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Papers by Takuya Matsuda

Research paper thumbnail of Hydrodynamic Calculations of Spherical Gravitational Collapse in the Scalar-Tensor Theory of Gravity

Progress of Theoretical and Experimental Physics, Apr 1, 1973

Research paper thumbnail of Gas flow in close binary star systems

arXiv (Cornell University), Feb 6, 2004

Research paper thumbnail of Numerical Simulation of the Surface Flow on the Companion Star in a Close Binary System II. Construction of Doppler maps and application to Galactic supersoft X-ray sources

arXiv (Cornell University), Feb 10, 2004

Research paper thumbnail of Application of the DSMC method to astrophysical flows

arXiv (Cornell University), Oct 9, 2001

Research paper thumbnail of Direct Monte Carlo simulations of accretion discs

arXiv (Cornell University), Oct 9, 2001

Research paper thumbnail of Bondi–Hoyle–Lyttleton accretion flow revisited: Analytic solution

Progress of theoretical and experimental physics, Nov 1, 2015

Research paper thumbnail of Numerical Computation of Two Dimensional Wind Accretion of Isothermal Gas

arXiv (Cornell University), May 28, 1998

Research paper thumbnail of 3D Finite Volume Simulation of Accretion Discs with Spiral Shocks

Astrophysics and space science library, 1999

Research paper thumbnail of Evolution of Galaxies and Secular Variation of Cosmic Rays, Magnetic Fields and Turbulence

Progress of Theoretical and Experimental Physics, Jun 1, 1970

Research paper thumbnail of Resonance between Primordial Gravitational Waves and Gravitationally Bound Systems

Progress of Theoretical and Experimental Physics, 1979

Research paper thumbnail of Numerical Simulation of the Interaction between an L1 Stream and an Accretion Disk in a Close Binary System

Progress of Theoretical and Experimental Physics, Oct 1, 2001

Research paper thumbnail of Towards steady-state solutions for supersonic wind accretion on to gravitating objects

Monthly Notices of the Royal Astronomical Society, Mar 1, 2000

Research paper thumbnail of Spiral shocks and accretion in discs

Monthly Notices of the Royal Astronomical Society, Dec 1, 1987

Research paper thumbnail of Spin-up and spin-down of an accreting compact object

Monthly Notices of the Royal Astronomical Society, Jun 1, 1987

Research paper thumbnail of Bondi–Hoyle–Lyttleton accretion flow revisited: Analytic solution

Progress of Theoretical and Experimental Physics, 2015

The time-steady equation for a 1D wind accretion flow, i.e. the Bondi-Hoyle-Lyttleton (BHL) equat... more The time-steady equation for a 1D wind accretion flow, i.e. the Bondi-Hoyle-Lyttleton (BHL) equation, is investigated analytically. The BHL equation is well known to have infinitely many solutions. Traditionally, the accretion radius has been assumed to be 2GM/v 2 ∞ , but its mathematical foundation has not been clarified because of the non-uniqueness of the solution. Here, we assume that the solution curves possess physically nice characteristics, i.e. velocity and line mass-density increase monotonically with radial distance. This condition restricts the accretion radius to the range (0.71 − 1.0) × 2GM/v 2 ∞. Further assumptions, specifically, that the solution curves for velocity and line mass-density are convex upward, restrict the accretion radius to (0.84 − 0.94) × 2GM/v 2 ∞ , and 0.90 × 2GM/v 2 ∞ , respectively. Therefore, we conclude that the accretion radius is almost uniquely determined to be 0.90 × 2GM/v 2 ∞ .

Research paper thumbnail of Drag on a gravitating sphere moving through a gas

On essaie de determiner dans quelle mesure la trainee sur un corps depend de la force gravitation... more On essaie de determiner dans quelle mesure la trainee sur un corps depend de la force gravitationnelle, afin d'evaluer l'echelle de temps correcte de la croissance des planetes

Research paper thumbnail of Application of DSMC method to astrophysical flows

Symposium - International Astronomical Union

The Direct Simulation Monte Carlo (DSMC) method, developed originally to calculate rarefied gas d... more The Direct Simulation Monte Carlo (DSMC) method, developed originally to calculate rarefied gas dynamical problems, is applied to continuous flow including shocks assuming that the Knudsen number is sufficiently small. In particular, we study the formation of spiral shocks in the accretion disc of a close binary system. The method involves viscosity and thermal conduction automatically, and can thus simulate turbulent viscosity.

