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The tidal disruption of a star by a supermassive black hole can result intransient radio emission. The electrons producing these synchrotron radioflares could either be accelerated inside a relativistic jet or externally byshocks resulting from an outflow interacting with the circumnuclear medium.Until now, evidence for the internal emission mechanism has been lacking;nearly all tidal disruption flare studies have adopted the external shock modelto explain the observed properties of radio flares. Here we report a resultthat presents a challenge to external emission models: we discovered across-correlation between the soft X-ray (0.3-1 keV) and 16 GHz radio flux ofthe tidal disruption flare ASASSN-14li. Variability features in the X-ray lightcurve appear again in the radio light curve, but after a time lag of about 13days. This demonstrates that soft X-ray emitting accretion disk regulates theradio emission. This coupling appears to be inconsistent with all previousexternal emission models for this source but is naturally explained if theradio emission originates from a freely expanding jet. We show that emissioninternal to an adiabatically expanding jet can also reproduce the observedevolution of the radio spectral energy distribution. Furthermore, both thecorrelation between X-ray and radio luminosity as well as our radio spectralmodeling imply an approximately linear coupling between the accretion rate andjet power.

Discovery of a time lag between the soft X-ray and radio emission of the tidal disruption flare ASASSN-14li: Evidence for linear disk-jet coupling