The DOI matches its Crossref record; 20 of the 20 references it cites were found in a registry or an index.
Tidal Dissipation in Rotating Solar‐Type Stars
Open accessAbstract
We calculate the excitation and dissipation of low-frequency tidal oscillations in uniformly rotating solar-type stars. For tidal frequencies smaller than twice the spin frequency, inertial waves are excited in the convective envelope and are dissipated by turbulent viscosity. Enhanced dissipation occurs over the entire frequency range rather than in a series of very narrow resonant peaks and is relatively insensitive to the effective viscosity. Hough waves are excited at the base of the convective zone and propagate into the radiative interior. We calculate the associated dissipation rate under the assumption that they do not reflect coherently from the center of the star. Tidal dissipation in a model based on the present Sun is significantly enhanced through the inclusion of the Coriolis force but may still fall short of that required to explain the circularization of close binary stars. However, the dependence of the results on the spin frequency, tidal frequency, and stellar model indicate that a more detailed evolutionary study including inertial and Hough waves is required. We also discuss the case of higher tidal frequencies appropriate to stars with very close planetary companions. The survival of even the closest hot Jupiters can be plausibly explained provided that the Hough waves they generate are not damped at the center of the star. We argue that this is the case because the tide excited by a hot Jupiter in the present Sun would marginally fail to achieve nonlinearity. As conditions at the center of the star evolve, nonlinearity may set in at a critical age, resulting in a relatively rapid inspiral of the hot Jupiter.
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Cites
Murray, C. D., & Dermott, S. F. (2000) · Cambridge University Press eBooks · doi:10.1017/cbo9781139174817 · Cited by 2,856
Orbital migration of the planetary companion of 51 Pegasi to its present location
Lin, D. N. C., Bodenheimer, P., & Richardson, D. C. (1996) · Nature · doi:10.1038/380606a0 · Cited by 1,235
Self-citationThe Current State of Solar Modeling
Christensen-Dalsgaard, J., Däppen, W., Ajukov, S. V., Anderson, E. R., Antia, H. M., Basu, S., Baturin, V. A., Berthomieu, G., Chaboyer, B., Chitre, S. M., et al. (1996) · Science · doi:10.1126/science.272.5266.1286 · Cited by 1,184
Goldreich, P., & Soter, S. (1966) · Icarus · doi:10.1016/0019-1035(66)90051-0 · Cited by 1,053
Butler, R. P., Wright, J. T., Marcy, G. W., Fischer, D. A., Vogt, S. S., Tinney, C. G., Jones, H. R. A., Carter, B. D., Johnson, J. A., McCarthy, C., et al. (2006) · The Astrophysical Journal · doi:10.1086/504701 · Cited by 914
Tidal Dissipation in Rotating Giant Planets
Ogilvie, G. I., & Lin, D. N. C. (2004) · The Astrophysical Journal · doi:10.1086/421454 · Cited by 386
Self-citationMeibom, S., & Mathieu, R. D. (2005) · The Astrophysical Journal · doi:10.1086/427082 · Cited by 288
Terquem, C., Papaloizou, J. C. B., Nelson, R. P., & Lin, D. N. C. (1998) · The Astrophysical Journal · doi:10.1086/305927 · Cited by 209
Self-citationTurbulent viscosity and Jupiter's tidal Q
Goldreich, P., & Nicholson, P. D. (1977) · Icarus · doi:10.1016/0019-1035(77)90163-4 · Cited by 206
Tidal dissipation in rotating giant planets
Ogilvie, G. I., & Lin, D. N. C. (2003) · CERN Document Server (European Organization for Nuclear Research) · Cited by 202
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Cited by
Leconte, J., Chabrier, G., Baraffe, I., & Levrard, B. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014337 · Cited by 348
Cameron, A. C., Guenther, E., Smalley, B., McDonald, I., Hebb, L., Andersen, J., Augusteijn, T., Barros, S. C. C., Brown, D. J. A., Cochran, W. D., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16922.x · Cited by 324
An orbital period of 0.94 days for the hot-Jupiter planet WASP-18b
Hellier, C., Anderson, D. R., Cameron, A. C., Gillon, M., Hebb, L., Maxted, P. F. L., Queloz, D., Smalley, B., Triaud, A. H. M. J., West, R. G., et al. (2009) · Nature · doi:10.1038/nature08245 · Cited by 277
INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT
Rogers, T. M., Lin, D. N. C., McElwaine, J. N., & Lau, H. H. B. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/772/1/21 · Cited by 262
Self-citationWASP-17b: AN ULTRA-LOW DENSITY PLANET IN A PROBABLE RETROGRADE ORBIT
Anderson, D. R., Hellier, C., Gillon, M., Triaud, A. H. M. J., Smalley, B., Hebb, L., Cameron, A. C., Maxted, P. F. L., Queloz, D., West, R. G., et al. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/709/1/159 · Cited by 208
Metadata
- Authors
- Ogilvie, G. I., & Lin, D. N. C.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2007-06
- Volume
- 661
- Issue
- 2
- Pages
- 1180-1191
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2093348988
- Cited by
- 358
- References
- 20
- FWCI
- 7.85
- Type
- journal article
- Language
- en
- Open access
- bronze
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