Theoretical Prediction of Presupernova Neutrinos and Their Detection

Abstract

Almost 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. Expected final online publication date for the Annual Review of Nuclear and Particle Science, Volume 70 is October 19, 2020. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics

“…In the event of a near-Earth (d < kpc) core-collapse supernova, future liquid xenon detectors will also be sensitive to neutrinos of all flavors that are emitted by a massive star in its silicon-burning stage, a few hours prior to core collapse [791,792]. Due to lower stellar temperatures before collapse, these "pre-supernova" neutrinos are O(10) softer than supernova neutrinos, and therefore require low thresholds for detection [793]. Figure 29 indicates that a next-generation liquid xenon experiment operating at 0.1 keV energy threshold would detect, in a 12 hour window prior to collapse, O(100) pre-supernova neutrinos from a massive star 200 pc away, e.g.…”

Observing Axion Emission from Supernova with Collider Detectors

“…This global network is called the Supernova Early Warning System (SNEWS) [53,54,55]. The calculation of the neutrino flux [27,56,57,58,59,60,61,62,63,64,65] shows that, if a SN progenitor is located within ∼ 1 kpc, the neutrino emission is large enough to be detected even before the SN core collapse. Such an increase of the pre-SN neutrino makes it possible to forecast the SN which occur within ∼ O(100) pc; for d SN 200 pc, an alert is possible O(1 − 10) hours before the core collapse [26,27].…”

“…The calculation of the neutrino flux [27,56,57,58,59,60,61,62,63,64,65] shows that, if a SN progenitor is located within ∼ 1 kpc, the neutrino emission is large enough to be detected even before the SN core collapse. Such an increase of the pre-SN neutrino makes it possible to forecast the SN which occur within ∼ O(100) pc; for d SN 200 pc, an alert is possible O(1 − 10) hours before the core collapse [26,27]. With the help of the pre-SN alert, we may know when the collider operation should be switched to the special one for the SN axion.…”

“…In addition, recently, Ref. [25] argued that, if a detector sensitive to ∼ 100 MeV photon is installed on a helioscope, detection of the axion from a nearby SN in the future may be possible with the help of the pre-SN neutrino alert [26,27].…”

Combined detection of supernova neutrino signals

“…As in the case of the core-collapse supernova neutrino burst, the presupernova neutrinos can be detected by various neutrino and dark matter experiments in several interaction channels [12]. Here we will limit our consideration to inverse beta-decay (IBD) channel in three experiments: KamLAND, Borexino and SK-Gd.…”