Planets Orbiting a Binary System
Because of the disturbing effects of a binary star system’s gravity, astronomers normally do not expect to find planets in such systems, but the research team was able to use the eclipses of the stars as a precise clock whose irregularities could be used to detect planets in orbit around the binary.
The most massive star at the center of the planetary system is a very small (just 2.3 times larger than Earth) and very hot (50,000 degrees Kelvin) white dwarf -- the burnt-out cinder left over when a Sun-like star dies. The other star in the pair is a modest but larger cool star with a mass only one-tenth that of the Sun. The two stars are joined in a very tight mutual orbit.
Due to a fortunate accident, Earth lies in the same plane as this binary star system, so every 3 hours and 7 minutes we can see the eclipse which occurs when the larger star moves in front of the smaller one.
The resulting dramatic change in the brightness of the system acts like a highly precise clock. Using the eclipses as tics of this clock, the team of astronomers was able to detect changes in the timings of the tics, which reveal the presence of two planets orbiting the pair of stars. The more massive planet is about 5.9 times more massive than Jupiter. It orbits the binary star every 15.5 years at a distance 6 Astronomical Units. (One AU is the Earth-Sun distance of 93 million miles.) Closer in, the other planet orbits every 7.75 years and is about 1.6 times more massive than Jupiter.
The planets may have been born along with their parent stars, but only if they were able to survive a dramatic event a million years ago: when the original primary star bloated itself into a red giant, it caused the secondary star to plunge down into the present very tight orbit, thereby casting off most of the original mass of the primary. Alternatively, the planets may have formed very recently from the cast off material.
Many of these Texas observations were in large part facilitated by George Miller, an astronomy and Plan II junior at The University of Texas at Austin, who became involved in the project through UT’s Freshman Research Initiative in Spring 2009. The Freshman Research Initiative offers first-year undergraduate students a unique opportunity to engage in cutting-edge research projects. Astronomy professor Don Winget is the project’s faculty leader. McDonald Observatory research scientist Mike Montgomery is the project’s research educator. Astronomy graduate student JJ Hermes is the project’s teaching assistant.
The discovery of planets outside our solar system is becoming more common -- to date, astronomers have confirmed nearly 500 such extrasolar planets. However, only a tiny fraction of these planets have been found to orbit stars which themselves are in binary or multiple systems, simply because there is little room between the stars for planets to form.
The two planets in NN Serpentis are not currently very close to the binary stars, but the double star system was not always as tight as it is now. Back when the present white dwarf star was a normal star, twice as massive as the Sun, the two stars were separated by about 1.5 AU, and eclipses would have happened about once every two years.
When the more massive star ended its normal life burning hydrogen in its core (as the Sun does now), it bloated itself into a red giant star, increasing its radius from about twice that of the Sun to more than 300 times larger, thereby engulfing the other star in its diffuse outer envelope. The friction of the companion star moving within the red giant made the less massive star plunge deep into the red giant -- a process very like the re-entry of a spacecraft in Earth’s atmosphere, called a “common envelope phase” by astronomers.
The dramatic change from a normal double star system to a tight binary containing a hot white dwarf must have been even more dramatic for any planets present beforehand: the loss of 75 percent of the original star’s mass meant that 75 percent of the original star’s gravity was also gone. This could easily result in the release of the planets, sending them careening off into space, or it may simply have resulted in a dramatic change in the planet’s orbits.
Given that the dangers for any such “first-generation” planets are so great, one must also consider a wild and equally dramatic “second-generation” alternative: The planets now seen around NN Serpentis were created only a million years ago during the common envelope phase when large amounts of gas and dust were cast off, forming a more massive version of a proto-planetary disk in which new and very different planets might have been formed. If so, then it is possible that these massive planets were in fact born after the death of the star that enabled their creation.
Whatever the origin of the resulting planetary system, one is reminded of the famous scene in the movie “Star Wars,” where the young Luke Skywalker watches the setting of a double star system from the circumbinary desert planet Tatooine. Unfortunately, the two planets discovered in NN Serpentis are giant gas planets and thus unfit for life as we know it. However, there may be undiscovered planets orbiting even closer to NN Serpentis, in the so-called “habitable zone” around the binary star where water could exist in liquid form. If so, it is possible that a real Tatooine lurks there waiting to be discovered, and a real binary star sunset waiting to be pondered.