Abstract
More than 30 years have passed since the successful detection of supernova (SN) neutrinos from SN 1987A. In the last few decades, remarkable progress has been made in neutrino detection techniques, through which it may be possible to detect neutrinos from a new source, presupernova (pre-SN) neutrinos. They are emitted from a massive star prior to core bounce. Because neutrinos escape from the core freely, they carry information about the stellar physics directly. Pre-SN neutrinos may play an important role in verifying our understanding of stellar evolution for massive stars. Observation of pre-SN neutrinos, moreover, may serve as an alarm regarding an SN explosion a few days in advance if the progenitor is located in our vicinity, enabling us to observe the next galactic SN. In this review, we summarize the current status of pre-SN neutrino studies from both the theoretical and observational points of view.
Highlights
Dark matter detectors to νxs via CEνNS is discussed in References 9–11
The nuclear weak processes [e.g., electron capture (EC), in which an electron is captured by a nucleus and a nuclear proton is changed to a neutron and β processes] enhance neutrino emission after iron-group elements are synthesized
It has been reported that pre-SN neutrino observations will make it possible to distinguish between the two types of CCSN progenitors—iron core-collapse supernovae (FeCCSNe) and electron-capture supernovae (ECSNe) [14]—and to impose restrictions on convective properties associated with oxygen shell (O shell) and silicon shell (Si shell) burning [15]
Summary
Massive stars—that is, stars with masses heavier than ∼8Mࣻ at the zero-age main sequence (ZAMS)—start their lives with hydrogen burning and end with a dynamical collapse of the central core (e.g., 20, 21). There are two types of progenitors that produce CCSNe. In most cases, the stellar core is mainly composed of iron (Fe core), and its collapse leads to an FeCCSN. The ignition temperature for hydrogen burning is ∼4 × 107 K, and it lasts ∼107 years for the 15Mࣻ model. Stars in this phase are observed as blue supergiants. Its surrounding hydrogen shell burning makes the pressure gradient larger at the bottom of the hydrogen shell and expands the hydrogen envelope Such a star is called a red supergiant (RSG). The helium core burning lasts ∼1.3 × 106 years in the 15Mࣻ model, and a carbon–oxygen.
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