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New Mass-Loss Measurements from Astrospheric Lyα Absorption
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Measurements of stellar mass-loss rates are used to assess how wind strength varies with coronal activity and age for solar-like stars. Mass loss generally increases with activity, but we find evidence that winds suddenly weaken at a certain activity threshold. Very active stars are often observed to have polar starspots, and we speculate that the magnetic field geometry associated with these spots may be inhibiting the winds. Our inferred mass-loss/age relation represents an empirical estimate of the history of the solar wind. This result is important for planetary studies as well as solar/stellar astronomy, since solar wind erosion may have played an important role in the evolution of planetary atmospheres.
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“However, observations are unsupportive: Fast mass loss only happens in the first ~200 Ma after Sun-like stars form (207, 208).”
From The Archean atmosphere (2020) · cites this paper as [207]
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Cites
Acuña, M. H., Connerney, J. E. P., F., N., Ness, Lin, R. P., Mitchell, D., Carlson, C. W., McFadden, J., Anderson, K. A., Rème, H., et al. (1999) · Science · doi:10.1126/science.284.5415.790 · Cited by 1,101
Ribas, I., Guinan, E. F., Güdel, M., & Audard, M. (2005) · The Astrophysical Journal · doi:10.1086/427977 · Cited by 871
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 411
Self-citationWood, B. E., Redfield, S., Linsky, J. L., Müller, H., & Zank, G. P. (2005) · The Astrophysical Journal Supplement Series · doi:10.1086/430523 · Cited by 283
Self-citationLinsky, J. L., & Wood, B. E. (1996) · The Astrophysical Journal · doi:10.1086/177238 · Cited by 277
Self-citationThe 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
Interaction of the solar wind with the local interstellar medium: A multifluid approach
Zank, G. P., Pauls, H. L., Williams, L. L., & Hall, D. T. (1996) · Journal of Geophysical Research Atmospheres · doi:10.1029/96ja02127 · Cited by 235 · cited 1×
“Brie y,hydrodynam ic m odelsofthe astrospheres,constrained by the VISM values in Table 1,are com puted using a four- uid code developed to m odelthe heliosphere and reproduce the observed heliospheric Ly absorption (Zank et al.1996;W ood,M uller,& Zank 2000).”
MethodSelf-citationSpots on the surface of Betelgeuse -- Results from new 3D stellar convection models
Freytag, B., Steffen, M., & Dorch, B. (2002) · Astronomische Nachrichten · doi:10.1002/1521-3994(200208)323:3/4 · Cited by 218
Lammer, H., Lichtenegger, H., Kolb, C., Ribas, I., Guinan, E. F., Abart, R., & Bauer, S. J. (2003) · Icarus · doi:10.1016/s0019-1035(03)00170-2 · Cited by 213
Evolution of the solar ionizing flux
Ayres, T. R. (1997) · Journal of Geophysical Research Atmospheres · doi:10.1029/96je03306 · Cited by 203 · cited 1×
“As we did in Paper 1,we com bine the m ass-loss/activity relation in Figure 3a with a known relation between activity and age, Fx / t 1:74 0:34 (Ayres 1997),to derive an em piricalm asslossevolution law forsolar-likestars: _M / t 2:33 0:55.”
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Research works printed but not linked: 3
- Lallement R., 1992, A&A, 266, 479
- Petit, P., etal 2005, MNRAS, in press
- Wood B. E., 2004, Living Rev. Sol. Phys., 1, 2
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Items 301–400 of 467
Nonlinear Alfvén Wave Model of Stellar Coronae and Winds from the Sun to M Dwarfs
Sakaue, T., & Shibata, K. (2021) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/abd3a9 · Cited by 10
“In order to quantify the stellar wind’s properties observationally, Wood et al. (2005) investigated the absorption signatures in stellar Lyα spectra, leading to the estimation of Ṁ ∼ 2×10−14 M⊙ yr−1 for EV Lac (M3.”
BackgroundThe infrared excess emission from nearby Gaia DR2 M dwarfs
Sgro, L. A., & Song, I. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2400 · Cited by 10
Wiegert, J., Liseau, R., Thébault, P., Olofsson, G., Mora, A., Bryden, G., Marshall, J. P., Eiroa, C., Montesinos, B., Ardila, D. R., et al. (2014) · arXiv (Cornell University) · doi:10.48550/arxiv.1401.6896 · Cited by 10
“The stellar mass loss rate of αCen A is of the order of that of the Sun, i.e. 2 ˆ 10´14 Md yr´1, and also the average wind velocity is similar, viz. υw „ 400 km s´1 (Wood et al. 2001, 2005)4.”
