Takashi Hosokawa ( NAOJ ) Daejeon, Korea Shu-ichiro Inutsuka (Kyoto) Hosokawa & Inutsuka, astro-ph/ also see, Hosokawa & Inutsuka, 2005, ApJ, 623, , ApJ, 646, , ApJ, 648L,131 Hosokawa, 2006, A&A, in press

Ionizing photons ( ) Dissociating photons ( ) Negative Feedback destroy molecular cloud and suppress star formation Positive Feedback shock front sweeps up H2 gas to trigger star formation V.S Radiative Feedback for Molecular Cloud (e.g., Whitworth 1979 ) (e.g., Elmegreen & Lada 1977) NGC3603 by HST CO Sh104 ; Deharveng et al. (2003) ( H2 → HI → HII ) ( compression of H2 )

Shock front sweeps up the ambient neutral medium. Reformation of molecules is triggered in the compressed layer. Karr & Martin (2003) HII CO 33pc Radiative Feedback for diffuse ISM Wisconsin H-alpha Mapper (WHAM) ; Haffner et al. (2003) Photoionization of the neutral medium : promising process to supply the diffuse warm ionized medium. ( HI → HII ) ( HI → H2 ) Negative Feedback Positive Feedback V.S W5 (e.g., Miller & Cox 1993 ) (e.g., Koyama & Inutsuka 2000 )

(1) HII regions expand in the molecular clouds (2) Expanding HII regions trigger the star formation and/or destroy the molecular cloud (3) HII region expands in the diffuse neutral medium Motivation THIS TALK HI H2H2 Hosokawa & Inutsuka, 2005, ApJ, 623, , ApJ, 646, 246 etc. In phases ( 3 ), what is the role of HII regions expanding in the neutral medium? 1.photoionization (HI→HII) 2. reformation of molecules (HI→H 2 ) Which is more efficient? Does the molecular formation occur?

continuity ： momentum eq. ： energy eq. ： equation of state ： Radiative transfer ： UV photon ( ) FUV photon ( ) freq. Dependent chemistry ： H + /H, O + /O, H/H 2, C + /CO (Nelson & Langer 1998) (Photoinization) (photodissociation) hydrodynamics : 2nd-order Godunov method Basic Equations 1D Radiation-Hydrodynamics Calculation 17 processes

Situation Study the physical/chemical structure of the shell Does molecular gas form from ambient neutral medium? Shock front Ionization front Cold Neutral Medium ( n~10/cc, T~100K ) Shell

Dynamical Evolution Snapshots Temperature Density Central star ： 41M sun, ambient medium ： CNM (n=10/cc) ( equilibrium state with typical FUV field ) Initial T Dense and cold shell is formed around the HII region density : n~1000/cc, temperature: T~30 K t=1Myr 3Myr 5Myr 9Myr7Myr

Shock front Ionization Front M-S life time H 2 are formed in the shell, but CO are hardly formed : Dark H 2 Intermediate gas phase between neutral medium and molecular clouds Accumulation of Molecules n CO /n H Z C n H2 /n H

Hunt of Predicted Gas Phase HI 21cm line emission C anadian G alactic P lane S urvey CGPS ; Taylor et al. (2003) galactic plane radio, IR angular resolution : about 1‘ distribution of HI, HII, CO, dust Channel Map Blue image:21cm emission, Red contour:CO HI Self-Absorption (HISA) ： absorption of colder HI against the emission by the warmer HI (T b ~100 K) Hunt the cold (T~a few ×10 K) HI

CGPS data in W5 HII region 21cm continuum (HII gas) T b =5K (bright) → 12.5K (dark) Image : 60μm dust emission Contour : 12 v LSR =-39.8 km/s  Ionized gas is surrounded with the dust shell.  Distribution of CO molecules show poor correlation with the dust shell.

CGPS data in W5 HII region HI 21cm v LSR =-39.8 km/s : T b =45K (bright) → 110K (dark)  Shell-like HISA feature is found around W5 HII region.  HISA feature overlaps with the dust shell. contour : 60μm dust emission

Summary We have studied the role of the HII region expanding in the diffuse neutral medium.  Numerical Calculation (in CNM) Cold (T~30K) and dense (n~1000/cc) shell is formed around HII region. H2 is formed in the shell, but CO is hardly formed. intermediate gas phase between the diffuse neutral medium and molecular clouds  Analysis with CGPS data ( in W5 HII region ) Shell-like HISA feature is found around ionized gas. The dust shell shows good correlation with the shell-like HISA. Distribution of CO molecules show poor correlation with both dust shell and HISA.