Stellar wind regimes of close-in extrasolar planets
Open accessAbstract
Close-in extrasolar planets of Sun-like stars are exposed to stellar wind conditions that differ considerably from those for planets in the solar system. Unfortunately, these stellar winds belong to the still unknown parameters of these planetary systems. On the other hand, they play a crucial role in a number of star-planet interaction processes that may lead to observable radiation events. In order to lay a foundation for the investigation of such interaction processes, we estimate stellar wind parameters on the basis of the solar wind model by Weber & Davis and study the implications of the stellar magnetic fields. Our results suggest that in contrast to the solar system planets, some close-in extrasolar planets may be obstacles in a sub-Alfvénic stellar wind flow. In this case, the stellar wind magnetic pressure is comparable to or even larger than the dynamic flow pressure. We discuss possible consequences of these findings for the wind–exoplanet interactions. Further, we derive upper limit estimates for the energies such stellar winds can deposit in the exoplanetary magnetospheres. We finally discuss the implications the sub-Alfvénic environment may have on the star–planet interaction.
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Stellar winds scale to magnetic fields and activity.
“Since stellar winds scale to magnetic fields and activity (e.g., Schrijver et al. 2003; Preusse et al. 2005; Cranmer & Saar 2011)”
From ABOUT EXOBIOLOGY: THE CASE FOR DWARF K STARS (2016) · cites this paper as Preusse et al. 2005
Section 3.2 (page unavailable) varies magnetic-field strength to study its influence on stellar-wind velocities, supporting the magnetic-field part of the claim. The paper does not establish that stellar winds scale with stellar activity; its discussion of activity in the Introduction concerns possible effects of star–planet interaction. (LLM, conf=0.84)
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Cites
Dynamics of the Interplanetary Gas and Magnetic Fields.
PARKER, E. N. (1958) · The Astrophysical Journal · doi:10.1086/146579 · Cited by 3,667 · see citing works
The Angular Momentum of the Solar Wind
Weber, E. J., & Leverett, J. D. (1967) · The Astrophysical Journal · doi:10.1086/149138 · Cited by 1,447 · see citing works
Lamers, H. J. G. L. M., & Cassinelli, J. P. (1999) · Cambridge University Press eBooks · doi:10.1017/cbo9781139175012 · Cited by 1,054 · see citing works
Perreault, P. D., & Akasofu, S. ‐. (1978) · Geophysical Journal International · doi:10.1111/j.1365-246x.1978.tb05494.x · Cited by 828 · see citing works
Vidal‐Madjar, A., Dsert, J.-M., Etangs, A. L. D., H�brard, G., Ballester, G. E., Ehrenreich, D., Ferlet, R., McConnell, J. C., Mayor, M., & Parkinson, C. D. (2004) · The Astrophysical Journal · doi:10.1086/383347 · Cited by 653 · see citing works
Nonlinear standing Alfvén wave current system at Io: Theory
Neubauer, F. M. (1980) · Journal of Geophysical Research Atmospheres · doi:10.1029/ja085ia03p01171 · Cited by 572 · see citing works
Measured Mass‐Loss Rates of Solar‐like Stars as a Function of Age and Activity
Wood, B. E., Müller, H., Zank, G. P., & Linsky, J. L. (2002) · The Astrophysical Journal · doi:10.1086/340797 · Cited by 407 · see citing works
On Stellar Activity Enhancement Due to Interactions with Extrasolar Giant Planets
Cuntz, M., Saar, S. H., & Musielak, Z. E. (2000) · The Astrophysical Journal · doi:10.1086/312609 · Cited by 319 · see citing works
Statistical properties of exoplanets
Santos, N. C., Israelian, G., Mayor, M., et al. (2003) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20021637 · Cited by 289 · see citing works
