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Galactic diffuse

Galactic diffuse. 「 Thermal emission from SNRs/SNe 」 Miyata 35min 「 Non-thermal emission from SNRs/SNe 」 Ozaki 15min 「ミリ秒パルサーの X 線観測」 Torii 15min 「高エネルギーガンマ線源の X 線対応天体探査」 Torii 10min 「超新星残骸と関連したパルサー、 AXP 、 SGR など」 Torii 15min 「銀河円盤 / 銀河中心領域： diffuse 編」 Kokubun 15min

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Galactic diffuse

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  1. Galactic diffuse • 「Thermal emission from SNRs/SNe」 Miyata 35min • 「Non-thermal emission from SNRs/SNe」 Ozaki 15min • 「ミリ秒パルサーのX線観測」 Torii 15min • 「高エネルギーガンマ線源のX線対応天体探査」 Torii 10min • 「超新星残骸と関連したパルサー、AXP、SGRなど」 Torii 15min • 「銀河円盤/銀河中心領域：diffuse 編」 Kokubun 15min • 「銀河円盤/銀河中心領域：discrete sources 編」 Yamauchi 15min

  2. Refereed Papers on Galactic diffuse sources • Thermal emission 26 • Non-thermal emission 6 • Pulsar 19 • SGR 3 • Supernova 3 • Galactic center, ridge 4 PhD Thesis on Galactic diffuse sources • Thermal emission 5 (+2) • Non-thermal emission 2 • Pulsar 3 • SGR 0 • Supernova 2 • Galactic center,ridge 4 (+1)

  3. Papers on Thermal Emission • Hiroshi Tsunemi, Emi Miyata, Bernd Aschenbach,Junko Hiraga, Daisuke Akutsu, Overabundnace of Calcium in the young SNR RX J0852-4622: evidence of over-production of 44Ti • Bamba, A. et al. Deep X-Ray Observations of Supernova Remnants G359.1-0.5 and G359.0-0.9 with ASCA • Hwang,Una, Petre,Robert, Hughes,JohnP.The X-Ray Line Emission from the Supernova Remnant W49B • Miyata,Emi, Tsunemi,Hiroshi,The Radial Structure of the Cygnus Loop Supernova Remnant: Possible Evidence of a Cavity Explosion • Tsunemi,Hiroshi, Miyata,Emi, Aschenbach,Bernd, Spectroscopic Study of the Vela-Shrapnel • Chen,Yang, Sun,Ming, Wang,Zhen-Ru, Yin,Q.F.An Analysis of the X-Ray Emission from the Supernova Remnant 3C 397 • Kinugasa,Kenzo, Tsunemi,Hiroshi, ASCA Observation of Kepler's Supernova Remnant • Yamauchi,Shigeo, Koyama,Katsuji, Tomida,Hiroshi, Yokogawa,Jun, Tamura,Keisuke, ASCA Observations of the Supernova Remnant G156.2+5.7 • Hughes,JohnP., Hayashi,Ichizo, Koyama,Katsuji, ASCA X-Ray Spectroscopy of Large Magellanic Cloud Supernova Remnants and the Metal Abundances of the Large Magellanic Cloud • Rho,Jeonghee, Petre,R., Mixed-Morphology Supernova Remnants • Harrus,IlanaM., Hughes,JohnP., Slane,PatrickO., Study of the Composite Supernova Remnant MSH 11-62 • Miyata,Emi, Tsunemi,Hiroshi, Kohmura,Takayoshi, Suzuki,Seiji, Kumagai,Shiomi, Metal-Rich Plasma at the Center Portion of the Cygnus Loop • Kinugasa,Kenzo, Torii,Ken'ichi, Tsunemi,Hiroshi, Yamauchi,Shigeo, Koyama,Katsuji, Dotani,Tadayasu, Discovery of X-Ray Emission from a Radio Supernova Remnant G352.7-0.1 • Hwang,Una, Hughes,JohnP., Petre,Robert, The X-Ray Iron Emission from Tycho's Supernova Remnant • Folgheraiter,E.L., Warwick,R.S., Watson,M.G., Koyama,K., G 32.1-0.9 - A new Galactic supernova remnant? • Vink,Jacco, Kaastra,JelleS., Bleeker,JohanA.M., X-ray spectroscopy of the supernova remnant RCW 86. A new challenge for modeling the emission from supernova remnants • Gotthelf, E. V.; Vasisht, G., Kes 73: A Young Supernova Remnant with an X-Ray--bright, Radio-quiet Central Source • Guo,Zhiyu, Burrows,DavidN., ASCA Observations of the Supernova Remnant VRO 42.05.01 • Hwang,U., Gotthelf,E.V., X-Ray Emission-Line Imaging and Spectroscopy of Tycho's Supernova Remnant • Blanton,ElizabethL., Helfand,DavidJ., ASCA Observations of the Composite Supernova Remnant G29.7-0.3 • Vink,J., Kaastra,J.S., Bleeker,J.A.M., A new mass estimate and puzzling abundances of SNR Cassiopeia A. • Fujimoto,Ryuichi, Tanaka,Yasuo, Inoue,Hajime, Ishida,Manabu, Itoh,Masayuki, Mitsuda,Kazuhisa, Sonobe,Takashi, Tsunemi,Hiroshi, Murakami,Hiroyuki, Koyama,Katsuji, Hayashi,Ichizo, Ikeda,Kazuaki, Rasmussen,Andy, Ricker,George, Becker,ChristopherM., ASCA Observation of the Supernova Remnant W49B • Hughes,JohnP., Hayashi,Ichizo, Helfand,David, Hwang,Una, Itoh,Masayuki, Kirshner,Robert, Koyama,Katsuji, Markert,Thomas, Tsunemi,Hiroshi, Woo,Jonathan, ASCA observations of the Large Magellanic Cloud supernova remnant sample: Typing supernovae from their remnants • Petre, R et al. The broad Band X-ray Spectrum of SN 1978K and Two Other Luminous X-ray sources in the Spiral Galaxy NGC1313 • Kohmura, Y. et al. Detection of X-rays from SN 1993J with ASCA • Holt,StephenS., Gotthelf,EricV., Tsunemi,Hiroshi, Negoro,Hitoshi, ASCA observations of Cassiopeia A • Hayashi,Ichizo, Koyama,Katsuji, Ozaki,Masanobu, Miyata,Emi, Tsumeni,Hiroshi, Hughes,JohnP., Petre,Robert, X-ray spectroscopy of SNR E0102-72 with the ASCA satellite • Miyata,Emi, Tsunemi,Hiroshi, Pisarski,Ryszard, Kissel,SteveE., The plasma structure of the north-east rim of the Cygnus Loop as observed with ASCA

