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1 Dusty Clumpy Torus (AGN) (BH) BH 3 BH 1 AGN () 1/3 (i) (ii) Kawaguchi(2003) 1/5 (iii) AGN : T. Kawaguchi & M. Mori, ApJL, 2010, 724, T. Kawaguchi & M. Mori, ApJ, 2011, 737,
2 Toshihiro KAWAGUCHI (Tsukuba U, Japan) (Kawaguchi & Mori 2010, ApJL; 2011 ApJ) 0. clump, clump 1. (sublimation) ~ ~ (Active Galactic Nuclei, AGNs): type 1 object Dusty Clumpy Torus / /X Accretion Disk type 1.5/1.8/1.9 Supermassive Black Hole (Dusty Clumpy Tori): type size: ~ 100pc ALMA, TMT ~ 0.1pc 10
3 0. AGN clump (Krolik & Begelman1988) 12AGN-to- torus (aspect ratio = H/r ~ 1) (~~100km/s) (~1500K) Dust torus smooth clumpy (clump1500k, clump) clumpy opacity (Honig & Beckert 07) : clumpy torus clump (Geballe et al. 2006; Shirahata et al. 2007) clump (Geballe et al. 2006; Shirahata et al. 2007) = =?
4 0. Clumps in Dusty Torus (1/2) (Vollmer, Beckert & Duschl 2004; Honig & Beckert 2007) BH r Cloud radius: R cloud M BH Conditions # self grav thermal pressure M cloud M Jeans # self grav tidal force by central BH R cloud R tidal marginal clumps c s r Rcloud 3 G M M cloud c 3G 2 s R 1. 5 BH cloud pc 20M cs r 3 k m / s 1 pc 3 cs 3 k m / s 1. 5 r 1 pc M M 1. 5 B H M M BH Clumps in Dusty Torus (2/2) (TK+Mori 11) R cloud, M cloud N H 1 6 n R g / c m cloud r 1 pc 5 T c m M M 2 cs r 3 k m / s 1 pc A V BH mag, 8 ( n c m M M 180mag (cf. Krolik+Begelman88~ 1/10) (Honig+06 V ~ 40 ) V BH 1400, A 0. 5 K 3 ) SED, silicate feature clump ~ 1/ volume filling factor ~ 0.03 clump ~ (Nenkova+08)
5 1. AGN dust torus : clump F_lambda * Kobayashi+1993 : observed : observed power law (accretion disk) (3bump) : fit 1500K ~ sublimation () ( = ) L 4r 2 a 2 T 4 (um) * BH (a: ()) 4 a 2 r subl p c 10 ~ L e r g / s 0. 5 T subl 1500 K ~months () 2 1. sublimation() 1/3 (Oknyanskij+Horne 01; Kishimoto+07; Nenkova+08) optical NIR (Minezaki+04) () (Data from Suganuma+06) (Barvainis 1987)
6 2.0 () 1AGN clumpy torus clump1500k clump (Honig et al. 2006) 2.1: () Flux cos (1 + 2 cos ) (limb darkening) ( 21.5) I2/5 &
7 cos= Face-on / Eage-on Face-on Edge-on frequency [Hz] (Laor & Netzer 89; (TK & Mori 11) Sun & Malkan 89; Hubeny+00) (cf. BLR) (TK & Mori 10,11). 2. (TK & Mori 10) (H/r)=1 z / R sub,0 BH+ R sub,0 flux r / R (1) BH sub,0 (2), () () =88(x sub )(0.1 x r sub,0 )
8 = TK, Pierens, Hure 2004 (TonS180) (R SG ~ 3000R Sch ~ 0.002pc) R SG Dusty Torus () 10R SG (lower limit, though) ~ 100R SG (1) (TK & Mori 2010) =88 ring 3. (transfer function) (t) (Blandford & McKee 82) ring 2 thin shell thick shell (Netzer 1990) 0 - Reprocess (t) convolution (t): : -- : (t)
9 3. (t) (t) (1) 1(; obs ) emissivity() clump () ( = ) (ESO) (Schartmann 07) (5/9) 1AGN (1.*)
10 3. (t) () (TK & Mori 10) (transfer function) =0.37 obs =25deg, R subl,0 ring 1/3(BH. ) 0deg 4. obs obs (11.*) (t) & & obs 1.8, 1.9? clump clump
11 obs - () - () : (8/9) : : (TK & Mori 11) ()
12 : (8/9) : : (TK & Mori 11) () () () : (8/9) : : (TK & Mori 11) : ()
13 : (8/9) : : (TK & Mori 11) () selected AGN selection bias 5. : (; Fukue 00, Madau 88) (ESO) (TK) AGN (NLS1, NLQ)? TonS180(TK+04), Ark564, Jiang+10 (cf. Hao+2010) F Ark564: no 3µm-bump (Rodriguez-Ardila & Mazzalay 2006) 1µm 5µm
14 ~800 AGN MRN: (Laor & Draine 1993) M/(L Edd /c 2 ) = 1, 10, 100, 1000 Super-Eddington Sub-Eddington () (H/r) max ) (~4-5K) BH (r Sch ) (TK 2003)
15 4. () down (1/5) 100 Super-Eddington accretion m = 10 1 Sub-Eddington (standard disk) 1000 (larger shade) - BH () : selection bias - ()
PowerPoint Presentation
原始活動銀河核における 巨大ブラックホール ( とバルジ ) の成長 川口俊宏 ( 国立天文台 光赤外研究部 ) 臨界降着率 (Eddington 降着率 ; M Edd =16 L Eddington /c 2 ): 放射圧 = 重力注意 : 球対称時の限界降着率 - Super-Eddingtonガス降着による巨大ブラックホールの成長 - 共進化 : バルジの成長を観測する計画の紹介 - 2 型
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1 17 object 1 observation 17.1 X electromagnetic wave photon 1 = c (17.1) c =3 10 8 ms ;1 m mm = 10 ;3 m m =10 ;6 m nm = 10 ;9 m 1 Hz 17.1 spectrum radio 2 infrared 3 visual light optical light 4 ultraviolet
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1 22 22.1 atomic line spectrum emission line absorption line atom proton neutronnuclei electron Z atomic number A mass number neutral atom ion energy level ground stateexcited state ionized state 22.2
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