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高能天文物理

The image shows the density distribution of a hypernova. An energetic explosion driven by both jets and disk winds leads to a large scale asymmetry in SN ejecta.
Hypernovae and GRB
Very Large Array radio image of a single millisecond duration burst known as FRB 121102 (a,b). This is the first localization of an FRB, conclusively showing an extragalactic origin. The dispersed pulse is shown in part c.
Localization of a Fast Radio Burst
AMR is used to resolve the finest structures in a hydro simulations.
CASTRO AMR
The 3D CASTRO simulation shows that many fluid instabilities occur during a PSN explosion.
3D pair-instability supernova model
The image shows the density structure of colliding shells ejected by a massive star before it dies. Such collisions can easily convert the kinetic energy of ejecta into thermal radiation.
3D radiation hydrodynamical simulation of Colliding Shells
This image is a slice through the interior of a supermassive star of 55,500 solar masses along the axis of symmetry. It shows the inner helium core in which nuclear burning is converting helium to oxygen, powering various fluid instabilities (swirling lines). This snapshot shows a moment one day after the onset of the explosion, when the radius of the outer circle would be slightly larger than that of the orbit of the Earth around the sun.
An exploding supermassive star
Astrophysicist Ken Chen ran simulations on supercomputers to better understand the physical conditions that create superluminious supernova.
Magnetar-powered Superluminous Supernovae
Distribution of the bulk velocity relative to the speed of light is shown as a function of the de-projected distance (normalized by r_s) from the core of the relativistic jet from M87. The dashed line represents the velocity scaling based on the conservation of energy flux density of the torsional Alfven waves under the WKB approximation, and the solid line denotes the escape speed along the jet parabolic streamline
Distribution of the bulk velocity relative to the speed of light
Distribution of the bulk velocity relative to the speed of light is shown as a function of the de-projected distance (normalized by r_s) from the core of the relativistic jet from M87. The dashed line represents the velocity scaling based on the conservation of energy flux density of the torsional Alfven waves under the WKB approximation, and the solid line denotes the escape speed along the jet parabolic streamline
Distribution of the bulk velocity relative to the speed of light
VLBA total intensity map of the M87 jet at 43 GHz (2-a), showing the synchrotron radiation of relativistic electrons. A hollow, edge-brightened emission of the jet up to ~ 500 r_s is clearly seen. A small circle indicates the size of the black hole shadow, which the GLT project is seeking to resolve with future sub-mm VLBI observations.
VLBA total intensity map of the M87 jet at 43 GHz (2-a)
VLBA total intensity map of the M87 jet at 43 GHz (2-a), showing the synchrotron radiation of relativistic electrons. A hollow, edge-brightened emission of the jet up to ~ 500 r_s is clearly seen. A small circle indicates the size of the black hole shadow, which the GLT project is seeking to resolve with future sub-mm VLBI observations.
VLBA total intensity map of the M87 jet at 43 GHz (2-a)
Accretion geometry of disks for LLAGN corresponding to low rate of mass accretion.
Accretion geometry of disks for LLAGN
Accretion geometry of disks for LLAGN corresponding to low rate of mass accretion.
Accretion geometry of disks for LLAGN
Accretion geometry of disks for high luminosity AGN corresponding to high rates of mass accretion.
Accretion geometry of disks for high luminosity AGN
