Cloudcloud collision Habe Ohta 1992 Takahira2014 Anathpindika2012 3

Cloud-cloud collision Habe & Ohta 1992 Takahira+2014 Anathpindika+2012 3

Inoue & Fukui (2013) p 6 cores are formed in the fiducial model. l 238, 59, 5. 3, 3. 6, 2. 7, 1. 0 Msun z [ pc ] 238 Msun Closeup view of the most massive core y [ pc ] Inoue & Fukui 2013 l Large effective Jeans mass is due to strong magnetic field and turbulence. Large mass accretion rate: d. M/dt = 4 × 10 -3 Msun/yr for 238 Msun core = 5 × 10 -4 Msun/yr for 59 Msun core

巨大星団での分子雲衝突 Westerlund 2 NGC 3603 • 銀河系の既知の若い巨大 星団は８例 • うち星雲が付随する星団 ４例の全てで２個の分子 雲が付随 大質量星一般では？ RCW 38 [DBS 2003]179 Age [Myr] Log. M* [Msun] Size [pc] 分子雲 NGC 3603 2. 0 4. 1 0. 7 ○ Westerlund 2 2. 0 4. 2 0. 8 ○ [DBS 2003]179 2 -4 3. 8 0. 5 ○ Westerlund 1 3. 5 4. 0 1. 0 × Trumpler 14 2. 0 4. 5 0. 5 -- Arches 2. 0 4. 3 0. 4 × Quintuplet 4. 0 2. 0 × RCW 38 <1. 0 -- 0. 8 ○ cluster 8

三裂星雲(M 20) Torii et al. 2011 • • • The Trifid Nebula(M 20) D ~ 1. 7 kpc (Lynds & Oneil 85) Open cluster with M* ~ 500 Mo Very young: ~ 0. 3 Myrs (Cernicharo+98） an exciting O 7. 5 star (~20 Mo) Low mass star formation is on-going - Spitzer young stellar objects （ Rho+06) - Cold dust cores（Cernicharo+98; Lefloch+08) • Previous molecular line studies are focused on the low mass star formation. (Cernicharo+98; Lefloch+08)

三裂星雲(M 20) Torii et al. 2011 • • • The Trifid Nebula(M 20) D ~ 1. 7 kpc (Lynds & Oneil 85) Open cluster with M* ~ 500 Mo Very young: ~ 0. 3 Myrs (Cernicharo+98） an exciting O 7. 5 star (~20 Mo) Low mass star formation is on-going - Spitzer young stellar objects （ Rho+06) - Cold dust cores（Cernicharo+98; Lefloch+08) • Previous molecular line studies are focused on the low mass star formation. (Cernicharo+98; Lefloch+08) (Rho+08)

三裂星雲(M 20) Torii et al. 2011 Image: HST(Hα, [SII], [OIII]) 11

RCW 120 (Spizter bubble S 7) • 距離 ~ 1. 3 kpc (Rodgers+1960) • 典型的なSpitzerバブル • 綺麗な 8μmリング構造 • 内部にO 8型星とHII領域 • リング上にYSOが集中 Green : 8 um Red : 24 um Blue : Hα × : exciting star ○ : Class Ⅰ △: Class Ⅱ 13

膨張モデルの理論計算（１次元計算：一様密度） • Zavagno et al. 2007 • RCW 120の再現 • 1 D numerical calculations (Hosokawa & Inutsuka 2005; 2006) • Collect & Collapse (Elmegreen & Lada 1977) • RCW 120(r~1. 7 pc)の形成タイ ムスケール = 0. 4 Myr (Zavagno+2007) • 膨張速度Vexp ~ 4 km/s Zavagno et al. (2007) 19