BackgroundClose Binaries with Infrared Excess: Destroyers of Worlds?Preprint
Matranga, M., Drake, J. J., Kashyap, V. L., Marengo, M., & Kuchner, M. J. (2016) · Cited by 10
Effects of charge exchange on plasma flow in the heliosheath and astrosheathes
Korolkov, S. D., & Измоденов, В. В. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae187 · Cited by 9
Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Alam, M. K., Kirk, J. A., Santos, L. A. D., McCreery, P., Allan, A., Owen, J. E., Vidotto, A. A., Allart, R., Bourrier, V., Espinoza, N., et al. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad50d4 · Cited by 9
“Given the young age of the HD 63433 system and its observed X-ray properties, such a large stellar wind outflow rate is consistent with empirical scaling relationships (e.g. Wood et al. 2005; Johnstone et al. 2015; Blackman & Owen 2016).”
BackgroundNamekata, K., Maehara, H., Notsu, Y., Honda, S., Ikuta, K., Nogami, D., & Shibata, K. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adfe70 · Cited by 17
“For active, young stars, both theoretical studies (S. R. Cranmer & S. H. Saar 2011; M. Shoda et al. 2023) and observational studies (B. E. Wood et al. 2005; A. A. Vi-dotto 2021) suggest that the ambient wind mass-loss rate is on the order of 10 − 12 M ⊙ yr − 1 , ∼ 100 times higher than the solar…”
Suzuki, T. K. (2012) · Earth Planets and Space · doi:10.5047/eps.2011.04.012 · Cited by 9
Effect of Magnetic Diffusion in the Chromosphere on the Solar Wind
Matsuoka, M., Suzuki, T. K., Tokuno, T., & Kakiuchi, K. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad496b · Cited by 9
“˙ M of the ideal MHD case, M0, is calibrated to explain the observational value ≈ 2 × 10 − 14 M ⊙ yr − 1 (Withbroe 1988; Wood et al. 2005, 2021), indicating that the cases with ambipolar diffusion (M2 and M3) cannot reproduce the average ˙ M of the current solar wind (Table 1).”
BackgroundOrganic Matter Responses to Radiation under Lunar Conditions
Matthewman, R., Crawford, I., Jones, A., Joy, K. H., & Sephton, M. A. (2016) · Astrobiology · doi:10.1089/ast.2015.1442 · Cited by 9
“The flux of the solar wind during the early history of the Sun is believed to have been hundreds of times higher than today (Wood et al., 2005; Cnossen et al., 2007; Lundin et al., 2007).”
BackgroundUV astronomy throughout the ages: a historical perspective
Linsky, J. L. (2018) · Astrophysics and Space Science · doi:10.1007/s10509-018-3319-9 · Cited by 9
Self-citationConstraints on the Structure of the Heliospheric Interface Based on Lyα Absorption Spectra
Wood, B. E., Измоденов, В. В., & Malama, Y. G. (2008) · Space Science Reviews · doi:10.1007/s11214-008-9369-5 · Cited by 9
“Only a small fraction of the Lyα spectra of nearby stars in the HST archive show direct evidence of heliospheric absorption (Wood et al. 2005b).”
BackgroundSelf-citationOBSERVATIONS OF MAIN-SEQUENCE STARS AND LIMITS ON EXOZODICAL DUST WITH NULLING INTERFEROMETRY
Liu, W. M., Hinz, P. M., Hoffmann, W. F., Brusa, G., Miller, D., & Kenworthy, M. A. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/693/2/1500 · Cited by 9
“If one adopts the value of 30 dM /dt (Wood et al. 2005) and estimates the timescale for removing grains via stellar wind drag (Chen et al. 2006, Equation 11), one finds that wind drag shortens the removal timescale of the grains by more than a factor of 20.”
BackgroundFlat-spectrum Radio Continuum Emission Associated with ϵ Eridani
Rodríguez, L. F., Lizano, S., Loinard, L., Chávez, M., Bastian, T. S., & Beasley, A. J. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf9a6 · Cited by 9
“This mass-loss rate is 3,300 times the solar value Ṁ = 2× 10−14M yr−1, and 110 times larger than the value obtained by Wood et al. (2005) for Eridani using the atmospheric Lyα absorption method.”
