by Bill Pellerin
OBJECT: HD 140283, HIP 76976
CLASS: Metal Poor Sub-Giant Star
R.A.: 15 h, 43 m, 1.86 s
DEC: -10° 56’ 5.62”
DISTANCE: 190 ly
OPTICS NEEDED: A small telescope, binoculars
Here’s an odd one. I first heard of this star while watching a Great Course lecture in the series ‘The Life and Death of Stars’ by Keivan Stassun. Interestingly, to me, I had never heard of this star before, but it may be one of the more fascinating stars in the sky. The very early universe had much smaller quantities of the heavy chemical elements in it. Why? Because the heavy elements are created (fused, actually) in stars, and in the early universe there had not been enough time for stars to form, live their lives, and seed the universe with these heavier elements. Why? Because the heavy elements are created (fused, actually) in stars and in the early universe there had not been enough time for stars to form, live their lives, and seed the universe with these heavier elements. By ‘heavier’, I mean those elements in the periodic table beyond hydrogen and helium.
This star has .4% of the quantity of heavy elements as our Sun (a 5 billion year old star). So, any stars that are still around that formed in the early universe would be expected to have low quantities of these heavier elements. In fact, astronomers use the chemical contents of stars as a clue to the age of the star. This star is deficient in these heavier elements that astronomers call ‘metals’ although these aren’t metals in the way we normally think of them. This low-metallicity star had to have begun shining in a very early era of the universe. Astronomers call this type of star a ‘Population II’ star (stars that formed much later are called ‘Population I’ stars… go figure). If you really want to investigate the earliest stars in the universe, these would be called Population III stars. For these stars there are no heavy elements at all; they’re all hydrogen and helium. No Population III stars have been identified.
ASTRONOMERS NOW KNOW THAT THE AGE OF THE UNIVERSE IS 13.8 (LATEST ESTIMATE) BILLION YEARS OLD. INTERESTINGLY, THE AGE OF THIS STAR IS ESTIMATED AT 14.46 +/- .8 BILLION YEARS, SO THE LOW END OF THE RANGE IS 13.66 BILLION YEARS.
It is relatively bright to earth-based observers because it is relatively close to us (as these things go) at 187 light-years. While there’s some uncertainty in the age, clearly the star can’t be older than the universe. What we can say for sure is that this was an early forming star.
This star also has a very high proper motion. Proper motion is its real motion across our sky and this star is moving at .13 milliarcseconds per hour, about 11.4 arcseconds in a year. This amount of motion could easily be detected astrometrically by amateurs. It would be fun to image the star field today, and do the same again and see the proper motion of the star.
This is a low-mass star with only about 85% of the mass of our Sun. Not until the ‘helium flash’ event at the end of the red giant phase does helium begin burning. Remember that the lower the mass of a star the longer it lives, and this one is an example of such a low mass star. It’s not a main-sequence star any more, and it’s not yet a red giant star, but it’s on the path leading from the main-sequence to the redgiant phase. Even though the star has moved off the main sequence, it’s still burning (fusing) hydrogen to helium. The age of the star is inferred from its position on the HR (Hertzsprung-Russell) diagram employing standard stellar evolution models. For HAS observers, you’ll want to catch this one early in the evening in September. By mid-month it sets at about 22:45. It’ll be an easy observation, though, and one you can catch just after you get your telescope set up or your binoculars out of the bag.