Biology
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20916912c&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #169.12; Bulletin of the American Astronomical Society,
Biology
Scientific paper
We present an analysis of the expected ultraviolet auroral emission strengths from extrasolar giant planets and the feasibility of detecting such exoplanetary aurora. Searching for and studying the ultraviolet auroral emission generated by extrasolar giant planets has unique advantages not offered by other methods. First, UV auroral emission is a means of detecting a planet directly as opposed to the indirect methods employed to date, such as radial velocity and pulsar timing. Second, the detection of an auroral signature would provide evidence of the presence of a planetary magnetic field. No other detection method can provide such evidence. Third, UV auroral emission could play a role in characterizing the near space environment around these planets, providing information about basic atmospheric composition and the deposition energies of the impacting particles. Fourth, ultraviolet wavelengths provide observational advantages compared to the optical. For instance, more favorable contrast ratios can be achieved and the UV diffraction limit allows planets to be detected at smaller angular separations to their host stars. Using Jupiter as a template and taking into account some basic properties involved in auroral production, possible emission fluxes were estimated for a given set of planetary system parameters. Potential candidate planets for UV observations are identified and the possibility of detecting UV auroral emissions with current and future technology is explored.
This research has been supported by NSF IGERT Grant No. DGE-9870713 through the Astrobiology Program at the University of Washington, Seattle.
Agol Eric
Cash Michele
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