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1
2 ( :YITP- W- ) ( )
3
4 1 M1
5 D1 ALMA NGC3256 D1 M1 X M1-2
6 a1 M2 a2 M1 a3 M1 CTA a4 M1 c1 M2 c2 D2 c3 M2 c4 M2 c5 M1 Gravitational Leptogenesis
7 a2 M1
8 ( ) Abstract ev(knee energy) 12 TopB ( ) Shadow 3torr 250km/s 300km/s 3torr Shadow 0.7cm Introduction 1 ( ) Maxwell ( ) power-law ( ) ev(knee energy)
9 Mach 1: ( :Simon P.Swordy) Motivation 3 3 Methods TopB X (ejecta) ( ) Shadow 1 ILESTA-1D 12.5µm 12 beam 9beam(1.6kJ) TopB
10 4 Results 2 3torr Shadow X 1.2cm 3torr Shadow 2 1.0cm delay time cm/s delay time cm/s cm/s 3: 3torr 4: 5 Discussion 2: 3torr /delay time:40ns 5 25nsec 3 (cm) 3torr ( ) 4 3torr X 3torr 50nsec 0.7cm 1.0cm Contact Discontinuity Forward flow Shock Reverse Shock 3torr 2.5 Reverse Shock 10 7 cm/s Shadow Shock
11 5: 25nsec 1 6 (T) (cm/s) log-log 3 1 AlfvénMach 1 2 r g ( ) 1.2cm 3 λ ii (ion-ion ) 12cm cm/s 1T 6: 6 Conclusion TopB 25nsec 0.7cm Contact Discontinuity Forward Shock 1T 7 Acknowledgement
12 a3 CTA M1
13 CTA Abstract ( ) (Cherenkov Telescope Array, CTA) TeV 3 AGILE TeV CTA MAGIC H.E.S.S. 3 TeV 1000 CTA ev 20 MeV 300 GeV LAT 20 MeV 30 GeV EGRET GeV TeV (Very High Energy, VHE) VHE VHE (Imaging Atmospheric Cherenkov Telescope, IACT) ( 1) : ( :CTA-Japan 2014) MAGIC (17 m 2, ), VERITAS (12 m 4, ), H.E.S.S. (12 m m, ) VHE
14 π 0,π ± τ s 2 2 π 0 n c/n θ c ( c ) ( ) 1 θ c = arccos = arccos. (1) nv nβ v n 1 VHE θ c 1 10km 100m IACT 2: (Konrad Berenlöhr 1998) 2 3: (Heinrich J. Völk, Konrad Berenlöhr 2008) 1.2 IACT 1.3 IACT IACT ( 1)
15 4 4: (Heinrich J. Völk, Konrad Berenlöhr 2008) 2 CTA (CTA) CTA : CTA (CTA 2016) 3 CTA CTA 1 3 GeV (Extragalactic Background Light, EBL) TeV MST SST 1: CTA 3 (LST) 23m 20 GeV 1 TeV (MST) 12m 100 GeV 10 TeV (SST) 4.3m 1 TeV 100 TeV 4 IACT 6 IACT CTA 1 IACT 6 Morphology
16 CTA Reference CTA-Japan Consortium 2014, 6: (Heinrich J. Völk, Konrad Berenlöhr 2008) CTA 1000 CTA 2016, F.A. Aharonian, W. Hofmann, A.K. Konopelko, & H.J. Völk 1997, Astroparticle Physics, 6, 343 Heinrich J. Völk, Konrad Berenlöhr 2009, Experimental Astronomy, 25, 173, airxiv: [astro-ph] Konrad Berenlöhr 1998, CORSIKA and SIM TELARRAY A package for the simulation of the imaging atmospheric Cherenkov technique and an investigation of important environmental parameters for such simulations. 7: CTA (CTA-Japam 2014) Crab LST 2
17 a4 M1
18 Abstract ( ) 100 GeV 10 TeV (AGN) AGN ( ) ( ) AGN CTA 1 (E TeV) : TeV (TeVCat2 2016) 2 AGN
19 (Active Galactic Nuclei)( 2) BL Lac AGN 2: 1 AGN 3 AGN Γ=10 2 (TeV) ( ) γ + γ e + + e (1) ( 3) X (Extragalactic Background Light) AGN
