Dynamical effects of the radiative stellar feedback on the H I-to-H2 transition

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Table 1

Physical parameters of a sample of PDRs illuminated by O stars.

Source	G₀	n_H	n_HII	d_star	Exciting star	G₀∕n_H	S_EUV∕S_FUV	τ_EUV	v_IF
	(Habing)	(cm⁻³)	(cm⁻³)	(pc)	(T_eff, spec. type)	(cm³)			(km s⁻¹)
California	16[6-32] ⁽²⁾ ^(†)	10³–10⁴ ⁽²⁾	0.1–5 × 10¹ ⁽³⁾	7.0 ⁽²⁾	37 000 K O7.5III ⁽²⁾	2.0 × 10⁻³	0.74 ⁽¹⁾	0.89	9.3 × 10⁻³
Horsehead	50[25-93] ⁽²⁾ ^(†)	10⁴–10⁵ ⁽²⁾	1–3.5 × 10² ⁽⁴⁾	3.5 ⁽⁵⁾	33 000 K O9.5V ⁽²⁾	6.4 × 10⁻⁴	0.35 ⁽¹⁾	3.99	9.5 × 10⁻⁴
Orion Bar	20 000 ⁽⁶⁾	10⁵ ⁽⁶⁾	2.5 × 10³ ⁽⁷⁾	0.30 ⁽⁷⁾	39 000 K O5.5V-O6V ⁽⁷⁾	0.2	0.94 ⁽¹⁾	3.80	0.79
Carina	5 000 ⁽⁸⁾ ^(†)	10⁵ ⁽⁸⁾	10² ⁽⁹⁾	2.0 ⁽⁸⁾	–	0.1	~1	1.01	0.58
S 106	8 × 10⁴ ⁽¹⁰⁾ ^(†)	3.1 × 10⁵ ⁽¹⁰⁾	1.5–6 × 10³ ^(10,11)	0.44 ^(10,12)	O7–9 ⁽¹⁰⁾	0.52	0.38 ⁽¹⁾	8.35	1.3
M 17	0.5–4 × 10⁴ ⁽¹³⁾ ^(†)	2 × 10⁷ ⁽¹³⁾	700 ^(14,15)	1.9 ⁽¹⁵⁾	O4 ⁽¹⁶⁾	2.3 × 10⁻³	1.18 ⁽¹⁾	6.73	1.5 × 10⁻²
IRAS 23133+6050	8 × 10⁴ ⁽¹⁰⁾ ^(†)	3.1 × 10⁵ ⁽¹⁰⁾	2 × 10³ ^(10,12)	0.1 ^(10,17)	O8.5–9.5 ⁽¹⁰⁾	0.52	0.24 ⁽¹⁾	1	0.73

Notes. G₀ is the FUV radiation field, n_H the PDR density, n_HII the H II region density, d_star the distance between star and PDR, the stellar temperature and type, the G₀ ∕n_H ratio, S_EUV ∕S_FUV the star UV emission rate ratio, τ_EUV the dust optical depth in the H II region, and v_IF the deduced ionization front velocity. ^(†)Free-space G₀ values given in the cited articles have here been converted to G₀ values at the cloud surface.

References. ⁽¹⁾Diaz-Miller et al. (1998), ⁽²⁾Habart et al. (2011), ⁽³⁾Boulanger et al. (1988), ⁽⁴⁾Compiègne et al. (2007), ⁽⁵⁾Schirmer et al. (2020), ⁽⁶⁾Joblin et al. (2018), ⁽⁷⁾Salgado et al. (2016), ⁽⁸⁾Wu et al. (2018), ⁽⁹⁾Harper-Clark & Murray (2009), ⁽¹⁰⁾Stock et al. (2015), ⁽¹¹⁾Israel & Felli (1978), ⁽¹²⁾Noel et al. (2005), ⁽¹³⁾ Sheffer & Wolfire (2013), ⁽¹⁴⁾ Watson et al. (1981), ⁽¹⁵⁾ Stutzki et al. (1988), ⁽¹⁶⁾ Hoffmeister et al. (2008), ⁽¹⁷⁾ Martín-Hernández et al. (2003).

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