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

@article{Kato2017NeutrinoEI,
  title={Neutrino Emissions in All Flavors up to the Pre-bounce of Massive Stars and the Possibility of Their Detections},
  author={Chinami Kato and Hiroki Nagakura and Shun Furusawa and Koh Takahashi and Hideyuki Umeda and Takashi Yoshida and Koji Ishidoshiro and Shoichi Yamada},
  journal={The Astrophysical Journal},
  year={2017},
  volume={848}
}
This paper is a sequel to our 2015 paper, Kato et al., which calculated the luminosities and spectra of electron-type anti-neutrinos ( ν ¯ e ) from the progenitors of core-collapse supernovae. Expecting that the capability to detect electron-type neutrinos ( ν e ) will increase dramatically with the emergence of liquid-argon detectors such as DUNE, we broaden the scope in this study to include all flavors of neutrinos emitted from the pre-bounce phase. We pick up three progenitor models of… 

Pre-supernova neutrino emission from massive stars and their detection

Recent progress of neutrino detectors makes it possible to detect pre-SN neutrinos, which are emitted from the core of massive stars before supernova explosions. Pre-SN neutrino observations will

Prospects for pre-supernova neutrino observation in future large liquid-scintillator detectors

Before massive stars heavier than (8 ⋯ 10) solar masses evolve to the phase of a gravitational core collapse, they will emit a huge number of MeV-energy neutrinos that are mainly produced in the

Neutrino signals of core-collapse supernovae in underground detectors

For a suite of fourteen core-collapse models during the dynamical first second after bounce, we calculate the detailed neutrino "light" curves expected in the underground neutrino observatories

Detectability of collective neutrino oscillation signatures in the supernova explosion of a 8.8  M⊙ star

In order to investigate the impact of collective neutrino oscillations (CNO) on the neutrino signal from a nearby supernova, we perform 3-flavor neutrino oscillation simulations employing the

Neutrinos from Beta Processes in a Presupernova: Probing the Isotopic Evolution of a Massive Star

We present a new calculation of the neutrino flux received at Earth from a massive star in the ∼24 hr of evolution prior to its explosion as a supernova (presupernova). Using the stellar evolution

Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over 10 s

Supernova neutrinos are crucially important to probe the final phases of massive star evolution. As is well known from observations of SN 1987A, neutrinos provide information on the physical

Online triggers for supernova and pre-supernova neutrino detection with cryogenic detectors

Supernovae (SNe) are among the most energetic events in the universe still far from being fully understood. An early and prompt detection of neutrinos is a one-time opportunity for the realization of

The neutrino emission from thermal processes in very massive stars in the local universe

We present a new overview of the life of very massive stars (VMS) in terms of neutrino emission from thermal processes: pair annihilation, plasmon decay, photoneutrino process, bremsstrahlung and

Neutrino Transport with Monte Carlo Method. I. Toward Fully Consistent Implementation of Nucleon Recoils in Core-collapse Supernova Simulations

The small energy exchange via nucleon recoils in neutrino–nucleon scattering is now supposed to be one of the important factors for successful explosions of core-collapse supernovae (CCSNe), as they

References

SHOWING 1-10 OF 71 REFERENCES

KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

In the late stages of nuclear burning for massive stars (M > 8 M⊙), the production of neutrino–antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star

PRE-SUPERNOVA NEUTRINO EMISSIONS FROM ONe CORES IN THE PROGENITORS OF CORE-COLLAPSE SUPERNOVAE: ARE THEY DISTINGUISHABLE FROM THOSE OF Fe CORES?

Aiming to distinguish two types of progenitors of core-collapse supernovae, i.e., one with a core composed mainly of oxygen and neon (abbreviated as ONe core) and the other with an iron core (or Fe

Neutrino spectra evolution during protoneutron star deleptonization

The neutrino-driven wind, which occurs after the onset of a core-collapse supernova explosion, has long been considered as the possible site for the synthesis of heavy $r$-process elements in the

Presupernova neutrino events relating to the final evolution of massive stars

When a supernova explosion occurs in neighbors around hundreds pc, current and future neutrino detectors are expected to observe neutrinos from the presupernova star before the explosion. We show a

SUPERNOVA EXPLOSIONS OF SUPER-ASYMPTOTIC GIANT BRANCH STARS: MULTICOLOR LIGHT CURVES OF ELECTRON-CAPTURE SUPERNOVAE

An electron-capture supernova (ECSN) is a core-collapse supernova (CCSN) explosion of a super-asymptotic giant branch (SAGB) star with a main-sequence mass MMS ∼ 7–9.5 M☉. The explosion takes place

Explosion Mechanisms of Core-Collapse Supernovae

Supernova theory, numerical and analytic, has made remarkable progress in the past decade. This progress was made possible by more sophisticated simulation tools, especially for neutrino transport,

The dynamics of neutrino-driven supernova explosions after shock revival in 2D and 3D

We study the growth of the explosion energy after shock revival in neutrino-driven explosions in two and three dimensions (2D/3D) using multi-group neutrino hydrodynamics simulations of an $11.2

THE SENSITIVITY OF CORE-COLLAPSE SUPERNOVAE TO NUCLEAR ELECTRON CAPTURE

A weak-rate library aimed at investigating the sensitivity of astrophysical environments to variations of electron-capture rates on medium-heavy nuclei has been developed. With this library, the
...