  In this paper we describe the global on-sky calibration strategy of the
LSPE-Strip instrument. Strip is a microwave telescope operating in the Q- and
W-bands (central frequencies of 43 and 95 GHz respectively) from the
Observatorio del Teide in Tenerife, with the goal to observe and characterise
the polarised Galactic foreground emission, and complement the observations of
the polarisation of the cosmic microwave background to be performed by the
LSPE-SWIPE instrument and other similar experiments operating at higher
frequencies to target the detection of the B-mode signal from the inflationary
epoch of the Universe. Starting from basic assumptions on some of the
instrument parameters (NET, 1/f noise knee frequency, beam properties,
observing efficiency) we perform realistic simulations to study the level of
accuracy that can be achieved through observations of bright celestial
calibrators in the Strip footprint (sky fraction of 30 %) on the determination
and characterisation of the main instrument parameters: global and relative
gain factors (in intensity and in polarisation), polarisation direction,
polarisation efficiency, leakage from intensity to polarisation, beams, window
functions and pointing model.
