Proceedings of International Conference on Physics in ... - KEK

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demonstration encourages four-beams full operation for the plasma heating. GEKKO-EXA LASER The “Gekko-EXA” laser is our great challenge for the next generation <strong>of</strong> the high field science, the energetic beam generation and their applications, and is under conceptual design. The “Gekko-EXA” has two kinds <strong>of</strong> operation mode, 1 PW at 100 Hz with a single beam and 0.2 EW as a single shot laser with two bundle beams, respectively, shown in fig. 6. These output power is ultrashort high-peak power laser with pulse duration <strong>of</strong> 10 fs. An effective laser gain over the extremely wide spectral width up to 500 nm is required for such short pulse amplification. The laser system is, therefore, based on the large-aperture optical parametric chirped-pulse amplification (LA-OPCPA). In the front end, the femto-second oscillator supplies seed pulses for both the pump laser and the white light generation in the LA-OPCPA. Because a temporal jitter between the pump beam and the seed pulse should be reduced as possible. The oscillator generates few cycle pulses with the considerably broad spectral width. A seed pulse for the pump laser is temporally stretched and amplified by using fibre amplifiers after a pulse picker and a pulse shaper. A part <strong>of</strong> the amplified pulse is used as a seed pulse <strong>of</strong> a repeatable amplification system, which based on highpower diode-pumped solid-state lasers (DPSSL) with cryogenic Yb:YAG ceramics[3] as a laser material. The repeatable pump source generates green laser pulses with 70 J pulse energy at 100 Hz repetition rate after second harmonic generation. The other part <strong>of</strong> the amplified pulse is divided into four beams and each <strong>of</strong> them seeded into the single-shot-based Nd:glass amplifier system. Pulse energy increases up to 3 kJ per beam. A bundle <strong>of</strong> four beams supplies 12 kJ (ω) in 1 ns and is frequencydoubled at 8.4 kJ. Two bundles are prepared as pump sources. On the other hand, the generated white coherent light is used as a seed pulse for the OPCPA system. Several hundreds mili-joules pulse energy is obtained after fibre and small-power (SP-) OPCPA stages. Then, in the LA- OPCPA with partially deuterated DKDP crystals, kilojoule class pulse energy is obtained with a more than 200 nm spectral width (FWHM). Using high-damagethreshold gratings and chirped mirrors in large aperture, 0.1 EW (1 kJ/ 10 fs) pulse beam is generated and two set <strong>of</strong> the pump beam and the seed pulse results in 0.2 EW. There are some key issues in “Gekko-EXA” laser design. Spectral dispersion compensation is considerably important to improve the temporal pulse contrast ratio up to 10 12 to reduce pre-pulses and a pedestal. Technologically, there are two significant optics to be developed, a grating and a large aperture chirped mirror, which have both high optical damage strength in J/cm 2 in an ultra-broadband up to 500 nm with a large aperture. Figure 7 shows an arrangement plan for the “Gekko- EXA” laser. The front end and the 1 PW/ 100 Hz laser system are in another room, which is not shown here. The kJ-pump-laser is at the next to the “Gekko” laser system. In the additional planed building, the booster amplifiers for 12 kJ, the second harmonic generator and the kJ-class OPCPA system are on the same floor. Two pulse compressors are in front <strong>of</strong> the target chamber. REFERENCE [1] G. M. Heestand, C. A. Haynam, P. J. Wegner, M. W. Bowers, S. N. Dixit, G. V. Erbert, M. A. Henesian, M. R. Hermann, K. S. Jancaitis, K. Knittel, T. Kohut, J. D. Lindl, K. R. Manes, C. D. Marshall, N. C. Mehta, J. Menapace, E. Moses, J. R. Murray, M. C. Nostrand, C. D. Orth, R. Patterson, R. A. Sacks, R. Saunders, M. J. Shaw, M. Spaeth, S. B. Sutton, W. H. Williams, C. C. Widmayer, R. K. White, P. K. Whitman, S. T. Yang, and B. M. Van Wonterghem, “Demonstration <strong>of</strong> highenergy 2ω (526.5 nm) operation on the National Ignition Facility Laser System,” Applied Optics, Vol. 47 Issue 19, pp.3494-3499 (2008). [2] N. Miyanaga, H. Azechi, K. A. Tanaka, T. Kanabe, T. Jitsuno, J. Kawanaka, Y. Fujimoto, R. Kodama, H. Shiraga, K. Knodo, K. Tsubakimoto, H. Habara, K. Sueda, H. Murakami, N. Morio, S. Matsuo, N. Sarukura, Y. Izawa, and K. Mima, “Technological Challenge and Activation <strong>of</strong> 10-kJ PW Laser LFEX for Fast Ignition at ILE,” Frontiers in Optics (FiO) 2008 paper: FWQ1. [3] J. Kawanaka, Y. Takeuchi, A. Yoshida, S. J. Pearce, R. Yasuhara, T. Kawashima, and H. Kan, “Highly Efficient Cryogenically_Cooled Yb:YAG Laser”, Laser Physics vol. 20, No. 1079-1084 (2010).
