Hiroshi Daisaka

Hitotsubashi University, Edo, Tōkyō, Japan

Are you Hiroshi Daisaka?

Claim your profile

Publications (32)33.5 Total impact

  • [Show abstract] [Hide abstract]
    ABSTRACT: We investigated whether outward Planetesimal Driven Migration (PDM) takes place or not in simulations when the self gravity of planetesimals is included. We performed $N$-body simulations of planetesimal disks with large width (0.7 - 4AU) which ranges over the ice line. The simulations consisted of two stages. The first stage simulations were carried out to see the runaway growth phase using the planetesimals of initially the same mass. The runaway growth took place both at the inner edge of the disk and at the region just outside the ice line. This result was utilized for the initial setup of the second stage simulations in which the runaway bodies just outside the ice line were replaced by the protoplanets with about the isolation mass. In the second stage simulations, the outward migration of the protoplanet was followed by the stopping of the migration due to the increase of the random velocity of the planetesimals. Due to this increase of random velocities, one of the PDM criteria derived in Minton and Levison (2014) was broken. In the current simulations, the effect of the gas disk is not considered. It is likely that the gas disk plays an important role in planetesimal driven migration, and we plan to study its effect in future papers.
    No preview · Article · Jan 2016
  • Source
    [Show abstract] [Hide abstract]
    ABSTRACT: There are scientific applications which require calculations with high precision such as Feynman loop integrals and orbital integrations. These calculations also need to be accelerated. We have been developing dedicated accelerator systems which consist of processing elements (PE) for high precision arithmetic operations and a programing interface. GRAPE9-MPX is our latest system with multiple Field Programmable Gate Array (FPGA) boards on which our developed PEs are implemented. We present the performance results for GRAPE9-MPX extended to have up to 16 FPGA boards for quadruple, hexuple, and octuple precision calculation. The achieved performance for a Feynman loop integral with 12 FPGA boards is 26.5 Gflops for quadruple precision, 13.2 Gflops for hexuple precision, and 6.36 Gflops for octuple precision. We show that our hardware implementation is 80 - 200 times faster than software implementations. We also give analysis of the performance results.
    Preview · Article · Dec 2015 · Procedia Computer Science
  • Source
    Yuki Yasui · Keiji Ohtsuki · Hiroshi Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: Using a local N-body simulation, we examine gravitational accretion of ring particles onto moonlet cores in Saturn's rings. We find that gravitational accretion of particles onto moonlet cores is unlikely to occur in the C ring and probably difficult in the inner B ring as well provided that the cores are rigid water ice. Dependence of particle accretion on ring thickness changes when the radial distance from the planet and/or the density of particles is varied: the former determines the size of the core's Hill radius relative to its physical size, while the latter changes the effect of self-gravity of accreted particles. We find that particle accretion onto high-latitude regions of the core surface can occur even if the rings' vertical thickness is much smaller than the core radius, although redistribution of particles onto the high-latitude regions would not be perfectly efficient in outer regions of the rings such as the outer A ring, where the size of the core's Hill sphere in the vertical direction is significantly larger than the core's physical radius. Our results suggest that large boulders recently inferred from observations of transparent holes in the C ring are not formed locally by gravitational accretion, while propeller moonlets in the A ring would be gravitational aggregates formed by particle accretion onto dense cores. Our results also imply that the main bodies of small satellites near the outer edge of Saturn's rings may have been formed in rather thin rings.
    Preview · Article · Dec 2014 · The Astrophysical Journal
  • Hiroshi Daisaka · Taiji Furusawa · Noriyuki Yanagawa
    [Show abstract] [Hide abstract]
    ABSTRACT: We analyse the effect of financial development and globalization (i.e. the reduction of trade costs) on income distribution when a financial institution is imperfect. Financial imperfection creates income inequality, by benefiting borrowers (entrepreneurs) and harming lenders through its effect of lowering the capital rental rate. We show that globalization changes income for both borrowers and lenders in the same direction. However, the poorer is the financial institution, the greater its effect for entrepreneurs and the smaller for lenders. We also examine the effect of financial development and globalization in an enriched model where individuals are different in their abilities as well as their capital endowments. We show that financial development mitigates capital misallocation while the reduction of trade costs will not improve efficiency.
    No preview · Article · Dec 2014 · Pacific Economic Review
  • Source
    [Show abstract] [Hide abstract]