20 3: BL Lac (F.Tavecchio et al. 1998) π TeV Mrk501 Mrk421 EBL EBL ( 4) 4: EBL (M.L.Ahnen et al. 2016) (Domingues et al. 2011) EBL Fermi, H.E.S.S., MAGIC TeV ev EBL 4 Fermi 1980 MAGIC( 5) H.E.S.S. VERITAS
21 EBL ( 7) : MAGIC 17 m 50 GeV 30 TeV 100 TeV 5 CTA Cherenkov Telescope Array AGN EBL CTA(Cherenkov Telescope Array) CTA 32 CTA 10 (10 14 ergcm 2 s 1 ) 3 (2 arcmin) (20 GeV) 10 (1-10 s) AGN ( 6) 2 6: PKS (H.Sol et al. 2013) H.E.S.S. CTA CTA Reference TeVCat2 tevcat2.uchicago.edu/ 2016 F.Tavecchio, L.Maraschi, & G.Chisellini ApJ. 509 (1998) 608 M.L.Ahnen et al. A&A. 590 (2016) A24 H.Sol et al. Aps. 43 (2013) 215
22 7: CTA Acknowledgement CTA- Japan Consortium
23 c1 M2
24 ( ) Abstract (Y.Zhang & A.Burrows 2013) CP 1 Introduction 2 Methods Maki et al (H 0 ) 2. (H e ) 3. (H νν ) MultiAngle- MultiEnergy F ρ ee ρ eµ ρ eτ F = ν ρ ν = ρ µe ρ µµ ρ µτ (1) ρ τe ρ τµ ρ ττ (ρ Wigner phase space density ) (P.Strack et al. 2005) - F t + v F r + p F p = i[h, F ] + C C SU(3) c αβγ λ γ f γ t + v f γ r + p f γ p = 2c αβγh α f β λ γ + C γ (2) f γ F (F = f γ λ γ )
25 3 Results v f γ r = 2c αβγh α f β λ γ (3) n e (H.Kikuchi & H.Suzuki 2012) 1 t = s, 6.26 s Survival Probability e e e e e e+05 r [km] 2: ν e t=0.127 s t=6.26 s Number Density [cm -3 ] 1e+38 1e+36 1e+34 1e+32 1e+30 1e+28 1e+26 1e e e e e e e+05 r [km] 1: t=0.127 s t=6.26 s 1 t = 6.26 s r = km s 6.26 s s 6.26 s 2 ν e 1 10MeV 2 t = s ν e ν µ, ν τ 6.26 s 4 Conclusion CP P (ν e ν e ) CP phase parameterδ (ν e ν µ ) 4% MultiAngle-MutiEnergy Collision term Reference Y.Zhang, & A.Burrows 2013, Phys. Rev. D 88, E.Wigner 1932, Phys. Rev. 40, 749 P.Strack, & A.Burrows 2005, Phys. Rev. D 71, H.Kikuchi, & H.Suzuki 2012, AIP Conf.Proc. 1484,397
26 c2 D2
27 ( ) Abstract, SNR Hα,,, SNR, SN1006, SNR, %, Cosmic-ray modified shock, ( ), (e.g, Helder et al. (2009); Morino et al. (2013, 2014)), T proper T down, η η = T proper T down T proper (1) RCW 86 SNR Hα 3 Hα 1871, 1196, 1325, km/s Rankine- Hugoniot T proper 6.8, 2.8, 3.4, kev 1 η 0.66, 0.18, 0.32 SNR Hα SNR 3 Hα 10 40% η ( ) 2 ρ < η < 2 ρ (2) ρ 0 ρ 0 Shimoda et al. (2015) ρ/ ρ 0
28 ρ/ ρ 0 = 0.3 SNR SN 1006 SNR SNR ρ/ ρ 0 = 0.1 SNR η Helder et al. (2013); Shimoda et al. (2015) Hα 4 2, Kolmogorov, ( ), (Inoue et al. (2009)) (Foward Shock) Inoue et al. (2013) 3 1: Hα z Hα 8, η Region V proper T proper T down η [10 8 cm s 1 ] [kev] [kev] 3 MHD Hα Inoue et al. (2013) MHD Inoue et al. (2013) Model 3 Kolmogorov P 1D (k) ρ k 2k 2 k 5/3 ρ/ ρ 0 = 0.1 ρ k, k, ρ 0 ρ = ( ρ 2 ρ 0) 2 Inoue et al. (2013) Section 2 Model 3 SN ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ±0.07 Mean/std. dev. 1.64/ / / /0.02 1: 1 Hα 8 Shimoda et al.
