Production and utilization of sugar beets

Suzaku and NuSTAR X-ray spectroscopy of γ Cassiopeiae and HD 110432

“…In the X-rays, however, γ Cas is quite anomalous. Previous observations (Mason et al 1976;Frontera et al 1987;White et al 1982;Murakami et al 1986;Horaguchi et al 1994;Haberl 1995;Smith et al 1998;Kubo et al 1998;Owens et al 1999;Robinson & Smith 2000;Robinson et al 2002;Smith et al 2004b;den Hartog et al 2006;Lopes de Oliveira et al 2010;Shrader et al 2015;Hamaguchi et al 2016) revealed an X-ray luminosity of ∼10 32−33 erg s −1 , the lack of drastic flux variations such as X-ray outbursts, the presence of the Fe K complex resolved into three emission lines from highly ionized Fe (Fe XXV Heα and Fe XXVI Lyα respectively at 6.7 and 7.0 keV) as well as quasi-neutral Fe (Fe I Kα at 6.4 keV). It has an exceptionally high plasma temperature beyond ∼10 keV, which is unseen in other classes of early-type stars.…”

“…The X-ray spectral modeling of γ Cas analogs is far behind these developments. In all previous work, the spectra were fitted only with phenomenological models comprised of several components of iso-thermal collisionally-ionized plasma emission (White et al 1982;Murakami et al 1986;Horaguchi et al 1994;Haberl 1995;Kubo et al 1998;Owens et al 1999;Robinson & Smith 2000;Smith et al 2004b;Shrader et al 2015;Hamaguchi et al 2016;Torrejón & Orr 2001;Lopes de Oliveira et al 2007;Torrejón et al 2012). Under the working hypothesis of this paper, we apply physical models developed for classical WD binaries to the two brightest γ Cas analogs.…”