    ABSTRACT: Higher order corrections in perturbative quantum field theory are required for precise theoretical analysis to investigate new physics beyond the Standard Model. This indicates that we need to evaluate Feynman loop diagram with multi-loop integral which may require multi-precision calculation. We developed a dedicated accelerator system for multi-precision calculation (GRAPE9-MPX). We present performance results of our system for the case of Feynman two-loop box and three-loop selfenergy diagrams with multi-precision.
    Full-text · Article · Oct 2014 · Journal of Physics Conference Series
  • Keiji Ohtsuki · Yuki Yasui · Hiroshi Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: We examine the gravitational capture probability of colliding particles in circumplanetary particle disks and accretion rates of small particles onto an embedded moonlet, using analytic calculation, three-body orbital integrations, and N-body simulations. Expanding our previous work, we take into account the Rayleigh distribution of particles' orbital eccentricities and inclinations in our analytic calculation and orbital integration and confirm agreement between them when the particle velocity dispersion is comparable to or larger than their mutual escape velocity and the ratio of the sum of the physical radii of colliding particles to their mutual Hill radius () is much smaller than unity. As shown by our previous work, the capture probability decreases significantly when the velocity dispersion is larger than the escape velocity and/or . Rough surfaces of particles can enhance the capture probability. We compare the results of three-body calculations with N-body simulations for accretion of small particles by an embedded moonlet and find agreement at the initial stage of accretion. However, when particles forming an aggregate on the moonlet surface nearly fill the Hill sphere, the aggregate reaches a quasi-steady state with a nearly constant number of particles covering the moonlet, and the accretion rate is significantly reduced compared to the three-body results.
    No preview · Article · Jun 2013 · The Astronomical Journal
  • Y. Yasui · K. Ohtsuki · H. Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: Using local N-body simulations, we investigate the process of accretion of small ring particles onto a larger moonlet in Saturn's rings.
    No preview · Article · Mar 2013
  • [Show abstract] [Hide abstract]
    ABSTRACT: We describe the design and performance of the GRAPE-MPs, a series of SIMD accelerator boards for quadruple/hexuple/octuple-precision arithmetic operations. Basic design of GRAPE-MPs is that it consists of a number of processing elements (PE) and memory components which handle data with quadruple/hexuple/octuple-precision. A GRAPE-MPs processor is implemented on a structured ASIC chip and an FPGA chip. GRAPE-MP (quadruple-precision) uses a structured ASIC chip from eASIC corp., which has 6 PE and operates with 100MHz clock cycle. The theoretical peak quadruple-precision performance of the single board is 1.2 Gflops and the achieved performance for the Feynman loop integrals is about 0.5 Gflops. GRAPE-MP4/6/8 (quadruple/hexuple/octuple-precision) uses an FPGA chip from Aletra corporation. For example, in the current implementation, MP8 has 10 PE with 70MHz operation clock cycle. We also present the performance results with the multiple GRAPE-MPs boards. The achieved performance of four MP8 boards is about 1.6 Gflops. It is roughly 90 times faster than the performance of a single core of a CPU with comparable precision. We show that our hardware based approach to evaluate the Feynman loop integrals in high precision arithmetic operations is highly effective.
    No preview · Conference Paper · Sep 2012
  • Source
    Keiji Ohtsuki · Hiroshi Daisaka · H. Tanaka
    [Show abstract] [Hide abstract]
    ABSTRACT: Viscosity in planetary rings arises from collisional and gravitational interactions between constituent particles. Angular momentum is transferred mainly through mutual collisions and gravitational encounters when the optical depth of the ring is low, while the formation of gravitational wakes significantly enhances the viscosity in dense rings (Daisaka, Tanaka, Ida 2001, Icarus 154, 296). On the basis of the formulation derived by Tanaka, Ohtsuki, and Daisaka (2003, Icarus 161, 144) and using analytic calculation, three-body orbital integration and N-body simulation, we investigate viscosity in self-gravitating planetary rings, both with and without the effect of particle spins. In the case of rings with low optical depth, we confirmed agreement between results of three-body calculation and N-body simulation. When the optical depth is low and the effect of particles' mutual gravity is weak, particles' surface friction with a reasonable range of a friction parameter tends to reduce their random velocity and, consequently, viscosity as well. However, in dense rings with gravitational wakes, the effect of self-gravity is dominant. We obtain ring viscosity for a wide range of parameter values, and derive an approximate expression which reproduces our numerical results. This work was supported by NASA's Outer Planets Research Program and the Cassini Project.