29 (2015) 1 1 T down 1 η > Reference Helder et al. 2009, Science 325, 719 Morino et al. 2014, A&A 557, A141 Morino et al. 2014, A&A 562, A141 Helder et al. 2013, MNRAS 435, 910 Shimoda et al. 2015, ApJ 803, 98 Inoue et al. 2009, ApJ 695, 825 Inoue et al. 2013, ApJL 772, L20 SNR ρ/ ρ 0 = % SN 1006 SNR ρ/ ρ 0 = % 2 Hα Acknowledgement Numerical com- putations were carried out on XC30 system at the Center for Computational Astrophysics (CfCA) of National Astronomical Observatory of Japan and K computer at the RIKEN Advanced Institute for Computational Science (No. hp120087). This work is supported by Grantin-aids from the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan, No. 15J08894 (J.S.), No (T. I.), No (Y. O.), and No. 15K05088 (R.Y.), No (A.B.). T. I. and R. Y. deeply appreciate Research Institute, Aoyama-Gakuin University for helping our research by the fund. R. Y. also thank ISSI (Bern) for support of the team Physics of the Injection of Particle Acceleration at Astrophysical, Heliospheric, and Laboratory Collisionless Shocks.
30 c3 M2
31 ( ) Abstract ( ) 0.1mm cm (UHECR) 1 Introduction 90 km 110 km 0.01 mm cm m e n E(t, x) = E 0 e i(ωt± ω 2 ω 2 p c x) (1) ω 2 p = 4πne2 m (2) X ω ω p ω > ω p k = ± ω 2 ω 2 p c (3)
32 (1) ω < ω p k = ±i ω 2 ωp 2 c (4) (1) e i(ωt kx) = e iωt e ikx (5) ω 2 ω = e iωt p 2 e± (6) c e x (5) e ω 2 ω 2 p c x x ω p u u c mẍ = ee 0 cos ωt (7) 2 Methods/Instruments and Observations HRO 53.75MHz HRO 2 51 MHz 2 3kHz d = ex (8) d = e2 E 0 m cos ωt (9) 1: 5σ
33 : 10 4 Discussion µm 1 : Results σ (0.03 s) 40 Hz : Conclusion 3: 3 ( )
34 CIB CIB 70 AGN TeV CIB 70 ( 10µm) µm 3 6 Reference RMG (CQ ) / ( ) 12 II / ( )
35 c4 M2
36 ( ) Abstract ev ejecta 1 Introduction 1 γ ( < ev ) (SNR) - M 3 1: (Gaisser 2006) 2:
37 2 Methods/Instruments and Observations XII ( 2) (TOP-B) X (ejecta) (1), (2), (3) 3 3 Setup Alfvén Mach M A 1 M A = v ej v A > 1 (1) v ej ejecta, v A Alfvén Mach - λ ii r g λ ii r g (2) 1.2 cm r g r g < 1.2 cm (3) 3: ILESTA1D ejecta ejecta E laser = 1 2 mv2 ej ejecta ILESTA1D XII
38 1: ILESTA1D laser energy 763 J/cm 2 (3 beam) 10 µm 1.3 ns g/cms cm/s 1527 J/cm 2 (6 beam) 10 µm 1.3 ns g/cms cm/s 2291 J/cm 2 (9 beam) 10 µm 1.3 ns g/cms cm/s 1527 J/cm µm 1.3 ns g/cms cm/s 2291 J/cm µm 1.3 ns g/cms cm/s 1527 J/cm 2 15 µm 1.3 ns g/cms cm/s 2291 J/cm 2 15 µm 1.3 ns g/cms cm/s um - ( ), µ m 3ns t=10 ns T 5 Torr ejecta ns 9 beam 10, 12.5, 15 µm 4 Results 9 H, 3.0 Torr, Target: Al, 12.5 µm ( 5, 6) 5 (0 50 ns) +x 5 ejecta cm/s ejecta 6 40 ns 532 nm cm/s 3 4T 4: ILESTA-1D (t=10 ns) : -, : - Target : Al, : 12.5 µm, (x= µm) :-x 5 Discussion ejecta ILESTA1D 5
39 1T 5: (39254) Al 12.5 µm/h 2 3Torr/ 7: 6 Conclusion 6: (39254) t = 40 ns Al 12.5 µm/h 2 3 Torr/ ejecta 1T ejecta ejecta 7 3 Reference Torr Thomas Gaisser, 2006, arxiv: v1 1T Hoshino & Shimada 2002, APJ, 572: cm/s Masahiro Hoshino,2001,Progress of Theoretical Physics
40 c5 Gravitational Leptogenesis M1
