Kazuo Makishima Department of Physics, University of Tokyo Research Center for the Early Universe, U. Tokyo Inst. of Physical & Chemical Research (RIKEN) Experimental High energy Astrophysics using satellite-borne X-ray instruments 1
2012/12/15 2012 at Nara - Cosmic X- — Share with γ-ray etc.   —— Space Station ——Japanese Solar QUCS2012 at Nara
Construction of Ginga (launched in 1987) The Instrumentation Team for the HXD (Hard X-ray Detector) on- board Suzaku (launched in 2005)
How macro properties of celestial objects described via first principle using fundamental constants ♦ c, e, h, mp, me, G, (εo) ♦Two important dimensionless constants: •  Fine structure constant (EM interaction strength) α = e² /4πε hc = 1/137 • Grav. i.s. const. (gravitational interaction strength) α ς = Gm ² /hc = 5.90 × 10−39 •  For any celestial object, ac:a = selr-gravitating energy : Coulomb repulsion energy (if not neutral) ♦The only macro variable: mass M (or N ≡ M /m )
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(Shakura & Sunyaev 1973) ♦ A BH of mass M radiating at η(0<η<1) times the Eddington limit: ♦ Thomson cross sect.:  σ (8π /3)(e² /4πε m c²)² ♦ Stefan-Boltzmann’s law:  ∑∑ = 4 π_R²_σT 4 S-B constant:  σ ≡ π k 160c²h³ ♦ Innermost radius (GR) :  R = 3Rs = 6GM /c² ♦ Disk temperature at t the innermost radius: kT = (5 / 8 π³)¹/4 (αςα²)-¹/4 ((m çc²)(m çc²)]¹/2 (η / N)¹/4 = 1.0 η 1/4 (M /10 M ⊕ )-1/4 keV 2012/12/15
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1. Physical settings cannot be chosen as you like Strong spatial gradients, Non steady-state, Explosive/Transient, Versatile processes, …… 2. Extreme (often exotic) physical conditions ρ> Pnuc,  kT >  mec²,  G.R.,  B >  4.4×10¹³  G, etc., where our knowledge may be insufficient…… 3. Long-range force (Grav, EM) + local interactions Strong non-linearity,  Self-interaction, Energy non-equipartition, Spont. struct. formation, ……
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Structure formation in CDM universe (Abel+12) Matter accretion onto a black hole CS2012 at Nara
✦ An ultra-compact star, in which the extreme gravity (10°g) is supported by degenerate pressure of neutrons. ♦ Formed by core collapse of a massive star.
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About half of ~40 known accreting binary X-ray pulsars have allowed detections of electron cyclotron resonance features (Landau level transisions) in their spectra (Makishima +99), at an energy of E = heB / m  = 1 1.6(B / 10 12 G)  keV. 2012/12/15 QUCS2012 at Nara 15
50 theor. support by Hashimoto, Hatsuda+12) ivovavion i crical TOOKUN標準準準準準ks 2012/12/15 QUCS2012 at Nara 16
♦ Isolated NSs with no evidence of mass accretion. Sometimes emitting repetitive intense soft gamma-ray flashes. ♦About 25 known. From P and dP/dt, B=10 14-15 G is suggested. ♦ X-ray lum. » spin-down lum. →not rotation powered. ♦ Radiating by consuming their magnetic energies. ♦ Suzaku → peculiar 2-comp. spectra. ♦ Emission mech. of hard component? ♦ With age, why the hard c. gets weaker but harder?
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Harding, A., & Lai, D. Rep. Prog. Phys. 69, 2631 (2006) Particle acceleration by induced electric fields E =v×B = 2e14 (P/30ms) -1 (B/1e12G)(R/10km)²  (V/m) (still « Schwinger limit…) 2012/12/15 QUCS2012 at Nara
“Photon Splitting” ♦ A 3rd QED effect: a photon interact with B- field and splits into two with lower energies. ♦ Cross section ∞ (B/Bcr) 6 (hv/mec²) 5 , with photon-polarization dependence. (Bialynicka-Birrla & Bialynicka-Birrla 70, Meszros & Ventura 79, Baring & Harding 01)
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A successor to Suzaku, to be launched in 2014 ♦ Soft XR mirror+Micro Calorimeter: 0.5-12 keV, ΔE/E~0.1% ♦ Soft XR mirrror+ XR CCD camera : 0.3-12 keV、Wide FOV of 40' ♦ Super Mirror + Hard XR Imager : 5~80 keV, imaging spectroscopu ♦ Soft GR Detector : 60~600 keV, Advance Compton camera
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