Research paper thumbnail of The rocket effect on a gravitating mass-losing object

Monthly Notices of the Royal Astronomical Society

Research paper thumbnail of Spiral shocks and accretion in discs

Monthly Notices of the Royal Astronomical Society

Research paper thumbnail of Mass and angular momentum loss from contact binary systems

Monthly Notices of the Royal Astronomical Society

Research paper thumbnail of Hydrodynamic Calculations of Spherical Gravitational Collapse in the Scalar-Tensor Theory of Gravity

Progress of Theoretical and Experimental Physics, Apr 1, 1973

Research paper thumbnail of Gas flow in close binary star systems

arXiv (Cornell University), Feb 6, 2004

Research paper thumbnail of Numerical Simulation of the Surface Flow on the Companion Star in a Close Binary System II. Construction of Doppler maps and application to Galactic supersoft X-ray sources

arXiv (Cornell University), Feb 10, 2004

Research paper thumbnail of Application of the DSMC method to astrophysical flows

arXiv (Cornell University), Oct 9, 2001

Research paper thumbnail of Direct Monte Carlo simulations of accretion discs

arXiv (Cornell University), Oct 9, 2001

Research paper thumbnail of Bondi–Hoyle–Lyttleton accretion flow revisited: Analytic solution

Progress of theoretical and experimental physics, Nov 1, 2015

Research paper thumbnail of Numerical Computation of Two Dimensional Wind Accretion of Isothermal Gas

arXiv (Cornell University), May 28, 1998

Research paper thumbnail of 3D Finite Volume Simulation of Accretion Discs with Spiral Shocks

Astrophysics and space science library, 1999

Research paper thumbnail of Evolution of Galaxies and Secular Variation of Cosmic Rays, Magnetic Fields and Turbulence

Progress of Theoretical and Experimental Physics, Jun 1, 1970

Research paper thumbnail of Resonance between Primordial Gravitational Waves and Gravitationally Bound Systems

Progress of Theoretical and Experimental Physics, 1979

Research paper thumbnail of Numerical Simulation of the Interaction between an L1 Stream and an Accretion Disk in a Close Binary System

Progress of Theoretical and Experimental Physics, Oct 1, 2001

Research paper thumbnail of Towards steady-state solutions for supersonic wind accretion on to gravitating objects

Monthly Notices of the Royal Astronomical Society, Mar 1, 2000

Research paper thumbnail of Spiral shocks and accretion in discs

Monthly Notices of the Royal Astronomical Society, Dec 1, 1987

Research paper thumbnail of Spin-up and spin-down of an accreting compact object

Monthly Notices of the Royal Astronomical Society, Jun 1, 1987

Research paper thumbnail of Bondi–Hoyle–Lyttleton accretion flow revisited: Analytic solution

Progress of Theoretical and Experimental Physics, 2015

The time-steady equation for a 1D wind accretion flow, i.e. the Bondi-Hoyle-Lyttleton (BHL) equat... more The time-steady equation for a 1D wind accretion flow, i.e. the Bondi-Hoyle-Lyttleton (BHL) equation, is investigated analytically. The BHL equation is well known to have infinitely many solutions. Traditionally, the accretion radius has been assumed to be 2GM/v 2 ∞ , but its mathematical foundation has not been clarified because of the non-uniqueness of the solution. Here, we assume that the solution curves possess physically nice characteristics, i.e. velocity and line mass-density increase monotonically with radial distance. This condition restricts the accretion radius to the range (0.71 − 1.0) × 2GM/v 2 ∞. Further assumptions, specifically, that the solution curves for velocity and line mass-density are convex upward, restrict the accretion radius to (0.84 − 0.94) × 2GM/v 2 ∞ , and 0.90 × 2GM/v 2 ∞ , respectively. Therefore, we conclude that the accretion radius is almost uniquely determined to be 0.90 × 2GM/v 2 ∞ .

Research paper thumbnail of Drag on a gravitating sphere moving through a gas

On essaie de determiner dans quelle mesure la trainee sur un corps depend de la force gravitation... more On essaie de determiner dans quelle mesure la trainee sur un corps depend de la force gravitationnelle, afin d'evaluer l'echelle de temps correcte de la croissance des planetes

Research paper thumbnail of Application of DSMC method to astrophysical flows

Symposium - International Astronomical Union

The Direct Simulation Monte Carlo (DSMC) method, developed originally to calculate rarefied gas d... more The Direct Simulation Monte Carlo (DSMC) method, developed originally to calculate rarefied gas dynamical problems, is applied to continuous flow including shocks assuming that the Knudsen number is sufficiently small. In particular, we study the formation of spiral shocks in the accretion disc of a close binary system. The method involves viscosity and thermal conduction automatically, and can thus simulate turbulent viscosity.

Research paper thumbnail of The rocket effect on a gravitating mass-losing object

Monthly Notices of the Royal Astronomical Society

Research paper thumbnail of Spiral shocks and accretion in discs

Monthly Notices of the Royal Astronomical Society

Research paper thumbnail of Mass and angular momentum loss from contact binary systems

Monthly Notices of the Royal Astronomical Society

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