Figure A3.
![The fried sub-grid that has fPAH, d = 0.5 and grain growth in the outer disc, depleting the wind of small grains. Each panel shows the mass-loss rate ($\log _{10}[\dot{M}]$, M⊙ yr−1) as a function of disc outer radius and outer surface density. The stellar masses are 0.1, 0.3, 0.6, 1.0, 1.5, and 3.0 M⊙ from top to bottom and the UV radiation field is 1, 10, 102, 103, 104, 105 G0 from left to right.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/526/3/10.1093_mnras_stad3054/1/stad3054figa3.jpeg?Expires=1749645223&Signature=SqjvhWiqTL7Y7xM3a~-n4BRGi3Xa5zOkwZUdA1X25cPdsh0YcNF1DEXpqqt2HsjO2KSD3VdCAFnb8lKttBw9hTTbzkg4GNhOjKEZp5V6ycdK0d3oSyAnHsEEN~n4t2fkOxa7etHpFDbT0UPbYhqF-CdMAUgpIPp27aa9yqrnf6kqb0jIF7WO2TTgv~La1cATU0fh85q1y-6pp~P1xQQlpSu7sk0W7XiPveDaNRC3XGeapf9K947QjogL0~r8~KsLCYVnFTHgBQQrX9cizgjPTXiCh24d2HbzfF0TfyLeAnJMfhmsY6yCYRMOqgp658if-34o65dF5x3vxzZOe4ZWPg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
The fried sub-grid that has fPAH, d = 0.5 and grain growth in the outer disc, depleting the wind of small grains. Each panel shows the mass-loss rate (|$\log _{10}[\dot{M}]$|, M⊙ yr−1) as a function of disc outer radius and outer surface density. The stellar masses are 0.1, 0.3, 0.6, 1.0, 1.5, and 3.0 M⊙ from top to bottom and the UV radiation field is 1, 10, 102, 103, 104, 105 G0 from left to right.
