Investigating the mystery of migrating 'hot Jupiters'

Investigating the mystery of migrating 'hot Jupiters'
The turbulent atmosphere of a hot, gaseous planet known as HD 80606b is shown in this simulation based on data from NASA's Spitzer Space Telescope. Credit: NASA/JPL-Caltech

The last decade has seen a bonanza of exoplanet discoveries. Nearly 2,000 exoplanets—planets outside our solar system—have been confirmed so far, and more than 5,000 candidate exoplanets have been identified. Many of these exotic worlds belong to a class known as "hot Jupiters." These are gas giants like Jupiter but much hotter, with orbits that take them feverishly close to their stars.

At first, hot Jupiters were considered oddballs, since we don't have anything like them in our own . But as more were found, in addition to many other smaller planets that orbit very closely to their stars, our solar system started to seem like the real misfit.

"We thought our solar system was normal, but that's not so much the case," said astronomer Greg Laughlin of the University of California, Santa Cruz, co-author of a new study from NASA's Spitzer Space Telescope that investigates hot Jupiter formation.

As common as hot Jupiters are now known to be, they are still shrouded in mystery. How did these massive orbs form, and how did they wind up so shockingly close to their stars?

The Spitzer telescope found new clues by observing a hot Jupiter known as HD 80606b, situated 190 light-years from Earth. This planet is unusual in that it has a wildly eccentric orbit almost like that of a comet, swinging very close to its star and then back out to much greater distances over and over again every 111 days. One side of the planet is thought to become dramatically hotter than the other during its harrowing close approaches. In fact, when the planet is closest to its host star, the side facing the star quickly heats up to more than 2,000 degrees Fahrenheit (1,100 degrees Celsius).

"As the planet gets closer to the star, it feels a burst of starlight, or radiation. The atmosphere becomes a cauldron of chemical reactions, and the winds ramp up far beyond hurricane force," said Laughlin, a co-author on the Spitzer study, which is accepted for publication in the Astrophysical Journal Letters.

HD 80606b is thought to be in the process of migrating from a more distant orbit to a much tighter one typical of hot Jupiters. One of the leading theories of hot-Jupiter formation holds that gas giants in distant orbits become hot Jupiters when the gravitational influences from nearby stars or planets drive them into closer orbits. The planets start out in eccentric orbits, then, over a period of hundreds of millions of years, are thought to gradually settle down into tight, circular orbits.

"This planet is thought to be caught in the act of migrating inward," said Julien de Wit of the Massachusetts Institute of Technology, Cambridge, lead author of the new study. "By studying it, we are able to test theories of hot Jupiter formation."

Spitzer previously studied HD 80606b in 2009. The latest observations are more detailed, thanks to a longer observing time—85 hours—and improvements in Spitzer's sensitivity to exoplanets.

"The Spitzer data are pristine," said de Wit. "And we were able to observe the planet for much longer this time, giving us more insight into its coldest temperature and how fast it heats up, cools down and rotates."

Investigating the mystery of migrating 'hot Jupiters'
Astronomers watched an exoplanet called HD 80606b heat up and cool off during its sizzling-hot orbit around its star. Credit: NASA/JPL-Caltech/MIT

A key question addressed in the new study is: How long is HD 80606b taking to migrate from an eccentric to a circular orbit? One way to assess this is to look at how "squishy" the planet is. When HD 80606b whips closely by its star, the gravity of the star squeezes it. If the planet is squishier, or more pliable, it can better dissipate this gravitational energy as heat. And the more heat that is dissipated, the faster the planet will transition to a circular orbit, a process known as circularization.

"If you take a Nerf ball and squeeze it a bunch of times really fast, you'll see that it heats up," said Laughlin. "That's because the Nerf ball is good at transferring that mechanical energy into heat. It's squishy as a result."

The Spitzer results show that HD 80606b does not dissipate much heat when it is squeezed by gravity during its close encounters - and thus is not squishy, but rather stiffer as a whole. This suggests the planet is not circularizing its orbit as fast as expected, and may take another 10 billion years or more to complete.

"We are starting to learn how long it may take for hot Jupiter migration to occur," said de Wit. "Our theories said it shouldn't take that long because we don't see migrating hot Jupiters very often."

"The long time scales we are observing here suggest that a leading migration mechanism may not be as efficient for hot Jupiter formation as once believed," said Laughlin.

The Spitzer study suggests that competing theories for hot Jupiter formation—in which form "in situ," or close to their stars, or smoothly spiral inward with the help of planet-forming disks—may be preferred.

The new study is also the first to measure the rotation rate of an exoplanet orbiting a sun-like star. Spitzer observed changes in the planet's brightness as the planet spun on its axis, finding a rotation period of 90 hours.

"Fifty years ago, we were measuring the rotation rates of planets in our own solar system for the first time. Now we are doing the same thing for orbiting other stars. That's pretty amazing," said Laughlin.

A rotation rate of 90 hours is much slower than what is predicted for HD 80606b, puzzling astronomers, and adding to the enduring mystique of hot Jupiters.

Explore further

Observations of an extreme-weather planet raise questions about hot Jupiters' origins

More information: Julien de Wit et al. DIRECT MEASURE OF RADIATIVE AND DYNAMICAL PROPERTIES OF AN EXOPLANET ATMOSPHERE, The Astrophysical Journal (2016). DOI: 10.3847/2041-8205/820/2/L33
Citation: Investigating the mystery of migrating 'hot Jupiters' (2016, March 29) retrieved 22 September 2019 from
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Mar 29, 2016
The Spitzer study suggests that competing theories for hot Jupiter formation—in which gas giants form "in situ," or close to their stars, or smoothly spiral inward with the help of planet-forming disks—may be preferred.

Basically, this means the current nebular theory of planet formation is sunk and a new story needs to be invented. Gaseous giants are not supposed to "form" close to the planet since the gaseous material is expected to be blown away by the strong light and heat pressures generated by the hosting star. Quite clearly the majority of present observations show that this is not the case.

Or else, planets simply do not "form" all by themselves from clouds of dust/gas surrounding a star. This kind of expected phenomenon has not been observed at all and hence is completely unscientific.

Given the presently observed make-up of all planets, it should be quite clear that the only way that they can form is via quick transformation of an existing blob of material.

Agreed, and the only blob big enough in a collapsing prestellar mass is the core itself, which I suggest is vulnerable to inertial displacement by disk instability of the much-more-massive surrounding envelope in the prestellar phase, prior to the formation of a protostar.
A much-greater overlying envelope supported by angular momentum is inherently unstable, promoting runaway positive feedback of inhomogeneities which breaks the radial symmetry of the envelope, causing it to clump and inertially displace the former core to a satellite status, conserving angular momentum in a process designated, 'flip-flop fragmentation'.

Essentially in the prestellar phase when the envelope is much more massive than the core, the greater inertial mass of the envelope wants to form a younger more-massive center by catastrophically projecting angular momentum outward; however in low metallicity stars, the displaced core may dissipate rather than continue to collapse to form a planet.

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