From: Harvard-Smithsonian Center for Astrophysics
Posted: Friday, April 29, 2011
A planet that we thought we knew turns out to be rather different than first suspected. Our revised view comes from new data released today by an international team of astronomers. They made their observations of the planet "55 Cancri e" based on calculations by Harvard graduate student Rebekah Dawson (Harvard-Smithsonian Center for Astrophysics), who worked with Daniel Fabrycky (now at the University of California, Santa Cruz) to predict when the planet crosses in front of its star as seen from Earth. Such transits give crucial information about a planet's size and orbit.
The team found that 55 Cancri e is 60 percent larger in diameter than Earth but eight times as massive. (A super-Earth has one to 10 times the mass of Earth.) It's the densest solid planet known, almost as dense as lead. Even better, the star it orbits is so close and bright that it's visible to the naked eye in the constellation Cancer the Crab. This makes it an excellent target for follow-up studies.
Dawson and Fabrycky's prediction played a crucial role in this new work by motivating the search for transits. When the planet was discovered by a Texas team in 2004, it was calculated to orbit its star every 2.8 days. Dawson and Fabrycky reanalyzed the data and found that 55 Cancri e was much closer to its star, orbiting it in less than 18 hours. As a result, the chances of seeing a transit were much higher.
Josh Winn of MIT and Smithsonian astronomer Matthew Holman brought the new calculation to Jaymie Matthews (University of British Columbia), who scheduled observations with Canada's MOST (Microvariability & Oscillations of STars) satellite. The research team found that 55 Cancri e transits its star every 17 hours and 41 minutes, just as Dawson and Fabrycky predicted.
"I'm excited that by calculating the planet's true orbital period, we were able to detect transits, which tell us so much more about it," said Dawson.
The new technique applies to planets discovered by the radial velocity method, in which astronomers hunt for a star that "wobbles" from the gravitational tug of an orbiting world.
The initial confusion about the orbit of 55 Cancri e arose because of natural gaps in the radial velocity data (because astronomers can only observe a star at night and when it's above the horizon). Sometimes these gaps introduce "ghost" signals that can masquerade as the planet's true signal.
Dawson and Fabrycky chose to analyze six planetary systems where the data seemed particularly ambiguous. In two cases they confirmed previous results, while some remained unclear. For 55 Cancri e, a period revision was certainly needed.
"It became very clear that the planet's actual orbital period was closer to 18 hours," stated Dawson.
This places the planet so close to its star that it's blasted with heat, baked to a temperature of 4,900 degrees F.
The star itself, 55 Cancri A, is a yellow star very similar to the Sun and located 40 light-years away. It's the brightest, closest star known to have a transiting planet.
Dawson recommends that the analysis method she developed with Fabrycky be used on future planet discoveries. "We've cleared up some confusion in the systems we studied, and we believe we've provided a way to avoid future confusion," she said.
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Companion release from UBC: http://www.publicaffairs.ubc.ca/2011/04/28/astronomers-unveil-portrait-of-"super-exotic-super-earth"-densest-known-rocky-planet/
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