This paper investigates the star formation rate ( SFR ) in the Solar neighbourhood .
First , we build the local age distribution function ( ADF ) with an updated sample of 442 star clusters located at less than 1 kpc from the Sun .
Next , we define the SFR , compute the individual mass evolution of a population of artificial clusters covering the broad range of parameters observed in actual clusters , and assume 100 M _ { \odot } as the low-mass limit for effective cluster observation .
This leads to a simulated ADF , which is compared to the low-noise Solar neighbourhood ADF .
The best match corresponds to a non-constant SFR presenting two conspicuous excesses for ages \leq 9 Myr and between 220 - 600 Myr ( the local starburst ) .
The average formation rate is \overline { SFR } \approx ( 2500 \pm 500 ) \mbox { $ \mbox { $ M _ { \odot } $ } Myr ^ { -1 } $ } , corresponding to the average surface formation rate \overline { \mbox { $ \Sigma _ { SFR } $ } } \approx ( 790 \pm 160 ) \mbox { $ \mbox { $ M _ { % \odot } $ } Myr ^ { -1 } kpc ^ { -2 } $ } .
These values are consistent with the formation rate inferred from embedded clusters ( ECs ) , but much lower ( \la 16 \% ) than that implied by field stars .
Both the local starburst and the recent star formation period require SFR \sim 2 \times \overline { SFR } to be described .
The simulations show that 91.2 \pm 2.7 \% of the clusters created in the Solar neighbourhood do not survive the first 10 Myr , which is consistent with the rate of EC dissolution .