  4. <700eV Supernovae • Extragalactic supernovae • SN1978K (NGC1313) • detected with ROSAT, ASCA (not Einstein) • type II SN in origin • spectrum: power-law (G~2.2) or thermal (kT=3keV,Z=0.2) • shock acceleration ? pulsar emission ? reverse shock ?

  5. SN1987A (LMC) • X-ray intensity increases during ASCA observations • SIS spectrum can be better fitted with NEI model logt~9.8

  6. 8days! • SN1993J • SN1993J は超新星爆発後 8 日後から観測できた。 • 鉄輝線が観測された。ライトカーブから reverse shock 起源  ミキシング ! DE > DE(optical)  6.4 keV の混入? • 自己相似解を用いて reverse shock & blast wave からの輻射を説明することができた。また reverse shock が晴れ上がるようすがみえた • 1995 年以後、「フロントショック」「リバースショック」などは暗くなったが、パルスサーチなどが継続して行われている。 • 2000年現在は、超新星爆発の内側が見えてくる、いわゆる「晴れ上がり」の時期に相当すると予測されている。 (shigeyama et.al 「1998年以後」) • この時、超新星内部で何が起きているかは謎が多いが、X線が観測されるとすれば、以下のようなことが考えられる。 • 1. 中心に新しいパルサーが誕生のパルス • 2. パルスではなくても、パルサーにより照射されたejecta からの輻射 • この「晴れ上がり」の観測は、超新星爆発と、新しい超新星残骸の間をつなぐ重要なデータとなる。 • upper limit でも、「爆発 7 年後」の輻射の強度を知ることは重要。