ResultCLOSE BINARIES WITH INFRARED EXCESS: DESTROYERS OF WORLDS?
Matranga, M., Drake, J. J., Kashyap, V. L., Marengo, M., & Kuchner, M. J. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/720/2/l164 · Cited by 9
“Wood et al. (2005) found that very active stars might lose mass at rates perhaps up to 10−12 M yr−1 (100 times that of the Sun), meaning 10–100 years of accumulated wind would be necessary to explain the dust.”
BackgroundWeakened Magnetic Braking Signals the Collapse of the Global Stellar Dynamo
Metcalfe, Τ. S., van Saders, J. L., Pinsonneault, M. H., Ayres, T. R., Kochukhov, O., Stassun, K. G., Finley, A. J., See, V., Ilyin, I. V., & Strassmeier, K. G. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae03bc · Cited by 8
“By contrast, the scatter in the Wood (2018) relation for GK dwarfs is roughly plus or minus a factor of two, which is consistent with the systematic noise floor estimated by Wood et al. (2005).”
Asteroid magnetization from the early solar wind
Anand, A., Carroll-Nellenback, J., Blackman, E. G., & Tarduno, J. A. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3086 · Cited by 8
Magnetic Field of Gas Giant Exoplanets and Its Influence on the Retention of Their Exomoons
魏, X. 星. W., & Lin, D. N. C. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad2843 · Cited by 9
“The mass loss rate ˙ M ⋆ = 4 πa 2 Nm p v evolves roughly as t − 2 (Wood et al. 2002, 2005), e.g., the solar mass loss rate at present is ∼ 10 12 g / s.”
BackgroundMagnetic activity optimal tracers: from radio to X-ray; the relevance of UV astronomy
Pagano, I. (2008) · Astrophysics and Space Science · doi:10.1007/s10509-008-9821-8 · Cited by 8
STELLAR WIND INDUCED SOFT X-RAY EMISSION FROM CLOSE-IN EXOPLANETS
Kislyakova, K. G., Fossati, L., Johnstone, C. P., Holmström, M., Zaitsev, V. V., & Lammer, H. (2015) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/799/2/l15 · Cited by 8
“Although little is known about the properties of winds from other stars, it is suspected that more active stars have mass fluxes that are significantly higher than the mass flux of the current solar wind (Wood et al. 2005; Holzwarth & Jardine 2007; Suzuki et al. 2013).”
BackgroundStability of Earth-Like N2 Atmospheres: Implications for Habitability
Lammer, H., Kislyakova, K. G., Güdel, M., Holmström, M., Erkaev, N. V., Odert, P., & Khodachenko, M. L. (2013) · Astrophysics and space science proceedings · doi:10.1007/978-1-4614-5191-4_4 · Cited by 9
MAXI J1957+032: An Accreting Neutron Star Possibly in a Triple System
Ravi, V. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9277 · Cited by 8
“Through the analysis of “astrospheric” Lyα absorption features from the collision regions between stellar winds and the interstellar medium, dwarf main-sequence stars are found to have comparable mass-loss rates to the Sun (i.e., M10 yr ;14 1» - - Wood et al. 2005).”
BackgroundSaikia, S. B., Jin, M., Johnstone, C. P., Lüftinger, T., Güdel, M., Airapetian, V., Kislyakova, K. G., & Folsom, C. P. (2020) · arXiv (Cornell University) · doi:10.48550/arxiv.2002.10460 · Cited by 8
“The indirect method of astrospheric Lyman-α measurements (Wood et al. 2001; Wood 2004; Wood et al. 2005) is the only technique that has provided observed wind mass loss rates for some nearby Sun-like stars.”
