Authors: Shivani P. Shah, Rana Ezzeddine, Alexander P. Ji, Terese Hansen, Ian U. Roederer, Márcio Catelan, Zoe Hackshaw, Erika M. Holmbeck, Timothy C. Beers, Rebecca Surman
First Authors Institution: Department of Astronomy, University of Florida, Gainesville, Florida, USA
Status: Resubmitted to ApJ [open access on Arxiv]
As someone who has
recently left their 20’s, I think a lot about how age shows up in my body. I can look up my birth date on the calendar, even count all the minutes of my existence, but I don’t need to go through all that work, something inside of me just feels… older. While the self realization of the unyielding passage of time on my mortal form may be daunting, I find solace in the fact that I’m no different than the stars –they also carry around their own clocks. Today’s paper is about an interesting technique to determine how old a star is, by looking at how much Uranium is “ticking” in its atmosphere.
The smallest hand of the clock
The technique is based on radioactive dating, a tool used in a variety of fields but most famously in Carbon Dating. Living things on earth have atoms of carbon in their bodies, some of which are carbon 14 (C14). C14 is a radioactive isotope of carbon, meaning it has a slightly different mass than other carbon atoms, and it decays over time. Even though it decays, C14 is regularly replaced while an organism is alive, and so the ratio between regular carbon and C14 within living things stays mostly steady. Once the flow of carbon 14 stops (aka something dies), the ratio between carbon and C14 changes as the latter decays. By 1) measuring what the remaining ratio is, and 2) understanding what the ratio is normally, we can 3) calculate how much time has passed for the correct amount to decay.
Radioactive dating isn’t just for living things. C14 decays at such a rate that you can use it up to around 50,000 years ago, but the same technique works for any element with a radioactive isotope. Our best estimate for the age of our planet and solar system comes from radioactive dating using different elements that have radioactive isotopes, but which decay at slower rates.
Uranium (U) is an element that is perfect for this, as its radioactive isotope takes billions of years to decay. Today’s paper is all about trying a new way to measure the abundance, or how much there is, of Uranium in stars, to find an age estimate for stars with radioactive dating. It’s known as Nucleocosmochronometry (a word that spans one and a half Scrabble boards).
Tiny atoms in massive stars
It might seem incredibly difficult to detect atoms in a massive star that is light years away, but it’s actually one of astronomy’s oldest tricks (astrobites has a whole guide about it!). Each element and molecule has its own characteristic fingerprint, its spectral signature, which is the specific wavelengths of light that it absorbs (called spectral lines). These can be measured in a lab, and then by looking at the light coming from a star and seeing which wavelengths are being absorbed we can tell what’s in the star’s atmosphere.
This works great until elements and molecules have lines very close to one another, which is a major challenge with Uranium. As it turns out, the typical line used to measure Uranium abundance is blended with both an Iron (Fe) line and a Cyanide (CN) feature. (Figure 1) It’s still possible to get a measurement, but today’s authors wanted to use two new Uranium lines to measure abundances and see how well they agreed with the single line method. Even though these new lines are blended too, by having three measurements the authors can do a better job of describing the certainty of the measurement by using statistics to compare the abundances measured between the three lines.
Do you have the time?
The authors measured the abundances of Uranium for four stars, and compared the results from a fit using just a single line measurement in each of the stars, to one using all of the U lines. They found that they had a pretty good agreement, the abundances from both methods were within a reasonable range of one another.
When they went to use the abundances to measure an age (Fig 2), they found ages that were similar to those calculated with just the single measurement. You might notice that the age estimates have big errorbars, some that stretch to an age older than the universe! There are clearly still some challenges with the method in general, in part because it’s hard to know how much Uranium was in the star to begin with. The authors chose these four stars for the study because they are examples of stars that should have had more Uranium. Regardless, the production rates of Uranium remain a big question mark.
The clocks keep spinning
It’s worth mentioning that the Uranium that makes these stellar clocks tick formed in merging neutron stars, the dramatic burst of atomic creation when two “dead” stars collide. A star’s clock, even its very existence is due in part to the stars that came before them. Makes me think about how even if my body feels old, that my time being alive has been traced through thousands of lifetimes similar to my own. 30
(+) be damned, I’m going for a walk.
Astrobite Edited by Jessie Thwaites
Featured Image Credit: Adapted from NASA and Image by macrovector on Freepik