Reconstructing the Extreme Ultraviolet Emission of Cool Dwarfs Using Differential Emission Measure Polynomials
نویسندگان
چکیده
Abstract Characterizing the atmospheres of planets orbiting M dwarfs requires understanding spectral energy distributions over planetary lifetimes. Surveys like MUSCLES, HAZMAT, and FUMES have collected multiwavelength spectra across type’s range T eff activity, but extreme ultraviolet (EUV, 100–912 Å) flux most these stars remains unobserved because obscuration by interstellar medium compounded with limited detector sensitivity. While targets observable EUV exist, there is no currently operational facility observing between 150 912 Å. Inferring exoplanet hosts in this regime critical to studying evolution heats top thermosphere drives atmospheric escape. This paper presents our implementation differential emission measure technique reconstruct cool dwarfs. We characterize method’s accuracy precision applying it Sun AU Mic. then apply three fainter dwarfs: GJ 832, Barnard’s star, TRAPPIST-1. demonstrate that strongest far-ultraviolet (FUV, 912–1700 lines, observed Hubble Space Telescope and/or Far Ultraviolet Spectroscopic Explorer, a coarse X-ray spectrum from either Chandra Observatory or XMM-Newton, we can Sun’s within factor 1.8, model’s formal uncertainties encompassing data. report integrated dwarf sample 2–7 depending on available data quality.
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2021
ISSN: ['2041-8213', '2041-8205']
DOI: https://doi.org/10.3847/1538-4357/abeaaf