Lunar Eclipse Calculator
Lunar Eclipse Calculator
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Danjon Scale — Total Eclipse Darkness Rating
Eclipse Frequency by Decade
Eclipse data sourced from NASA/GSFC Five Millennium Catalog of Lunar Eclipses (eclipse.gsfc.nasa.gov) and EclipseWise (Fred Espenak). Times accurate to ±1 minute for 2026–2032.
Upcoming eclipses, contact times, and Blood Moon data — 2026 to 2032
A lunar eclipse is one of the most dramatic and accessible astronomical events visible to the naked eye. Unlike solar eclipses — which require you to be in a narrow path of totality — a lunar eclipse can be seen from anywhere on Earth where the Moon is above the horizon during the event. This Lunar Eclipse Calculator is your complete reference guide to upcoming lunar eclipses from 2026 through 2032, providing eclipse dates, types, contact times, duration, umbral magnitude, geographic visibility, and Saros series information sourced from NASA/GSFC and EclipseWise (Fred Espenak). Lunar eclipses occur when the Earth passes directly between the Sun and the Moon, casting its shadow across the lunar surface. There are three distinct types: penumbral eclipses, where the Moon passes through Earth's outer shadow and experiences only a subtle darkening; partial eclipses, where part of the Moon enters Earth's darker inner shadow (the umbra) and a clear dark 'bite' is visible; and total lunar eclipses — commonly called Blood Moons — where the Moon is fully immersed in the umbra and glows a striking deep red or orange color. This red color occurs because Earth's atmosphere refracts and bends sunlight around the edges of the planet, filtering out blue wavelengths while allowing red and orange light to reach the Moon. This tool covers twelve upcoming lunar eclipses — including six total (Blood Moon) events. The next is the spectacular total lunar eclipse on March 3, 2026, with an umbral magnitude of 1.151 and nearly an hour of totality visible across East Asia, Australia, the Pacific, and the Americas. The deepest eclipse in this period is the June 26, 2029 total eclipse, with an extraordinary umbral magnitude of 1.844 — one of the deepest in decades — producing over 1 hour and 42 minutes of totality. The New Year's Eve 2028 total eclipse (December 31) will be visible across Europe, Africa, Asia, and Australia, making it widely observed worldwide. For each eclipse, this calculator provides the standard contact times: P1 (penumbral begins), U1 (partial begins), U2 (totality begins), Greatest (deepest point), U3 (totality ends), U4 (partial ends), and P4 (penumbral ends). Times are stored in UTC and automatically converted to your local time zone using your browser's timezone or a manual UTC offset selection. You can filter eclipses by year, type (Total/Partial/Penumbral), and visibility region (Americas, Europe, Africa, Asia, Australia, Pacific), and export the filtered list as a CSV file for offline reference. The Saros cycle is the 18-year, 11-day, 8-hour astronomical period after which eclipses of the same series repeat in nearly the same geometry. The 2026 March 3 eclipse belongs to Saros 133, the 27th of 71 total eclipses in that series; the 2028 December 31 eclipse belongs to Saros 125; and the deepest 2029 June 26 eclipse is from Saros 130. Understanding Saros series helps eclipse enthusiasts track eclipse families across centuries. The Danjon scale (L0 to L4) rates the darkness and color of total lunar eclipses at mid-totality. An L0 eclipse is nearly invisible — very dark brown or black — while an L4 eclipse is bright copper-red or orange with visible surface detail. The exact Danjon rating depends on Earth's current atmospheric conditions (volcanic aerosols, dust, cloud cover at the eclipse limb) and cannot be predicted precisely in advance. However, eclipses with higher umbral magnitudes tend to produce more dramatic coloration. Whether you are a casual skywatcher hoping to catch the next Blood Moon, an astrophotographer planning your setup, an educator teaching eclipse geometry, or simply curious about when the next lunar eclipse will be visible from your country, this calculator provides the complete, accurate information you need — all sourced from NASA/GSFC Five Millennium Catalog data and EclipseWise ephemeris computations.
