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We address the question of whether the formation of high‐mass stars is similar to or differs from that of solar mass stars through new molecular line observations and modelling of the accretion flow around the massive protostar IRAS20126+4104. We combine new observations of NH 3 (1,1) and (2,2) made at the Very Large Array (VLA), new observations of CH 3 CN(13–12) made at the Submillimeter Array, previous VLA observations of NH 3 (3,3) and NH 3 (4,4) and previous Plateau de Bure observations of C 34 S(2–1), C 34 S(5–4) and CH 3 CN(12–11) to obtain a data set of molecular lines covering 15–419 K in excitation energy. We compare these observations against simulated molecular line spectra predicted from a model for high‐mass star formation based on a scaled‐up version of the standard disc–envelope paradigm developed for accretion flows around low‐mass stars. We find that in accord with the standard paradigm, the observations require both a warm, dense, rapidly rotating disc and a cold, diffuse infalling envelope. This paper suggests that accretion processes around  10  M ⊙   stars are similar to those of solar mass stars.

The standard model of star formation applied to massive stars: accretion discs and envelopes in molecular lines