News Release
March 22, 2006
Carnegie contacts:
Alan Boss at boss@dtm.ciw.edu or
202-478-8858
John Debes at debes@dtm.ciw.edu or
202-478-8862
Catherine Hier-Majumder at catherine@dtm.ciw.edu or 202-478-8846
Hannah
Jang-Condell at hannah@dtm.ciw.edu or 202-478-8863
Alycia
Weinberger at weinberger@dtm.ciw.edu or 202-478-8852
Media representatives who wish to attend the AbSciCon 2006 contact Jonas Dino Jonas.Dino@nasa.gov or 1 650-604-5612
Ideas on gas-giant planet formation take shape
Washington, D.C. Rocky planets such as Earth and Mars are born when small particles smash together to form larger, planet-sized clusters in a planet-forming disk, but researchers are less sure about how gas-giant planets such as Jupiter and Saturn form. Is core accretion—the process that creates their smaller, terrestrial cousins—responsible? Or could an alternate model known as disk instability—in which the planet-forming disk itself actually fragments into a number of planet-sized clumps—be at work? Could both be possible under different circumstances?
Recent work from the Carnegie Institution’s Department of Terrestrial Magnetism explores both possibilities. This and other relevant work regarding planet formation is presented at the NASA Astrobiology Science Conference (AbSciCon) 2006 at the Ronald Reagan Building in Washington, D.C. March 26-30. See http://abscicon2006.arc.nasa.gov/ for details.
Carnegie Fellow Hannah Jang-Condell1 has devised a method to catch the early stages of gas-giant core accretion in the act. If actively accreting cores exist, they should leave a gravitational “dimple” in the planet-forming disk—even if the cores are only a fraction the size of Jupiter. Since disk instability would result in planet-sized fragments straight away, the existence of these young, intermediate-sized cores would be a clear indicator of core accretion.
The telltale gravitational dimples resemble craters on the Moon with sunlight shining in from the side: the inside of the edge nearest the star is shadowed, while the star-facing edge is illuminated. The bright side heats up and the shadowed side remains cool, yielding a distinct thermal pattern that an Earth-based observer should be able to see in the infrared spectrum. “If we could detect this signature in a protoplanetary disk, it would indicate the presence of a young planetary body that could go on to form a gas-giant via core accretion,” Jang-Condell said.
In some situations, however, core accretion seems an unlikely model for gas-giant planet formation. For example, theoretical computer models by DTM staff member Alan Boss2 suggest that disk instability best explains planet formation around M dwarf stars, which have masses from one tenth to one half that of the Sun. Core accretion would likely take more than 10 million years around these small, gravitationally weak stars, while disk instability happens quickly enough to yield gas-giant planets in as little as 1,000 years.
“M dwarf stars dominate the stellar population in the solar neighborhood, and so are attractive targets for searching for habitable planets,” Boss said. “The models show that gas-giant planets are indeed likely to form…at distances sufficiently large enough to permit the later formation of habitable, terrestrial planets.”
Other talks and posters
on planet formation at the conference include: A study of organic matter
in the planet-forming disks of three young stars, ranging in age from less
than one million to over 300 million years3;
methods to detect water ice, methane ice, and silicate dust in the planet-forming
disks of distant stars4; and a method to deduce the composition
of far-off planets based on their mass and radius5.
___________
Talk and poster schedule subject to change. See http://abscicon2006.arc.nasa.gov/agenda.php for
the latest information.
1Hannah Jang-Condell, “Planet
Shadows in Disks as Signatures of Core Formation”
Tuesday, March 28, 2006, 10:40am
Reagan Center, Horizon B conference room, Session 12: Exploring Planets
Around Other Stars II
2Alan Boss, “Planetary
System Formation Around M Dwarf Stars”
Wednesday, March 29, 2006, 10:40am
Reagan Center, Polaris B conference room, Session 24: Astronomical Topics
General Session
3Alycia Weinberger
et al., “Observations of Hydrocarbons in Circumstellar
Disks”
Tuesday, March 28, 2006, 5:05pm
Reagan Center, Polaris B conference room, Session 19: Extraterrestrial
Prebiotic Chemistry I
4John Debes
et al., “Dust
and Ices in the Scattered Light of Planet Forming Disks”
Poster displayed throughout the conference. Poster session Monday night,
March 27, 2006, 6-8pm
Reagan Center, Atrium Hall
5Catherine
Hier-Majumder and Sara Seager,
“Mass-Radius Relations for Planets”
Poster displayed throughout the conference. Poster session Monday night,
March 27, 2006, 6-8pm
Reagan Center, Atrium Hall
____________
The
Carnegie Institution of Washington has been a pioneering force in basic scientific
research since 1902. It is a private, nonprofit organization with six research
departments throughout the U.S. Carnegie scientists are leaders in plant
biology, developmental biology, astronomy, materials science, global ecology,
and Earth and planetary science. See www.carnegieinstitution.org
This work is supported by the NASA Astrobiology Institute (NAI). The NAI, founded in 1998, is a partnership between NASA, 16 major U.S. teams and six international consortia. NAI's goal is to promote, conduct, and lead integrated multidisciplinary astrobiology research and to train a new generation of astrobiology researchers. For more information about the NAI on the Internet, visit: http://nai.nasa.gov/