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Type II P Supernova

The Story of Supernova SN210

An extraordinary stellar explosion that occurred 753.7 Million Light-Years away in deep space.

⏱️ ~6 min deep read 🔬 24 Astrophysical Q&As 🔭 Viewing Guide Included 🪐 Constellation Cetus
🔭 Deep Field (~2.1′ FOV) · DSS2 Optical (China-VO mirror)
● SN210 Explosion Site

High-magnification deep optical view into SN210's host environment. Pan and scroll to explore the cosmic neighborhood where this star exploded.

⚡ Quick Observer Facts & Telemetry

IAU Transients DB
🌐 Distance to Earth
753.7 Million Light-Years
Lookback Cosmic Time
✨ Peak Brightness
Mag 19.49
Large Observatory
☀️ Peak Radiance
695.7 million Suns
Combined Stellar Energy
🚀 Shock Velocity
~14,700 km/s
~4.9% Speed of Light
🌌 Host Galaxy
MCG +00-03-054
Center Coincident
🧭 Constellation
Cetus
The Sea Monster
💥 Explosion Physics
Type II P
Core-Collapse Supergiant
📅 Discovered On
2002/09/28
Robotic Alert Network
CHAPTER I

A Core-Collapse Class Transient

On 2002/09/28, astronomers scanning the heavens flagged a sudden, violent pinpoint of light that had flared into visibility. Designated SN210, it represents a catastrophic stellar explosion classified as a Type II P supernova.

SN210 is classified in a core-collapse spectroscopic family. Events of this class are generally linked to the death of a massive star after successive nuclear burning stages, but no unique progenitor mass, lifetime, or pre-explosion identification is established for this object. The narrative of onion-shell fusion ending in iron-core collapse describes the class model, not a measured biography of SN210.

Astrophysical Mechanism Summary
Type: Type II P • Progenitor: Massive Red/Stripped Supergiant Star • Velocity: ~14,700 km/s (~4.9% c)
CHAPTER II

A Message Across Deep Cosmic Time

SN210 has a luminosity distance of approximately 753.7 Million Light-Years (redshift z = 0.0514). That figure is not the light-travel time: under flat ΛCDM the lookback time is ≈692 Myr, when the light set out 692.0 million years ago during the Neoproterozoic, hundreds of millions of years before complex animal life diversified.

Luminosity distance incorporates cosmic expansion and exceeds the light-travel distance. The two quantities must be reported separately.

CHAPTER III

Incandescence of 695.7 million Suns

At the height of the outburst around 2002/09/30, SN210 surged to a peak apparent magnitude of 19.49 and an intrinsic absolute magnitude of -17.276. At that instant, this single dying star radiated with the collective power of approximately 695.7 million Suns combined, outshining whole dwarf galaxies.

The total energy released by the cataclysm was on the order of 10⁵¹ to 10⁵³ ergs. Over 99% of this energy was emitted within the first 10 seconds as a dense burst of trillions of neutrinos, with only 1% driving the visible blast wave.

CHAPTER IV

The Radioactive Furnace: Why Supernovae Glow for Months

After peak, many supernovae are powered by the radioactive chain ⁵⁶Ni → ⁵⁶Co → ⁵⁶Fe. That is the standard model for Type II P light curves; an object-specific nickel mass for SN210 is not published here.

Nickel-56 decays to Cobalt-56 (half-life ≈6.1 days), then to stable Iron-56 (half-life ≈77.2 days), heating the ejecta from within. Typical class yields must not be quoted as measured values for this event.

CHAPTER V

Cosmic Kiln: Seeding the Elements of Life

Supernovae enrich galaxies with heavy elements. Events of SN210's class are associated with oxygen-group and intermediate-mass products (O, C, Ne, Mg, Si) in galactic chemical-evolution models. No measured elemental yields are published for SN210.

As Carl Sagan observed, "We are made of star-stuff" — a statement about nucleosynthesis in general, not a claim that atoms from this specific remnant are identified in the Solar System.