    Preview · Article · May 2012 · The Astronomical Journal
  • Y. Yasui · K. Ohtsuki · H. Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: Using local N-body simulation, we examine viscosity of planetary rings consisting of spinning, self-gravitating particles for a wide range of parameters, including the cases of dense rings with temporary aggregate formation.
    No preview · Article · Mar 2012
  • J. Makino · H. Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: In this paper, we describe the design and performance of GRAPE-8 accelerator processor for gravitational N-body simulations. It is designed to evaluate gravitational interaction with cutoff between particles. The cutoff function is useful for schemes like TreePM or Particle-Particle Particle-Tree, in which gravitational force is divided to short-range and longrange components. A single GRAPE-8 processor chip integrates 48 pipeline processors. The effective number of floating-point operations per interaction is around 40. Thus the peak performance of a single GRAPE-8 processor chip is 480 Gflops. A GRAPE-8 processor card houses two GRAPE-8 chips and one FPGA chip for PCI-Express interface. The total power consumption of the board is 46W. Thus, theoretical peak performance per watt is 20.5 Gflops/W. The effective performance of the total system, including the host computer, is around 5Gflops/W. This is more than a factor of two higher than the highest number in the current Green500 list.
    No preview · Conference Paper · Jan 2012
  • Source
    [Show abstract] [Hide abstract]
    ABSTRACT: We describe the implementation and performance of dense matrix multiplication and LU decomposition on the GRAPE-DR SIMD accelerator board. A GRAPE-DR card, with 4 GRAPE-DR chips, has the theoretical peak DP performance of 819 Gflops. Each GRAPE-DR chip has 512 processing elements and operates with 400MHz clock cycle. each PE can perform one addition and one multiplication in every two clock cycles. The measured performance of matrix multiplication is 730 Gflops for the multiplication of matrices with size 51200 by 2048 and 2048 by 51200. The performance of LU decomposition is 480 Gflops for the problem size of 51200.
    Preview · Article · Dec 2011 · Procedia Computer Science
  • Source
    [Show abstract] [Hide abstract]
    ABSTRACT: We describe the design and performance of the GRAPE-MP board, an SIMD accelerator board for quadrupleprecision arithmetic operations. A GRAPE-MP board houses one GRAPE-MP processor chip and an FPGA chip which handles the communication with the host computer. A GRAPE-MP chip has 6 processing elements (PE) and operates with 100MHz clock cycle. Each PE can perform one addition and one multiplication in every clock cycle. The architecture of the GRAPE-MP is similar to that of the GRAPE-DR. It is implemented using the structured ASIC chip from eASIC corp. A GRAPE-MP processor board has the theoretical peak quadruple-precision performance of 1.2 Gflops. As a preliminary result, we present the performance of the GRAPE-MP board for two target applications. The performance of the numerical integration of Feynman loop is 0.53 Gflops. The performance of a N-body simulation with the second order leapfrog schema is 0.505 Gflops for N = 1984, which is more than 10 times faster than the performance of the host computer.
    Full-text · Article · Dec 2011 · Procedia Computer Science
  • Source
    [Show abstract] [Hide abstract]
    ABSTRACT: Ultraluminous infrared galaxies (ULIRGs) with multiple (≥3) nuclei are frequently observed. It has been suggested that these nuclei are produced by multiple major mergers of galaxies. The expected rate of such mergers is, however, too low to reproduce the observed number of ULIRGs with multiple nuclei. We have performed high-resolution simulations of the merging of two gas-rich disk galaxies. We found that extremely massive and compact star clusters form from the strongly disturbed gas disks after the first or second encounter between the galaxies. The mass of such clusters reaches ~108M ☉ and their half-mass radii are 20-30 pc. Since these clusters consist of young stars, they appear as several bright cores in the galactic central region (~kpc). The peak luminosity of these clusters reaches ~10% of the total luminosity of the merging galaxy. These massive and compact clusters are consistent with the characteristics of the observed multiple nuclei in ULIRGs. Multiple mergers are not necessary to explain multiple nuclei in ULIRGs.
    Full-text · Article · Nov 2011 · The Astrophysical Journal
  • Source
    Y. Yasui · K. Ohtsuki · H. Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: Saturn's rings are composed of many icy particles, and angular momentum is transported due to collision and gravitational interaction between these particles. Viscosity in the rings arising from such interactions between particles governs the rate of dynamical evolution and structure formation in the rings. We examine the effect of surface friction on the viscosity and the dependence of the viscosity on optical depth and distance from Saturn, using local N-body simulation. We derive semi-analytic formula that approximately reproduces our numerical results.
    Preview · Article · Oct 2011
  • Source
    Hiroshi Daisaka · Taiji Furusawa