An extrasolar planet that transits the disk of its parent star
Konacki, M., Torres, G., Jha, S., & Sasselov, D. (2003) · Nature · doi:10.1038/nature01379 · Cited by 272 · see citing works
Evidence for Planet‐induced Chromospheric Activity on HD 179949
Shkolnik, E. L., Walker, G. A. H., & Bohlender, D. (2003) · The Astrophysical Journal · doi:10.1086/378583 · Cited by 244 · see citing works
The effect of tidal locking on the magnetospheric and atmospheric evolution of “Hot Jupiters”
Grießmeier, J.-M., Stadelmann, A., Penz, T., Lammer, H., Selsis, F., Ribas, I., Guinan, E. F., Motschmann, U., Biernat, H. K., & Weiss, W. W. (2004) · Astronomy & Astrophysics · doi:10.1051/0004-6361:20035684 · Cited by 237 · see citing works
Self-citationMagnetically-Driven Planetary Radio Emissions and Application to Extrasolar Planets
Zarka, P., Treumann, R. A., Ryabov, B. P., et al. (2001) · Astrophysics and Space Science · doi:10.1023/a:1012221527425 · Cited by 201 · see citing works
On the Star-Magnetosphere Interaction of Close-in Exoplanets
Ip, W., Kopp, A., & Hu, J.-H. (2004) · The Astrophysical Journal · doi:10.1086/382274 · Cited by 201 · see citing works
Self-citationGlobal energy deposition during the January 1997 magnetic cloud event
Lu, G., Baker, D. N., McPherron, R. L., et al. (1998) · Journal of Geophysical Research Atmospheres · doi:10.1029/98ja00897 · Cited by 195 · see citing works
A Search for Radio Emission from Extrasolar Planets
Bastian, T. S., Dulk, G. A., & Leblanc, Y. (2000) · The Astrophysical Journal · doi:10.1086/317864 · Cited by 182 · see citing works
On the possibility of coherent cyclotron emission from extrasolar planets
Farrell, W. M., DESCH, M. D., & Zarka, P. (1999) · Journal of Geophysical Research Atmospheres · doi:10.1029/1998je900050 · Cited by 175 · see citing works
Rostoker, G., Akasofu, S. ‐., Baumjohann, W., et al. (1988) · Space Science Reviews · doi:10.1007/bf00173876 · Cited by 162 · see citing works
Are Superflares on Solar Analogues Caused by Extrasolar Planets?
Rubenstein, E. P., & Schaefer, B. E. (2000) · The Astrophysical Journal · doi:10.1086/308326 · Cited by 158 · see citing works
Magnetic acceleration of winds from solar-type stars
Belcher, J. W., & MacGregor, K. B. (1976) · The Astrophysical Journal · doi:10.1086/154853 · Cited by 149 · see citing works
Goldreich, P., & Julian, W. H. (1970) · The Astrophysical Journal · doi:10.1086/150486 · Cited by 139 · see citing works
Planetary Companions to the Metal‐rich Stars BD −10o3166 and HD 52265
Butler, R. P., Vogt, S. S., Marcy, G. W., Fischer, D. A., Henry, G. W., & Apps, K. (2000) · The Astrophysical Journal · doi:10.1086/317796 · Cited by 131 · see citing works
Baliunas, S. L., Henry, G. W., Donahue, R. A., et al. (1997) · The Astrophysical Journal · doi:10.1086/310442 · Cited by 93 · see citing works
An Assessment of the Rotation Rates of the Host Stars of Extrasolar Planets
Barnes, S. A. (2001) · The Astrophysical Journal · doi:10.1086/323373 · Cited by 81 · see citing works
Sun, W., Xu, W. Y., & Akasofu, S. ‐. (1998) · Journal of Geophysical Research Atmospheres · doi:10.1029/97ja03458 · Cited by 76 · see citing works
On the Double‐Planet System around HD 83443
Butler, R. P., Marcy, G. W., Vogt, S. S., Tinney, C. G., Jones, H. R. A., McCarthy, C., Penny, A. J., Apps, K., & Carter, B. D. (2002) · The Astrophysical Journal · doi:10.1086/342471 · Cited by 67 · see citing works
On the Double Planet System Around HD 83443
Butler, R. P., Marcy, G. W., Vogt, S. S., et al. (2002) · University of Hertfordshire Research Archive (University of Hertfordshire) · Cited by 50 · see citing works
Magnetospheric response to the IMF : Substorms.