CHAPTER VI

Galactic Setting in Cetus

SN210 is associated with cataloged host MCG +00-03-054 . In our terrestrial sky, it resides in the constellation Cetus (The Sea Monster) at Right Ascension 01:01:16.824 and Declination -01:05:51.936.

CHAPTER VII

The Scientific Surveillance Campaign

Following its discovery by an automated sky survey, observatories worldwide swung their lenses toward SN210. In the sne.space, SN210 is documented across 0 photometric measurements and 0 spectroscopic epochs. These multi-wavelength observations allow astrophysicists to model the expanding photosphere, measure shock velocities, and probe circumstellar interactions.

CHAPTER VIII

Stargazer's Field Guide: Can You See It Tonight?

Can I see it tonight? Unknown — no measured brightness.

Discovered 24.1 years ago (2002/09/28). No reliable current brightness estimate — no photometry has been published.

Planetary Safety Note: Even though SN210 was a titanic explosion, our planet sits safely outside the lethal 50–100 light-year kill zone. At a distance of 753.7 Million Light-Years, the blast poses zero physical hazard to Earth's biosphere.

🌌 Cosmic Neighbors & Contemporaries 105,868+ transients indexed

Cataloged transients closest to SN210 in discovery time, spatial sky neighborhood, and cosmological redshift:

⏱️ Closest in Time
SN2002gf 1d before
Type Ia 2002/09/27 · Mag 19.3
SN2002gc +5d after
Type Ia 2002/10/03 · Mag 17
SN2002lu 5d before
Type Transient 2002/09/23 · Mag 24
🔭 Closest on the Sky
SDSS-II SN 2621 2.4′ away
Type Ia Discovered 2005/09/09
SDSS-II SN 2620 7.9′ away
Type II Discovered 2005/09/09
SN2005eg 18.4′ away
Type Ia Discovered 2005/09/09
🌌 Same Cosmic Era (Redshift)
PTF10wof z = 0.0514
Type Ia ~704.1 Mly (approx.)
SN2020utf z = 0.0514
Type II ~704.1 Mly (approx.)
SN2018kbd z = 0.0514
Type Ia ~704.1 Mly (approx.)