Understanding Lunar Eclipses
What Is a Lunar Eclipse?
A lunar eclipse occurs when the Earth aligns directly between the Sun and the Full Moon, casting Earth's shadow onto the lunar surface. Eclipses only happen at Full Moon, but not every Full Moon produces an eclipse because the Moon's orbit is tilted about 5.1 degrees relative to the ecliptic — Earth's orbital plane. Eclipses only occur when a Full Moon coincides with the Moon being near one of the two orbital nodes where the Moon's orbit crosses the ecliptic. There are three types: penumbral (Moon passes through Earth's faint outer shadow only), partial (Moon partly enters the dark inner umbra), and total (Moon is fully engulfed in the umbra, turning red — the 'Blood Moon'). Total lunar eclipses occur roughly once every 1.5 years on average, though they cluster in pairs or triads within a few years of each other.
How Are Eclipse Times Calculated?
Precise lunar eclipse times are computed using solar and lunar ephemerides — mathematical models of planetary motions derived from gravitational theory and radar measurements. NASA's primary reference is the JPL DE406 ephemeris (used by EclipseWise/Fred Espenak) and DE430 for more recent work. The key parameter is the gamma value — the minimum angular distance between the Moon's center and Earth's shadow axis, measured in Earth equatorial radii at the Moon's distance. Contact times (P1, U1, U2, Greatest, U3, U4, P4) are determined by when this geometry produces specific angular relationships between the shadow radii and the Moon's disk. Umbral magnitude = (umbra radius + Moon radius − |gamma|) / (2 × Moon radius). A value ≥ 1.0 indicates a total eclipse. All times in this tool are pre-computed from NASA/GSFC Five Millennium Catalog data. Local time conversion is done client-side by adding the user's UTC offset.
Why Do Lunar Eclipses Matter?
Lunar eclipses have captivated humanity for millennia — ancient astronomers used them to measure Earth's radius, determine the Moon's distance, and confirm Earth is spherical (from the curved shadow edge). Today, they remain one of the most accessible astronomical phenomena: no special equipment is needed, they last hours, and they are visible hemisphere-wide. For astrophotographers, total lunar eclipses are prime opportunities to capture the Blood Moon's deep red color. For educators, they demonstrate orbital mechanics and the geometry of shadows. Scientists study lunar eclipses to measure changes in Earth's atmospheric opacity — a volcanic eruption can darken the shadow significantly, as seen after the 1991 Pinatubo eruption. Amateur astronomers use contact timing to verify positional accuracy of eclipse predictions and calibrate local telescope alignments.
Limitations and Data Precision
All contact times in this tool are pre-computed reference data from NASA/GSFC and EclipseWise, accurate to within ±1 minute for eclipses through 2032. Precise ephemeris-level accuracy requires accounting for the Moon's varying orbital speed, Earth's rotation (Delta-T correction), and the exact lunar distance at eclipse time (which affects shadow size). The Delta-T correction for near-future eclipses (2026–2032) is approximately 70–80 seconds — less than two minutes — and does not materially affect observing plans. Visibility regions in this tool are continent-level only; for precise local circumstances (Moon altitude, azimuth, and moonrise/moonset during eclipse), the U.S. Naval Observatory Lunar Eclipse Computer provides the most exact topocentric results. Danjon scale ratings cannot be predicted in advance because they depend on Earth's atmospheric conditions on eclipse day.
Formulas
Measures the fraction of the Moon's diameter immersed in Earth's umbral shadow at greatest eclipse. γ (gamma) is the minimum distance of the Moon's center from the shadow axis in Earth radii. Values ≥ 1.0 indicate a total eclipse; < 0 indicates penumbral only.
After one Saros period, the Sun, Earth, and Moon return to nearly the same relative geometry, producing an eclipse with similar characteristics. The 8-hour remainder shifts each successive eclipse ~120° west in longitude.
