1. Supernova remnants (SNR) as ideal laboratories of hot plasmas Koyama Katsuji, Kyoto, and Osaka University
Allow me to make an excuse remark …
To specialist (astronomer) = OK
What are Chandrasekhar mass, Hubble
constant, Stellar structure, SN and SNR.
(2) To general public (citizen) = OK
Big bang, Black hole
Between (1) and (2) is very difficult.
My talk is limited area of Astronomy
: Hot plasma and Nucleosynthesis in SNRs

2. After14 Gys: Islands: Cosmos
Immediate after (0.4 Mys) the Big Bang: Chaos: “Ripples on the Pacific Ocean” only H, He
Cluster of
Galaxies
100 G stars
C, O, Si, Fe
Q: when and where ?
A: SN, SNR
After14 Gys: Islands: Cosmos

3. What is SN, SNR ?
By nuclear fusion, massive stars accumulate heavy elements in the interior
(1) >10 M◎ : Fe core
Core collapse
supernova (CC SN:
He, C, Ne, O)
C+Ne+O
white dwarf
degeneracy
pressure
(2) 8-10 M◎ :C, Ne, O
(white dwarf:
degeneracy pressure)
Explosive fusion
Ia supernova (Ia SN : Fe)
Supernova Remnant
(SNR)= Shock Heated
Hot Plasma

4. Hot Plasma Space Plasma vs Laboratory Plasma
Fundamental physics
and
Physical parameters
are obtained from
Laboratory Work
Applied to the Space
Space proper Science
Are laboratory works always more accurate and reliable than the space ? No !

5. Steady nuclear fusion in laboratory is very difficult, almost impossible  to keep hot plasma for long time is difficult.
Laboratory plasma is always transient
in a short time scale.
Space plasma is also transient, but the time scale is extremely long  quasi-stable
Space is better than laboratory to study
transient plasma
Q: What is transient in the SNR plasma ?
A: Shock-heating and relaxation process

6. Expanding velocity (v) Random velocity (T)
Transient Plasma =Ionizing plasma (IP)
Expanding velocity (v)
Random velocity (T)
Free Expansion( v) X
Electron temperature, Te
Ionization temperature: Tz
IP : (Te > Tz)  CIE (Te=Tz)
Shock
Heated
Gas
In most of the SNR,
Te > Tz (IP) .
Standard Scenario
Time t (~1000 ys)

7. No laboratory spectrum is like this !Ne Mg Si S Ar Ca Fe
X-ray Spectrum
of IC 443
(CC SNR)
Ohnishi et al. 2013
All these lines come from highly ionized atoms
No laboratory spectrum is like this !
Temperature kTe~ 0.6 keV is too low to make highly ionized iron  Tz is higher than 0.6 keV
to excite the lines  Recombination of free electron
Discovery of Te< Tz plasma
= Ｒｅｃｏｍｂｉｎｇ　Ｐｌａｓmａ (RP)

8. Excitation electron < Recombination of free electron
He-like ion:
Excitation electron <　 Recombination of free electron
RRC
1S1

9. log r (pc) log t (year) Origin of Recombining Plasma
Rarefaction in an early phase of CC SN
High density Circum Stellar Medium (CSM ) Te=Tz  Break out to low density Inter Stellar Medium (ISM)
Adiabatic expansion 　Te is cooled down Te<Tz
CSM
High density
ISM
Low density
log t (year)
log r　(pc) 1 RP

10. From these line fluxes, we can determine the abundance of each elementMg Si S Ar Ca Fe
The key issue is whether the plasma is ionizing, recombining, or equilibrium and
what is the transient time

11. Whether ionizing or recombining, and the transient time, historical SNe are important. We can depict the data of each time epoch, then can make quantitative model (theory).
log t (s)
SN185 : Himiko unified Japan (Yamatai Koku)
This is my
“Star-of-bethlehem”
Southern Cross
SN1006
SN1573
(Tycho’s SN)
SN1604
(Kepler’s SN

