≡ Menu

Do All Stars Form as Binaries?

Interesting news this morning that begins with the Very Large Array in New Mexico, which a team of astronomers has been using to look at star formation. Their target: The Perseus molecular cloud, a stellar nursery about 600 light years from Earth. Clouds like this are sufficiently large (this one is about 50 light years in length) and dense to permit molecules to form, with molecular hydrogen (H2) being the most common, along with carbon monoxide (CO).

SC2_5_350

Although we can’t see into them in visible light (they appear as holes in the starry background because dust and gas obscure the stars forming inside, as well as background stars), such molecular clouds are ideally suited for study with radio telescopes. The VLA survey, called VANDAM (VLA Nascent Disk and Multiplicity) surveyed all the young stars in the Perseus cloud, including both single and multiple stars at separations down to < 20 AU. And now a duo of astronomers has supplemented the VLA data with observations from the James Clerk Maxwell Telescope in Hawaii, the latter helping to reveal the clumps of higher density called ‘dense cores’ — think of them as egg-shaped ‘cocoons’ — within which young stars form.

Image: Radio image of a very young binary star system, less than about 1 million years old, that formed within a dense core (oval outline) in the Perseus molecular cloud. According to the new paper, all stars likely form as binaries within dense cores. Credit: SCUBA-2 survey image by Sarah Sadavoy, CfA.

Sarah Sadavoy (Max-Planck-Institut für Astronomie) and Steven Stahler (UC-Berkeley) found 55 young stars in 24 multiple star systems (all but five of these are binary) and 45 single star systems in the Perseus cloud. All the widely separated binaries (> 500 AU) were made up of Class 0 stars (less than 500,000 years old), and were aligned with the long axis of the dense core. The older Class I binary stars (between 500,000 and 1 million years old) were closer together (separations ~ 200 AU) and showed no such alignment.

These alignments may not be random. For the authors have produced a mathematical model that explains the observations, and it’s a model with a twist. What they deduce is that stars like the Sun — all of them — are born with a companion. Says Stahler:

“We ran a series of statistical models to see if we could account for the relative populations of young single stars and binaries of all separations in the Perseus molecular cloud, and the only model that could reproduce the data was one in which all stars form initially as wide binaries. These systems then either shrink or break apart within a million years.”

A wide binary as considered here is one with a separation of more than 500 AU, which would mean that the original binary companion to our Sun, assuming it once existed, would have been about 17 times further out than Neptune is today. Nemesis? Only in that this would have been a companion to our star, though not one that, like the conjectured Nemesis once considered as a hypothesis for driving asteroid collisions with the Earth, stayed in our neighborhood.

protostars750

Image: This infrared image from the Hubble Space Telescope contains a bright, fan-shaped object (lower right quadrant) thought to be a binary star that emits light pulses as the two stars interact. The primitive binary system is located in the IC 348 region of the Perseus molecular cloud and was included in the study by the Berkeley/Harvard team. Credit: NASA, ESA and J. Muzerolle, STScI.

In fact, the outcome based on Sadavoy and Stahler’s models is that the Sun’s companion escaped long ago. This would not be an uncommon result, for the early period of star formation would be turbulent. The wide binaries from the early period of star formation either break into separate stars or else shrink into tighter orbits to form tight binaries. Stahler again:

“As the egg contracts, the densest part of the egg will be toward the middle, and that forms two concentrations of density along the middle axis. These centers of higher density at some point collapse in on themselves because of their self-gravity to form Class 0 stars. Within our picture, single low-mass, sunlike stars are not primordial. They are the result of the breakup of binaries.”

An interesting result, and keep this in mind (from the paper): “If our model continues to provide a good fit to other star-forming regions, then the mass fraction of dense cores that becomes stars is double what is currently believed.”

In trying to learn how binary and multiple star systems form, we’ve begun to produce computer simulations examining the behavior of collapsing masses of gas, as well as simulating how young multiple stars behave as they emerge from their gas clouds. What this work addresses is the fact that among the population of young stars, binaries exist in higher proportion. The authors point to the need for higher resolution studies in other star-forming regions to continue the systematic analysis of the role of binaries in early stellar evolution.

The paper is Sadavoy and Stahler, “Embedded Binaries and Their Dense Cores,” accepted at Monthly Notices of the Royal Astronomical Society (preprint). This UC-Berkeley news release is helpful.

tzf_img_post

{ 10 comments… add one }
  • don wilkins June 15, 2017, 12:41

    I like Niven’s and Benford’s explanation in Starship better. Perhaps less scientific but definitely more fun.

  • Ronald June 15, 2017, 17:33

    Very fascinating! I may have missed something, but my question is: what determines whether such a binary ends up as binary or as two single stars?

    • Paul Gilster June 15, 2017, 20:04

      Ronald, the authors discuss the problem but don’t offer a conclusive solution:

      “Our model further predicts that most wide binaries break apart, although some shrink to become tighter systems. We have considered two modes of binary breakup – core splitting and stellar ejection. Under either mode, we obtain equally good fits to the observed populations of embedded stars. Deeper and higher-resolution studies of more evolved stars may help decide which picture is correct.”

      The actual breakup process is going to need a lot more work, I think.

  • kzb June 16, 2017, 8:15

    Here’s my theory for what it’s worth: in these clouds, the space density of stars is quite high . Close encounters between stellar systems may be common, and the gravitation interplay releases many of the binary stars. Also some may be captured from their original partners.

  • djlactin June 16, 2017, 9:40

    Another option is that the ‘binaries’ actually include smaller undetected (undetectable?) companions that are ejected by 3-body interactions, and carry some angular momentum away with them, so that the remaining pairs contract.

  • DJ Kaplan June 16, 2017, 13:41

    Does that make Jupiter a failed star?

    • Alexander Tolley June 16, 2017, 14:33

      That’s why Clarke’s “Old Ones” used a monolith to correct the situation. ;)

      More seriously, planets like Jupiter could have very long periods warmth if some artificial means could be used to ignite some fusion in the core. Imagine life inhabiting a warm (HZ level) biosphere from the “surface” to the upper atmosphere. Whilst only a fraction of a Dyson swarm in surface area, the living volume of a sphere bounded by the atmosphere, and perhaps 10,000 km deep would be immense. Post-humans could build structures that would contain vast amounts of living space that would be a home even after the sun dies and goes cold.

  • Geoffrey Hillend June 17, 2017, 19:01

    A red dwarf needs to be over 80 times the mass of Jupiter before internal pressures are high energy to start nuclear fusion.

    Core splitting would leave some large masses orbiting our Sun at 500 Au. The problem with Stellar ejection is that the gravity another star or the Sun would have to eject the binary. It seems improbable that all star systems had to undergo ejection due to the great distances between star systems, and gravitation attraction of a barycenter of 500 Au binary. Proxima Centauri is 12, 95o Au from Alpha Centauri, a lot farther away than 500 Au, and it did not get ejected.

  • kzb June 20, 2017, 7:51

    But could Proxima have been formed coevally with A and B, at its current average distance?

    I would say Proxima was “nearly” ejected (or stolen). In fact I wonder if there was only one of the A and B stars initially present instead of two, if Proxima would indeed have escaped?

Leave a Comment