high energy astrophysicsmosir/pub/2011/2011-09-26/10...2011/09/26 · hideyo kunieda nagoya...
TRANSCRIPT
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Hideyo Kunieda Nagoya University
Violent Universe Explored by
Japanese X-ray Satellites
Asia Academic Seminar
CPS 8th International School of Planetary Science
September 30, 2011 at Awaji
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Lecture Plan
II. High energy phenomena 2. Supernova remnants (SNR)
3. Neutron stars and blackholes
4. Active Galactic Nuclei(AGN)
5. Cluster of galaxies and Cosmology
September 30, 10:45-12:00
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II-2 :Supernova remnants (SNR)
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Supernova Remnants (SNR)
M < 0.5 Msolar H He
M < 3 Msolar H He C/O-----------------------White dwarf
3Msolar < M < 8Msolar C O Ne Mg
Ty I SN ----------------------Scatter all mass
8Msolar < M < 30Msolar Si Fe/Ni
Ty II SN ----------------------Neutron stars
30Msolar < M ---------------------------------------Black holes
(1) Evolution of main sequence stars
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(2) Evolution of Supernovae
Gravitational ε of collapsed star --> Neutrino (99%)
--> Kinetic E (1 %)
Shock wave enhances density, reduces speed
Kinetic ε ---> Thermal ε
Sweep-up surrounding gas --> Shell
High density --> X-rays (∝T1/2 n2)
Effective cooling by X-rays when T ~ 106 K
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半径(pc)
Tem
per
ature
D
ensi
ty
Shell(High density
High Emissivity)
High Temp.
Low Density
1 atom/cc
107 K~1 keV
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Visible
10 light year
X-rays
5 x 107 K
Cas-A (1680 AD)
Photograph courtesy NASA/ESA/Hubble Heritage Team
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Record of Supernovae
Year(AD) Constellation Name of objects
185 Centaurus G314.4-2.3
386 Sagittarius G11.2-0.3
1006 Lupus SN1006
1054 Taurus Crab Nebula
1181 Cassiopeia 3C58
1572 Cassiopeia Tycho
1604 Ophiuchus Kepler
1680 Cassiopeia Cas A
1987 LMC 1987A
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SN1987A
Before After
Visible
Expanding Ring
observed by Hubble
X-ray image by Chandra
Jan. 2000
Half year later Ginga discovered X-rays from
--> Projenitor hit by shock wave
Anglo-Austrian Observatory
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Cas A X-ray Spectra
Si
Fe
Thermal Brems
+
Emission lines
Non-uniform
explosion
Different dist.
of elements
http://www.u.phys.nagoya-u.ac.jp/r_e/r_e3_4.html
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Multi-waveband observations
X-ray observation by Suzaku
Tycho SNR with Suzaku
8 arcmin
Left:
Slow
0.15”/year
Expansion
(Chandra)
Right:
Fast
0.45”/year
Expansion
(Chandra)
Fe rich
shell
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(3) Dynamics of SNR Tycho SNR with Suzaku
Fe-K line Outer
Inner Fe-K line
Broadening
Multiple
lines yield
δE ~ 40 eV
8 arcmin
Outer Inner
Furuzawa
et al.
