![The remnant of the SN1006. The surveyed area is indicated by the large green circle. The centre of the survey (the centroid of the X-ray emission) is marked with a green cross, and that of the Ha emission, by the small yellow circle. This is a composite i The remnant of the SN1006. The surveyed area is indicated by the large green circle. The centre of the survey (the centroid of the X-ray emission) is marked with a green cross, and that of the Ha emission, by the small yellow circle. This is a composite i](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/resultados99_103.jpg?itok=hTOCkeTq)
Type-Ia supernovae are thought to occur when a white dwarf made of carbon and oxygen accretes sufficient mass to trigger a thermonuclear explosion. The accretion could be slow, from an unevolved (main-sequence) or evolved (subgiant or giant) star (the single-degenerate channel), or rapid, as the primary star breaks up a smaller orbiting white dwarf (the double-degenerate channel). A companion star will survive the explosion only in the single-degenerate channel. Both channels might contribute to the production of type-Ia supernovae, but the relative proportions of their contributions remain
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