • "Man-days": One person working one day
  • Estimation:

    • "3-day task"
    • "2-week project" = 10 working days
    • "6-month project" = ~130 working days
  • Milestones:

    • "Deliverable due Day 30"
    • "Phase 1 complete Day 45"
    • "Final deadline Day 90"
  • Agile/Scrum:

    • Sprint: 14 days (2 weeks) typical
    • Daily standup: Every day, 15 minutes
    • Sprint review: End of 14-day sprint

3. Astronomy and Planetary Science

Planetary rotation periods measured in days:

  • Planetary "days" (rotation period):

    • Mercury: 58.6 Earth days
    • Venus: 243 Earth days (slower than its year!)
    • Earth: 1 day (23 hours 56 min sidereal)
    • Mars: 1.03 days (24 hours 37 min) - called a "sol"
    • Jupiter: 0.41 days (9 hours 56 min)
    • Saturn: 0.45 days (10 hours 33 min)
    • Uranus: 0.72 days (17 hours 14 min)
    • Neptune: 0.67 days (16 hours 6 min)
  • Orbital periods (years in days):

    • Mercury year: 88 Earth days
    • Venus year: 225 Earth days
    • Mars year: 687 Earth days
    • Earth year: 365.25 days
  • Mars missions:

    • Use "sols" (Mars days) for mission planning
    • Sol 1, Sol 2, Sol 3... (rovers like Curiosity, Perseverance)
    • Communication delay: 3-22 minutes (depends on planets' positions)
  • Astronomical events:

    • Lunar month: 29.53 days (new moon to new moon)
    • Eclipse cycles: Saros cycle = 6,585.3 days (18 years, 11 days)

4. Weather and Climate

Weather patterns measured in days:

  • Forecasting:

    • 1-day forecast: Very accurate (~90%)
    • 3-day forecast: Accurate (~80%)
    • 7-day forecast: Moderately accurate (~65%)
    • 10+ day forecast: Less reliable
  • Weather phenomena:

    • Heat wave: 3+ consecutive days above threshold
    • Cold snap: 2+ days below freezing
    • Drought: 15+ days without significant rain
  • Seasonal patterns:

    • Growing season: Number of frost-free days (150-200+ days)
    • Rainy season: 90-180 days (tropics)
    • Winter: Shortest day (winter solstice) vs. longest night
  • Degree days:

    • Heating degree days (HDD): Measure of cold
    • Cooling degree days (CDD): Measure of heat
    • Base 65°F: Sum of daily degrees below/above
  • Climate records:

    • "Hottest day on record"
    • "100 days above 90°F" (Phoenix averages 110+ days)
    • "Consecutive days of rain" (record: 331 days, Kauai)

5. Finance and Business

Financial operations measured in days:

  • Payment terms:

    • Net 30: Payment due 30 days after invoice
    • Net 60: Payment due 60 days after invoice
    • 2/10 Net 30: 2% discount if paid within 10 days, otherwise due in 30
  • Interest calculation:

    • Daily interest: Annual rate ÷ 365 days
    • Grace period: 21-25 days (credit cards)
    • Late fees: Applied after due date + grace period
  • Financial metrics:

    • Days sales outstanding (DSO): Average days to collect payment
    • Days payable outstanding (DPO): Average days to pay suppliers
    • Days inventory outstanding (DIO): Average days inventory held
  • Trading:

    • "Trading day": Stock market open day (weekdays, excluding holidays)
    • NYSE: ~252 trading days per year
    • Settlement: T+2 (trade day + 2 business days)
  • Bonds:

    • Accrued interest calculated by day
    • 30/360 day count convention (assumes 30-day months)
    • Actual/365: Uses actual calendar days

6. Data Storage and Computing

Digital retention measured in days:

  • Backups:

    • Daily backups: 7 days retained (1 week)
    • Weekly backups: 30 days retained (1 month)
    • Monthly backups: 365 days retained (1 year)
  • Logs:

    • Server logs: 30-90 days retention typical
    • Security logs: 90-365 days (compliance requirements)
    • Application logs: 14-30 days
  • Caching:

    • Browser cache: 30 days default
    • CDN cache: 1-30 days depending on content
    • DNS cache: 1 day (86,400 seconds TTL common)
  • Data retention policies:

