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中央研究院天文及天文物理研究所
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高能天文物理

Image of the black hole in M87, obtained by the Event Horizon Telescope Collaboration.
Image of the Black Hole in M87
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

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 (9)

尚賢 Shang, Hsien cv 研究員
研究興趣: 理論及計算天文物理，恆星及行星形成，磁流體動力學，噴流，隕石
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: 理論與計算天文物理: 大質量恆與超新星爆炸, 星際介質, 超大質量黑洞, 第一代恆星與星系
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 訪問學者 (八戸工業高等専門学校)
卜宏毅 Pu, Hung Yi cv 訪問學者 (師範大學)
研究興趣: 黑洞天文物理，廣義相對論性磁流體力學, 廣義相對論性輻射轉移, 吸積盤與噴流理論
紀柏特 Jeter, Britton Harold cv 博士後研究
研究興趣: 黑洞、活動星系核、噴流、可變性和計算天文物理學
包傑夫 Bower, Geoffrey cv 資深研究天文學家

期刊論文 (192)

  1. Chen K-J; Tang C-Y; Whalen DJ; Ho M-Y; Tsai S-H; Ou P-S; Ono M, "How Population III Supernovae Determined the Properties of the First Galaxies" , ApJ: 964(1), id.91 (12pp), Mar, 2024 [SCI] ( ADS | Fulltext )
  2. Ono M; Nozawa T; Nagataki S; Kozyreva A; Orlando S; Miceli M; Chen K-J, "The impact of effective matter mixing based on three-dimensional hydrodynamical models on the molecule formation in the ejecta of SN 1987A" , ApJS: 271(1), id.33 (57pp), Mar, 2024 [SCI] ( ADS | Fulltext )
  3. Chen K-J; Whalen DJ; Woosley SE; Zhang W, "Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-Instability Supernovae" , ApJ: 955(1), id.39 (12pp), Sep, 2023 [SCI] ( ADS | Fulltext )
  4. Hirotani K; Shang H; Krasnopolsky R; Nishikawa K-I, "Two-dimensional Particle-in-Cell simulations of axisymmetric black hole magnetospheres: angular dependence of the Blandford-Znajek flux" , ApJ: 943(2), id.164 (19 pp.), Feb, 2023 [SCI] ( ADS | Fulltext )
  5. Cemeljic M; Yang H; Yuan F; Shang H, "Formation of episodic jets and associated flares from black hole accretion systems" , ApJ: 933(1), id.55 (13pp), July, 2022 [SCI] ( ADS | Fulltext )
  6. Umetsu K; Ueda S; Hsieh B-C; Nonino M; Chiu IN; Oguri M; Molnar SM; Koekemoer AM; Tam S-I, "Line-of-sight Elongation and Hydrostatic Mass Bias of the Frontier Fields Galaxy Cluster Abell 370" , ApJ: 934(2), id.169, Aug, 2022 [SCI] ( ADS | Fulltext )
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  8. Wu M-R; George M; Lin C-Y; Xiong Z, "Collective fast neutrino flavor conversions in a 1D box: Initial conditions and long-term evolution" , Phys Rev D: 104(10), id.103003, Nov, 2021 [SCI] ( ADS | Fulltext )
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  11. Bower GC; Dexter J; Asada K; ..., Ho P; Inoue M; ...; Matsushita S; ...; Nakamura M; ...; Rao R; et al., "ALMA Observations of the Terahertz Spectrum of Sagittarius A*" , ApJL: 881(1), id. L2 (7 pp.), Aug, 2019 [SCI] ( ADS | Fulltext )
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  13. Park J; Hada K; Kino M; Nakamura M; ...; Asada K; et al., "Kinematics of the M87 Jet in the Collimation Zone: Gradual Acceleration and Velocity Stratification" , ApJ: 887(2), id. 147 (27 pp.), Dec, 2019 [SCI] ( ADS | Fulltext )
