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 small (just 2.3 times larger than Earth) and hot (89,500° Fahrenheit [49,700° Celsius]) 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 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 that 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 of 6 Astronomical Units (AU) — one AU is the Earth-Sun distance of 93 million miles (150 million kilometers). Closer in, the other planet orbits every 7.75 years, and it 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 recently from the cast-off material.
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 has been found to orbit stars that 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 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 2 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 resulting release of orbital energy and angular momentum within the short span of a few decades resulted in the loss of 75 percent of the red giant’s mass, leaving only the intensely hot core of the original star and a relatively unscathed companion star orbiting extremely close to the newly created white dwarf.
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 protoplanetary disk in which new and very different planets might have been formed. If so, then it is possible that these massive planets were born after the death of the star that enabled their creation.
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 small (just 2.3 times larger than Earth) and hot (89,500° Fahrenheit [49,700° Celsius]) 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 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 that 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 of 6 Astronomical Units (AU) — one AU is the Earth-Sun distance of 93 million miles (150 million kilometers). Closer in, the other planet orbits every 7.75 years, and it 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 recently from the cast-off material.
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 has been found to orbit stars that 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 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 2 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 resulting release of orbital energy and angular momentum within the short span of a few decades resulted in the loss of 75 percent of the red giant’s mass, leaving only the intensely hot core of the original star and a relatively unscathed companion star orbiting extremely close to the newly created white dwarf.
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 protoplanetary disk in which new and very different planets might have been formed. If so, then it is possible that these massive planets were born after the death of the star that enabled their creation.