    • GDPR: 30 days to fulfill deletion request
    • Email: Auto-delete after 90 days (some organizations)
    • Trash/recycle bin: 30 days before permanent deletion

7. Habits and Personal Development

Habit formation measured in days:

  • Popular beliefs:

    • "21 days to form a habit" (myth - actually varies widely)
    • "30-day challenge" (fitness, meditation, etc.)
    • "90-day transformation programs"
  • Research findings:

    • Average habit formation: 66 days (range: 18-254 days)
    • Simple habits: 18-30 days
    • Complex habits: 200+ days
  • Streaks:

    • "100-day streak" on language apps (Duolingo)
    • "30-day yoga challenge"
    • "365-day photo project" (one photo per day for a year)
  • Reading goals:

    • "Read every day for 30 days"
    • "One book per week" = finish in 7 days
    • "365 books in a year" = 1 per day

When to Use sidereal days

1. Telescope Pointing and Tracking

Professional observatories use sidereal time to point telescopes:

Right Ascension (RA): Celestial equivalent of longitude, measured in hours of sidereal time (0h to 24h)

Local Sidereal Time (LST): The current RA crossing the meridian

Pointing formula: If LST = 18h 30m, objects with RA ≈ 18h 30m are currently at their highest point (zenith)

Tracking rate: Telescope motors rotate at the sidereal rate (1 rotation per 23h 56m 4s) to follow stars across the sky as Earth rotates

Example:

  • Vega: RA = 18h 37m
  • When LST = 18:37, Vega crosses the meridian (highest in sky)
  • Observer can plan observations when object will be optimally placed

2. Astrophotography

Long-exposure astrophotography requires tracking at the sidereal rate:

Problem: Earth's rotation makes stars trail across the image during long exposures

Solution: Equatorial mounts with sidereal drive motors:

  • Rotate at exactly 1 revolution per sidereal day
  • Keep stars fixed in the camera's field of view
  • Enables exposures of minutes to hours without star trailing

Adjustment: Solar rate ≠ sidereal rate; photographers must use sidereal tracking for stars, solar tracking for Sun/Moon

3. Satellite Orbit Planning

Satellite engineers use sidereal time for orbit design:

Sun-synchronous orbits: Satellites that always cross the equator at the same local solar time

  • Orbital period is chosen to precess at the solar rate, not sidereal rate

Geosynchronous orbits: Satellites that hover over one point on Earth

  • Orbital period = 1 sidereal day (23h 56m 4s)
  • NOT 24 hours! Common misconception.

Molniya orbits: High-eccentricity orbits with period = 0.5 sidereal days for optimal high-latitude coverage

4. Very Long Baseline Interferometry (VLBI)

Radio astronomers use VLBI to achieve ultra-high resolution:

Technique: Combine signals from radio telescopes across continents

Timing requirement: Sidereal time must be synchronized to nanosecond precision across all telescopes

Result: VLBI can resolve features 1,000 times smaller than Hubble Space Telescope (angular resolution ~0.0001 arcseconds)

Application: Measures Earth's rotation variations by observing quasars at precise sidereal times

5. Navigation and Geodesy

Sidereal time is used for precise Earth orientation measurements:

Earth Orientation Parameters (EOPs):

  • Polar motion (wobble of Earth's axis)
  • UT1 (Earth rotation angle, related to Greenwich sidereal time)
  • Length of day variations

GPS accuracy: GPS navigation requires knowing Earth's orientation to ~1 meter precision, necessitating sidereal time corrections

Tidal forces: Moon and Sun create tidal bulges that affect Earth's rotation, causing sidereal day variations at the millisecond level

6. Space Navigation

Spacecraft use sidereal reference frames:

Star trackers: Autonomous spacecraft orientation using star patterns

  • Compare observed stellar positions with catalog
  • Catalog uses sidereal coordinates (RA/Dec)

Interplanetary navigation: Voyager, New Horizons, and other deep-space probes navigate using sidereal reference frames (ICRF)

Mars rovers: Use Martian sidereal time ("sols") for mission planning

  • 1 Mars sol = 24h 39m 35s (Mars rotates slower than Earth)

7. Amateur Astronomy

Amateur astronomers use sidereal time for planning:

Planispheres: Rotating star charts that show which constellations are visible at any given sidereal time and date

Computerized telescopes: GoTo mounts require accurate sidereal time for automatic star finding

Observation logs: Record sidereal time of observations for repeatability


Additional Unit Information

About Day (d)

How many hours are in a day?

