Table 1.
Frequencies (third column) of nodeless torsional modes in the companion (M2 = 1.25 M⊙), for a range of spins ν (first column) and polar field strengths Bp (second column) via expression (2).
| ν (Hz) | Bp (1013 G) | Mode freq. (ℓ = 2, ℓ = 4) (Hz) | |
|---|---|---|---|
| 0 | 0 | 24.22 | 51.35 |
| 2 | 0 | 20.89 | 47.55 |
| 4 | 0 | 17.55 | 43.75 |
| 0 | 1 | 24.22 | 51.35 |
| 0 | 10 | 24.24 | 51.39 |
| 0 | 100 | 25.74 | 54.88 |
| 0.5 | 80 | 24.37 | 52.69 |
| 1 | 76 | 23.44 | 51.52 |
| 2 | 72 | 21.69 | 49.41 |
Notes. The core EOS is APR4 (Akmal et al. 1998), while the Douchin & Haensel (2001) fit governs the crust, which occupies the outermost 0.973 km of the star; such a model is able to explain the QPOs observed in the giant flare tails of SGR 1806–20 and SGR 1900+14 (Colaiuda & Kokkotas 2011). Bold numbers match the QPOs in GRB 211211A’s precursor, and/or the spin and magnetic field strengths predicted if a 2g2-mode resonance breaks the crust ∼1.08 ± 0.20 s prior to coalescence (see Sect. 2.1).
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