Where R_umbra is the umbral shadow radius at the Moon's distance, d_min is the Moon's closest approach to the shadow center, and v_moon is the Moon's orbital velocity (~1.023 km/s). Deeper eclipses (smaller d_min) produce longer totality, up to a theoretical maximum of ~107 minutes.
Reference Tables
Upcoming Total Lunar Eclipses (2026–2032)
| Date | Umbral Magnitude | Totality Duration | Saros | Best Visibility |
|---|---|---|---|---|
| March 3, 2026 | 1.151 | 58 min | 133 | E Asia, Australia, Pacific, Americas |
| December 31, 2028 | 1.246 | 71 min | 125 | Europe, Africa, Asia, Australia |
| June 26, 2029 | 1.844 | 102 min | 130 | Americas, Europe, Africa |
| December 20, 2029 | 1.117 | 54 min | 135 | E Asia, Australia, Pacific, Americas |
| April 25, 2032 | 1.189 | 65 min | 122 | Asia, Australia, Pacific |
| October 18, 2032 | 1.104 | 48 min | 127 | Americas, Europe, Africa |
Danjon Scale — Lunar Eclipse Brightness
| Scale | Brightness | Color | Description |
|---|---|---|---|
| L0 | Very dark | Dark brown/black | Moon nearly invisible at mid-totality; often after volcanic eruptions |
| L1 | Dark | Gray-brown | Little surface detail visible; dark coloration throughout |
| L2 | Moderate | Deep red/rust | Typical eclipse; dark center with brighter edge; some detail |
| L3 | Bright | Brick-red | Bright eclipse with yellowish rim; surface features clearly visible |
| L4 | Very bright | Copper/orange | Vivid orange-red; sharp limb; full surface detail visible |
Worked Examples
Contact Time Conversion — March 3, 2026 Eclipse
New York (UTC-5): 11:04 − 5 hours = 06:04 EST on March 3
London (UTC+0): 11:04 + 0 hours = 11:04 GMT on March 3
Tokyo (UTC+9): 11:04 + 9 hours = 20:04 JST on March 3
Understanding Eclipse Depth from Magnitude
Umbral magnitude 1.844 means the Moon's center passes 0.844 Moon-diameters past the edge of the umbra
For comparison, the threshold for total is 1.000 (Moon just fits inside the umbra)
A typical total eclipse has magnitude 1.1–1.4
Magnitude 1.844 is exceptionally deep — the Moon passes nearly through the center of Earth's shadow
Totality duration: approximately 102 minutes (1 hr 42 min) — near the theoretical maximum
Saros Series Prediction
One Saros = 6,585.3 days = 18 years, 11 days, 8 hours
Previous eclipse: March 3, 2026 − 18 years 11 days = February 20, 2008
The February 2008 total lunar eclipse was indeed a Saros 133 event (umbral mag 1.111)
Next eclipse: March 3, 2026 + 18 years 11 days = March 14, 2044
The 8-hour shift means the 2044 eclipse will be centered ~120° west of the 2026 event
How to Use This Calculator
Check the Countdown
The live countdown at the top shows the exact days, hours, minutes, and seconds until the next upcoming lunar eclipse, plus a separate countdown to the next total Blood Moon. This updates every second in real time.
Filter by Year, Type, or Region
Use the filter panel on the left to narrow down eclipses. Select a specific year, choose Total/Partial/Penumbral only, or filter to eclipses visible from your continent. All matching eclipses appear in the results list.
Click Any Eclipse for Full Details
Click on any eclipse card to expand it and see the complete phase timeline bar, umbral magnitude indicator, all seven contact times (P1 through P4), Saros series number, obscuration percentage, and eclipse depth classification.
Set Your Time Zone for Local Times
Your browser's time zone is auto-detected. Toggle 'Show times in local time zone' to switch all contact times from UTC to your local time. You can also manually adjust the UTC offset if needed, then export as CSV or print for offline reference.
Frequently Asked Questions
When is the next total lunar eclipse (Blood Moon)?