Luminosity evolution of pulsar outer magnetospheric accelerators as a function of neutron star spin down luminosity. Two extreme chemical compositions of the neutron star envelopes are considered. The red curves correspond to a heavy element envelope, while the blue and black curves correspond to a light element envelope. The solid, dash-dotted, and dash-dot-dot-dot curves represent numerical solutions, while dashed and dotted ones represent analytical solutions. The circles, squares, and triangles designate the pulsars detected by the Fermi satellite: the green filled circles show the radio loud gamma-ray pulsars, while the blue filled squares show the radio quiet ones. From Hirotani 2013, ApJ, 766, 98.
Luminosity evolution of pulsar outer magnetospheric accelerators as a function of neutron star spin down luminosity.
Luminosity evolution of pulsar outer magnetospheric accelerators as a function of neutron star spin down luminosity. Two extreme chemical compositions of the neutron star envelopes are considered. The red curves correspond to a heavy element envelope, while the blue and black curves correspond to a light element envelope. The solid, dash-dotted, and dash-dot-dot-dot curves represent numerical solutions, while dashed and dotted ones represent analytical solutions. The circles, squares, and triangles designate the pulsars detected by the Fermi satellite: the green filled circles show the radio loud gamma-ray pulsars, while the blue filled squares show the radio quiet ones. From Hirotani 2013, ApJ, 766, 98.
Luminosity evolution of pulsar outer magnetospheric accelerators as a function of neutron star spin down luminosity.
Schematic picture (side view) of a pulsar magnetosphere. The filled circle on the left denotes the neutron star, which rotates along the vertical axis (dash-dotted line) with angular frequency "Omega". The magnetic dipole axis (short dashed line) is inclined to the rotation axis with angle "alpha". The neutron star has the magnetic dipole moment with strength. As the neutron star spins down, its rotational energy is dissipated in the form of the Poynting flux (i.e., outward flow of electro-magnetic energy), rest-mass and kinetic energies of the electrons and positrons, and the gamma-ray energies. The solid curves designate the magnetic field lines. In the convex side of the lower bounding magnetic field line, a high vacuum is maintained, because charged particles efficiently escape across the light cylinder (vertical long dashed line on the right). As a result, an electric field arises along the local magnetic field lines in the red, shaded region. In this ‘outer-magnetospheric particle accelerator’, electrons (e-) and positrons (e+) are created by photon-photon collisions and accelerated by the magnetic-field-aligned electric field in the opposite directions along the magnetic field lines. Gamma-rays are emitted mostly outwards by the out-going particles (e+). The gamma-ray luminosity is essentially determined by the trans-magnetic-field thickness of the accelerator, which is, in turn, controlled by the efficiency of the photon-photon collisions that take place within the accelerator.
Schematic picture (side view) of a pulsar magnetosphere.
Accretion geometry of disks for LLAGN (upper panel) and high luminosity AGN (lower panel) corresponding to high and low rates of mass accretion respectively. (Liu & Taam 2009, ApJ, 707, 233.)
Accretion geometry of disks for LLAGN and high luminosity AGN corresponding to high and low rates of mass accretion respectively.
Prototype of Graphitic Core for Two-Fluid Molten-Salt Heat-Exchanger
Prototype of Graphitic Core for Two-Fluid Molten-Salt Heat-Exchanger
Figure 5 of "Pulsar Outer-gap Electrodynamics: Hardening of Spectral Shape in the Trailing Peak in Gamma-ray Light Curve", Kouichi Hirotani, Astrophys. J. 733, Letters 49-53 (2011).
Spectral Hardening in the Trailing Peak of Gamma-ray Pulsar Light Curve

本所高能天文物理研究方向包括了雙星系統與星系中心流向黑洞吸積之特性，雙星系統中子星及黑洞的形成，從獨立磁化中子星或伽瑪射線雙星系統成員之高能幅射機制。

研究人員 (6)

浅田圭一 Asada, Keiichi cv 副研究員長聘
研究興趣: 活躍星系核,特長基線干涉儀之偏振測量
陳科榮 Chen, Ke-Jung cv 助研究員
研究興趣: 計算天文物理, 超新星模型,核天文物理,宇宙學
溫志懿 Wen, Chih-Yi cv 研究技師
研究興趣: 儀器控制, 程式設計, 高能物理
廣谷幸一 Hirotani, Kouichi cv 副教授級學者
研究興趣: 高能天文物理
中村雅德 Nakamura, Masanori cv GLT/VLBI 計畫研究科學家
包傑夫 Bower, Geoffrey cv 資深研究天文學家

期刊論文 (150)

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