Exactly 24 hours in a standard civil day.

This is a defined constant: 1 day = 24 hours = 1,440 minutes = 86,400 seconds.

Exception: Daylight Saving Time transitions create days with 23 hours (spring forward) or 25 hours (fall back) in regions that observe DST.

How many seconds are in a day?

Exactly 86,400 seconds in a standard day.

Calculation: 24 hours × 60 minutes × 60 seconds = 86,400 seconds

Since 1967, this equals 793,927,920,332,800,000 caesium-133 oscillations (~794 quadrillion).

Exception: Days with leap seconds have 86,401 seconds (last occurred December 31, 2016).

Is every day exactly 24 hours long?

For civil timekeeping: Yes. The day is defined as exactly 24 hours (86,400 seconds).

For Earth's rotation: No. Earth's actual rotation period varies:

  • Gradually slowing (~1.7 milliseconds per century) due to tidal friction from Moon
  • Seasonal variations (±1 millisecond) from atmospheric/oceanic changes
  • Irregular variations from earthquakes, ice melt, core-mantle coupling

Solution: Leap seconds occasionally added to keep clock time synchronized with Earth's rotation (within 0.9 seconds).

What's the difference between a solar day and a sidereal day?

Solar day (24 hours):

  • Time from one solar noon to the next (sun at highest point)
  • What we use for civil timekeeping
  • Accounts for Earth's orbit around sun

Sidereal day (23 hours, 56 minutes, 4 seconds):

  • Time for Earth to rotate 360° relative to distant stars
  • Used in astronomy for telescope tracking
  • ~4 minutes shorter than solar day

Why the difference? After Earth rotates 360° (one sidereal day), it has moved ~1° along its orbit. It must rotate an additional ~1° (~4 minutes) for the sun to return to the same position in the sky.

Result: 365 solar days per year, but 366 sidereal days per year (one extra rotation due to orbit).

Why does February have 28 days?

Historical reasons:

  1. Roman calendar (753 BCE):

    • Originally 10 months, 304 days (March-December)
    • Winter was monthless period
  2. Numa Pompilius reform (c. 713 BCE):

    • Added January and February
    • Romans considered even numbers unlucky
    • Made most months 29 or 31 days
    • February got leftover days: 28 (occasionally 29)
  3. Julius Caesar (45 BCE):

    • Julian calendar: 365.25-day year
    • Added day to February every 4 years (leap year)
    • February remained shortest month
  4. Pope Gregory XIII (1582):

    • Gregorian calendar reform
    • Refined leap year rules
    • February kept 28/29-day structure

Why not fix it? Changing calendar would disrupt billions of systems worldwide (contracts, software, cultural traditions).

How many days are in a year?

Common year: 365 days Leap year: 366 days

Solar/tropical year (Earth's orbit): 365.2422 days (365 days, 5 hours, 48 minutes, 46 seconds)

Leap year rules (Gregorian calendar):

  • Divisible by 4: Leap year (2024, 2028)
  • Divisible by 100: Not leap year (2100, 2200)
  • Divisible by 400: Leap year (2000, 2400)

Average Gregorian year: 365.2425 days (very close to true solar year)

Other calendar systems:

  • Islamic calendar: 354 days (lunar)
  • Hebrew calendar: 353-385 days (lunisolar, variable)
  • Julian calendar: 365.25 days (old system, now obsolete)

What is a leap second?

A leap second is an extra second added to clocks to keep atomic time synchronized with Earth's rotation.

Why needed:

  • Earth's rotation gradually slowing (tidal friction)
  • Atomic clocks run at constant rate (86,400 seconds per day)
  • Without leap seconds, clock time would drift from solar time

How it works:

  • Added at end of June 30 or December 31
  • Clock reads 23:59:59 → 23:59:60 → 00:00:00 (next day)
  • That day has 86,401 seconds instead of 86,400

History:

  • 27 leap seconds added between 1972-2016
  • Last one: December 31, 2016
  • None added since (Earth's rotation has been speeding up slightly)

Controversy:

  • Causes problems for computer systems
  • Proposed to abolish in favor of letting atomic time drift (then add "leap hour" every few centuries)

How do different cultures define when a day starts?