Tycho SNR Discovered by Tycho Brahe in 1572
Furuzawa et al. Furuzawa,2009:ApJ...693L..61F
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(3) Dynamics of SNR
Inner
Tycho SNR with Suzaku
8 arcmin
km/s
In In
In
Out Out Out
In - out
In - out In - out
Si S Fe
Tycho SNR
Radial expansion
ΔVFe ~ 3000 km/s
Expanding shell at 2000-3000km/s
Furuzawa et al. Furuzawa,2009:ApJ...693L..61F
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Tycho SNR
Si
Si S
S Ar Ca
Extend internal structure of progenitor
Expanding shell at 2000-3000km/s
Furuzawa et al. Hayato et al.,2010:ApJ...725..894H
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Infrared
(Akari) X-ray
By Ishihara
(SUZAKU)
Plasma
Dust
Molecular cloud Radio(CO)
Tycho SNR
Multi-waveband observations
Ishihara et al.2010:A&A...521L..61I
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Wavelength (μm)
FL
ux
(Jy
)
Warm Dust Clod Duzt
あかり
あかり あかり
400年
Infrared images by Akari
Left:
Clod Dust (~20K)
Right:
Warm Dust (~100K)
Ishihara et al.2010:A&A...521L..61I
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Schematic View of the shell region
Multi-waveband observations
X-ray
Ejecta of
SNR
Swept up
ISM Interstellar
Matter(ISM)
Shock
front
Depletion
Mixture of 107K Plasma
and 100K Dust
Molecular gas +
+ 20 K Dust
X-ray Infrared Infrared
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SN1006(1006)
Acceleration of
High energy particles
E>1014 eV electrons
Production of
Cosmic rays
(protons)? Thermal component
(Brems +emission lines)
Non-thermal
Power law
component
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(3) Products of Super novae
Hot plasmas --> Hot Inter-Stellar Medium(HISM)
Dense core (Neutron stars, Black holes)
Nuclear synthesis --> Pollution of ISM
--> material for the next generation stars
--> Contraction of B --> Acceleration of e-
--> Supply of Energy and abundance to ISM
Acceleration of high energy particlesCosmic rays
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II-3 : Neutron stars and blackholes
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1. X-ray binaries
(1) Mass Accretion from Companion Stars
(Copyright )Scientific American
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II-4 : Active Galactic Nuclei(AGN)
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Active galactic nuclei (AGN)
Bright nucleus > total radiation of stars 1011
Ionization source! Stellar emission
Emission lines instead of absorption lines
Narrow
Broad
V>2000km/s
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Optical images
of galaxies Eliptical
galaxies
Barred
Galaxy
Spiral
galaxies
AGN
M 87
Hubble Space Telescope
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Mass estimation of nuclei
Nuclear gas motion
v2/r = GM/r2
v=500km/s、
Radius: r=18pc
M> 109 Msolar
Blue shift <-- Approaching
Red shift <-- Reseeding
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Active galactic nuclei Narrow
Emission lines
Broad
Emission Lines
Absorption Torus
Absorption Torus
BLR Cloud
NLR Cloud
Ty I AGN
Ty II AGN
Black Hole and
Accretion Disk
http://www.astro.isas.ac.jp/xjapan/asca/3/agn/
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X-rays from AGN
Cont.
Bright
Nucleus
Power Law Comp.
Res
idual
Fe-K
Line
Illuminated
Acc. disk
Fe-K
Strong
X-ray
Source
James N, Reeves et al, 2007, Publ. Astron. Soc.Japan, 59, 301
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Doppler Effect
Relativistic Orbital Velocity
Gravitational
Red Shift
X-ray energy(keV)
Model
Calcuration
ASCA
MCG-6-30-15
X-ray
Energy
Suzaku
6.4keV
ν = (1 - rg/r)1/2 ν em
Fabian et al, 1989, Mon. Not. R. astr. Soc, 238, 729
Tanaka,Y et al, 1995, Natur., 375, 659 Miniutti, H et al, 2007, Progress of Theoretical Physics Supplement, 169, 260
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How large red shift could be?
Rin could be as small as 3Rg
If BH is rotating, Rin could be < 3Rg
then red shift could be larger
Red shift to 5keV is sure--> but
Rotating Kerr BH is not clear yet Continuum level
affects the red shift
MCG-6-30-15
How small the inner most radius could be?
