Other
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21734325l&link_type=abstract
American Astronomical Society, AAS Meeting #217, #343.25; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
This paper reports Very Large Array (VLA) observations at 325 and 1425 MHz during and near the periastron passage of HD 80606b on 2007 November 20. We obtained 3σ limits of 1.7 mJy and 48 microJy at 325 and 1425 MHz, respectively, equivalent to planetary luminosity limits of 2.3 x 1024 erg/s and 2.7 x 1023 erg/s. Unfortunately, these are orders of magnitude above the Jovian value (at 40 MHz) of 2 x 1018 erg/s. The motivation for these observations was that the planetary magnetospheric emission is driven by a stellar wind-magnetosphere interaction so that the planetary luminosity should be elevated near periastron. We estimate that, near periastron, HD 80606b might be as much as 3000x more luminous than Jupiter. Transit observations of HD 80606b provide stringent constraints on the planetary mass and radius, and, because of the planet's highly eccentric orbit, its rotation period is likely to be "pseudo-synchronized" to its orbital period, allowing a robust estimate of the former. Consequently, we are able to make a robust estimate of the emission frequency of the planetary magnetospheric emission and find it to be around 60--90 MHz. While this is too low for our reported observations, we compare HD 80606b to other high eccentricity systems and assess the detection possibilities for both near-term and more distant future systems. Of the known high eccentricity planets, only HD 80606b is likely to be detectable, as the others (HD 20782Bb and HD 4113) are both lower mass and longer rotational periods, which imply a weaker magnetic field strengths. Both the forthcoming "EVLA low band" system, which will operate as low as 65 MHz, and the Low Frequency Array (LOFAR) may be able to improve upon our planetary luminosity limits for HD 80606b, and do so at a more optimum frequency.
Blank David L.
Farrell William M.
Lazio Joseph T. W.
Shankland Paul D.
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