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

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 http://sci.esa.int/planck/ C, O, Si, Fe Q: when and where ? A: SN, SNR After14 Gys: Islands: Cosmos

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

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 !

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

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)

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)

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

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 2 3 1 RP

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

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). 10 11 12 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

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 9 10 11 12 Iron Ion Fraction Ionizing plasma We know the ion fraction from the spectrum , then we can obtain the abundances of each element

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)

Fujiwara, Teika (藤原定家） Meigetsuki (明月記）, Vol 52 Ia 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

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

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

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

Fermi Acceleration V=6000 km/s Ping-Pong ball on the moving frame SN1006 2003-4-09 2012-4-23 V=6000 km/s Winkler et al. 2013 Ping-Pong ball on the moving frame

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

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

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

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

Thank you

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) 1 2 3

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

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) -- 100 (very rapid tarnsfer) Free Expansion( v) RS X RS 1-ly

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)

Thank you again