R136c is an exceptionally massive and luminous star located near the centre of the R136 star cluster in the Tarantula Nebula (30 Doradus) in the Large Magellanic Cloud. Spectroscopically it is classified as WN5h, a subtype of Wolf–Rayet stars that shows strong ionized helium emission together with hydrogen lines. Its surface temperature is very high (around 50,000 kelvin), and it is among the hottest and brightest members of its cluster.

Key characteristics

R136c is notable for extreme physical properties that place it among the most massive known stars. Estimates commonly quoted in the literature put its current mass on the order of a few hundred times the mass of the Sun and its luminosity at millions of times solar output. That prodigious energy output is powered by core hydrogen fusion dominated by the CNO cycle, which is efficient in very hot, high-mass stars and helps explain the star's enormous luminosity. The star also drives powerful stellar winds, shedding material at a high rate and enriching its surroundings.

  • Spectral type: WN5h (Wolf–Rayet with hydrogen)
  • Surface temperature: ≈50,000 K (very hot)
  • Mass: estimated on the order of 100–300 M☉ in many studies; values vary by method — see sources linked below
  • Bolometric luminosity: several million L☉ in published estimates

Environment and discovery

R136c sits in the dense, young core of R136, itself the central concentration of the giant star-forming region NGC 2070 in 30 Doradus. High-resolution observations with space- and ground-based telescopes in the 1990s and later resolved the cluster into multiple very massive stars; R136c was identified as one of these exceptional objects and has been studied as part of efforts to understand how the most massive stars form and evolve in relatively low-metallicity environments like the Large Magellanic Cloud.

Binary status and high-energy emission

There is strong suspicion that R136c may be a close binary or multiple system. Hard X-ray emission from the region is consistent with colliding-wind binaries, where powerful winds from two massive components interact and produce high-energy radiation. If a companion exists it likely contributes only a modest fraction of the system's total light, but it can significantly affect the wind structure and mass-loss history. Investigations of radial velocity shifts and direct imaging continue to refine the star's multiplicity status; the candidate scenario is discussed in several observational papers.

Evolutionary stage and possible fates

R136c is extremely young in astronomical terms but already shows a Wolf–Rayet spectrum, indicating that core nuclear burning and heavy mass loss have exposed chemically processed layers. Its subsequent evolution depends on how much mass it loses and how fast it rotates: it might pass through or skip a luminous blue variable (LBV) phase, evolve into hydrogen-poor Wolf–Rayet stages, and eventually build up an oxygen-dominated core. At the end of its life it may explode as a core-collapse supernova or a more energetic hypernova, potentially produce a long gamma-ray burst under the right conditions, or collapse directly into a black hole with little visible explosion.

Notable facts and uncertainties

Because R136c lies in a crowded and bright region, precise measurement of its fundamental parameters remains challenging and model-dependent. Mass and luminosity estimates vary with the adopted distance, extinction, spectral modelling, and assumptions about multiplicity. Nevertheless, R136c is an important object for testing theories of massive-star formation, stellar winds and the end stages of the most massive stars. For further observational details and modelling results see the literature and dedicated reviews of the R136 cluster and massive Wolf–Rayet stars (mass estimates, binary candidacy).

Researchers continue to monitor R136c across the electromagnetic spectrum to improve constraints on its mass-loss rate, wind composition and interactions with neighbours. Its extraordinary properties make it a key case for understanding how the most massive stars influence their host clusters and the interstellar medium in starburst regions.