A Four Planet System in Orbit, Directly Imaged and Remarkable

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The era of directly imaging exoplanets has only just begun, but the science and viewing pleasures to come are appealingly apparent.

This evocative movie of four planets more massive than Jupiter orbiting the young star HR 8799 is a composite of sorts, including images taken over seven years at the W.M. Keck observatory in Hawaii.

The movie clearly doesn’t show full orbits, which will take many more years to collect. The closest-in planet circles the star in around 40 years; the furthest takes more than 400 years.

But as described by Jason Wang,  an astronomy graduate student at the University of California, Berkeley, researchers think that the four planets may well be in resonance with each other.

In this case it’s a one-two-four-eight resonance, meaning that each planet has an orbital period in nearly precise ratio with the others in the system.

The black circle in the center of the image is part of the observing and analyzing effort to block the blinding light of the star, and thus make the planets visible.

The images were initially captured by a team of astronomers including Christian Marois of the National Research Council of Canada’s Herzberg Institute of Astrophysics, who analyzed the data.  The movie animation was put together by Wang, who is part of the Berkeley arm of the Nexus for Exoplanet System Science (NExSS), a NASA-sponsored group formed to encourage interdisciplinary exoplanet science.

The star HR 8799 has already played a pioneering role in the evolution of direct imaging of exoplanets.  In 2008, the Marois group announced discovery of three of the four HR 8799 planets using direct imaging for the first time. On the same day that a different team announced the direct imaging of a planet orbiting the star Fomalhaut.


This false-color composite image traces the motion of the planet Fomalhaut b, a world captured by direct imaging. (NASA, ESA, and P. Kalas, University of California, Berkeley and SETI Institute)

HR 8799 is 129 light years away in the constellation of Pegasus.  By coincidence, it is quite close to the star 51 Pegasi, where the first exoplanet was detected in 1995.  It is less than 60 million years old, Wang said, and is almost five times brighter than the sun.

Wang said that the animation is based on eight observations of the planets since 2009.  He then used a motion interpolation algorithm to draw the orbit between those points.

Much can be learned from the motion of the planets, however long it may take for them to circle their sun.  Based on the Keck observations, astronomers have concluded that the four planets orbit in roughly Keplerian motion around the star — almost circular, but not entirely.

Jason Wang is a graduate student in astronomy at the University of California, Berkeley.

The planets are quite far from each other, which is to be expected due to their enormous size.   Because of those large separations, Wang said astronomers will be watching to see if the system is stable or if some of the planets may be ejected from the system.

Although the first three HR 8799 planets were officially discovered in 2008,  researchers learned afterwards that the planets had actually already been observed.  The “precovery” had been made in 1998 by the NICMOS instrument on the Hubble Space Telescope, but was teased out only after a newly developed image-processing technique was installed.

Christian Marois was part of the team that discovered HR 8799 using direct imaging. He is also on the engineering and science teams of the Gemini Planet Imager, which he helped design and build.

The fourth HR 8799 planet was found after further observations in 2009–2010.  That planet orbits inside the first three planets, but is still fifteen times the distance from its sun than Earth to our sun.  (The team working with Marois included Quinn Konopacky of the University of California, San Diego, Bruce Macintosh of Stanford University, Travis Barman of the University of Arizona and Ben Zuckerman of UCLA.)

James Graham is leader of the Berkeley NExSS group, and he was struck by some of the connections between what has been found around HR 8799 and what exists in our own solar system.

For instance, he said that “it’s delightful that these recently discovered planets exhibit the same type of harmony exhibited by the Galilean moons, Io, Europa, and Ganymede (1:2:4) and illustrating some of the connections between our own solar system and those orbiting other stars. ”

The outer planet orbits inside a dusty disk like our Kuiper Belt. It is one of the most massive disks known around any star within 300 light years of Earth, and there is room in the inner system for rocky planets.

Both Wang and Marois are also on the team operating the Gemini Planet Imager, a cutting-edge addition to the Gemini South telescope in Atacama Desert of Chile.

The GPI includes a next-generation adaptive optics instrument that allows for much clearer seeing through the Earth’s atmosphere by correcting for turbulence.  The result is better direct imaging.   A key goal of the GPI project is to image large extrasolar planets orbiting at distances from their host stars similar to, or greater than, between Jupiter and our sun.

This looping animation of a series of images taken between November 2013 and April 2015 with the Gemini Planet Imager (GPI) on the Gemini South telescope in Chile shows the exoplanet Beta Pictoris b orbiting the star Beta Pictoris. In the images, the star is at the center of the left-hand edge of the frame; it is hidden by the Gemini Planet Imager’s coronagraph. We are looking at the planet’s orbit almost edge-on. (M. Millar-Blanchaer, University of Toronto; F. Marchis, SETI Institute)

The idea for the HR 8799 movie came from a similar, but less elaborate, orbital animation of a planet detected by GPI circling the star Beta Pictoris.

It was initially thought (and hoped) that the planet might transit in front of Beta Pictoris,  providing a unique opportunity to learn the radius of the planet and thus understand the size of the atmosphere.  Unfortunately, the geometry of the planet’s orbit doesn’t quite line up in a way that would have the planet pass in front of the star from our point of view.

However, although the planet doesn’t transit, what is called its Hill sphere does. The Hill sphere is the region surrounding the planet where its gravitational influence dominates over the gravitational influence of the star. As a result, the remnants of the disk left over from planet formation, planetary rings and moons could transit the star later this year and may be detectable.

Those smaller bodies are unlikely to be the subject of any evocative movie animations, but direct imaging will be bringing many more of them to us in the days ahead.

“The Beta Pic animation looked so cool that we’ve wanted to do more,” Wang said, explaining why the HR 8799 movie was made.  “We wanted to make one that was even more impactful for the audience and could begin to show what one of these systems looks like.”

I think they succeeded.

 

 

 

 

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Marc Kaufman
Marc Kaufman is the author of two books about space: "Mars Up Close: Inside the Curiosity Mission” and “First Contact: Scientific Breakthroughs in the Search for Life Beyond Earth.” He is also an experienced journalist, having spent three decades at The Washington Post and The Philadelphia Inquirer. While the “Many Worlds” column is supported and informed by NASA’s Astrobiology Program, any opinions expressed are the author’s alone.

To contact Marc, send an email to marc.kaufman@manyworlds.space.

7 thoughts on “A Four Planet System in Orbit, Directly Imaged and Remarkable

    1. Thanks for yr question. Jason Wang told me that the team didn’t think they had enough data yet to make those projections. I think they also wanted to highlight the fact that they have data now for 8 years, and that the orbits for those years are entirely firm.
      But who knows, maybe at nine years they’ll infer a full orbit.

      Marc

  1. That’s a very intriguing thing to see the exoplanets in motion. I have few questions from the animation:
    1. Is the innermost planet coming in contact with the ‘coronal’ ejection of the star during it’s orbit?
    2. What causes the pulsations in the brightness (dimming and brightening) of the planets? Is it a result of the extrapolation of the eight observations over 7 years?

    1. This reply from Jason Wang:

      1. The “coronal ejection” actually diffraction in our telescope optics and not real flaring from the star. The challenge with direct imaging is removing the glare of the star to see the planets, and the features you see there are leftover glare that our algorithm couldn’t remove.

      2. This is actually due to the fact that this movie is a compilation of images taken at two wavelengths. When the planets look fainter, the observations were taken at at shorter wavelengths when the planet gets fainter and the star gets brighter, making the planets look harder to see.

      Thanks for the questions and comments. Glad people really like it!

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