Different traditions begin the day at different times:

Midnight (00:00) - Modern civil time:

  • Used by most countries for official purposes
  • Inherited from Roman tradition
  • Convenient for business (avoids confusion around midday)

Sunset - Jewish and Islamic tradition:

  • Hebrew calendar: Day begins at sunset
  • Islamic calendar: Day begins at sunset
  • Biblical: "And there was evening, and there was morning—the first day"
  • Makes sense for agricultural societies

Dawn/Sunrise - Ancient Egypt, Hinduism:

  • Egyptian day began at sunrise
  • Hindu day traditionally begins at sunrise
  • Natural marker of "beginning" of daylight

Noon - Ancient Babylonians (some periods):

  • Based on sun at highest point
  • Astronomical reference

Modern inconsistency:

  • Civil day: Midnight
  • Religious calendars: Often sunset
  • Common language: "Day" often means daylight hours only

How old am I in days?

Formula: Age in days = (Years × 365.25) + extra days since last birthday

Example:

  • Born January 1, 2000
  • Today is November 26, 2024
  • Age: 24 years, 329 days
  • Days: (24 × 365.25) + 329 ≈ 9,095 days

Online calculators:

  • Many websites calculate exact age in days
  • Account for actual leap years experienced
  • Can calculate down to hours/minutes/seconds

Milestones:

  • 1,000 days: ~2.7 years old
  • 10,000 days: ~27.4 years old ("10,000-day birthday")
  • 20,000 days: ~54.8 years old
  • 30,000 days: ~82.2 years old (if reached)

Why is a week 7 days?

Ancient origins:

  1. Babylonian astronomy (c. 2000 BCE):

    • Seven visible celestial bodies: Sun, Moon, Mercury, Venus, Mars, Jupiter, Saturn
    • Each "ruled" one day
    • 7-day planetary week
  2. Biblical/Jewish tradition:

    • Genesis creation story: God created world in 6 days, rested on 7th
    • Sabbath (7th day) holy day of rest
    • Commandment: "Remember the Sabbath day"
  3. Roman adoption:

    • Romans adopted 7-day week (1st-3rd century CE)
    • Named days after planets/gods
    • Spread throughout Roman Empire
  4. Global spread:

    • Christianity spread 7-day week with Sunday as holy day
    • Islam adopted 7-day week with Friday as holy day
    • Now universal worldwide

Why not 10 days?

  • French Revolution tried 10-day week (1793-1805) - failed
  • USSR tried 5-day and 6-day weeks (1929-1940) - abandoned
  • 7-day week too culturally embedded to change

Day names (English):

  • Sunday: Sun's day
  • Monday: Moon's day
  • Tuesday: Tiw's day (Norse god)
  • Wednesday: Woden's day (Odin)
  • Thursday: Thor's day
  • Friday: Frigg's day (Norse goddess)
  • Saturday: Saturn's day

Can a day ever be longer or shorter than 24 hours?

For civil timekeeping: Usually no. A day is defined as exactly 24 hours (86,400 seconds).

Exceptions:

  1. Leap seconds:

    • Day with leap second = 86,401 seconds (0.001% longer)
    • 27 instances between 1972-2016
    • Adds one second at end of June 30 or December 31
  2. Daylight Saving Time:

    • "Spring forward" day: 23 hours (lose 1 hour)
    • "Fall back" day: 25 hours (gain 1 hour)
    • Only in regions observing DST
  3. Time zone transitions:

    • Crossing International Date Line can skip or repeat a day
    • Country changing time zones can alter day length
  4. Earth's actual rotation:

    • Varies by ±1 millisecond seasonally
    • Gradually slowing (~1.7 ms per century)
    • But civil day remains fixed at 86,400 seconds

Historical:

  • Ancient "seasonal hours" made days vary by season
  • Equal 24-hour days standardized with mechanical clocks (1300s)

About Sidereal Day (sidereal day)

How long is a sidereal day in standard time?

