KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

Asakura, Kiyotaka; Gando, A.; Gando, Y.; Hachiya, Takahiko; Hayashida, S.; Ikeda, H.; Inoue, K.; Ishidoshiro, K.; Ishikawa, T.; Ishio, S.; Koga, M.; Matsuda, Sumio; Mitsui, Tadao; Motoki, D.; Nakamura, K.; Obara, Shigeru; Oura, Toshiaki; Shimizu, I.; Shirahata, Y.; Shirai, J.; Suzuki, A.; Tachibana, Hideki; Tamae, K.; Ueshima, K.; Watanabe, Hiroko; Xu, B. D.; Kozlov, A.; Takemoto, Y.; Yoshida, S.; Fushimi, K.; Piepke, A.; Banks, Thomas; Berger, B. E.; Fujikawa, B. K.; O’Donnell, T.; Learned, J. G.; Maricic, J.; Matsuno, S.; Sakai, M.; Winslow, L. A.; Efremenko, Y. V.; Karwowski, H. J.; Markoff, D. M.; Tornow, W.; Detwiler, J. A.; Enomoto, S.; Decowski, M. P.

doi:10.3847/0004-637x/818/1/91

Cited by 64 publications

(54 citation statements)

References 46 publications

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“…This is because both the luminosity and average energy increase with density. The detections of e n in the pre-bounce phase are hence more suitable as an alert of an imminent supernova (Asakura et al 2016;Yoshida et al 2016). In fact, we may be able to issue an alert a few days before core collapse for Fe-core progenitors if neutrinos obey the normal mass hierarchy.…”

Section: Event Numbers At Detectorsmentioning

confidence: 99%

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

Kato

Nagakura

Furusawa

et al. 2017

ApJ

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This paper is a sequel to our 2015 paper, Kato et al., which calculated the luminosities and spectra of electron-type anti-neutrinos ( e n ) from the progenitors of core-collapse supernovae. Expecting that the capability to detect electron-type neutrinos ( e n ) 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 electron capture supernovae (ECSNe) and iron-core collapse supernovae (FeCCSNe). We find that the number luminosities reach ∼10 57 s -1 and ∼10 53 s -1 at maximum for e n and e n , respectively. We also estimate the numbers of detection events at terrestrial neutrino detectors including DUNE, taking flavor oscillations into account and assuming the distance to the progenitors to be 200 pc. It is demonstrated that e n from the ECSN progenitor will be undetected at almost all detectors, whereas we will be able to observe 15,900 e n at DUNE for the inverted mass hierarchy. From the FeCCSN progenitors, the number of e n events will be largest for JUNO, 200-900 e n , depending on the mass hierarchy, whereas the number of e n events at DUNE is 2100  for the inverted mass hierarchy. These results imply that the detection of e n is useful to distinguish progenitors of FeCCSNe from those of ECSNe, while e n will provide us with detailed information on the collapse phase regardless of the type and mass of the progenitor.

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Section: Event Numbers At Detectorsmentioning

confidence: 99%

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

Kato

Nagakura

Furusawa

et al. 2017

ApJ

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“…(Duan & Kneller 2009) and references therein), and at a basic level for presupernova neutrinos (Asakura et al 2016;Kato et al 2015Kato et al , 2017. Similarly to the burst neutrinos, presupernova neutrinos undergo adiabatic, matterdriven, conversion inside the star.…”

Section: Oscillations Of Presupernova Neutrinosmentioning

confidence: 99%

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

Patton

Lunardini

Farmer

et al. 2017

ApJ

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We present a new calculation of the neutrino flux received at Earth from a massive star in the ∼ 24 hours of evolution prior to its explosion as a supernova (presupernova). Using the stellar evolution code MESA, the neutrino emissivity in each flavor is calculated at many radial zones and time steps. In addition to thermal processes, neutrino production via beta processes is modeled in detail, using a network of 204 isotopes. We find that the total produced ν e flux has a high energy spectrum tail, at E > ∼ 3 − 4 MeV, which is mostly due to decay and electron capture on isotopes with A = 50 − 60. In a tentative window of observability of E > ∼ 0.5 MeV and t < 2 hours pre-collapse, the contribution of beta processes to the ν e flux is at the level of ∼ 90% . For a star at D = 1 kpc distance, a 17 kt liquid scintillator detector would typically observe several tens of events from a presupernova, of which up to ∼ 30% due to beta processes. These processes dominate the signal at a liquid argon detector, thus greatly enhancing its sensitivity to a presupernova.

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“…The total emissivities of all these processes, over a range of temperatures and densities, were discussed in detail by Itoh and Kohyama (1983); Itoh et al (1989Itoh et al ( , 1992Itoh et al ( , 1996a . The differential rates and emissivities of selected process have been discussed by several authors (Odrzywolek 2007;Dutta et al 2004;Ratkovic et al 2003;Misiaszek et al 2006;Kato et al 2015;Asakura et al 2016). In this section, we summarize the formalism relevant to our calculation.…”

Section: Thermal Processesmentioning

confidence: 99%

“…These neutrinos could become detectable months before the collapse, during the oxygen-burning phase, for the closest supernova candidate, Betelgeuse. Days or hours before (silicon-burning phase) might be more realistic for a star a few kiloparsecs away (Odrzywolek and Heger 2010;Asakura et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Presupernova Neutrinos: Realistic Emissivities from Stellar Evolution

Patton

Lunardini

Farmer

2017

ApJ

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We present a new calculation of neutrino emissivities and energy spectra from a massive star going through the advanced stages of nuclear burning (presupernova) in the months before becoming a supernova. The contributions from beta decay and electron capture, pair annihilation, plasmon decay, and the photoneutrino process are modeled in detail, using updated tabulated nuclear rates. We also use realistic conditions of temperature, density, electron fraction and nuclear isotopic composition of the star from the state of the art stellar evolution code MESA. Results are presented for a set of progenitor stars with mass between 15 M ⊙ and 30 M ⊙ . It is found that beta processes contribute substantially to the neutrino emissivity above realistic detection thresholds of few MeV, at selected positions and times in the evolution of the star.

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KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

Cited by 64 publications

References 46 publications

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

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

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

Presupernova Neutrinos: Realistic Emissivities from Stellar Evolution

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