Inferring the physics of protoplanetary disc evolution from the irradiated Cygnus OB2 region - A comparison of viscous and MHD wind-driven scenarios

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Table 1

Summary of fiducial cases identified in Section 4.1 that are best able to reproduce disc fraction evolution and the $M_{disc} - {\dot{M}}_{acc, ⋆}$ ${M_{{\rm{disc}}}} - {{\dot M}_{{\rm{acc}}, \star }}$ relation in low and highly irradiated regions.

Scenario	$ℱ_{FUV}$ ${{\cal F}_{{\rm{FUV}}}}$	f_PAH	τ_acc,0
MHD wind-driven	$F_{FUV, 10 G_{0}}$ ${F_{{\rm{FUV}},10{{\rm{G}}_0}}}$	0.1	τ_acc,0,short
	$ℱ_{FUV,CygnusOB2}$ ${{\cal F}_{{\rm{FUV,CygnusOB2}}}}$	0.1	τ_acc,0,long
Viscous	$F_{FUV, 10 G_{0}}$ ${F_{{\rm{FUV}},10{{\rm{G}}_0}}}$	0.1	τ_acc,0,short
	$ℱ_{FUV,CygnusOB2}$ ${{\cal F}_{{\rm{FUV,CygnusOB2}}}}$	0.1	τ_acc,0,long

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