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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 5.

Time evolution of the neutrino number luminosity for the ﹩15\ {M}_{\odot }﹩ progenitor model. The origin of the horizontal axis corresponds to the time the dynamical simulation is started. Dotted and solid lines show the results for ﹩{{\nu }}_{{e}}﹩ and ﹩{\bar{{\nu }}}_{{e}}﹩ , respectively. Colors distinguish the different reactions. In the collapse phase, only the total luminosity is shown for ﹩{\nu }_{e}﹩ (pink dotted), since it is the quantity that the dynamical simulation provides. Note that the same number of ﹩{\nu }_{e}﹩ and ﹩{\bar{\nu }}_{e}﹩ is produced from electron–positron pair annihilations (red solid).

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