Oct 5, 2017

The helium explosion at the surface sets out the final journey of a dying star


Ji-an Jiang (The University of Tokyo)

Mamoru Doi(The University of Tokyo)

Toshikazu Shigeyama(The University of Tokyo)

Keiichi Maeda(Kyoto University)

& the other members of MUSSES


An international astronomical team led by Ji-an Jiang, a graduate student of the University of Tokyo, and Mamoru Doi (U-Tokyo) has found the evidence that the brightest stellar explosions in our universe could be triggered by the helium nuclear explosion at the surface of a white dwarf (star), by carrying out survey observations with the wide-field camera mounted on the 8.2-m Subaru telescope, the Hyper Suprime-Cam. This study was reported in Nature published on Oct. 5, 2017 (Japanese Standard Time).

Figure1: Upper panels: The first two-days observations of a peculiar type Ia supernova, MUSSES1604D, with Subaru/Hyper Suprime-Cam (left and middle) and follow-up observations with the Gemini-North telescope about one month after the first observation (right). Lower panels: Schematic light curves of MUSSES1604D (green circles denote the stages that the supernova is staying during observations).
Credit: Institute of Astronomy, the University of Tokyo


Many stars end their lives through a spectacular explosion. Most massive stars will finally explode as a supernova. Though a white dwarf is the remnant of an intermediate mass star like our Sun, it may explode as well if a white dwarf is a member of a close binary star system where two stars orbit around each other. This type of supernovae is classified as Ia.

Because of the uniform and extremely high brightness (about 5 billion times brighter than the Sun) of type Ia supernovae, they are widely used as the standard candle for the distance measurement in astronomy. The most successful example using type Ia supernovae is the discovery of the accelerating expansion of our universe (Nobel prize in physics 2011). Though the great success has been made in the type Ia supernova cosmology, we are still puzzled by the essential issues of what the progenitor systems of type Ia supernovae are and how type Ia supernova explosions are ignited.

In order to find new clues to figure out these long-standing issues, Jiang and his collaborators aim to catch type Ia supernovae within a few days, or even a day, after their explosions (hereafter "early-phase type Ia supernovae"), using the Hyper Suprime-Cam mounted on the Subaru telescope, the most powerful survey facility in the world. Their scientific project was established in 2016, named as "MUSSES", an abbreviation of "the MUlti-band Subaru Survey for Early-phase type Ia supernovae (SNe Ia)", including researchers from the University of Tokyo, Kyoto University, the National Astronomical Observatory of Japan (NAOJ) and other institutions in Japan and foreign countries.

“We discovered over 100 supernova candidates in one night with Subaru/Hyper Suprime-Cam, including several supernovae that had only exploded a few days earlier. Not only that, a type Ia supernova, named MUSSES1604D, soon after the explosion has been discovered. Surprisingly, MUSSES1604D in the first few days was much brighter than we expected, and we also found other peculiarities of this amazing object through follow-up observations with many large telescopes around the world,” said Jiang.

In order to figure out the origin of this mysterious object, intensive computational simulations were conducted by Toshikazu Shigeyama (U-Tokyo) and Keiichi Maeda (Kyoto University), based on different kinds of theoretical models. After more than 3-months discussions and numerous computational experiments, they finally confirmed that the features of this supernova are not consistent with predictions from popular scenarios, but instead, can be naturally explained by a specific explosion mechanism. In this scenario, the accumulation of helium on the surface of the white dwarf first ignites explosive helium burning and shock waves generated by this precursor event propagate inward, and eventually ignite carbon burning in the core of the white dwarf. "Once we noticed the possibility of this He detonation scenario, every peculiarity was just readily explained. This is the first robust evidence that one theoretically predicted stellar explosion mechanism proposed in early 1980’s, does truly exist in our universe," said Maeda.

Figure 2: The astronomical art of a pre-explosion white dwarf triggered by the helium explosion at its surface. The nuclear explosion of the surface helium layer triggers inward shock waves, and the central carbon nuclear fusion is subsequently ignited.
Credit: Institute of Astronomy, the University of Tokyo


This result answers how the explosion of type Ia supernovae can be ignited for the first time and has opened the door to the essential understanding of these spectacular phenomena in our universe. Moreover, considering that type Ia supernovae are bright sources and have been used as a standard candle in the distant universe, this finding also brings astronomers new ideas to further promote the accuracy of the cosmological use of type Ia supernovae. Jiang's team will carry out further investigations by keep running the MUSSES project. "We are expecting to find many more supernovae within a day of the explosion, which should bring us further insight on the mechanism of supernovae. A more precise understanding of their history and behavior will help all researchers to perform more accurate cosmological measurement,” said Doi. Details of their study were published in Nature on Oct. 5, 2017 (Japanese Standard Time).


Publication details

Journal Nature
Title A hybrid type la supernova with an early flash triggered by helium-shell detonation
Authors Ji-an Jiang*, Mamoru Doi, Keiichi Maeda, Toshikazu Shigeyama, Ken’ichi Nomoto et al.
DOI 10.1038/nature23908
Paper link http://www.nature.com/nature/journal/v550/n7674/full/nature23908.html?foxtrotcallback=true


Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)

National Astronomical Observatory of Japan

Subaru Telescope, National Astronomical Observatory of Japan

Center for Computational Astrophysics, National Astronomical Observatory of Japan

Kyoto University


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