Answer: 23 hours, 56 minutes, 4.091 seconds (or 86,164.091 seconds)

This is the time for Earth to rotate exactly 360 degrees relative to distant stars.

Precise value: 1 mean sidereal day = 86,164.0905 seconds

Comparison to solar day:

  • Solar day: 86,400 seconds (24 hours)
  • Sidereal day: 86,164.091 seconds
  • Difference: ~236 seconds shorter (~3 min 56 sec)

Important: This is the mean sidereal day. Earth's actual rotation rate varies slightly (milliseconds) due to tidal forces, atmospheric winds, earthquakes, and core-mantle coupling.

Why is a sidereal day shorter than a solar day?

Answer: Because Earth orbits the Sun while rotating—requiring extra rotation to bring the Sun back to the same sky position

Step-by-step explanation:

  1. Starting point: The Sun is directly overhead (noon)

  2. One sidereal day later (23h 56m 4s): Earth has rotated exactly 360° relative to stars

    • But Earth has also moved ~1° along its orbit around the Sun
    • The Sun now appears slightly east of overhead
  3. Extra rotation needed: Earth must rotate an additional ~1° (taking ~4 minutes) to bring the Sun back overhead

  4. Result: Solar day (noon to noon) = sidereal day + ~4 minutes = 24 hours

Orbital motion causes the difference: Earth moves ~1°/day along its 365-day orbit (360°/365 ≈ 0.986°/day). This ~1° requires ~4 minutes of extra rotation (24 hours / 360° ≈ 4 min/degree).

Consequence: Stars rise ~4 minutes earlier each night relative to solar time, shifting ~2 hours per month, completing a full cycle annually.

Is sidereal time the same everywhere on Earth?

Answer: No—Local Sidereal Time (LST) depends on longitude, just like solar time zones

Key concepts:

Local Sidereal Time (LST): The Right Ascension (RA) currently crossing your local meridian

  • Different at every longitude
  • Changes by 4 minutes for every 1° of longitude

Greenwich Mean Sidereal Time (GMST): Sidereal time at 0° longitude (Greenwich meridian)

  • Global reference point, like GMT/UTC for solar time

Conversion: LST = GMST ± longitude offset

  • Positive (add) for east longitudes
  • Negative (subtract) for west longitudes

Example:

  • GMST = 12:00
  • New York (74°W): LST = 12:00 - (74°/15) = 07:04
  • Tokyo (139.75°E): LST = 12:00 + (139.75°/15) = 21:19

Duration is universal: A sidereal day (23h 56m 4s) is the same length everywhere—only the current sidereal time differs by location.

Do geosynchronous satellites orbit every 24 hours or 23h 56m?

Answer: 23h 56m 4s (one sidereal day)—NOT 24 hours!

This is one of the most common misconceptions about satellites.

The physics: For a satellite to remain above the same point on Earth's surface, it must orbit at Earth's rotational rate relative to the stars, not relative to the Sun.

Why sidereal?

  • Earth rotates 360° in one sidereal day (23h 56m 4s)
  • Satellite must complete 360° orbit in the same time
  • This keeps satellite and ground point aligned relative to the stellar background

If orbit were 24 hours: The satellite would complete one orbit in one solar day, but Earth would have rotated 360° + ~1° (relative to stars) during that time. The satellite would drift ~1° westward per day, completing a full circuit westward in one year!

Geostationary orbit specifics:

  • Altitude: 35,786 km above equator
  • Period: 23h 56m 4.091s (1 sidereal day)
  • Velocity: 3.075 km/s

Common examples: Communications satellites, weather satellites (GOES, Meteosat)

How many sidereal days are in a year?

Answer: Approximately 366.25 sidereal days—one MORE than the number of solar days!

Precise values:

  • Tropical year (season to season): 365.242199 mean solar days
  • Sidereal year (star to star): 365.256363 mean solar days
  • Sidereal days in tropical year: 366.242199 sidereal days

One extra day: There is exactly one more complete rotation relative to stars than we experience sunrises.

Why?