  14. Ueda S; Ichinohe Y; Kitayama T; Umetsu K, "Line-of-Sight Gas Sloshing in the Cool Core of Abell 907" , ApJ: 871(2), id. 207 (6 pp.), Feb, 2019 [SCI] ( ADS | Fulltext )
  15. Hirotani K; Pu H-Y; Outmani S; ...; Matsushita S; Kong AKH, "High-energy and Very High Energy Emission from Stellar-mass Black Holes Moving in Gaseous Clouds" , ApJ: 867(2), id. 120 (13 pp.), Nov, 2018 [SCI] ( ADS | Fulltext )
  16. Hirotani K; Pu HY; Matsushita S, "Lightning black holes as unidentified TeV sources" , JApA: 39(4), id. 50 (8 pp.), Aug, 2018 [SCI] ( ADS | Fulltext )
  17. Nakamura M; Asada K; Hada K; Pu H-Y; ...; Tseng C-Y; ...; Koyama S; et al., "Parabolic Jets from the Spinning Black Hole in M87" , ApJ: 868(2), id. 146 (28 pp.), Dec, 2018 [SCI] ( ADS | Fulltext )
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  22. Pu H-Y; Wu K; Younsi Z; Asada K; Mizuno Y; Nakamura M, "Observable Emission Features of Black Hole GRMHD Jets on Event Horizon Scales" , ApJ: 845(2), 160, Aug, 2017 [SCI] ( ADS | Fulltext )
  23. Toala JA; Marston AP; Guerrero MA; Chu YH; Gruendl RA, "Hot Gas in the Wolf-Rayet Nebula NGC 3199" , ApJ: 846(1), 76, Sept, 2017 [SCI] ( ADS | Fulltext )
  24. Asada K; Nakamura M; Pu H-Y, "Indication of the Black Hole Powered Jet in M87 by VSOP Observations" , ApJ: 833(1), 56, Dec, 2016 [SCI] ( ADS | Fulltext )
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  26. Hirotani K; Pu H-Y; Lin LC-C; Chang H-K;Inoue M; Kong AKH; Matsushita S; Tam P-HT, "Lepton acceleration in the vicinity of the event horizon: High-energy and Very-high-energy emissions from rotating black holes with various masses" , ApJ: 833(2), 142, Dec, 2016 [SCI] ( ADS | Fulltext )
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  30. Tseng C-Y; Asada K; Nakamura M; Pu H-Y; Algaba J-C; Lo W-P, "Structural Transition in the NGC 6251 Jet: an Interplay with the Supermassive Black Hole and Its Host Galaxy" , ApJL: 833(2), 288, Dec, 2016 [SCI] ( ADS | Fulltext )
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  32. Hirotani K, "Three-dimensional Non-vacuum Pulsar Outer-gap Model: Localized Acceleration Electric Field in the Higher Altitudes" , ApJ: 798(2), L40, Jan, 2015 [SCI] ( ADS | Fulltext )
  33. Lin LCC; Hu C-P; Kong AKH; Yen DC-C; Takata J; Chou Y, "Long-term X-ray Variability of Ultraluminous X-ray Sources" , MNRAS: 454(2), 1644-1657, Dec, 2015 [SCI] ( ADS | Fulltext )
  34. Pu H-Y; Nakamura M; Hirotani K; Mizuno Y; Wu K; Asada K, "Steady General Relativistic Magnetohydrodynamic Inflow/Outflow Solution Along Large-Scale Magnetic Fields That Thread A Rotating Black Hole" , ApJ: 801(1), 56, March, 2015 [SCI] ( ADS | Fulltext )
  35. Urata Y; Huang K; Asada K; Hirashita H; Inoue M; Ho PTP, "A New Era of Submillimeter GRB Afterglow Follow-Ups with the Greenland Telescope" , Advances in Astronomy, Article ID 165030, 2015 [SCI] ( ADS | Fulltext )