    [Show abstract] [Hide abstract]
    ABSTRACT: To investigate dynamic paths of network formation of free trade agreements (FTAs), we conduct simulations of Goyal and Joshi's (2006) model of FTA network formation game with many countries. We compare the results between two protocols regarding the choice of the pair that decides if they form (or sever) an FTA link in each round in the network evolution. The first protocol is the random protocol in which a pair of countries is randomly chosen in each period. The other protocol is the maximum protocol in which the country that has the largest incentive can propose to form or sever an FTA link. We find that with the random protocol, FTA evolution processes reach the complete FTA network in some cases but its likelihood becomes smaller if the number of countries grows. With the maximum protocol, the network evolution always ends with a unique final FTA network for each case of n ∈ {3, 4, · · · , 100} countries. The final FTA network may or may not be the complete network.
    Preview · Article · Jul 2011 · Review of International Economics
  • Y. Yasui · K. Ohtsuki · H. Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: Using local N-body simulation for planetary rings consisting of self-gravitating particles with surface friction, we examine the dependence of viscosity on various parameters such as optical depth and normal and tangential restitution coefficients.
    No preview · Article · Mar 2011
  • Source
    Junko K. Daisaka · Junichiro Makino · Hiroshi Daisaka
    [Show abstract] [Hide abstract]
    ABSTRACT: As of April 2010, 48 TNO (trans-Neptunian Object) binaries have been found. This is about 6% of known TNOs. However, in previous theoretical studies of planetary formation in the TNO region, the effect of binary formation has been neglected. TNO binaries can be formed through a variety of mechanisms, such as a three-body process, dynamical friction on two massive bodies, inelastic collisions between two bodies etc. Most of these mechanisms become more effective as the distance from the Sun increases. In this paper, we describe our study on three-body process using direct $N$-body simulations. We found that chaos-assisted-capture (CAC) is the dominant channel of binary formation. We systematically changed the distance from the Sun, the number density of planetesimals, and the radius of the planetesimals and studied the effect of the binaries on the collision rate of planetesimals. In the TNO region, binaries are involved in 1$/$3–1$/$2 of collisions, and the collision rate increases by a factor of a few compared to the theoretical estimate for direct two-body collisions. Thus, it is possible that the binaries significantly enhance the collision rate and reduce the growth timescale. In the terrestrial planet region, binaries are less important, because the ratio between the Hill radius and the physical size of the planetesimals is relatively small. Although the time scale of our simulations is short, they clearly demonstrated that the accretion process in the TNO region is quite different from that in the terrestrial planet region.
    Preview · Article · Feb 2011 · Publications- Astronomical Society of Japan
  • Source
    [Show abstract] [Hide abstract]
    ABSTRACT: We studied the formation process of star clusters using high-resolution N-body/smoothed particle hydrodynamcs simulations of colliding galaxies. The total number of particles is 1.2x10^8 for our high resolution run. The gravitational softening is 5 pc and we allow gas to cool down to \sim 10 K. During the first encounter of the collision, a giant filament consists of cold and dense gas found between the progenitors by shock compression. A vigorous starburst took place in the filament, resulting in the formation of star clusters. The mass of these star clusters ranges from 10^{5-8} Msun. These star clusters formed hierarchically: at first small star clusters formed, and then they merged via gravity, resulting in larger star clusters.
    Full-text · Article · Jan 2011 · Proceedings of the International Astronomical Union
  • [Show abstract] [Hide abstract]
    ABSTRACT: We performed high resolution simulations of galaxy-galaxy merging in order to investigate the mechanism of a starburst. The multiphase nature of the interstellar medium is correctly taken into account in our model, which allows the use of a realistic star formation model. In these simulations, we for the first time found that the shock-induced starburst involving star cluster (SC) formation takes place during the first encounter. Detailed analyses show that the SC formation is mainly driven by hierarchical mergings of proto (smaller) SCs. Our result implies that SCs can become much more massive than the local Jeans mass of the SC forming region.
    No preview · Article · Jun 2010

Publication Stats

248 Citations
33.50 Total Impact Points

Institutions

  • 2008-2014
    • Hitotsubashi University
      Edo, Tōkyō, Japan
  • 2007
    • National Astronomical Observatory of Japan
      Edo, Tokyo, Japan
  • 2001-2003
    • The University of Tokyo
      • Department of Astronomy
      白山, Tōkyō, Japan
  • 1999
    • Tokyo Institute of Technology
      • Earth and Planetary Sciences Department
      Edo, Tōkyō, Japan