Figure A2.
![The fried sub-grid that has fPAH, d = 1.0 and ISM-like dust in the outer disc. 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/stad3054figa2.jpeg?Expires=1749645621&Signature=JDinUZPEaYDsIeSLAv3VYkuUhes96Hvb50palPnYMxiL-h2DazB60uUKt9tL2YdQAcdIdX-Cr2iS5KAgSENBWZz7~XH53A-TM1JPL8HLAp2t2eDpjYKfAlzbTxvZnWoMcZNBya3dR3JgW4S2suRP3fOLmzOckXZ5cG9kZ9p8zdyFYYX-c9uwtEYclsKZi5nAB9bW-fmufqgpzYhdldDzN~6hQOeDGt721-tYDa~rH6yNCny~PCbBRoSIQiAsCLff0a1RNVNMuVfSxwkZnEonGrlAlk58FN6svqtWYrc2gsCvyXQlUQPYtj1h7CIOqCUITJdmbScvac4vaKdoXEQ1zQ__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
The fried sub-grid that has fPAH, d = 1.0 and ISM-like dust in the outer disc. 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.