MethodShematovich, V. I., Бисикало, Д. В., Tsurikov, G., & Zhilkin, A. G. (2024) · Astronomy Reports · doi:10.1134/s1063772924700744 · Cited by 7
Testing the Rossby Paradigm: Weakened Magnetic Braking in Early K-type Stars
Metcalfe, Τ. S., Petit, P. M., van Saders, J. L., Ayres, T. R., Buzasi, D. L., Kochukhov, O., Stassun, K. G., Pinsonneault, M. H., Ilyin, I. V., Strassmeier, K. G., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/add40a · Cited by 7
“…paper, the authors note: “We have in the past estimated that M values measured in this way should be accurate to within about a factor of 2 ( B. E. Wood et al. 2005 ) , with important systematic uncertainties including the unknown degree of variation in ISM properties from star to star and…”
Mass Loss on the Red Giant Branch: Plasmoid-driven Winds above the RGB Bump
Mullan, D. J., & MacDonald, J. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab4658 · Cited by 7
Accretion from Winds of Red Giant Branch Stars May Reveal the Supermassive Black Hole in Leo I
Pacucci, F., & Loeb, A. (2022) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ac9b21 · Cited by 7
“Note that this is at least ∼ 105 times larger than the solar value of 2 × 10−14 M yr−1 (Wood et al. 2005).”
BackgroundEvolution of Dust and Small Bodies: Physical Processes
Mann, I. B. (2008) · Lecture notes in physics · doi:10.1007/978-3-540-76935-4_7 · Cited by 7
“Wood et al. [ 84 ] studied the density of neutral hydrogen around selected stars by spectroscopically detecting the absorption of neutral hydrogen distributed along the line of sight in stellar brightness data.”
BackgroundThe early Earth under a superflare and super-CME attack: prospects for life
Airapetian, V., Glocer, A., & Gronoff, G. (2015) · Proceedings of the International Astronomical Union · doi:10.1017/s174392131600226x · Cited by 7
Evolution of Energetic Particle Fluxes in the Early Heliosphere
Yeghikyan, A. G. (2017) · Astrophysics · doi:10.1007/s10511-017-9491-8 · Cited by 7
Constraints Imposed by the Square-root Spin-down Law on Coronal Wind Parameters
Skumanich, A. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab1b24 · Cited by 7
Kulikov, Y. N., Lammer, H., Lichtenegger, H., Penz, T., Breuer, D., Spohn, T., Lundin, R., & Biernat, H. K. (2007) · Space sciences series of ISSI · doi:10.1007/978-0-387-74288-5_8 · Cited by 7
Lammer, H., Hanslmeier, A., Schneider, J. L., Статева, И., Barthélémy, M., Belu, A. R., Бисикало, Д. В., Bonavita, M., Eybl, V., du Foresto, V. C., et al. (2010) · Solar System Research · doi:10.1134/s0038094610040039 · Cited by 7
“The amount of absorption is propor tional to the stellar wind ram pressure and therefore yields estimates of the mass loss rate (Wood et al., 2002, 2005).”
BackgroundTrimble, V., Aschwanden, M. J., & Hansen, C. J. (2006) · Publications of the Astronomical Society of the Pacific · doi:10.1086/506157 · Cited by 8
Energy Input of EUV, Solar Wind, and SEPs at Mars: MAVEN Observations During Solar Minimum
Jolitz, R. D., Rahmati, A., Brain, D. A., Lee, C. O., Lillis, R. J., Thiemann, E. M. B., Eparvier, F. G., Mitchell, D. L., Halekas, J. S., Larson, D. E., et al. (2023) · Journal of Geophysical Research Space Physics · doi:10.1029/2022ja030884 · Cited by 6
Catching the wisps: Stellar mass-loss limits from low-frequency radio observations
Bloot, S., Vedantham, H. K., Kavanagh, R. D., Callingham, J. R., & Pope, B. J. S. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452722 · Cited by 6
Moór, A., Ábrahám, P., Kóspál, Á., Su, K. Y. L., Rieke, G. H., Vida, K., Cataldi, G., Bódi, A., Bognár, Z., Cseh, B., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2595 · Cited by 6
Bagheri, F., Lopez, R., & Pham, K. H. (2024) · Frontiers in Astronomy and Space Sciences · doi:10.3389/fspas.2024.1398379 · Cited by 6
Khodachenko, M. L., Sasunov, Y. L., Arkhypov, O. V., Alexeev, I. I., Belenkaya, E. S., Lammer, H., Kislyakova, K. G., Odert, P., Leitzinger, M., & Güdel, M. (2013) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921313011174 · Cited by 6
“Combining the stellar mass loss measurements of (Wood et al., 2005) with the results of (Newkirk, 1980) for the age-dependence of stellar wind velocity, Grießmeier et al. (2007) proposed a method for calculation of stellar wind density nsw and velocity vsw at a given orbital location of an…”
MethodKislyakova, K. G., Holmström, M., Lammer, H., & Erkaev, N. V. (2014) · Astrophysics and space science library · doi:10.1007/978-3-319-09749-7_7 · Cited by 6
The Primordial Solar Wind as a Sculptor of Terrestrial Planet Formation
Spalding, C. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aaf478 · Cited by 5
Elias-López, A., Cantiello, M., Viganò, D., Sordo, F. D., Kaur, S., & Soriano-Guerrero, C. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adf057 · Cited by 7
“Given the intrinsic uncertainties, here we simply assume a representative solar value, ˙ M ⋆ = ˙ M ⊙ ≃ 400 km s − 1 (Wood et al. 2005), thus neglecting the large spatial and time variability measured for the Sun (e.g., Fig.”
