SN 1987A – The Best Studied Supernova of All Time

SN 1987A

Remnant of SN 1987A seen in light overlays of different spectra. ALMA data (radio, in red) shows newly formed dust in the center of the remnant. Hubble (visible, in green) and Chandra (X-ray, in blue) data show the expanding shock wave

On February 24, 1987, SN 1987A, a supernova in the outskirts of the Tarantula Nebula in the Large Magellanic Cloud occurred visible to the naked eye. It was the closest observed supernova since Kepler’s Supernova  SN 1604, which occurred in the Milky Way itself.[5]

SN 1987A – The Best Studied Supernova of all Time

Due to the relative proximity to Earth, SN 1987A became one of the best studied supernovae of all time. After its discovery was announced, nearly every telescope in the southern hemisphere was able to observe the event. Not only light but also particle emission was detected. The Kamiokande II neutrino telescope is positioned in the Kamioka mine in Japan. It recorded the arrival of 9 neutrinos within an interval of 2 seconds and 3 more neutrinos 9 to 13 seconds later. Almost the same thing was detected by the IMB detector in a salt mine in Ohio. A third neutrino telescope in Russia also recorded the event. On Earth, a total of 25 neutrinos were detected out of several billions that were produced in the explosion. Neutrinos have the ability to travel through Earth’s entire diameter and are very hard to even detect. However, the detection of the neutrinos confirmed the theoretical expectations for the core collapse of a massive star. Further, scientists previously believed that explosions of massive stars occurred at their live’s end and the supernova of 1987 provided a confirmation for the theory.


A supernova (from Latin stella nova, super ‘new star, beyond’; plural supernovae) is the brief, bright illumination of a massive star at the end of its lifetime by an explosion that destroys the original star itself. The luminosity of the star increases millions to billions of times, and for a short time it becomes as bright as an entire galaxy. There are two basic mechanisms by which stars can become supernovae:

  1. Massive stars with an initial mass  of more than about eight solar masses, whose core collapses at the end of their evolution and after their nuclear fuel is used up. This can result in a compact object, such as a neutron star (pulsar) or a black hole. This process is called a collapse or hydrodynamic supernova.
  2. Stars of lower mass, which in their preliminary final stage accrete material as white dwarfs (e.g. from a companion in a binary star system), collapse by their own gravity and are torn apart by the onset of carbon burning. This phenomenon is called thermonuclear supernova or Type Ia supernova.

Well known supernovae are the 1987A supernova in the Large Magellanic Cloud discussed in this article, and Kepler’s supernova (1604). Especially the latter and Tycho Brahe‘s supernova (1572) have inspired astronomy,[6] as they have finally refuted the classical conception of the immutability of the fixed star sphere. The best known supernova remnant is the Crab Nebula (supernova 1054) in the constellation of Taurus.[7]

A Core Collapse Supernova

Scientist found out that SN 1987A appears to be a core-collapse supernova, which means that there should be a neutron star given the size of the original star. Indeed, the neutrino data indicate that a compact object did form at the star’s core, but it has not been detected so far. It could be also possible that the large amounts of material fell back on the neutron star, so that it further collapsed into a black hole.

After the Explosion

Around SN 1987A there can be seen bright rings, material from the stellar wind of the progenitor. The rings were ionized by the ultraviolet flash from the supernova explosion, and consequently began emitting in various emission lines. That means that these rings were not visible until several months after the actual supernova and the process could be studied through spectroscopy. Around 2001, the expanding supernova ejecta collided with the inner ring, which caused its heating as well as generation of x-rays.

In June 2015, it was reported that images from the Hubble Space Telescope and the Very Large Telescope demonstrate the emissions from the matter making up the rings are fading as the clumps are destroyed by the shock wave. The ring will probably fade away between 2020 and 2030. As the shock wave passes the circumstellar ring it will trace the history of mass loss of the supernova’s progenitor and provide useful information for discriminating among various models for the progenitor of SN 1987A.

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