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tokens: compared with that of J1846−0258. The differences between the behaviour of J1119−6127 and J1846−0258 suggest that the peculiar spin frequency evolution of J1119−6127 reveal processes not well understood during the transition from a high- B radio pulsar to a magnetar. The net spin-down we observed following the X-ray bursts implies a release of a large amount of rotational energy. Assuming the canonical neutron star moment of inertia of I 45 = 10 45 g cm 2 , the rotational energy released can be estimated as This is ∼20 times of the total X-ray outburst energy, and in fact we did not observe obvious correlation between the X-ray light curve presented in Coti Zelati et al. ( 2018 ) and the radio flux densities nor the spin-frequency evolution. For a time span of ∼100 days, the spin-down power gives us an averaged luminosity of ∼4.4 × 10 36 erg s −1 , about two times larger than the normal spin-down luminosity. While only a small portion of the spin-down energy goes into radio and X-ray, we could expect much stronger high energy emissions from the pulsar (e.g. γ-ray) if energy loss via high energy radiation is the main energy-loss mechanism. Such a high spin-down luminosity could also power strong relativistic particle outflows that can brighten the pulsar wind nebula (Blumer et al. 2017 ). A complete picture of the PSR J1119−6127 event is likely to be that ultra-strong magnetic fields powered the X-ray bursts and triggered an additional torque that produced the peculiar spin frequency evolution. The fact that the polarization PA changed significantly following the X-ray bursts indicates that the magnetic field might have changed. If we assume that the spin-down process is dominated by dipole braking, the surface magnetic field strength can be estimated as where P and are the spin period and spin-period derivative. Applying equation ( 2 ) on our measurements of P and of PSR J1119−6127, we found that after the X-ray burst the surface magnetic field strength can reach as high as ∼9 × 10 13 G, which is more than two times stronger than the normal field strength. Under such assumptions, the fast increase and slow recovery of as shown in the third panel of Fig. 1 indicate similar evolution of the surface magnetic field strength of the pulsar. This suggests that the X-ray bursts triggered some reconfiguration of the magnetosphere of the pulsar, resulting in the increase of the apparent field strength. The energy of the global dipolar field external to the neutron star can be estimated as and in order to increase the magnetic field strength from ∼4 × 10 13 G to ∼9 × 10 13 G a total amount of energy of ∼2 × 10 45 erg is needed. This is more than one order of magnitude larger than the spin-down power released following the X-ray bursts. Energies either from multipole (and/or internal) magnetic fields or neutron star interior need to be converted to the strong dipolar field and/or distort the magnetic field. Under such a scenario, the slow recoveries of