Erratum: Resonant shattering flares as multimessenger probes of the nuclear symmetry energy (Monthly Notices of the Royal Astronomical Society DOI: 10.1093/mnras/stab764)

The paper eResonant shattering flares as multimessenger probes of the nuclear symmetry energy f was published in MNRAS, 504, 1129-1143 (2021). During further study of the topic after publication of the paper, we found a scaling error in our calculation of the density-weighted average shear speed in the neutron star crust (ct). A constant factor of 4π had been lost due to erroneously substituting the density integral o v er radius with the crust mass, rather than the integral over volume. This has resulted in all reported values throughout the work being 4 π lower than they should be. As our conclusions are drawn from the correlations of, and fractional changes in, Pc t with the i-mode frequency and the EOS parameters, this constant factor does not affect any of our conclusions. The corrected values of Pc t are still only a small fraction of the speed of light ( < 0.5 per cent), and so the new magnitude will not affect these correlations. The change in magnitude may however affect any reader who wishes to use the correlations we found to relate the shear speed for an EOS to its approximate i-mode frequency. Applying the correction to the values used in our paper is trivial, but for completeness we list all of the changes: (i) The x-axes of Figure 5, the y-axis of Figure 15, and the labels on Figure 16 should be multiplied by 4 π, i.e. the units should be 4 × 10⁶cm/s, not 10⁶cm/s. (ii) In Table 1, the value in the caption should be 6.0 × 10⁷cm/s, and the values in the table should be, in order: 4.8 × 10⁷cm/s, .6.2 × 10⁷cm/s, 2.3 × 10⁷cm/s, and 5.2 ×10⁴cm/s. In addition to amending this error, we would also like to take the opportunity to mention some extra details of the NS crust model used for our EOSs. In the model we have used, the bulk matter components of the CLDM are parameterised by the symmetry energy parameters J , L and K sym . What we have not yet mentioned is that in addition to these, there is also a set of parameters associated with the surface energy of the nuclear clusters, which we determine by a fit to microscopic calculations of nuclei in neutron-rich matter as detailed in Balliet et al. ( 2021 ). These extra parameters were not directly mentioned in the original paper, as they are a part of the model described in the cited paper. Ho we ver, these parameters can be very important for i-mode frequencies as they affect the density of the crust-core transition, and so we take this opportunity to point them out and more clearly direct the reader to the paper in which they were calculated.