A binary model of long-period radio transients and white dwarf pulsars
Horváth, C., Rea, N., Hurley-Walker, N., McSweeney, S. J., Perley, R. A., & Lenc, E. (2026) · Nature Astronomy · doi:10.1038/s41550-025-02760-y · Cited by 5
The Future of Solar Modelling: Requirements for a New Generation of Solar Models
Buldgen, G., Canocchi, G., Saux, A. L., Baturin, V. A., Trampedach, R., Валерьевна, О. А., Ayukov, S. V., Pradhan, A. K., Pain, J., Kunitomo, M., et al. (2025) · Solar Physics · doi:10.1007/s11207-025-02508-x · Cited by 5
“Observationally, Wood et al. (2005) proposed ˙ M ∝ t − 2 .”
UV astronomy and the investigation of the origin of life
de Castro, A. I. G., & Canet, A. (2021) · Elsevier eBooks · doi:10.1016/b978-0-12-819170-5.00002-6 · Cited by 7
Space Weather in the Saturn–Titan System
Burne, S., Bertucci, C. L., Sergis, N., Morales, L., Achilleos, N., Sánchez‐Cano, B., Collado‐Vega, Y. M., Dasso, S., Edberg, N. J. T., & Kurth, W. S. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acc738 · Cited by 5
“…conditions on unmagnetized bodies is especially important to learning about the evolution of their atmospheric structure, as particle escape increases significantly (e.g., Jakosky et al. 2015) and also because a higher rate of solar storms occurred in early solar system history (Wood et al. 2005).”
BackgroundLi production by stellar flares in young open clusters
Tatischeff, V., & Thibaud, J. P. (2008) · New Astronomy Reviews · doi:10.1016/j.newar.2008.06.013 · Cited by 5
Stellar Coronal and Wind Models: Impact on Exoplanets
Vidotto, A. A. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_26 · Cited by 5
“Wood et al. (2002, 2005) found a relation between the mass-loss rate per unit surface area A?”
BackgroundSimulations of Magnetised Stellar-Wind Bubbles
Mackey, J., Green, S., & Moutzouri, M. (2020) · Journal of Physics Conference Series · doi:10.1088/1742-6596/1620/1/012012 · Cited by 5
Radio Observations as an Exoplanet Discovery Method
Lazio, T. J. W. (2017) · Springer eBooks · doi:10.1007/978-3-319-30648-3_9-1 · Cited by 5
Lynch, B. J., Wood, B. E., Jin, M., Török, T., Sun, X., Palmerio, E., Osten, R. A., Vidotto, A. A., Cohen, O., Alvarado‐Gómez, J. D., et al. (2023) · doi:10.3847/25c2cfeb.2dd884d5 · Cited by 8
Self-citationExtreme Space Weather in Time: Effects on Earth
Airapetian, V. (2018) · Elsevier eBooks · doi:10.1016/b978-0-12-812700-1.00025-x · Cited by 4
Stellar activity and magnetic shielding
Grießmeier, J. ‐., Khodachenko, M. L., Lammer, H., Grenfell, J. L., Stadelmann, A., & Motschmann, U. (2009) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921309992961 · Cited by 6
“One can clearly see that for a young star (0.7 Gyr), all planets in a habitable zone between 0.1 and ∼0.3 AU have magnetospheric altitudes lower than the critical altitude level, so that strong erosion is likely.”
BackgroundMethodInfluentialFrom the Heliosphere to the Local Bubble—What Have We Learned?
