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S. J. Murphy, A. Pigulski, D. W. Kurtz, J. C. Suárez, G. Handler, L. A. Balona, B. Smalley, K. Uytterhoeven, R. Szabó, A. O. Thygesen, V. Elkin, M. Breger, A. Grigahcène, J. A. Guzik, J. M. Nemec, J. Southworth, Erratum: Asteroseismology of KIC 11754974: a high-amplitude SX Phe pulsator in a 343-d binary system, Monthly Notices of the Royal Astronomical Society, Volume 436, Issue 3, 11 December 2013, Page 2877, https://doi.org/10.1093/mnras/stt1749
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The paper ‘Asteroseismology of KIC 11754974: a high-amplitude SX Phe pulsator in a 343-d binary system’ was published in MNRAS, 432, 2284 (2013). An error was inadvertently introduced in this paper during copyediting when the term ‘F0’ was globally replaced by ‘F1’. This error first occurs in section 4.3 of the paper, paragraph 2 of that section. Therefore, the ratio that reads ‘P(F1)/P(F1)’ should have read ‘P(F1)/P(F0)’. Instances of ‘F0’ occurring alone were also affected. The correct Table 6 is shown below. The publisher apologizes for this error.
Characteristics of the best representative rotating model. The first five columns have their usual meanings, then headings are mean density, equatorial rotation velocity, inclination of the stellar rotation axis to the line of sight, fundamental radial mode frequency f(F0), first overtone radial mode frequency f(F1), the base-10 logarithm of the period of F0, and the period ratio of F1 and F0. The model has metallicity [Fe/H] = −0.52, convective efficiency, αMLT = 0.5 and overshooting dov = 0.3. See Section 5.2 for model selection criteria.
| Mass . | Radius . | Teff . | Age . | log g . | |$\bar{\rho }$| . | veq . | i . | f(F0) . | f(F1) . | log P(F0) . | P(F1)/P(F0) . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) . | (R⊙) . | (K) . | (Myr) . | (cgs) . | . | (km s−1) . | (deg) . | (d−1) . | (d−1) . | . | . |
| 1.53 | 1.764 | 7256 | 1465.93 | 4.129 | 0.392 | 34.18 | 47|$^{+7}_{-15}$| | 16.327 | 21.1 | −1.213 | 0.773 |
| Mass . | Radius . | Teff . | Age . | log g . | |$\bar{\rho }$| . | veq . | i . | f(F0) . | f(F1) . | log P(F0) . | P(F1)/P(F0) . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) . | (R⊙) . | (K) . | (Myr) . | (cgs) . | . | (km s−1) . | (deg) . | (d−1) . | (d−1) . | . | . |
| 1.53 | 1.764 | 7256 | 1465.93 | 4.129 | 0.392 | 34.18 | 47|$^{+7}_{-15}$| | 16.327 | 21.1 | −1.213 | 0.773 |
Characteristics of the best representative rotating model. The first five columns have their usual meanings, then headings are mean density, equatorial rotation velocity, inclination of the stellar rotation axis to the line of sight, fundamental radial mode frequency f(F0), first overtone radial mode frequency f(F1), the base-10 logarithm of the period of F0, and the period ratio of F1 and F0. The model has metallicity [Fe/H] = −0.52, convective efficiency, αMLT = 0.5 and overshooting dov = 0.3. See Section 5.2 for model selection criteria.
| Mass . | Radius . | Teff . | Age . | log g . | |$\bar{\rho }$| . | veq . | i . | f(F0) . | f(F1) . | log P(F0) . | P(F1)/P(F0) . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) . | (R⊙) . | (K) . | (Myr) . | (cgs) . | . | (km s−1) . | (deg) . | (d−1) . | (d−1) . | . | . |
| 1.53 | 1.764 | 7256 | 1465.93 | 4.129 | 0.392 | 34.18 | 47|$^{+7}_{-15}$| | 16.327 | 21.1 | −1.213 | 0.773 |
| Mass . | Radius . | Teff . | Age . | log g . | |$\bar{\rho }$| . | veq . | i . | f(F0) . | f(F1) . | log P(F0) . | P(F1)/P(F0) . |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) . | (R⊙) . | (K) . | (Myr) . | (cgs) . | . | (km s−1) . | (deg) . | (d−1) . | (d−1) . | . | . |
| 1.53 | 1.764 | 7256 | 1465.93 | 4.129 | 0.392 | 34.18 | 47|$^{+7}_{-15}$| | 16.327 | 21.1 | −1.213 | 0.773 |