Baker, D. N., Bargatze, L. F., & Zwickl, R. D. (1986) · Journal of geomagnetism and geoelectricity · doi:10.5636/jgg.38.1047 · Cited by 45 · see citing works
An assessment of the rotation rates of the host stars of extrasolar planets
Barnes, S. A. (2001) · CERN Document Server (European Organization for Nuclear Research) · Cited by 41 · see citing works
Takeda, Y., Sato, B., Kambe, E., et al. (2002) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/54.6.1041 · Cited by 39 · see citing works
Predicted infrared brightness of stars within 25 parsecs of the sun
Johnson, H. M., & Wright, C. D. (1983) · The Astrophysical Journal Supplement Series · doi:10.1086/190905 · Cited by 24 · see citing works
An interpretation of Akasofu's substorm parameter
D’Angelo, N., & Goertz, C. K. (1979) · Planetary and Space Science · doi:10.1016/0032-0633(79)90031-x · Cited by 19 · see citing works
Mass loss from the infrared star CIT 6
Mufson, S. L., & Liszt, H. S. (1975) · The Astrophysical Journal · doi:10.1086/153962 · Cited by 7 · see citing works
Planet Host Stars: Mass, Age and Kinematics
Chen, Y., & Zhao, G. (2002) · 天文和天体物理学研究：英文版 · doi:10.1088/1009-9271/2/2/151 · Cited by 6 · see citing works
Gamma-Ray Burst Sequences in Hardness Ratio-Peak Energy PlanePreprint
Cui, X., Liang, E., & Lu, R. (2005) · arXiv (Cornell University) · doi:10.48550/arxiv.astro-ph/0504371 · Cited by 5 · see citing works
Flagged first, then by citations
Research works printed but not linked: 2
- [21]21. Laws, C., Gonzalez, G., Walker, K. M., et al. 2003 [arXiv:astro-ph/0302111] · arXiv
- [26]26. Paetzold, M., Carone, L., & Rauer, H. 2004, ArXiv Astrophysics e-prints
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ABOUT EXOBIOLOGY: THE CASE FOR DWARF K STARS
Cuntz, M., & Guinan, E. F. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/827/1/79 · Cited by 77 · see citing works
“Since stellar winds scale to magnetic fields and activity (e.g., Schrijver et al. 2003; Preusse et al. 2005; Cranmer & Saar 2011), it can be assumed that winds are most dense in young, magnetically active stars and planets at close-in HTDs (as given for late-K and M dwarfs) are most affected.”
Background
- Authors
- Preusse, S., Kopp, A., Büchner, J., & Motschmann, U.
- Affiliations
- Max Planck Society (DE)
- Technische Universität Braunschweig (DE)
- Venue
- Astronomy & Astrophysics
- Publisher
- EDP Sciences
- Published
- 2005-04-18
- Volume
- 434
- Issue
- 3
- Pages
- 1191-1200
- ISSN
- 0004-6361 (ISSN-L)
- 1432-0746
- OpenAlex
- W2062679170
- Cited by
- 76
- References
- 35
- Citations by year
- 2026: 1 · 2024: 4 · 2023: 2 · 2022: 1 · 2021: 4 · 2020: 4 · 2019: 3 · 2018: 6 · 2017: 5 · 2016: 2 · 2015: 2 · 2014: 2 · 2013: 6
- FWCI
- 3.30
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Astronomy and Astrophysics (publishedVersion)
- Springer Link (Chiba Institute of Technology) (submittedVersion)
- Max Planck Institute for Plasma Physics (submittedVersion)
- Max Planck Digital Library (submittedVersion)
- MPG.PuRe (Max Planck Society) (submittedVersion)
- Funders
- International Max Planck Research School for Environmental, Cellular and Molecular Microbiology
- Max-Planck-Gesellschaft
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Solar and Space Plasma Dynamics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Ionosphere and magnetosphere dynamics
- Keywords
- stellar winds, close-in exoplanets, star-planet interaction, stellar magnetic fields, sub-Alfvénic flow, exoplanet magnetospheres, solar-type stars
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