The origin of abundance gradients in the Milky Way: the predictions of different models

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Table 2:

Models successes and failures. The second column shows the successes, while the third column indicates the failures.
Model	Successes	Failures
1	good agreement for the $SFR/SFR_{\odot }$	$\Sigma_{\rm gas}$ not reproduced in the outer Galactic disk
		abundance gradients completely flat
2	good agreement for the $SFR/SFR_{\odot }$	too low $\Sigma_{\rm gas}$ in the inner disk
	increased slope of the gradients in the outer disk	abundance gradients too flat in the inner disk
3	good agreement for the $SFR/SFR_{\odot }$	too low $\Sigma_{\rm gas}$
	$\Sigma_{\rm gas}$ increases in the outer part of the disk	abundance gradients too flat in the inner disk
	slope of abundance gradients more pronunced in the outer disk
4	good agreement for the $SFR/SFR_{\odot }$	$\Sigma_{\rm gas}$ not reproduced in the outer Galactic disk
		abundance gradients increase along the galactic disk
5	good agreement for the $SFR/SFR_{\odot }$	$\Sigma_{\rm gas}$ not reproduced in the outer Galactic disk
	slope of abundance gradients more pronunced in the inner disk	abundance gradients increase in the outer Galactic disk
6	good agreement for the $SFR/SFR_{\odot }$	$\Sigma_{\rm gas}$ increases along radius
	abundance gradients in good agreement with the observed data
7	good agreement for the $SFR/SFR_{\odot }$	$\Sigma_{\rm gas}$ too low in the inner part of the Galactic disk
	abundance gradients in good agreement with the observed data

Source LaTeX | All tables | In the text

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