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- W2076981639 abstract "The problem of detecting Jovian‐sized planets orbiting white dwarf stars is considered. Significant IR excesses result from warm Jupiters orbiting a white dwarf of Teff = 10,000 K at a distance of ∼103 white dwarf radii (corresponding to ∼102 Jupiter radii or a few tenths of an AU) with an orbital period of ∼100 days. Such a planet will have a 10 μm flux density at its Wien peak that is comparable to the emission of the white dwarf at that wavelength. Although the white dwarf is much hotter than the planet, the planet will have peak brightness at the IR, well into the Rayleigh‐Jeans tail of the white dwarf; plus, Jovians are about 10 times larger than white dwarfs, so there is a substantial gain in the planet‐to‐star brightness contrast as compared to planets around main‐sequence stars. In the solar neighborhood, there are 51 white dwarf stars within 13 pc of the Sun. At 10 pc, the IR flux density of warm Jupiters (a few hundred kelvins) will fall in the range 10–100 μJy, which should be observable with SIRTF." @default.
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- W2076981639 date "2001-10-01" @default.
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- W2076981639 title "Spectral Energy Distribution Signatures of Jovian Planets around White Dwarf Stars" @default.
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- W2076981639 doi "https://doi.org/10.1086/323288" @default.
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