41 Gravitational Leptogenesis ( ) Abstract gravitational leptogenesis CP odd 1 Introduction WMAP η n B /n γ 10 9 (1) gravitational leptogenesis (S.H.S. Alexander et al. 2006) SM B L B L U(1) SM (M. Trodden 1999) µ j µ B = µj µ L ( ) g 2 (2) = n f 32π 2 W µν a W aµν g 2 32π 2 F µν µν F n f = 3 W F SU(2) L U(1) Y field strength W µν = 1 2 ϵµναβ W αβ (3) B L B L (V.A. Kuzmin et al. 1985) SM B L leptogenesis B L L B (M. Fukugita & T. Yanagida 1986) gravitational leptogenesis L 2 Review of Gravitational Leptogenesis SM a gravitational leptogenesis (S.H.S. Alexander et al. 2006) F B L 2 B L µ j µ L = N l r 16π 2 R R (4)
42 where j µ L = l iγ µ l i + ν i γ µ ν i, R R = 1 2 ϵαβγδ ρσ R αβρσ R γδ (5) N l r R R N l r SM 3 N l r = 3 4 µ GeV R R Pontryagin density Robertson-Walker 0 Sakharov CP CP L = F (ϕ)r R (6) ϕ CP odd F ϕ CMB (A.Lue et al. 1999) R R ds 2 = dt 2 + a 2 (t)[(1 h + )dx 2 (7) + (1 + h + )dy 2 + 2h dxdy + dz 2 ] a(t) = e Ht CP h L = (h + ih )/ 2, h R = (h + + ih )/ 2 (8) 7 6 h L = 2i Θ a ḣ L, h R = 2i Θ a ḣ R (9) where Θ = 8HF 2 ϕ/m P l (10) slow-roll F ϕ F = 0 Θ = 0 h L h R R R = 0 4 n n = 1 ( H 72π 4 M P l ) 2 ( ΘH 3 µ ) 6 (11) H cut off µ (H/M P l ) 2 Θ CP violation H 3 (µ/h) 6 leptogenesis n B /n = 4/11 s 7n B 1 n/s = ( n H s M P l ) 1/2 ( µ M P l ) 5 (12) H µ T r 1 TeV H/M P l < 10 4 H GeV < µ < GeV SUSYGUT 3 Conclusion leptogenesis GUT
43 Reference S.H.S. Alexander, M.E. Peskin, & M.M. Sheikh-Jabbari 2006, Phys. Rev. Lett. 96, M. Trodden 1999, Rev. Mod. Phys. 71, 1463 V.A. Kuzmin, V.A. Rubakov, & M.E. Shaposhnikov 1985, Phys. Lett. B155, 36 M. Fukugita, & T. Yanagida 1986, Phys. Lett. B174, 45 A. Lue, L.M. Wang, & M. Kamionkowski 1999, Phys. Rev. Lett. 83, 1506
44
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18 I ( ) (1) I-1,I-2,I-3 (2) (3) I-1 ( ) (100 ) θ ϕ θ ϕ m m l l θ ϕ θ ϕ 2 g (1) (2) 0 (3) θ ϕ (4) (3) θ(t) = A 1 cos(ω 1 t + α 1 ) + A 2 cos(ω 2 t + α
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ETL NEWS 1999.9 ETL NEWS 1999.11 Establishment of an Evaluation Technique for Laser Pulse Timing Fluctuations Optoelectronics Division Hidemi Tsuchida e-mail:tsuchida@etl.go.jp A new technique has been
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5 H Boltzmann Einstein Brown 5.1 Onsager [ ] Tr Tr Tr = dγ (5.1) A(p, q) Â = Tr Âe βĥ Tr e βĥ = dγ e βh (p,q) A(p, q) dγ e βh (p,q) (5.2) e βĥ A(p, q) p q Â(t) = Tr Â(t)e βĥ Tr e βĥ = dγ() e βĥ(p(),q())
Microsoft Word - 11問題表紙（選択）.docx
A B A.70g/cm 3 B.74g/cm 3 B C 70at% %A C B at% 80at% %B 350 C γ δ y=00 x-y ρ l S ρ C p k C p ρ C p T ρ l t l S S ξ S t = ( k T ) ξ ( ) S = ( k T) ( ) t y ξ S ξ / t S v T T / t = v T / y 00 x v S dy dx
meiji_resume_1.PDF
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X X 1 1 2 Free Electron Laser: FEL 2.1 2 2 3 SACLA 4 SACLA [1]-[6] [7] 1: S N λ [9] XFEL OHO 13 X [8] 2 2.1 2(a) (c) z y y (a) S N 90 λ u 4 [10, 11] Halbach (b) 2: (a) (b) (c) (c) 1 2 [11] B y = n=1 B
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String Gas Cosmology References Brandenberger & Vafa, Superstrings in the early universe, Nucl.Phys.B316(1988) 391. Tseytlin & Vafa, Elements of string cosmology, Nucl.Phys.B372 (1992) 443. Brandenberger,
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