Möbius, E. (2008) · Space Science Reviews · doi:10.1007/s11214-008-9477-2 · Cited by 5
Khodachenko, M. L., Lammer, H., Lichtenegger, H., Grießmeier, J. ‐., Holmström, M., & Ekenbäck, A. (2008) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921309030622 · Cited by 4
Measurement of stellar and substellar winds using white dwarf hosts
Walters, N., Farihi, J., Dufour, P., Pineda, J. S., & Izzard, R. G. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1885 · Cited by 4
The Environment of the Young Earth in the Perspective of An Young Sun
Airapetian, V. (2016) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921317004288 · Cited by 4
“Figure 1 shows the total mass-loss rates from Sun at at the three evolutionary phases of the Sun, 0.7 Gyr, 2 and 4.65 Gyr (the current epoch) superimposed on the range of empirically derived mass-loss rates for solar-like stars at various phases of evolution (Wood et al. 2005).”
BackgroundInfluentialSignatures of Star-Planet Interactions
Shkolnik, E. L., & Llama, J. (2017) · Springer eBooks · doi:10.1007/978-3-319-30648-3_20-1 · Cited by 4
Mars Environment and Magnetic Orbiter Scientific and Measurement Objectives
Leblanc, F., Langlais, B., Fouchet, T., Barabash, S., Breuer, D., Chassefière, É., Coates, A. J., Dehant, V., Forget, F., Lammer, H., et al. (2009) · Astrobiology · doi:10.1089/ast.2007.0222 · Cited by 4
“The past EUV flux is thought to have been up to 10 times larger 4.1 Ga ago (Ribas et al., 2005), whereas the solar wind flux may have been up to 100 times larger at the same epoch (Wood et al., 2005).”
InfluentialAerts, C., Christensen-Dalsgaard, J., & Kurtz, D. W. (2009) · Astronomy and astrophysics library · doi:10.1007/978-1-4020-5803-5_1 · Cited by 4
Güdel, M. (2015) · Encyclopedia of Astrobiology · doi:10.1007/978-3-662-44185-5_1700 · Cited by 4
Solar wind and its evolutionPreprint
Suzuki, T. K. (2016) · Cited by 4
Solar models with protosolar accretion and turbulent mixing
Kunitomo, M., Buldgen, G., & Guillot, T. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555104 · Cited by 3
Korolkov, S. D., & Измоденов, В. В. (2026) · Advances in Space Research · doi:10.1016/j.asr.2026.02.062 · Cited by 3
“…as acknowledged by the authors, many spectra exhibit substantial noise, and some spectral features interpreted merely as noise could potentially indicate neutral wind absorption (e.g., the absorption at approximately 1215.1 ˚A in the spectrum of HD 128987 in Figure 7 Wood et al., 2005b).”
InfluentialPinotti, R., & de Mello, G. F. P. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3260 · Cited by 3
“…with masses between 0.6 and 1.5 solar masses, the high-activity phase is very short-lived and directly connected to the evolution of rotation (Wood et al. 2002, 2005; Ribas et al. 2005; Ribas et al. 2010; do Nascimento et al. 2016) for both high-energy XUV photons and winds, and only very…”
BackgroundInfluentialPotential of the Solar Energy on Mars
Rugescu, D. R., & Dan, R. (2010) · InTech eBooks · doi:10.5772/8060 · Cited by 3
“For example, observations by Wood et al. (2005) of the absorption characteristic of the solartype G star τ-Boo, estimated as being 500-million-year-old, indicate that its mass loss is about 20 times less than the loss rate given by the mass loss power law, for a star with a similar age.”
BackgroundInfluentialPagano, I. (2013) · Springer eBooks · doi:10.1007/978-94-007-5615-1_10 · Cited by 3
The young Sun and its influence on planetary atmospheres
Güdel, M., & Kasting, J. F. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511933875.013 · Cited by 3
Stellar activity and winds shaping the atmospheres of Earth-like planets
Lueftinger, T., Güdel, M., Saikia, S. B., Johnstone, C. P., Kulterer, B. M., Kochukhov, O., & Kislyakova, K. G. (2018) · Proceedings of the International Astronomical Union · doi:10.1017/s174392131900293x · Cited by 3
“Stellar wind estimates are confronted with similar issues: although indirect estimations are available (Wood et al. 2005), little systematics can be inferred for stars at young ages (Johnstone et al. 2015a; Johnstone et al. 2015b).”
