Researchers to study thermonuclear reaction rates to determine how much of certain elements exploding stars can produce
We are all made from stars. And that's not just a beautiful metaphor.
Apart from hydrogen, as many have heard from the Carl Sagan and Neil DeGrasse Tyson Cosmos series, every ingredient in the human body is made from elements forged by stars.
The calcium in our bones, the oxygen we breathe, the iron in our blood - all those are forged in the element factories of stars. Even the carbon in our apple pie.
Stars are giant element furnaces. Their intense heat can cause atoms to collide, creating new elements - a process known as nuclear fusion. That process is what created chemical elements like carbon or iron - the building blocks that make up life as we know it.
It sounds pretty simple, but it is a very intricate process. And there are still many uncertainties.
Professors Sumner Starrfield and Frank Timmes, both from Arizona State University, and Professor Christian Iliadis, from the University of North Carolina at Chapel Hill, hope to resolve some of those uncertainties.
"Broad brush we have a good idea that massive stars become one kind of supernova and binary stars with white dwarfs become another type of supernova. We know a lot about what may have caused the explosions but there are many unexplained parts that need to be worked out," said Starrfield, Regents' Professor in ASU's School of Earth and Space Exploration.
The team was awarded a NASA grant of nearly $700,000 to better understand how supernovae evolve to an explosion. The study is aimed at determining how much of certain elements a star can produce.
Inside these element factories, how much carbon for our apple pies gets made, how much calcium is available to make our bones, depends on their nuclear reaction rates.
For example, as shown in the recent movie "The Martian", if you were trying to make water, you would take hydrogen and oxygen and some energy and put it together in a container and it would make water at a certain rate depending on the temperature of the container. Add more heat, and the reaction speeds up, producing more water.
A similar thing happens inside stars - except it's nuclear reactions releasing a factor of one million times more energy than a chemical reaction. Stars run on nuclear reactions. Smash together a carbon nucleus and a helium nucleus inside the furnace of a star, and out pops the oxygen we breathe. Speed up that reaction, and the star yields more oxygen.
Researchers use computers and solve equations to predict how a star evolves. Part of that input into how stars evolve are nuclear reaction rates. One set rate has been used to arrive at an estimate of how much of a certain element a star can produce. But is that number optimal? Is it some super optimistically high value, or it pessimistically low?
"What we will define is a meaningful range, given the uncertainties of what is measured here on Earth, of what actually comes out. At the end of the day, what we are going to know is the variation - how much variation is there in a star's output. How much calcium or carbon comes out of the star?" said Timmes, an astrophysicist in ASU's School of Earth and Space Exploration.
Investigating the range of elements that a star can produce is based on what is measured in the terrestrial laboratory. This is where nuclear physicist Iliadis, who recently published a textbook on the nuclear physics of stars, fits in; he's the experimentalist providing the data on the nuclear fusion reaction rates and their uncertainties.
"It is not quite "The power of the Sun, in the palm of my hands", as muttered by Dr. Octavius in Spiderman 2; nevertheless we do measure with our accelerator facilities the very same nuclear fusion reactions that occur in stars," said Iliadis.
But uncertainties are inherent in lab measurements. What you want to do is connect what you do in the lab with what you see in the night sky. And that's Starrfield's contribution - he's an expert in dead and dying suns. He will use the reaction rates from Iliadis in new calculations of how different types of stars can become supernovae.
This proposal ties in a tight loop experiments done here on earth with observations in the night sky. For over two decades Timmes has been doing modeling of stars; the models he creates will serve as the glue between what is measured on earth by Iliadis and what is seen in the dark night sky by Starrfield.
The team is going to be checking roughly 50 of the most important nuclear reaction rates for producing elements that form the building blocks of life as we know it. And just as important, some of these reaction rates are useful in nuclear fusion experiments to produce clean power on Earth.
As a star ages, hydrogen and then helium nuclei fuse to form heavier elements. These reactions continue in stars today as lighter elements are transformed into heavier ones.
Late in life, most stars will explode, ejecting the elements they forged into interstellar space. If a star is heavy enough, or has a close companion, it will explode in a supernova that creates many heavy elements including iron and nickel. The explosion also disperses the different elements across the galaxy, scattering the stellar material that will eventually make up planets, including Earth.
Provided by Arizona State University