ESA
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Structure of the BH vicinity
Determined by Suzaku
45°
Broader at Edge-on X-ray energy(keV)
Model
Calcuration
Gravitational
Red Shift
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Galactic Center Region
Chandra X-ray Image of GC
350 ly
90 ly
200 ly
Sgr B2
Radio Arc
Sgr A*
Sgr C
Galactic Plane
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X-ray Spectrum
of the Galactic Center
6 7 X-ray Energy (keV)
6.4 keV
6.7
keV
6.9
keV
X-r
ay I
nte
nsi
ty
Emission lines of
Fe at different
ionization state
Hot Plasma
CCD Spectral
Resolution
Fluorescence
Neutral 6.4 keV
He-like ion 6.7 keV
H-like ion 6.9 keV
Koyama et al., 2007, Publ. Astron. Soc. Japan, 59, 245
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Sgr A*
6.7 keV
Line mapping
Hot Plasma
30 pc
6.4 keV
Line Mapping
Reflection
Nebulae
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Galactic Center Region
Galactic Plane Molecular Cloud
Sgr B2
Galactic
Center
Chandra X-ray Image of GC
350 ly
90 ly
200 ly
Sgr B2
Radio Arc
Sgr A*
Sgr C
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Bright X-ray Source at Galactic Center?
Very bright
350 years ago!
Central Luminosity
350 years ago
Central Luminosity
90 years ago
Massive Black hole
was very active!
Murakami, H et al, 2003, Astron. Nachr, 324, 125
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ASCA
1994
Chandra
2000
XMM
2004
Suzaku
2005 X-ray
XMM
Suzaku
X-ray Front approaching
to molecular clouds
K. Koyama Koyama et al., 2008, Publ. Astron. Soc. Japan, 60, 201
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II-5 : Cluster of galaxies
and Cosmology
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Structure of C. G. Visible(Stars) X-rays(Gas density2) Gas temp.
柴田D
Fig. 7.2
R. Shibata et al., 2001,ApJ , 549 , 228
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Temperature Density
Emission
Measure
Abundance
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Abundance
Distribution
Concentration at cores
Nucleus-synthesis
Ty Ia/Ty II SNR
Scatter of galactic gases
Galactic wind、
Ram pressure
Ezawa et al.,1997, ApJ...490L..33E
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Mass of C. G.
Galaxies(stars) 1011x103 Msolar
Intra-cluster gas
V= 4π(16Mpc x tan 2°)3 /3=2 x 1073
V x 0.001/NA/2 x 1033g = 5.4 x 1014 Msolar
Dark matter>1015 Msolar
Vilial mass(8keV、1000km/s)
Lubin et al. 1996, ApJ...460...10
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Lecture Plan
I. Basic processes in High energy astronomy
I-1: Why X-ray astronomy?
I-2: Emission mechanisms
I-3: Energy sources
II. High energy phenomena
II-1: Stellar X-ray emission
September 30, 9:00-10:15
II-2: Supernova remnants (SNR)
II-3: Neutron stars and blackholes
II-4: Active Galactic Nuclei
II-5: Cluster of galaxies and Cosmology
September 30, 10:45-12:00
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X-ray Telescope
Hard X-ray Telescope
Extension
12
m F
L
Hard X-ray Imagers
6 m
FL
f
ixed
ben
ch
Calorimeter
High resolution
spectrometer
Soft X-ray telescope Nagoya
Univ.
Astro-H satellite 2014〜
Soft γ-ray Detector
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X-ray Telescope
21 Suzaku
00 01 02 03 04 05 06 07 08 09 10 11 12 13 14 15 16 17
Current
missions
ISAS/JAXA
missions
Ballons
Chandra
Newton
SUMIT
InFOCμS
HEFT HERO
Small Missions
GLAST
ATHENA
International
X-ray Observatory
Hard X-ray Astronomy
Astro-H
X-ray missions in 21st Century
ASTROSAT
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References • http://www.u.phys.nagoya-u.ac.jp/r_e/r_e3_4.html
• Furuzawa et al., 2009, Doppler-Broadened Iron X-Ray Lines From Tycho's Supernova Remnant : ApJ...693L..
• Hayato et al., 2010, Expansion Velocity of Ejecta in Tycho's Supernova Remnant Measured by Doppler Broadened X-ray Line Emission : ApJ...725..894H
• Ishihara et al., 2010, Origin of the dust emission from Tycho's SNR : A&A...521L..61I
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