  7. Elemental abundance ejecta  type of SN Cas-A, Kepler, Tycho, W49B, 3C397, RCW86, Kes73, G156, Cygloop, Vela 44Ti source: RXJ0852 LMC SNRs ISM  cosmic abundance, metallicity gradient RCW86, VRO 42.05.01, G352.7, Puppis-A, Cygloop LMC SNRs CSM  type of SN RCW86, Cygloop spatial distribution Cas, Kepler, W49B, RCW86, Cygloop Plasma structure Non-equilibrium Ionization almost all SNRs are ionizing Thermal equilibrium not yet confirmed equilibrium or not Shock structure (Interaction with interstellar cloud) Evaporation 3C397, W44, G32.1 Reflection shock Cygloop Dynamics Doppler velocity mapping of Cas-A Plasma code Puppis-A, Cygloop, Kepler consider thermal structure (LMC SNRs) Topics of Thermal Emission from SNRs

  8. Elemental abundance • ejecta  type of SN • Cas-A, Tycho, Kepler, W49B, 3C397, RCW86, Kes73, RXJ0852, G156, Cygloop, Vela, SMC/LMC SNRs Cas-A Tycho Kepler W49B 3C397 Kes73 G156 (center) Cygloop (center) E0102 N49 N63 N132D

  9. Elemental abundance • Vela fragments

  10. Elemental abundance • Cygnus Loop

  11. Elemental abundance • Cygnus Loop

  12. Nucleosynthesis of SNe Ia II (15M ) Nomoto et al. (1984) Thielemann et al. (1993)

  13. Determination of SN Type Tycho Kepler W49B

  14. Determination of SN Typecase of Cygnus Loop

  15. Nucleosynthesis of SNe Ia II (15M ) Nomoto et al. (1984) Thielemann et al. (1993)

  16. Determination of SN Typecase of Cygnus Loop

  17. detected by COMPTEL • Elemental abundance • 44Ti source: RXJ0852-4622 44Ti – (t1/2~60yr)  44Sc – (t1/2~3.9hr) 44Ca 1157 keV 68 & 78 keV Ca abundance 8±5 Si<1, S<0.2 Tsunemi et al (2000)

  18. RCW86 • Elemental abundance • ISM  cosmic abundance, metallicity gradient • RCW86, VRO 42.05.01, G352.7, Puppis-A, Cygloop • LMC SNRs G352.7 VRO42.05.01 N23 N49

  19. North-west North-east Eastern knot West East hook • Elemental abundance • ISM  cosmic abundance, metallicity gradient • Puppis-A Tamura PhD

  20. Elemental abundance • CSM  type of SN • RCW86, Cygloop • spatial distribution • Cygloop Miyata & Tsunemi (1999)

  21. E0102 • Plasma structure • Non-equilibrium Ionization • almost all SNRs are ionizing • Thermal equilibrium • not yet confirmed equilibrium or not Hayashi et al (1993) Miyata PhD

  22. Si S • G359.1-0.5 • radio: shell, X-ray: center-filled 1.86 keV  He-like Si 2.61 keV  H-like S  two components exists ! 0.6keV for Si, 4.4keV for S Bamba et al. (2000)

  23. Si Fe ASCA discovered, but not yet published • Shock structure (Interaction with interstellar cloud) • Evaporation • 3C397, W44, G32.1 • Reflection shock • Cygloop • Dynamics • Doppler velocity mapping of Cas-A

  24. Cas-A observed with Chandra Hwang et al. (2000)

  25. Remaining Problems • Low cosmic abundance • ASCA can determine only relative abundance • To determine absolute value, need to detect C, N, O emission lines • Some hints are to consider the thermal structure of remnant • Plasma code • need more resolving power than ASCA/SIS • Chandra emission line project • no need further ASCA observations • no need further ASCA observations

  26. Remaining Problems • Thermal equilibrium • Several methods

  27. Targets for AO-8 (1) Bulge 10ksX8 + 20ksX2 = 120ks 国分/金田 (2) Flux-limited radio SNRs 30ks X 6 = 180ks 鳥居 (3) GeV 天体 40ks X 5=200ks 河合 total: 500ks

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