  36. Asada K; Nakamura M; Doi A; Nagai H; Inoue M, "Discovery of Sub- to Superluminal Motions in the M87 Jet: An Implication of the Acceleration from Sub-relativistic to Relativistic Speeds" , ApJL: 781(1), L2, Jan, 2014 [SCI] ( ADS | Fulltext )
  37. Bower GC; Markoff S; Brunthaler A; et al., "The Intrinsic Two-dimensional Size of Sagittarius A*" , ApJ: 790(1), 1, July, 2014 [SCI] ( ADS | Fulltext )
  38. Hirotani K, "Does a strong particle accelerator arise very close to the light cylinder in a pulsar magnetosphere?" , MNRAS: 442(1), L43-L45, July, 2014 [SCI] ( ADS | Fulltext )
  39. Inoue M; Algaba-Marcos JC; Asada K; Chang C-C; Chen M-T; Han J; Hirashita H; Ho PTP; Hsieh S-N; Huang T; Jiang H; Koch PM; Kubo DY; Kuo C-Y; Liu B; Martin-Cocher P; Matsushita S; Meyer-Zhao Z; Nakamura M; Nishioka H; Nystrom G; Pradel N; Pu H-Y; Raffin PA; Shen H-Y; Snow W; Srinivasan R; Wei T-S; Blundell R; Burgos R; Grimes P; Keto E; Paine S; Patel N; Sridharan TK; Doeleman SS; Fish V; Brisken W; Napier P, "Greenland telescope project: Direct confirmation of black hole with sub-millimeter VLBI" , Radio Science: 49(7), 564-571, July, 2014 [SCI] ( ADS | Fulltext )
  40. Kuo C-Y; Asada K; Rao R; Nakamura M; Algaba JC; Liu HB; Inoue M; Koch PM; Ho PTP; Matsushita S; Pu H-Y; Akiyama K; Nishioka H; Pradel N, "Measuring Mass Accretion Rate onto the Supermassive Black Hole in M87 Using Faraday Rotation Measure with the Submillimeter Array" , ApJL: 783(2), L33, March, 2014 [SCI] ( ADS | Fulltext )
  41. Nakamura M; Meier DL, "A Magnetohydrodynamic Model of The M87 Jet. II. Self-consistent Quad-shock Jet Model for Optical Relativistic Motions and Particle Acceleration" , ApJ: 785(2), 152, April, 2014 [SCI] ( ADS | Fulltext )
  42. Hirotani K, "Luminosity Evolution of Gamma-Ray Pulsars" , ApJ: 766(2), 98, April 1, 2013 [SCI] ( ADS | Fulltext )
  43. Nakamura M; Asada K, "The Parabolic Jet Structure in M87 as a Magnetohydrodynamic Nozzle" , ApJ: 775(2), 118-128, Oct, 2013 [SCI] ( ADS | Fulltext )
  44. Asada K; Nakamura M, "The Structure of the M87 Jet: A Transition from Parabolic to Conical Streamlines" , ApJL: 745(2), L28, Feb, 2012 [SCI] ( ADS | Fulltext )
  45. Taam RE; Liu BF; Yuan W; Qiao E, "Disk Corona Interaction: Mechanism for the Disk Truncation and Spectrum Change in Low-luminosity Active Galactic Nuclei" , ApJ: 759(1), 65, Nov 1, 2012 [SCI] ( ADS | Fulltext )
  46. Hirotani K, "Pulsar Outer-gap Electrodynamics: Hardening of Spectral Shape in the Trailing Peak in the Gamma-Ray Light Curve" , ApJ: 733(2), L49, June, 2011 [SCI] ( ADS | Fulltext )
  47. Wang RB; Hirotani K, "Death Line of Gamma-Ray Pulsars with Outer Gaps" , ApJ: 736(2), 127, Aug 1, 2011 [SCI] ( ADS | Fulltext )
  48. Asada K; Nakamura M; Inoue M; Kameno S; Nagai H, "Multi-Frequency Polarimetry Toward S5 0836+710: A Possible Spine-Sheath Structure For The Jet" , ApJ: 720(1), 41-45, 2010 [SCI] ( ADS | Fulltext )