  • Earth makes 366.25 complete 360° rotations relative to stars per year
  • But we experience only 365.25 sunrises because we orbit the Sun
  • One rotation is "used up" by Earth's orbit around the Sun

Thought experiment: Stand on a rotating platform while walking around a lamp. If you walk one complete circle around the lamp (1 orbit), you'll have spun around 2 complete times relative to the room walls (2 rotations): 1 from walking the circle + 1 from the platform spinning.

Can I use a regular clock to tell sidereal time?

Answer: Not directly—sidereal clocks run about 4 minutes faster per day than solar clocks

Clock rate difference:

  • Solar clock: Completes 24 hours in 1 solar day (86,400 seconds)
  • Sidereal clock: Completes 24 sidereal hours in 1 sidereal day (86,164.091 seconds)
  • Rate ratio: 1.00273791 (sidereal clock ticks ~0.27% faster)

Practical result: After one solar day:

  • Solar clock reads: 24:00
  • Sidereal clock reads: 24:03:56 (3 min 56 sec ahead)

Modern solutions:

  • Sidereal clock apps: Smartphone apps calculate LST from GPS location and atomic time
  • Planetarium software: Stellarium, SkySafari show current LST
  • Observatory systems: Automated telescopes use GPS-synchronized sidereal clocks

Historical: Mechanical sidereal clocks used gear ratios of 366.2422/365.2422 to run at the correct rate

You can calculate: LST from solar time using formulas, but it's complex (requires Julian Date, orbital mechanics)

Why do astronomers use sidereal time instead of solar time?

Answer: Because celestial objects return to the same position every sidereal day, not solar day

Astronomical reason:

Stars and galaxies are so distant they appear "fixed" in the sky:

  • A star at RA = 18h 30m crosses the meridian at LST = 18:30 every sidereal day
  • Predictable, repeatable observations

If using solar time: Stars would cross the meridian ~4 minutes earlier each night, requiring daily recalculation of observation windows

Practical advantages:

1. Simple telescope pointing:

  • Object's RA directly tells you when it's overhead (LST = RA)
  • No date-dependent calculations needed

2. Repeatable observations:

  • "Observe target at LST = 22:00" means the same sky position regardless of date

3. Right Ascension coordinate system:

  • Celestial longitude measured in hours/minutes of sidereal time (0h to 24h)
  • Aligns naturally with Earth's rotation

4. Tracking rate:

  • Telescopes track at sidereal rate (1 revolution per 23h 56m 4s)
  • Keeps stars fixed in the field of view

Historical: Before computers, sidereal time made astronomical calculations much simpler

What is the difference between a sidereal day and a sidereal year?

Answer: A sidereal day measures Earth's rotation; a sidereal year measures Earth's orbit

Sidereal Day:

  • Definition: Time for Earth to rotate 360° on its axis relative to stars
  • Duration: 23h 56m 4.091s (86,164.091 seconds)
  • Reference: Distant "fixed" stars
  • Use: Telescope tracking, astronomy observations

Sidereal Year:

  • Definition: Time for Earth to orbit 360° around the Sun relative to stars
  • Duration: 365.256363 days (365d 6h 9m 9s)
  • Reference: Position relative to distant stars (not seasons)
  • Use: Orbital mechanics, planetary astronomy

Key distinction:

  • Day = rotation (Earth spinning)
  • Year = revolution (Earth orbiting)

Tropical vs. Sidereal Year:

  • Tropical year: 365.242199 days (season to season, used for calendars)
  • Sidereal year: 365.256363 days (star to star)
  • Difference: ~20 minutes, caused by precession of Earth's axis

The 20-minute precession effect: Earth's axis wobbles with a 26,000-year period, causing the vernal equinox to shift ~50 arcseconds/year westward against the stellar background. This makes the tropical year (equinox to equinox) slightly shorter than the sidereal year (star to star).

Does the Moon have a sidereal day?

