Hawking Radiation of Weyl Neutrinos in a Rectilinearly Non-uniformly Accelerating Kinnersley Black Hole Quantum thermal effect of Weyl neutrinos in a rectilinearly non-uniformly accelerating Kinnersley black hole is investigated by using the generalized tortoise coordinate transformation. The equation that determines the location, the Hawking temperature of the event horizon and the thermal radiation spectrum of neutrinos are derived. Our results show that the location and the temperature of the event horizon depend not only on the time but also on the angle. Published as: Chin.Phys. 11 (2002) 661-665 arXiv categories: gr-qc [gr-qc/0204005] Hawking Radiation of Weyl Neutrinos in a Rectilinearly Non-uniformly Accelerating Kinnersley Black Hole11footnote 1Supported by the NNSF of China under Grant number: 19875019 Hawking Radiation of Weyl Neutrinos in a Rectilinearly Non-uniformly Accelerating Kinnersley Black Hole 1 1 1 Supported by the NNSF of China under Grant number: 19875019 Wu Shuang-Qing and Cai Xu Institute of Particle Physics, Hua-Zhong Normal University, Wuhan 430079, China E-mail: sqwu@iopp.ccnu.edu.cn Quantum thermal effect of Weyl neutrinos in a rectilinearly non-uniformly accelerating Kinnersley black hole is investigated by using the generalized tortoise coordinate transformation. Keywords : Hawking radiation, Weyl neutrino, non-stationary Kinnersley black hole, generalized tortoise coordinate transformation PACC : 0420, 9760L 1 Introduction The discovery of Hawking radiation [ 1 ] [ 1 ] {}^{\cite[cite]{[\@@bibref{}{Hawk}{}{}]}} has not only solved some contradictions inside black hole thermodynamics but also revealed a profound intrinsic relations among quantum mechanics, thermodynamics and general relativity. It is an important subject of black hole physics to investigate the thermal properties of various black holes. [ 2 ] [ 2 ] {}^{\cite[cite]{[\@@bibref{}{Zhao}{}{}]}} Thanks to the existence of various astrophysical processes such as evaporation and accretion, [ 3 ] [ 3 ] {}^{\cite[cite]{[\@@bibref{}{XM}{}{}]}} a black hole in the universe must change with time, thus to make a deeper investigation on the Hawking radiation of an evaporating black hole is of much significance to understand such dark celestial bodies as black holes. In recent years, researches on the Hawking radiation of non-stationary black holes attract much more attention, but most of these studies concentrated on the quantum thermal effect of scalar fields. The investigation of the Hawking radiation of fermions in the non-static black holes is merely limited to those in spherically symmetric ones. [ 2 ] [ 2 ] {}^{\cite[cite]{[\@@bibref{}{Zhao}{}{}]}} Recently, by making use of the generalized tortoise transformation proposed by Zhao Zheng, [ 2 ] [ 2 ] {}^{\cite[cite]{[\@@bibref{}{Zhao}{}{}]}} Wu and Cai [ 4 ] [ 4 ] {}^{\cite[cite]{[\@@bibref{}{WC1}{}{}]}} has successfully dealt with the Hawking radiation of Dirac particles in a non-stationary Kerr black hole. [ 5 ] [ 5 ] {}^{\cite[cite]{[\@@bibref{}{CM}{}{}]}} They simultaneously treated the first-order and second-order Dirac equations and derived both the event horizon equation and the Hawking temperature which coincide with previous results. [ 6 ] [ 6 ] {}^{\cite[cite]{[\@@bibref{}{NK}{}{}]}} A New quantum effect observed in the thermal radiation spectrum of fermions probably originates from the coupling of the spin of [ 4 ] to cope with the Hawking radiation of massless fermions namely Weyl neutrinos in a rectilinearly non-uniformly accelerating Kinnersley black hole. [ 7 ] [ 7 ] {}^{\cite[cite]{[\@@bibref{}{Kinn}{}{}]}} The corresponding quantum thermal effect of scalar particles in the same space-time has already been studied in Ref. [ 8 ] . Eq. ( 10 ) shows that r h subscript 𝑟 ℎ r_{h} depends not only on v 𝑣 v but also on θ 𝜃 \theta . This means that the location of the event horizon and the shape of the black hole change with time. 4 Hawking temperature To investigate the Hawking radiation of Weyl neutrinos, we are now in a position to consider the second-order form of the Weyl equation. 6 Conclusions Equations ( 10 ) and ( 26 ) give the location and the temperature of event horizon, which depend not only on the advanced time v 𝑣 v but also on the polar angle θ 𝜃 \theta . They are just the same results as that obtained in the discussion of the thermal radiation of scalar fields. [ 8 ] [ 8 ] {}^{\cite[cite]{[\@@bibref{}{LZ}{}{}]}} Equation ( 25 ) shows the Hawking radiation spectrum of Weyl neutrinos in a rectilinearly non-uniformly accelerating Kinnersley black hole. This study and those in Refs. [4,12-14] manifest that the method of generalized coordinate transformation is a powerful tool to investigate black hole radiation. Zhao Zheng [ 2 ] [ 2 ] {}^{\cite[cite]{[\@@bibref{}{Zhao}{}{}]}} further extended this transformation in the static and stationary cases to that in the non-static and non-stationary cases and have made several discussions about the quantum thermal effects of scalar fields in various black holes and that of Dirac particles in some non-static and spherically symmetric black holes. But this method meets great difficulties when it is applied to the Hawking radiation of Dirac particles in a most general space-time such as a non-static and non-spherically symmetric black hole or a non-stationary axisymmetry black hole. They indicate that this theory becomes a fairly integrated system. The method developed by us is applicable not only to discussing the Hawking radiation of Weyl neutrinos in a non-static and non-spherically symmetric Kinnersley black hole with arbitrarily acceleration and that of electrons in a non-stationary axisymmetry black hole, but also, in principle, to studying the quantum thermal effect of any space-time with a non-degenerate event horizon. [ 14 ] [ 14 ] {}^{\cite[cite]{[\@@bibref{}{WC4}{}{}]}} Also it is easily extended to discuss the Hawking effect of fields with an arbitrary spin.