Astronomers simulate how white dwarf stars merge and become a supernova

Astronomers simulate how white dwarf stars merge and become a supernova
A series of snapshots of the merger of two equal size white dwarf stars from 36 seconds prior to the explosion until 10 seconds afterwards. The colour-coding indicates the density of material, which is increasing from blue to red. Please note the different scaling on the plots. Image: Max Planck Institute for Astrophysics

(PhysOrg.com) -- Supernovae are spectacular events: Suddenly somewhere in the heavens a "new star" lights up and shines as bright as a whole galaxy consisting of billions of stars. The mechanisms behind these cosmic catastrophes are varied.

Researchers at the Max Planck Institute for Astrophysics in Garching have now used computer simulations to confirm that some of these bright supernovae are due to the merger of two , compact massive stars at the end of their lifetime. As supernovae are used by astronomers to measure cosmic distances and study the expansion history of our Universe, understanding their mechanism is one of the key challenges in astrophysics. (Nature, January 7th, 2010)

Intermediate-mass stars such as our Sun end their lives as white dwarfs consisting of carbon and oxygen. The stellar fusion reactor in their centre is no longer active due to a lack of fuel. The stars have only the size of the Earth, but a high density. One teaspoon of matter would weigh about as much as a car on our planet.

In a binary system, two such exotic white dwarfs can form. As they orbit each other, they emit gravitational waves. The resulting energy loss shrinks the orbit, the stars approach each other and ultimately they merge. It has long been speculated that these events may produce Type Ia supernova explosions.

The supernova research group at the Max Planck Institute for Astrophysics has now performed of two merging white dwarfs in unprecedented detail. In the case of equal masses of the two white dwarfs, the merger is particularly violent. Part of the material of one white dwarf crashes into the other and heats up the carbon/oxygen material such that a thermonuclear explosion triggers (see Figure). This disrupts the stars in a .

"With our detailed explosion simulations, we could predict observables that indeed closely match actual observations of Type Ia supernovae," explains Friedrich Röpke of the supernova team. Therefore it has been demonstrated that white dwarf mergers contribute to Type Ia supernovae, although this scenario probably cannot account for all these explosions.

"Supernovae are among the brightest observed cosmic explosions," explains Wolfgang Hillebrandt, director at the Max Planck Institute for Astrophysics and co-author of the Nature article. "How they form, however, remains largely unknown. With our simulations we have now shed light on at least part of the old riddle of the progenitors of Type Ia supernovae."

Further support for the picture that Type Ia supernovae originate from mergers of white dwarfs comes from a recent paper by another supernova research group at MPA. In an upcoming Nature publication, they show that the bulk of observed cannot be due to the white dwarf gradually accreting material from a normal companion star - the standard theory so far. At present the only alternative is the merger of two white dwarf .


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More information: Rüdiger Pakmor, Markus Kromer, Friedrich K. Röpke, Stuart A.Sim, J Ashley J. Ruiter, Wolfgang Hillebrandt, Sub-luminous type Ia supernovae from the mergers of equal-mass white dwarfs with M~0.9 M_solar, Nature, January 7, 2010
Citation: Astronomers simulate how white dwarf stars merge and become a supernova (2010, January 7) retrieved 23 July 2019 from https://phys.org/news/2010-01-astronomers-simulate-white-dwarf-stars.html
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Jan 07, 2010
". . . they show that the bulk of observed supernovae cannot be due to the white dwarf gradually accreting material from a normal companion star - the standard theory so far. At present the only alternative is the merger of two white dwarf stars."

Merger?

white dwarf and neutron star? And come to think of it, a white dwarf and any sufficient mass?

The bloody thing only needs to reach Chandrasekhar's limit. I cannot imagine it generally matters how, or what, it eats to get there.

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