2016ApJ...818...91A

Query : 2016ApJ...818...91A

2016ApJ...818...91A - Astrophys. J., 818, 91 (2016/February-2)

KamLAND sensitivity to neutrinos from pre-supernova stars.

ASAKURA K., GANDO A., GANDO Y., HACHIYA T., HAYASHIDA S., IKEDA H., INOUE K., ISHIDOSHIRO K., ISHIKAWA T., ISHIO S., KOGA M., MATSUDA S., MITSUI T., MOTOKI D., NAKAMURA K., OBARA S., OURA T., SHIMIZU I., SHIRAHATA Y., SHIRAI J., SUZUKI A., TACHIBANA H., TAMAE K., UESHIMA K., WATANABE H., XU B.D., KOZLOV A., TAKEMOTO Y., YOSHIDA S., FUSHIMI K., PIEPKE A., BANKS T.I., BERGER B.E., FUJIKAWA B.K., O'DONNELL T., LEARNED J.G., MARICIC J., MATSUNO S., SAKAI M., WINSLOW L.A., EFREMENKO Y., KARWOWSKI H.J., MARKOFF D.M., TORNOW W., DETWILER J.A., ENOMOTO S., DECOWSKI M.P. (The KamLAND Collaboration)

Abstract (from CDS):

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 evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of 25 M_☉ at a distance less than 690 pc with 3σ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community.

Abstract Copyright: ∼

Journal keyword(s): neutrinos - supernovae: general

Simbad objects: 11

Full paper

View the references in ADS

Number of rows : 11

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2024	#notes
1	* 3 Cet	s*r	00 04 30.1187522978	-10 30 34.278904524		6.541	4.924			K3Ib	110	0
2	NAME LMC	G	05 23 34.6	-69 45 22			0.4			~	17459	0
3	* 119 Tau	s*r	05 32 12.7516308641	+18 35 39.251766506	8.63	6.41	4.33	2.55	1.13	M2Iab-Ib	278	0
4	SN 1987A	SN*	05 35 28.020	-69 16 11.07						SNIIpec	4942	2
5	* alf Ori	s*r	05 55 10.30536	+07 24 25.4304	4.38	2.27	0.42	-1.17	-2.45	M1-M2Ia-Iab	1672	0
6	* sig CMa	s*r	07 01 43.1480404483	-27 56 05.389225598	7.08	5.20	3.47	2.15	1.15	K5Ib	176	0
7	* pi. Pup	LP*	07 17 08.55678	-37 05 50.8962	5.57	4.32	2.70	1.46	0.55	K4III	110	0
8	* h01 Pup	s*r	08 11 21.4934302224	-39 37 06.758795424	7.79	6.03	4.42	3.22	2.34	K4.5Ib	63	0
9	* eta Car	Em*	10 45 03.545808	-59 41 03.95124	6.37	7.03	6.48	6.123	4.41	LBV	2442	0
10	* alf Sco	s*r	16 29 24.45970	-26 25 55.2094	4.08	2.75	0.91	-0.64	-1.87	M1.5Iab+B2Vn	746	0
11	* eps Peg	LP*	21 44 11.1561394	+09 52 30.031152	5.61	3.91	2.39	1.34	0.58	K2Ib-II	446	0

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