- Title: A Class of Eccentric Binaries with Dynamic Tidal Distortions Discovered With Kepler
- Authors: Susan E. Thompson, Mark Everett, Fergal Mullally, Thomas Barclay, Steve B. Howell, Martin Still, Jason Rowe, Jessie L. Christiansen, Donald W. Kurtz, Kelly Hambleton, Joseph D. Twicken, Khadeejah A. Ibrahim, and Bruce D. Clarke
- First Author’s Institution: NASA Ames Research Center, Moffett Field, CA
- Paper Status: Published in ApJ (2012)
The Kepler satellite is really good at finding things that go bump in the night. Even though the spacecraft was crippled and has been repurposed as K2, there are tons of data to analyze. While Kepler’s specialty is hunting for exoplanets, it also finds lots of interesting stars along the way. As a rule, the more we look at stars imaged by Kepler, the more oddballs we find. This paper by Thompson et al. describes a new category of eccentric binary stars discovered by Kepler and dubs them “heartbeat stars.”
As you can see, heartbeat star light curves somewhat resemble an echocardiogram, which is what got them their name. But what is physically causing this odd pattern?
In a traditional eclipsing binary star system, we see a dip in the light curve when one star passes in front of the other. Heartbeat stars, on the other hand, do not always eclipse. Instead, they have extremely elliptical orbits, which causes the two stars to spend a short amount of time very close together as they race past each other and a long amount of time farther apart. The main dip and subsequent peak of the “heartbeat” signature occurs when the stars are closest together and tidal forces are incredibly strong.
When tidal forces affect a star, they distort its shape and cause brightness variations. If you visualize two perfectly spherical stars orbiting each other, the out-of-eclipse luminosity should be constant. But if the two stars slightly distort each another with tidal forces, they become somewhat squished and more like ellipsoids than spheres. As a result, you see more star surface area during one part of the orbit than another, and that causes a slight increase in overall brightness.
Now, imagine dialing this effect up by drastically increasing the orbital eccentricity. Instead of happily orbiting in circles with constant velocity, the two stars spend most of their time far apart, and a few harrowing hours racing past each other. Or, to put it another way: hours and hours of boredom punctuated by moments of sheer terror. This is a heartbeat star.
Tidally distorted light curves were first theorized in 1995, but the first well-studied example was published in 2011 using Kepler light curves. This paper presents 17 new systems on top of four that were previously known, and successfully models how the tidal distortions contribute to light curves. They also measure radial velocity points for some systems and show that these are generally consistent with the orbital solution.
The discovery of so many heartbeat stars raises an important question: how can they exist at all? Over time, the orbits of relatively short-period systems (it only takes these stars several days to fully orbit each other!) should become less eccentric and more circular. But if this always happened, we wouldn’t see any “heartbeats” at all. One possible explanation could be the presence of a so-called third body—a faint star or planet that perturbs the orbit and keeps it eccentric. But this is not fully understood.
A smaller effect seen in many heartbeat star light curves is pulsations. These are the little wiggles in the red light curves above—one or both stars are pulsing in and out, or “breathing,” as they orbit (see a similar situation explored in this astrobite). The authors find that the majority of the heartbeat star pulsations are some harmonic of the orbital period. This suggests that tidal distortions may be causing the pulsations, and is a very interesting topic for follow-up studies.