Abstract X-ray Emission from Magnetars and Its Physical Interpretation T. Enoto ∗ , KIPAC, Stanford University, CA, 94305-4085, USA † K. Makishima, Dep. <strong>of</strong> Physics, The University <strong>of</strong> Tokyo ‡ , and Suzaku Magnetar Team Recent astronomy has been accumulating evidence that a subset <strong>of</strong> neutron stars has an ultra strong magnetic filed, ∼ 10 10−11 T. These enigmatic sources are called magnetars, and their field is believed to be stronger than those (∼ 10 8 T) <strong>of</strong> normal pulsars by 2–3 orders <strong>of</strong> magnitudes. Since such a field exceeds the QED critical field, 4.4 × 10 9 T, magnetars are a promising laboratory in the universe for the high-field physics. Using the Japanese astrophysical satellite Suzaku, we performed X-ray observations <strong>of</strong> ∼9 magnetars. We found a systematic trend <strong>of</strong> the wide-band X-ray spectra, which is considered to be related with the strong field physics (e.g., photon splitting). MAGNETIC FIELD OF NEUTRON STARS Celestial objects, especially compact objects such as black holes and neutron stars (NSs), are ideal laboratories to examine the extreme physics, which cannot be attained through the ground experiments. For example, astronomical observations have been revealed that NSs exhibit a strong magnetic field (B ∼ 10 8 T), an intense photon field (its maximum luminosity at L ∼ 10 38 erg s −1 ), and a high gravity field (its gravitational redshift at z ∼ 0.2). Thanks to recent sensitive detectors, we acquired an observational approach to study these exotic physics. Figure 1: An X-ray image <strong>of</strong> the Crab Nebula obtained by the Chandra observatory [1]. The Crab pulsar locates at the center <strong>of</strong> the Nebula. NSs are born after a gravitational collapse <strong>of</strong> a massive star. Since their mass and radii are estimated to be M ∼ 1.4 − 2.1M⊙ and R ∼ 10 km, this compact star is ∗ JSPS (Japan Society for the Promotion <strong>of</strong> Science) Fellow, e-mail: enoto@stanford.edu † Address: Stanford University, Kavli Institute for Particle Astrophysics & Cosmology, Physics Astrophysics Building, 452 Lomita Mall, MC 4085, Stanford, CA 94305-4085, USA ‡ Address: Department <strong>of</strong> Physics,School <strong>of</strong> Science, The University <strong>of</strong> Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan believed to be supported by a degeneracy pressure <strong>of</strong> neutrons. Electromagnetic waves from NSs have been detected by various wavelengths with their stellar rotations. Therefore, most NSs are called “pulsars”. For example, Figure 1 shows an X-ray image <strong>of</strong> the Crab Nebula, which was formed at a historically recorded supernova in 1054. At the center <strong>of</strong> this nebula, the Crab pulsar is rotating at its period <strong>of</strong> P ∼ 33 ms and its period derivative <strong>of</strong> ˙ P ∼ 4.2×10−13 s s−1 . So far, pulsations and their derivatives have been measured from more than 1500 normal NSs, which are plotted on the P - ˙ P diagram in Figure 2, mainly distributed around P ∼ 0.4 s and ˙ P ∼ 10−15 s s−1 . Since most <strong>of</strong> normal pulsars exhibit a long-term timing stability, they are though to be isolated NSs1 Pdot (s/s) 10 −8 10 −9 10 −10 10 −11 10 −12 10 −13 10 −14 10 −15 10 −16 10 −17 10 −18 10 −19 10 −20 10 −21 10 13 G 10 12 G 10 11 G 10 10 G 10 9 G 10 14 G Bcr 10 15 G 10−3 10 0.01 0.1 1 10 −22 Period (s) Figure 2: (a) A P - ˙ P diagram <strong>of</strong> pulsars, including rotation-powered pulsars (black), SGRs (red stars), and AXPs (blue circles) after [2], http://www.atnf.csiro. au/research/pulsar/psrcat/. Dotted lines <strong>of</strong> negative slopes represent constant magnetic field grids. Following a standard pulsar model [3], emission from normal isolated NSs can be powered by their rotational energy loss. Let us assume the loss <strong>of</strong> the rotation energy, d/dt(0.5IP 2 ) is eventually converted into a magnetic dipole radiation (e.g., electromagnetic wave), where I = 10 45 g cm 2 is a momentum <strong>of</strong> inertia <strong>of</strong> the NS. Then, 1 “Isolated” means that the NS is not a binary system (accretionpowered pulsars), where mass accretion from a companion star make the pulsation fluctuate.
