THE EVOLUTION OF SOLAR FLUX FROM 0.1 nm TO 160 μm: QUANTITATIVE ESTIMATES FOR PLANETARY STUDIES

By M. Claire, J. Sheets, Martin Cohen, I. Ribas, V. Meadows, David C. Catling. 2012

204 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/812ee3773bbbb42ad39f36505f272765c6c4fb0b

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In Astronomy and Astrophysics

Citations in the corpus

The Surface UV Environment on Planets Orbiting M Dwarfs: Implications for Prebiotic Chemistry and the Need for Experimental Follow-up (2017, methodology): “To establish a basis of comparison between Mdwarfs and Sunlike stars, we use the model of Claire et al. (2012) to calculate the spectra of the young Sun at 3.9 Ga.”
Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets (2016, methodology): “Our modern solar spectrum was modeled by Chance & Kurucz (2010), and our “Archean” Sun uses a modified spectrum based on the wavelength-dependent solar evolution correction from Claire et al. (2012) for 2.7 Ga.”
Strange messenger: A new history of hydrogen on Earth, as told by Xenon (2018, background): “It is observed that older sunlike stars emit less X-ray and FUV radiation (Zahnle and Walker, 1982; Ribas et al., 2005; Claire et al., 2012; Tu et al., 2015).”
Transient reducing greenhouse warming on early Mars (2016, unknown): “…, 1965; Clough et al. , 1992; Rothman et al. , 2013; Murphy and Koop , 2005; Gruszka and Borysow , 1997; Baranov et al. , 2004; Wordsworth et al. , 2010; Pierrehumbert , 2011; Hansen and Travis , 1974; Claire et al. , 2012; Béguier et al. , 2015; Goldblatt et al. , 2013; Schaefer et al. , 2016].”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, methodology): “Güdel et al. (1997), Ribas et al. (2005) and Claire et al. 2012 analyzed multiwavelength EUV observations by the ASCA, ROSAT, EUVE, FUSE and IUE satellites of solar proxies with ages <4.6 Gyr and found that the EUV flux is saturated during the first 100 Myr at a value ∼100 times that of the…”
How Hospitable Are Space Weather Affected Habitable Zones? The Role of Ion Escape (2017, unknown): “Finally, to approximate the spectrum of the young Sun at 0.7 Gyr, we used the data obtained from the parameterization of the two young solar analogs of the Sun at around 0.7 Gyr, k 1 Cet, and EK Dra ( Claire et al. 2012 ) .”
HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, background): “Claire et al. (2012) have shown a similar change with wavelength for a small sample of Sun-like stars.”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, methodology): “For X-rays, the “Sun in Time” sample was used with ages between ≈ 100 Myr and ≈ 5 Gyr (Güdel et al. 1997), and this was complemented with the corresponding decay laws for the extreme-ultraviolet and far ultraviolet radiation (Ribas et al. 2005) and also near-UV (Claire et al. 2012).”
The habitability of Proxima Centauri b. I. Irradiation, rotation and volatile inventory from formation to the present (2016, background): “While the variation of XUV emissions with time is relatively well constrained for Sun-like stars (Ribas et al. 2005; Claire et al. 2012), the situation for M dwarfs (and especially mid-late M dwarfs) is far from understood.”
Origin and loss of nebula-captured hydrogen envelopes from ‘sub’- to ‘super-Earths’ in the habitable zone of Sun-like stars (2014, methodology): “…hydrogen envelopes from protoplanets with ‘sub-‘to ‘super-Earth’ masses, during the XUV saturated phase of a Sun-like star (e.g., Ayres 1997; Güdel et al. 1995; Güdel 1997; Güdel et al. 1997; Guinan et al. 2003; Ribas et al. 2005; Claire et al. 2012), in the habitable zone (HZ) at 1 AU.”