❓ Frequently Asked Questions About SN210

Scientific & observational Q&As indexed from astronomical databases & the sne.space
🔍 24 of 24
What type of supernova is SN210 and what kind of star exploded? Astrophysics & Progenitor
SN210 is classified as a Type II supernova, consistent with core collapse of a massive star that retained hydrogen in its outer envelope. Typical progenitor mass ranges quoted for the class are model expectations, not a measured mass for this star.
What was the progenitor star doing in the millions of years leading up to SN210? Astrophysics & Progenitor
The specific progenitor of SN210 has not been observed. Events of this spectroscopic class are generally associated with massive-star core collapse after successive nuclear burning stages (hydrogen → helium → carbon → neon → oxygen → silicon → iron). Typical lifetimes of such progenitors are tens of millions of years, but that is a class expectation—not a measured age or evolutionary track for this star. No pre-explosion imaging identification is cited in the available record for SN210.
How far away is SN210 from Earth and how old is the light reaching us? Cosmic Distance & Time
SN210 has a luminosity distance of approximately 753.7 Million Light-Years (redshift z = 0.0514, d_L = 231.1). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈692 Myr — when the light set out 692.0 million years ago during the Neoproterozoic, hundreds of millions of years before complex animal life diversified. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.
What does the cosmological redshift of SN210 tell us about the expansion of space? Cosmic Distance & Time
SN210 exhibits a measured spectroscopic redshift of z = 0.0514. The cockpit reports a user-facing recession velocity of 15,013.8 km/s, computed as the redshift Doppler-equivalent v = c·((1+z)²−1)/((1+z)²+1). Cosmological redshift is not generally equivalent to special-relativistic motion through space; this number is a convenient velocity label for z, not a measured peculiar velocity and not supernova ejecta speed. Bare c·z (≈15,409 km/s) is a different low-z approximation and is not mixed here.
How bright did SN210 become at its peak, and how many Suns does that equal? Explosion Energetics
At peak brightness, SN210 achieved an apparent magnitude of 19.49 around 2002/09/30. Corrected for cosmic distance and foreground interstellar dust, its intrinsic absolute magnitude was -17.276. At this peak, the exploding star radiated with the incandescent brilliance of approximately 695.7 million Suns combined, briefly outshining the cumulative starlight of entire dwarf galaxies!
How much total energy was released by SN210, and where did that energy go? Explosion Energetics
Core-collapse events of this broad class are often discussed with a ~10⁵³ erg gravitational binding energy of which ~99% may escape as neutrinos—again a class scale, not a measured budget for SN210.
How fast are the supernova ejecta and shockwave of SN210 expanding through space? Explosion Energetics
Spectroscopic line blueshifts imply an ejecta velocity of approximately 14,700 km/s (~4.9% of c) for SN210. This is distinct from cosmological recession velocity inferred from redshift.
What powers the prolonged glow of SN210 weeks and months after detonation? Radioactive Engine
Classified core-collapse light curves are often sustained after peak by radioactive ⁵⁶Ni → ⁵⁶Co → ⁵⁶Fe decay, with typical nickel yields of order 0.05–0.15 solar masses—again a class scale, not a measured yield for SN210. Shock-breakout heating may dominate the earliest optical flash; without a published bolometric fit, neither nickel mass nor the dominant power source is established for this event.
What chemical elements did SN210 create and disperse into the universe? Nucleosynthesis & Elements
Events of SN210's broad spectroscopic class are discussed in galactic chemical evolution as sources of oxygen-group and intermediate-mass elements (and, for some channels, iron-peak material). No measured elemental yields are published for SN210.
Did SN210 leave behind a black hole, a neutron star, or nothing at all? Cosmic Remnant
A core-collapse explosion associated with SN210's class forges an ultra-dense compact stellar remnant at the center of the detonation. If the progenitor had an initial mass under ~20 solar masses, it left behind a neutron star (pulsar)—packing the mass of our entire Sun into a city-sized sphere barely 20 kilometers wide, spinning dozens or hundreds of times per second. If the progenitor exceeded ~25–30 solar masses, gravity overcame neutron degeneracy pressure, creating a permanent stellar-mass black hole.
What will SN210's explosion site look like in 1,000 to 10,000 years? Cosmic Remnant
Supernova remnants in general evolve through free-expansion, Sedov–Taylor, and radiative phases over centuries to millennia, sometimes becoming bright X-ray shells and occasionally compressing nearby molecular clouds. These are standard remnant-evolution models, not forecasts measured for SN210. Whether this site will trigger star formation, reach particular X-ray temperatures, or match Cassiopeia A depends on local density and magnetic field—none of which are constrained by the data shown here.
In which galaxy did SN210 explode, and where is it located relative to the galactic center? Galactic Environment
SN210 is cataloged with host galaxy MCG +00-03-054. No secure nuclear offset is published in this record.