Answer: Yes—the Moon's sidereal day is 27.322 Earth days, but it's tidally locked to Earth

Moon's sidereal rotation: Time for Moon to rotate 360° relative to stars = 27.322 days

Tidal locking: The Moon's rotation period equals its orbital period around Earth (both 27.322 days)

Consequence: The same face of the Moon always points toward Earth

  • We only see ~59% of Moon's surface from Earth (libration allows slight wobbling)
  • The "far side" never faces Earth

Moon's "solar day" (lunar day):

  • Time from sunrise to sunrise on Moon's surface: 29.531 Earth days
  • Different from Moon's sidereal day (27.322 days) for the same reason Earth's solar day differs from sidereal day
  • Moon orbits Earth while rotating, requiring extra rotation to bring the Sun back to the same position

Lunar missions: Apollo missions and rovers used "lunar days" for mission planning—each day-night cycle lasts ~29.5 Earth days (2 weeks daylight, 2 weeks night)

How is sidereal time measured today?

Answer: Using atomic clocks, GPS, and Very Long Baseline Interferometry (VLBI) observations of distant quasars

Modern measurement system:

1. International Atomic Time (TAI):

  • Network of ~450 atomic clocks worldwide
  • Defines the second with nanosecond precision
  • Provides base timescale

2. UT1 (Universal Time):

  • Earth's rotation angle (actual rotation measured continuously)
  • Monitored by VLBI observations of quasars

3. VLBI technique:

  • Radio telescopes across continents simultaneously observe distant quasars
  • Time differences reveal Earth's exact orientation
  • Accuracy: ~0.1 milliseconds (0.005 arcseconds rotation)

4. ICRF (International Celestial Reference Frame):

  • Defines "fixed" stellar background using ~300 quasars billions of light-years away
  • Replaces older vernal equinox reference (which shifts due to precession)

5. GPS satellites:

  • Amateur astronomers and observatories use GPS for accurate time and location
  • Software calculates LST from UTC, GPS coordinates, and Earth orientation parameters

Calculation chain:

  1. Atomic clocks provide UTC
  2. Earth orientation parameters (EOP) give UT1
  3. Sidereal time formulas convert UT1 → GMST
  4. Longitude correction gives LST

Accuracy: Modern systems know Earth's orientation to ~1 centimeter (as a position on Earth's surface), requiring sidereal time precision of ~0.001 seconds

Why so complex? Earth's rotation is not uniform:

  • Tidal forces (Moon/Sun) slow rotation by ~2.3 ms/century
  • Atmospheric winds cause daily variations (milliseconds)
  • Earthquakes can shift rotation by microseconds
  • Core-mantle coupling affects long-term drift

Continuous monitoring ensures astronomical observations remain accurate.

Will sidereal time ever be replaced by something else?

Answer: Unlikely—it's fundamental to astronomy, tied directly to Earth's rotation and stellar positions

Why sidereal time persists:

1. Physical basis: Directly tied to Earth's rotation relative to the universe

  • Not an arbitrary human convention like time zones
  • Essential for understanding celestial mechanics

2. Coordinate system: Right Ascension (celestial longitude) is measured in sidereal hours

  • All star catalogs, telescope systems, and astronomical databases use RA/Dec
  • Replacing it would require re-cataloging billions of objects

3. Telescope tracking: All telescope mounts track at the sidereal rate

  • Mechanically and electronically built into equipment
  • Solar tracking is used only for Sun/Moon

4. International standards: IAU, observatories, space agencies globally use sidereal time

  • Standardized formulas and software

5. No alternative needed: Sidereal time does its job perfectly for astronomy

Evolution, not replacement:

  • Old reference: Vernal equinox (shifts due to precession)
  • New reference: ICRF quasars (effectively fixed)
  • Future: Increasingly precise atomic timescales and Earth rotation monitoring

Non-astronomical contexts: Civil society will continue using solar time (UTC) for daily life—there's no need for most people to know sidereal time

Conclusion: Sidereal time is here to stay as long as humans do astronomy from Earth. Even space-based observatories use sidereal coordinate systems for consistency with ground observations.


Conversion Table: Day to Sidereal Day

Day (d)Sidereal Day (sidereal day)
0.50.501
11.003
1.51.504
22.006
55.014
1010.027
2525.068
5050.137
100100.274
250250.685
500501.369
1,0001,002.738

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What is the conversion factor from Day to Sidereal Day?

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NIST Time and Frequency

National Institute of Standards and TechnologyOfficial time standards and definitions

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Bureau International des Poids et MesuresDefinition of the SI base unit for time

Last verified: December 3, 2025