BackgroundPast solar wind flux recorded in solar-gas-rich meteorites
Obase, T., & Nakashima, D. (2022) · Icarus · doi:10.1016/j.icarus.2022.115290 · Cited by 3
The empirical upper limit for mass loss of cool main sequence stars
Lednicka, A., & Stȩpień, K. (2008) · Astronomische Nachrichten · doi:10.1002/asna.200710968 · Cited by 3
“(Note that, according to the results of Wood et al. 2005, the proportionality between MLR and X-ray luminosity breaks down for the most active stars).”
MethodResultRed giant winds driven by Alfvén waves with magnetic diffusion
Suzuki, T. K., Ohnaka, K., & Yasuda, Y. (2025) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psaf058 · Cited by 2
“…they expand, and the mass-loss rate due to stellar winds drastically increases from ˙ M ∼ 10 − 14 − 10 − 12 M ⊙ yr − 1 during the main sequence (MS) phase (Wood et al. 2005; Cranmer & Saar 2011) to ˙ M ∼ 10 − 4 M ⊙ yr − 1 in the final stage on the asymptotic giant branch (AGB) phase…”
Yang, Y.-P. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae2864 · Cited by 2
“Wood et al. 2005).”
InfluentialCai, J., Dang, T., Lei, J., Zhang, B. Z., Yao, Z., Chen, J., Xu, X., Xiao, S., & Zhang, T. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555227 · Cited by 2
Schreyer, E., & Murray-Clay, R. A. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag293 · Cited by 2
Vázquez, M., Πάλλη, Ε., & Montañés-Rodríguez, P. (2010) · Astronomy and astrophysics library · doi:10.1007/978-1-4419-1684-6_2 · Cited by 4
From the Heliosphere to the Local Bubble—What Have We Learned?
Möbius, E. (2008) · Space sciences series of ISSI · doi:10.1007/978-1-4419-0247-4_35 · Cited by 2
Magnetic activity at Mars – Mars Surface Magnetic Observatory
Vennerstrøm, S., Menvielle, M., Merayo, J. M. G., & Falkenberg, T. V. (2012) · Planetary and Space Science · doi:10.1016/j.pss.2012.08.001 · Cited by 2
Key problems in cool-star astrophysics
Pagano, I., Ayres, T. R., Lanzafame, A. C., Linsky, J. L., Montesinos, B., & Marcello-Rodonò (2006) · Astrophysics and Space Science · doi:10.1007/s10509-005-9018-3 · Cited by 2
Self-citationThe impact of stellar activity on planets
Ribas, I. (2006) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921307010678 · Cited by 2
“More recent results (Wood et al. 2005), however, question the suitability of an extrapolation back in time to very young ages and suggest a change in regime for an age of about 0.7 Gyr.”
ResultInfluentialAtmospheric pressure and CO2 concentration of potential habitable planet HD40307g
Tian, F. (2013) · Science China Earth Sciences · doi:10.1007/s11430-013-4757-4 · Cited by 2
Stellar Coronal and Wind Models: Impact on Exoplanets
Vidotto, A. A. (2017) · Springer eBooks · doi:10.1007/978-3-319-30648-3_26-2 · Cited by 2
Solar Variability and Climate Impact on Terrestrial Planets
Bertaux, J. (2007) · Space sciences series of ISSI · doi:10.1007/978-0-387-48341-2_35 · Cited by 2
Vida, K., Leitzinger, M., Kriskovics, L., Seli, B., Odert, P., Kovács, O. E., Korhonen, H., & van Driel-Gesztelyi, L. (2019) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · doi:10.48550/arxiv.1901.04229 · Cited by 2
“Stellar wind in cool stars is measured as interaction with the interstellar medium as astrospheric absorption seen in Lyα (Wood et al. 2002, 2005), or as free–free emission originating from fully ionised winds (Güdel et al. 2002; Gaidos et al. 2000; Fichtinger et al. 2017), and its detection was…”
BackgroundLang, K. R. (2009) · Astronomy and astrophysics library · doi:10.1007/978-3-540-76953-8_9 · Cited by 2
Titova, A., Измоденов, В. В., & Korolkov, S. D. (2025) · Publications of the Astronomical Society of Australia · doi:10.1017/pasa.2025.33 · Cited by 1
Radio Prospects of Extrasolar Aurorae Polaris as a Probe of Planetary Magnetism
Ä°smail, K. A. Y. A., & Daylan, T. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adde5c · Cited by 1
“…loss-radial magnetic flux relation with the X-ray luminosity-magnetic flux relation to find which is flatter than the empirical relations of B. E. Wood et al. (2002, 2005), and it can account for young and active main-sequence stars while still explaining the discrepancy with the empirical…”
Modeling Atmospheric Ion Escape from Kepler-1649 b and c over Time
Li, H., Dong, C., Xie, L., He, X., Chin, L., Wang, X., Yan, H.-L., Qin, J. J., Mayne, N. J., Mak, M. T., et al. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae1a65 · Cited by 1
Korolkov, S. D. (2026) · Advances in Space Research · doi:10.1016/j.asr.2026.05.041 · Cited by 1
Imaging Magnetically Driven Astrospheres: A Forward Modeling Approach
Wu, Z., Doorsselaere, T. V., He, J., Sana, H., Jannsen, N., Chen, T., Wang, W., & Sun, Z. (2026) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae7369 · Cited by 1
“Subsequent observations demonstrated that several nearby stars exhibit similar astrospheric absorption features (Wood et al. 2005b,a, 2021).”