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  50. Takata J; Chang H-K, "Non-thermal emissions from outer magnetospheric accelerators of middle-aged pulsars" , MNRAS: 392(1), 400-412, Jan, 2009 [SCI] ( ADS | Fulltext )
  51. Takata J; Taam RE, "Probing the Pulsar Wind in the gamma-ray Binary System PSR B1259-63/SS 2883" , ApJ: 702(1), 100-113, Sep 1, 2009 [SCI] ( ADS | Fulltext )
  52. Tsai A-L; Matsushita S; et al., "Molecular Superbubbles and Outflows from the Starburst Galaxy NGC 2146" , PASJ: 61(2), 237-250, Apr 25, 2009 [SCI] ( ADS | Fulltext )
  53. Urata Y; Huang KY; Im M; Lee I; Deng J; et al., "Swift GRB GRB071010B : outlier of the Epeak− Eγ and Eiso − Epeak− tjet Correlations" , ApJ: 706(1), L183-L187, November 20, 2009 [SCI] ( ADS | Fulltext )
  54. Hirotani K, "Outer-gap versus Slot-gap Models for Pulsar High Energy Emissions: The Case of the Crab Pulsar" , ApJ: 688(1), L25-L28, Nov 20, 2008 [SCI] ( ADS | Fulltext )
  55. Taam RE; Liu BF; Meyer F; Meyer-Hofmeister E, "On the Properties of Inner Cool Disks in the Hard State of Black Hole X-Ray Transient Systems" , ApJ: 688(1), 527-536, Nov 20, 2008 [SCI] ( ADS | Fulltext )
  56. Takata J; Chang H-K; Shibatga S, "Particle Acceleration and Non-thermal Emission in Pulsar Outer Magnetospheric Gap" , MNRAS: 386(2), 748-758, May, 2008 [SCI] ( ADS | Fulltext )
  57. Hirotani K, "High-energy Emission from Pulsar Outer Magnetospheres" , ApJ: 662(2), 1173-1176, Jun 20, 2007 [SCI] ( ADS | Fulltext )
  58. Takata J; Chang HK, "Pulse Profiles, Spectra and Polarization Characteristics of Non-Thermal Emissions from the Crab-Like Pulsars" , ApJ: 670(1), 677-692, Nov 20, 2007 [SCI] ( ADS | Fulltext )
  59. Takata J; Chang HK; Cheng KS, "Polarization of high-energy emissions from the Crab pulsar" , ApJ: 656(2), 1044-1055, Feb 20, 2007 [SCI] ( ADS | Fulltext )
  60. Hirotani K, "High-energy Emission from Pulsar Magnetospheres" , MPLA: 21(17), 1319-1337, Jun 7, 2006 [SCI] ( ADS | Fulltext )
  61. Takata J; Shibata S; Hirotani K; Chang H-K, "A two-dimensional electrodynamical outer gap model for γ-ray pulsars: γ-ray spectrum" , MNRAS: 366(4), 1310-1328, Mar, 2006 [SCI] ( ADS | Fulltext )
  62. Kitayama T; Ueda S; Okabe N; Akahori T; Hilton M; Hughes JP; Ichinohe Y; Kohno K; Komatsu E; Lin Y-T; Miyatake H; Oguri M; Sifón C; Takakuwa S; Takizawa M; Tsutsumi T; Van Marrewijk J; Wollack EJ, "Galaxy clusters at z 1 imaged by ALMA with the Sunyaev-Zel'dovich effect" , PASJ: 75(2), 311-337, April, 2023 [SCI] ( ADS | Fulltext )
  63. Garrel C; Pierre M; Valageas P; Eckert D; Marulli F; Veropalumbo A; Pacaud F; Clerc N; Sereno M; Umetsu K; Moscardini L; Bhargava S; Adami C; Chiappetti L; Gastaldello F; Koulouridis E; Le Fevre J-P; Plionis M, "The XXL survey. XLVI. Forward cosmological analysis of the C1 cluster sample" , A&A: 663, id.A3 (18 pp), July, 2022 [SCI] ( ADS | Fulltext )
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