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Neutrino Emissions in All Flavors up to the Pre-bounce of Massive Stars and the Possibility of Their Detections

  • Authors: Chinami Kato, Hiroki Nagakura, Shun Furusawa, Koh Takahashi, Hideyuki Umeda, Takashi Yoshida, Koji Ishidoshiro, and Shoichi Yamada

2017 The Astrophysical Journal 848 48.

  • Provider: AAS Journals

Caption: Figure 4.

Nuclear charts indicating in different colors the nuclear species with the reaction rates for EC (left) and ﹩{\beta }^{-}﹩ decay (right) given in the LMSH (black; Langanke et al. 2003), LMP (red; Langanke & Martínez-Pinedo 2001), ODA (blue; Oda et al. 1994), FFN (green; Fuller et al. 1985), and TACHI (yellow; Tachibana & Yamada 1995; Tachibana 2000; Yoshida & Tachibana 2000; Koura et al. 2003; Koura 2004; Koura et al. 2005) tables, as well as using the approximation formula (yellow; Equation (22)).

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