The next total lunar eclipse is on March 3, 2026. It will be visible from East Asia, Australia, the Pacific, and large parts of the Americas. The eclipse begins when the Moon enters Earth's penumbra at 08:44 UTC, with totality (the Blood Moon phase) lasting from 11:04 to 12:02 UTC — about 58 minutes. The umbral magnitude is 1.151, meaning the Moon is fully immersed in Earth's umbra. After that, the next total eclipses are December 31, 2028, then June 26, 2029 (the deepest eclipse of the period with magnitude 1.844), and December 20, 2029.
Why does the Moon turn red during a total lunar eclipse?
During a total lunar eclipse, the Moon is fully inside Earth's umbra and receives no direct sunlight. However, Earth's atmosphere acts like a lens, refracting and bending sunlight around the edge of the planet. This refraction filters out most blue and green wavelengths (which scatter in the atmosphere, causing blue skies) and allows red and orange wavelengths to reach the Moon. The result is the striking deep red, rust, or orange color known as the 'Blood Moon.' The exact shade depends on Earth's current atmospheric conditions — volcanic eruptions, dust storms, and cloud cover at the eclipse's limb can darken or redden the Moon significantly.
What is umbral magnitude and how does it relate to eclipse depth?
Umbral magnitude is the fraction of the Moon's diameter that is immersed in Earth's umbral (inner) shadow at the moment of greatest eclipse. A value of 0 means the Moon just grazes the umbra's edge (a very shallow partial), 0.5 means half the Moon's diameter is in the umbra, and values at or above 1.0 indicate a total eclipse (the entire Moon fits inside the umbra). Values above 1.5 produce deep totality with very dark coloration, and values above 1.8 (like the June 2029 eclipse at 1.844) represent extraordinarily deep eclipses with the longest possible totality durations. Negative umbral magnitude values mean a penumbral-only eclipse.
What is a Saros cycle and why is it important?
A Saros cycle is an astronomical period of approximately 6,585.3 days — about 18 years, 11 days, and 8 hours — after which the Sun, Earth, and Moon return to nearly the same relative geometry. This means eclipses in the same Saros series repeat with very similar characteristics (contact times, magnitude, and duration) roughly every 18 years. Because of the 8-hour fractional day, each successive eclipse in a series shifts about 120 degrees westward in longitude. After three Saros periods (one Exeligmos = 54 years, 33 days), eclipses recur at nearly the same geographic location. The 2026 March 3 eclipse belongs to Saros 133, the 27th of 71 total eclipses in that 1,262-year series.
Can I see a lunar eclipse with the naked eye?
Yes — lunar eclipses are one of the most accessible astronomical events because no special equipment is needed. Total and partial eclipses are clearly visible to the naked eye from anywhere the Moon is above the horizon. Total eclipses are especially dramatic as the Moon turns deep red. Penumbral eclipses are the exception — the Moon's dimming is very subtle and may only be noticeable near maximum coverage (greater than about 70% penumbral magnitude). Binoculars enhance the view for any eclipse type. The best viewing conditions are away from artificial lights, with the Moon high in the sky and clear skies. Contact times mark the key moments to observe — U1 for the start of the shadow bite, U2 for Blood Moon onset, and Greatest for the deepest red.
What is the Danjon scale and can I predict it for an upcoming eclipse?
The Danjon scale (L0 to L4) rates the brightness and color of the Moon during total eclipse totality. L0 is nearly black (Moon barely visible), L1 is dark gray/brown, L2 is deep red or rust, L3 is brick-red with a bright rim, and L4 is bright copper or orange with visible lunar surface detail. Unfortunately, the Danjon rating cannot be predicted in advance because it depends on Earth's atmospheric transparency at the moment of eclipse — primarily the amount of dust, aerosols, and cloud cover along the eclipse limb at the time. After major volcanic eruptions (like Pinatubo in 1991), eclipses can become extremely dark (L0–L1). During normal atmospheric conditions, eclipses typically rate L2–L3. The rating is determined by observers worldwide after the event.