Imaging the planet-sized companion of a nearby star

October 15, 2010
A processed infrared image of the star GJ 758 and its planet/brown-dwarf companion (circled). The image was taken by the Clio instrument on the MMT Observatory. Credit: MMTO and T. Currie, et al.

( -- Of the nearly 500 extra-solar planets that have been confirmed to date, only about a dozen have actually been seen in images. Because planets are so much fainter than their host stars, special techniques are needed to obtain such images, and even these work only when circumstances are optimum, for example, when the stellar system is viewed face-on and the planet is far enough away from the star.

Nearly all planetary detections use more common methods that monitor stellar wobble or stellar brightness variations (due to transiting or lensing). Besides being visually dramatic, direct imaging has the advantage of readily determining a planet's distance from the star, and sampling its light directly. If the planet is a giant (as large or larger than Jupiter), then it may have an internal heat source as well as a reflecting atmosphere, in which case it can stand out more distinctly from its stellar host at . Astronomers trying to improve the statistics of imaged planets are on the lookout for nearby stellar systems which might permit discovery or the direct detection of an extrasolar planet.

The MMT Observatory has a relatively new , called Clio, that can take advantage of the superb angular resolution possible there. Daniel Fabrycky and Ruth Murray-Clay, along with four colleagues, used Clio to image the nearby star GJ 758 (located only about 50 light-years away from earth) and its previously detected companion. Their infrared images not only showed the planet, but allowed them to measure its flux well enough to estimate its temperature and mass, the latter depending on its age and on models of planet evolution.

The scientists report that the object orbiting GJ 758 has an atmospheric temperature of about 290 degrees Centigrade or about 560 kelvin. If the planet is as young as about one billion years, it has a mass of between 10 and 20 Jupiter-masses; if it is as old as 8.7 billion years, then its mass is more likely twice as large. In either case the mass result is a particularly important conclusion for three reasons. First, the companion might not be a "planet" at all. It appears large enough to be a small star, a so-called "brown dwarf" - not big enough to burn hydrogen (as occurs in a star's nuclear furnace), but able to burn deuterium (deuterium, a hydrogen-like atom with one neutron in its nucleus along with one proton, fuses into helium at lower temperatures than does hydrogen). If the companion is a brown-dwarf, then it would be an exception to the postulated "brown-dwarf desert" theory in which stellar companions can be or other but (for unknown reasons) not easily brown dwarfs.

The other two important conclusions are equally provocative. In the context of this , its large size seems to exclude (or at least make less likely) those theories of planet/companion formation in which mass is steadily accreted by the growing planet, the alternative being that it grows as the result of sticking collisions between smaller bodies. Moreover, if the companion really is a small star, then GJ 758 is actually a binary star and not a planetary system - and one of the smallest known binaries at that.

Explore further: The star, the dwarf and the planet

Related Stories

The star, the dwarf and the planet

October 19, 2006

Astronomers have detected a new faint companion to the star HD 3651, already known to host a planet. This companion, a brown dwarf, is the faintest known companion of an exoplanet host star imaged directly and one of the ...

Team using Subaru Telescope makes major discovery

December 3, 2009

An international team of scientists that includes an astronomer from Princeton University has made the first direct observation of a planet-like object orbiting a star similar to the sun.

Six new planets discovered

June 14, 2010

( -- An international team, including Oxford University scientists, has discovered six diverse new planets, from 'shrunken-Saturns' to 'bloated hot Jupiters', as well a rare brown dwarf with 60 times the mass ...

A sub-stellar Jonah: Brown dwarf survives being swallowed

August 2, 2006

Using ESO's Very Large Telescope, astronomers have discovered a rather unusual system, in which two planet-size stars, of different colours, orbit each other. One is a rather hot white dwarf, weighing a little bit less than ...

Recommended for you

Bursts of methane may have warmed early Mars

January 24, 2017

The presence of water on ancient Mars is a paradox. There's plenty of geographical evidence that rivers periodically flowed across the planet's surface. Yet in the time period when these waters are supposed to have run—three ...

Gaia turns its eyes to asteroid hunting

January 24, 2017

While best known for its surveys of the stars and mapping the Milky Way in three dimensions, ESA's Gaia has many more strings to its bow. Among them, its contribution to our understanding of the asteroids that litter the ...

Dwarf galaxies shed light on dark matter

January 23, 2017

The first sighting of clustered dwarf galaxies bolsters a leading theory about how big galaxies such as our Milky Way are formed, and how dark matter binds them, researchers said Monday.

One of the brightest distant galaxies known discovered

January 23, 2017

An international team led by researchers from the Instituto de Astrofísica de Canarias (IAC) and the University of La Laguna (ULL) has discovered one of the brightest "non-active" galaxies in the early universe. Finding ...


Adjust slider to filter visible comments by rank

Display comments: newest first

not rated yet Oct 16, 2010
Excellent news, but the musings on planet vs brown dwarf is kind of pointless. The distinction depends on the favoured theory of planet formation - core accretion vs gravitational instability - both of which have merits. If giant planets form just like brown dwarfs and stars via gravitational instability then there is no reasonable distinction. A "brown dwarf" burns deuterium for ~50 million years and after that it is slowly contracting as its heat trickles away, much like a cooling gas giant. A Main Sequence star however undergoes significant structural changes due to the proton-burning process and is quite distinctive. Brown-dwarfs are more like planets and less like stars, but it's an argument that serves little purpose anyway. Just try not to muddy the waters so much.
1 / 5 (2) Oct 16, 2010
... (pre)image (pro)pion (re)Ceres (dis)core (pri)geddon ...

Please sign in to add a comment. Registration is free, and takes less than a minute. Read more

Click here to reset your password.
Sign in to get notified via email when new comments are made.