Date: July 11th, 2012
Title: Astronomy Word of the Week : White Dwarf
Podcaster: Dr. Christopher Crockett
Organization: United States Naval Observatory
Description: After a star exhausts its fuel supply, it evaporates into space and leaves behind a hot, dense core. The astronomy word of the week is “white dwarf”.
Bio: Dr. Christopher Crockett is an astronomer at the United States Naval Observatory in Flagstaff, Arizona. His research involves searching for planets around very young stars (“only” a few million years old). It is hoped that the results from this research will help constrain models of planet formation and lead to a better understanding of where, when, and how often planets form. Chris is also passionate about astronomy outreach and education and will talk for hours about the Universe if you let him.
Today’s Sponsor: This episode of “365 days of Astronomy” is sponsored by iTelescope.net – Expanding your horizons in astronomy today. The premier on-demand telescope network, at dark sky sites in Spain, New Mexico and Siding Spring, Australia.
White dwarfs are the hot, dense remnants of long dead stars. They are the stellar cores left behind after a star has exhausted its fuel supply and blown its bulk of gas and dust into space. These exotic objects mark the final stage of evolution for most stars in the universe – including our sun – and light the way to a deeper understanding of cosmic history.
A single white dwarf contains roughly the mass of our sun in a volume no bigger than our planet. Their small size makes them difficult to find – no white dwarfs can be seen with the naked eye. The light they generate comes from the slow, steady release of prodigious amounts of energy stored up after billions of years spent as a star’s nuclear powerhouse.
White dwarfs are born when a star shuts down. A star spends most of its life in a precarious balance between gravity and outward gas pressure. The weight of a couple octillion tons of gas pressing down on the stellar core drives densities and temperatures high enough to ignite nuclear fusion – the fusing together of hydrogen nuclei to form helium. The steady release of thermonuclear energy prevents the star from collapsing on itself.
Once the star runs of hydrogen in its center, the star shifts to fusing helium into carbon and oxygen. Hydrogen fusion moves to a shell surrounding the core. The star inflates and becomes a “red giant”. For most stars – our sun included – this is the beginning of the end. As the star expands and the stellar winds blow at an increasingly ferocious rate, the star’s outer layers escape the relentless pull of gravity.
As the star evaporates, it leaves behind its core. The exposed core, now a newly born white dwarf, consists of an exotic stew of helium, carbon, and oxygen nuclei swimming in a sea of highly energetic electrons. The combined pressure of the electrons holds up the white dwarf, preventing further collapse towards an even stranger entity like a neutron star or black hole.
The infant white dwarf is incredibly hot and bathes the surrounding space in a glow of ultraviolet light and x-rays. Some of this radiation is intercepted by the outflows of gas that have left the confines of the now dead star. The gas responds by fluorescing with a rainbow of colors called a planetary nebula. These nebulae – like the Ring Nebula in the constellation Lyra – give us a peek into our sun’s future.
The white dwarf now has before it a long, quiet future. As the trapped heat trickles out, it slowly cools and dims. Eventually it will become an inert lump of carbon and oxygen floating invisibly in space: a black dwarf. But the universe isn’t old enough for any black dwarfs to have formed. The first white dwarfs born in the earliest generations of stars are still, 14 billion years later, cooling off. The coolest white dwarfs we know of, with temperature around 4000 degrees, may also be some of the oldest relics in the cosmos.
But not all white dwarfs go quietly into the night. White dwarfs that orbit other stars lead to highly explosive phenomena. The white dwarf starts things off by siphoning gas off its companion. Hydrogen is transferred across a gaseous bridge and spilled onto the white dwarf’s surface. As the hydrogen accumulates, its temperature and density reach a flash point where the entire shell of newly acquired fuel violently fuses releasing a tremendous amount of energy. This flash, called a nova, causes the white dwarf to briefly flare with the brilliance of 50,000 suns and then slowly fade back into obscurity.
If the gas collects fast enough, however, it can push the entire white dwarf past a critical point. Rather than a thin shell of fusion, the whole star can suddenly come back to life. Unregulated, the violent release of energy detonates the white dwarf. The entire stellar core is obliterated in one of the most energetic events in the universe: a Type 1a supernova! In one second, the white dwarf releases as much energy as the sun does in its entire 10 billion year lifetime. For weeks or months, it can even outshine an entire galaxy.
Such brilliance makes Type 1a supernovae visible from across the universe. Astronomers use them as “standard candles” to measure distances to the farthest reaches of the cosmos. Observations of detonating white dwarfs in distant galaxies led to a discovery that netted the 2011 Nobel prize in physics: the expansion of the universe is accelerating! Dead stars have breathed life into our most fundamental assumptions about the nature of time and space.
White dwarfs – the cores left behind after a star has exhausted its fuel supply – are sprinkled throughout every galaxy. Like a stellar graveyard, they are the tombstones of nearly every star that lived. Once the sites of stellar furnaces where new atoms were forged, these ancient fossils have been repurposed as an astronomer’s tool that have upended our understanding of the evolution of the universe.
End of podcast:
365 Days of Astronomy
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