Where is SN210 located in the night sky and which constellation is it in? Sky Coordinates
In the celestial sphere, SN210 is located at Right Ascension 01:01:16.824 and Declination -01:05:51.936, situated in the constellation Cetus (The Sea Monster). Because its declination is -01:05:51.936, it is favorably placed for Southern Hemisphere observatories.
How much Milky Way interstellar dust obscures our view of SN210? Interstellar Dust
Along this line of sight, the catalog records a Milky Way foreground color excess of E(B−V) = 0.0318 mag (source: published extinction estimate), corresponding to roughly A_V ≈ 0.10 mag for R_V = 3.1. Band-specific corrections (e.g. A_r) differ from A_V and should be applied when available. Map-based values (IRSA / Schlafly & Finkbeiner 2011) must not be claimed unless that map was actually queried.
Across which photometric filter bands was SN210 monitored? Astronomical Observations
No calibrated photometry is published for SN210. Without multi-epoch flux measurements, neither a light curve nor a peak magnitude can be established. Follow-up imaging from survey alert streams would be required to map its brightness evolution.
What did astronomical spectroscopy reveal about SN210's chemical makeup? Astronomical Observations
No spectrum has been published for SN210. Without spectroscopy, its chemical composition, expansion velocity, and physical classification cannot be established. Classification spectra from follow-up observatories would be required to identify diagnostic absorption and emission lines.
Who discovered SN210 and how was it first detected? Discovery & History
SN210 was officially reported on 2002/09/28 by an automated robotic transient sky survey. Discoveries are typically flagged by high-cadence robotic survey telescopes (such as ATLAS, ZTF, Pan-STARRS, ASAS-SN, or Gaia) and worldwide amateur astronomers scanning the night sky, followed by rapid spectroscopic classification by international observatories.
How many scientific publications and observatories have contributed data to SN210? Scientific Research
Data for SN210 are compiled from international astronomical notices, the IAU Transient Name Server (TNS), and peer-reviewed astrophysical journals.
What other names and survey identifiers exist for SN210? Cross-Identifications
Throughout global alert streams and survey databases, SN210 has also been designated as: SN200210, SN 210, SN2002-3325-1-0210. These cross-matched identifiers allow astronomers to cross-reference observations across the Zwicky Transient Facility (ZTF), the Asteroid Terrestrial-impact Last Alert System (ATLAS), Pan-STARRS, Gaia Photometric Science Alerts, and the IAU Transient Name Server (TNS).
How does SN210 contribute to measuring the Hubble Constant and the scale of the cosmos? Cosmology & Distance Ladder
As a core-collapse supernova, SN210 provides independent cosmological distance calibrations via the Expanding Photosphere Method (EPM) and the Standard Candle Method for Type II supernovae (SCM-II). By correlating the physical expansion speed of the photosphere (measured via spectroscopic Doppler shifts) with its photometric color temperature, astronomers determine direct geometric distances independent of secondary distance ladders.
Could gravitational waves or neutrinos from SN210 be detected on Earth? Multi-Messenger Astronomy
Core-collapse supernovae like SN210 are premier targets for multi-messenger astrophysics! During the collapse of the iron core, an intense burst of 10⁵⁸ neutrinos escaped into space hours before the shock broke out through the stellar surface (as famously seen in SN 1987A). Furthermore, violent core asymmetries and non-axisymmetric core bounce can emit high-frequency gravitational waves detectable by advanced interferometers (LIGO, Virgo, KAGRA) for events within the Milky Way and Local Group.
How does SN210 compare to famous historical supernovae like SN 1987A or the Crab Supernova? Historical Comparison
Compared to historical landmarks like SN 1987A in the Large Magellanic Cloud (168,000 light-years away, naked-eye peak m = 2.9) or the Crab Supernova of 1054 (6,500 light-years away), SN210 occurred at a distance of 753.7 Million Light-Years. While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like SN210 allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.
Can I see SN210 tonight with a backyard telescope or binoculars? Backyard Observation
Unknown — no measured brightness. SN210 was discovered 8814 days ago (2002/09/28), but no calibrated photometry is published for it, so its current apparent magnitude cannot be stated. Without a magnitude there is no basis for a telescope-aperture recommendation. Use the coordinates and airmass chart above to plan a follow-up observation and report what you measure.
Does the radiation or shockwave from SN210 pose any threat to Earth? Planetary Safety
No, Earth is in zero danger. Supernovae are violent events emitting powerful gamma rays, X-rays, and cosmic rays; however, the astrophysical 'lethal kill zone' for our planet's protective ozone layer is estimated at 50 to 100 light-years. At a distance of 753.7 Million Light-Years, the inverse-square law dilutes the radiation by quintillions of times, making SN210 completely harmless to our biosphere and purely a fascinating spectacle for human exploration.
Data sourced from IAU TNS, ALeRCE, WISeREP, and the sne.space. View All General Astrophysics FAQs →
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