Table 1: Summarised descriptions of the main GDCE model parameters.
Parameter Short description

k Small positive integer used to parametrize the mass

infall rate F.

$\Delta$ Time after the start of stellar formation, after which

delayed-production elements start being ejected.

$\omega$ Efficiency of interstellar gas conversion into stars.

u₀ Arbitrary parameter in the mass infall rate F.

u₁ Time of transition between simple and Clayton

model, multiplied by $\omega$ .

u₂ Time when residue formation becomes efficient,

multiplied by $\omega$ .

$u_{T_{{\rm G}}}$ Age of the Galactic disk, multiplied by $\omega$ .

j IMF slope corresponding to residues that evaporate.

$\Gamma$ Dilution of ISM due to residue evaporation.

$f_{1~{\rm Fe}}$ Fe yield divided by Fe solar abundance today

(prompt contribution).

$f_{2~{\rm Fe}}$ Fe yield divided by Fe solar abundance today

(delayed contribution).

$f_{{\rm total~Eu}}$ Eu yield divided by Eu solar abundance today.

$f_{1~{\rm Eu}}$ Prompt contribution of $f_{{\rm total~Eu}}$ .

$f_{2~{\rm Eu}}$ Delayed contribution of $f_{{\rm total~Eu}}$ .

$f_{1~{\rm Th}}$ Th yield divided by Th solar abundance today.

$\chi$ Relation between $f_{1~{\rm Th}}$ and $f_{{\rm total~Eu}}$ .

**Table 1:** Summarised descriptions of the main GDCE model parameters.
Parameter	Short description
k	Small positive integer used to parametrize the mass
	infall rate F.
$\Delta$	Time after the start of stellar formation, after which
	delayed-production elements start being ejected.
$\omega$	Efficiency of interstellar gas conversion into stars.
u₀	Arbitrary parameter in the mass infall rate F.
u₁	Time of transition between simple and Clayton
	model, multiplied by $\omega$ .
u₂	Time when residue formation becomes efficient,
	multiplied by $\omega$ .
$u_{T_{{\rm G}}}$	Age of the Galactic disk, multiplied by $\omega$ .
j	IMF slope corresponding to residues that evaporate.
$\Gamma$	Dilution of ISM due to residue evaporation.
$f_{1~{\rm Fe}}$	Fe yield divided by Fe solar abundance today
	(prompt contribution).
$f_{2~{\rm Fe}}$	Fe yield divided by Fe solar abundance today
	(delayed contribution).
$f_{{\rm total~Eu}}$	Eu yield divided by Eu solar abundance today.
$f_{1~{\rm Eu}}$	Prompt contribution of $f_{{\rm total~Eu}}$ .
$f_{2~{\rm Eu}}$	Delayed contribution of $f_{{\rm total~Eu}}$ .
$f_{1~{\rm Th}}$	Th yield divided by Th solar abundance today.
$\chi$	Relation between $f_{1~{\rm Th}}$ and $f_{{\rm total~Eu}}$ .

Source LaTeX | All tables | In the text

	1 Introduction
	2 Nucleocosmochronological analysis
	3 Conclusions
	References