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Proceedings <stron
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Conference poster
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Preface The international conferenc
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Recent progress of
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Figure 1: The Pulse Intensity-Durat
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Figure 3: The attosecond metrology
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THE QED EFFECTIVE ACTION In quantum
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Figure 2: Turning points in the com
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[5] A. Ringwald, “Pair production
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QED IN ULTRA-INTENSE LASER FIELDS
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form e + nγL → e ′ + γ where
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ection(s) associated with the exter
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This is listed in Tab.1. The effect
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the spectrum of ph
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pf f f pi p x2 x1 k ki p pi Figure
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STRONG FIELD DYNAMICS IN HEAVY-ION
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Possible effects of</strong
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Figure 3: Flux tube structure <stro
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Abstract Yoctosecond photon pulse g
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emsstrahlung or inelastic pair anni
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Abstract Fields, Instantons, and Cu
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the dispersion relation p0 = Ep −
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CRITICAL BEHAVIOR OF CHARMONIUM: QC
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different masses m 0 i ̸= mi only
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ON THE UNRUH EFFECT ∗ Ralf Schüt
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Abstract Can we detect ”Unruh rad
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Equipartition Theorem The stochasti
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Abstract Quantum fields and static
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The relation between acceleration a
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= γ WISP ; ; ALP HP(mγ ′ > 0) .
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Figure 4: Exclusion limit (95% C.L.
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Probing extremely light fields via
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Figure 1: Second harmonic generatio
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Abstract Dynamical view of<
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(a) longitudinal momentum distribut
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Exact solutions of
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Pair production in heat bath Finall
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Table 1: Related ideas in strong fi
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Abstract Non-linear charge transpor
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under the assumption of</st
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Brilliant hardγ-production ande +
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each other. Thus the E field rotate
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ACKNOWLEDGMENTS This work is based
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ϵ is the energy of</strong
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of the sampling eq
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Abstract SCHWINGER LIMIT ATTAINABIL
Page 100 and 101: To find it we use the integral calc
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Page 104 and 105: A way to quantify the irreversible
Page 106 and 107: Figure 4: Pair production vs time f
Page 108 and 109: of the quantum flu
Page 110 and 111: Phenomena H. Schwarz and H. Hora Ed
Page 112 and 113: In USA, LLNL has a user’s facilit
Page 114 and 115: field triggering such phenomena is
Page 116 and 117: QGP is studied by using the particl
Page 118 and 119: Fig. (1): Presentation of</
Page 120 and 121: REFERENCES [1] P.A. Franken, A.E. H
Page 122 and 123: of electron. When
Page 124 and 125: splitting, no one has succeeded to
Page 126 and 127: Abstract WIDE-BAND X-RAY OBSERVATIO
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Page 136 and 137: egime. As analogous to a convention
Page 138 and 139: With extremely high-peak power lase
Page 140 and 141: Abstract Flying Mirror as a tool to
Page 142 and 143: Reflected light intensity (μJ/sr/n
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Page 147 and 148: CURRENT STATUS OF LFEX LASER AND EX
Page 149: which were comparable to those befo
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Page 155 and 156: 1 0.8 0.6 0.4 0.2 B 2 z E 2 T 0.5 1
Page 157 and 158: First order quantum correction to t
Page 159 and 160: dE (1) dt = ¯he4 m 2 12πɛ0p 5 i
Page 161 and 162: Next, let us consider the origin <s
Page 163 and 164: Abstract NONCANONICAL LIE PERTURBAT
Page 165 and 166: with C (2) µ = Γ (2) µ − ˆ L
Page 167 and 168: log N (PIC particle) When the condi
Page 169: Abstract X-RAY GENERATION VIA LASER
Page 173 and 174: The electron beam is bent to the du
Page 175 and 176: INVESTIGATING THE ONE-PHOTON ANNIHI
Page 177: As a representative characteristics
Page 182 and 183: the interference terms ⟨ϕIϕh⟩
Page 184 and 185: P r o g r a m of P
Page 186 and 187: 11:55 lunch & group photo [85] [Rec
Page 188: List of Participan
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