12. Time history of recombination and ionization
Bare Ion
H-like
He-like Li-like 1
Recombining
Plasma
0.1
0.01
log t (s) for n=1cm-3
Iron Ion Fraction
Ionizing
plasma
We know the ion fraction from the spectrum , then we can obtain the abundances of each element

13. Nucleosynthesis in massive star 1
C+Ne+O
white dwarf
 Si--Fe
Ia Supernova
: Ia SN
8-10 M◎ :C, Ne, O
(white dwarf)
 Explosive fusion (Si--Fe)

14. Fujiwara, Teika (藤原定家） Meigetsuki (明月記）, Vol 52Ia SN CC
SN1006
Fujiwara, Teika (藤原定家） Meigetsuki　(明月記）, Vol 52
一條院 寛弘三年 四月二日 葵酉 夜以降 騎官中 有大客星 如螢惑 光明動耀 連夜正見南方 或云 騎陣将軍星本体 増変光
Conste-
llation
star
Uchida et al. 2013
100 ly
Then 1000 years after
Koyama et al. 1996

15. Nucleosynthesis in massive star 2
Core collapse
supernova
: CC SN
>10 M◎
He, C, Ne, O, Si
SNR observations are
“Anatomy” of massive stars

16. The progenitor stars are constrained to be ~25 M◎ Ia CC
Yasumi et al. 2013

17. High energy electrons = Synchrotron radiation
Another topics : To thermal equilibrium, but in SN1006 opposite evolution (high temperature component becomes much higher).
High energy electrons = Synchrotron radiation
Ex=3keV (B/1μG)(Ee/1014 eV)2
Koyama et al. 1996

18. Fermi Acceleration V=6000 km/s Ping-Pong ball on the moving frame
SN1006
V=6000 km/s
Winkler et al. 2013
Ping-Pong
ball
on the
moving
frame

19. Cosmic Rays : The Highest Energy Particles in the Universe : What is the Accelerator ?
Knee Energy
~1015 eV
E-3.0
Bellow Knee, Galactic Origin
Above Knee, Extra Galactic
LHC

20. Flatter Γ  Higher efficiency for the acceleration
North Rim
East Rim
What is an
injector to the
Fermi
accelerator ?
SN1006:
Synchrotron
Radiation =
Power-law with
index 　Γ
Flatter Γ  Higher efficiency for the acceleration
Γ vs kT North Rim vs East Rim
Koyama &Bamba 2006

21. Flatter Γ is from higher kT
Γ-map
kT-map
Higher
Flatter
Steeper
Lower
Flatter Γ is from higher kT
Injector is a high energy tail of hot plasma

22. Conclusion Space is better for the transient plasma than laboratory.
2. Using the transient plasma physics,
we have established the
Nucleosynthesis of stars and supper
novae.
Anti-equilibrium of temperature:
the Fermi acceleration is discovered in the SNR plasma

23. Thank you

24. log r (pc) log t (year) Rarefaction in an early phase
Canonical　Diffusive Shock Acceleration　
Emax～ (v/2000 km/s)(B/10μG) 1014 eV
< Knee Energy (1015 eV)
CSM
High density
ＩSM
Low density 1
log r　(pc)
log t (year)

25. Another big problem is missing energy
Kinematic energy (=1/2Mv2) of Ia and CC SN
are ~1051 erg. A large fraction should be converted to the thermal energy: kT = 3mv2/16
However observed thermal energy (kTe) is ~1049 erg
This large missing energy would be contained in protons and other ions (the ion temperature kTi).
But, no evidence is so far observed.
Space plasma proper problem: large scale low density plasma.
Solved by the observation of Tycho SNR

26. Te=TFe me/mFe , 10-5 at the reverse shock front (RS)
Then TFe  Te as time goes.
Question: How quick this energy transfer process.
Parameter β
β=10-5 (slow transfer)
(very rapid tarnsfer)
Free Expansion( v) RS X RS
1-ly

27. Energies of Kα & Kβ , and intensity ratio (Kα/Kβ ) are functions of Te and distribution of ion fraction.
These are determined by β and nt.
Simulations are right panels;
The results are,
n~2×10-24 g/cm3
β ~　0.01 (large
energy is still in ions)

28. Thank you again