InfluentialDeeper solar wind penetration on the Moon’s farside from noble gas records
Zhang, X.-H., Su, F., Li, Y.-J., Liu, Z.-H., Li, J.-N., Zhang, Y.-N., Qin, L., Liu, R.-R., Man, F., Xu, B., et al. (2026) · Nature Geoscience · doi:10.1038/s41561-026-02042-w · Cited by 1
The YREC Stellar Evolution Code: Public Data Release
Pinsonneault, M. H., van Saders, J. L., Cao, L., Tayar, J., Delahaye, F., Morales, L. M., Patton, R. A., Rendina, M. C., Zinn, J., Claytor, Z. R., et al. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae71cf · Cited by 1
“The magnetic field is scaled assuming a linear ( Rossby-scaled ) dynamo and pressure equipartition at the photosphere: , following the observed correlation of with X-ray luminosity ( B. E. Wood et al. 2005 ) and the scaling of the X-ray luminosity with Rossby number ( N. Pizzolato et al. 2003 ) .”
Solar and stellar coronae and winds
Jardine, M. (2016) · Proceedings of the International Astronomical Union · doi:10.1017/s174392131700374x · Cited by 1
“One indirect method of doing this, developed by Brian Wood, uses the enhanced absorption in the hydrogen wall of stellar astrospheres as a measure of the local mass loss rate (see, for example, Wood et al. (2005)).”
MethodStellar Coronal and Wind Models: Impact on Exoplanets
Vidotto, A. A. (2017) · Springer eBooks · doi:10.1007/978-3-319-30648-3_26-1 · Cited by 1
Aerts, C., Christensen-Dalsgaard, J., & Kurtz, D. W. (2009) · Astronomy and astrophysics library · doi:10.1007/978-1-4020-5803-5_8 · Cited by 1
Hydrogen ENA-cloud observation and modeling as a tool to study star-exoplanet interaction
Lammer, H., Kislyakova, K. G., Holmström, M., Khodachenko, M. L., & Grießmeier, J. ‐. (2011) · Springer eBooks · doi:10.1007/978-94-007-2573-7_3 · Cited by 1
Müller, H., Frisch, P. C., Fields, B. D., & Zank, G. P. (2008) · Space sciences series of ISSI · doi:10.1007/978-1-4419-0247-4_31 · Cited by 1
Self-citationThe lunar 40Ar/36Ar antiquity indicator in the presence of a lunar paleomagnetosphere
Poppe, A. R., Garrick‐Bethell, I., Fatemi, S., & Grava, C. (2024) · Icarus · doi:10.1016/j.icarus.2024.116079 · Cited by 1
Evolution of stellar winds from the Sun to red giants
Suzuki, T. K. (2008) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921309029901 · Cited by 1
“Recent observations have shown that younger stars are more active than main sequence stars, giving considerably larger X-ray and UV flux luminosity (Güdel 2004) and higher wind mass flux (Wood et al. 2005).”
Background
Metadata
- Authors
- Wood, B. E., Müller, H.-R., Zank, G. P., Linsky, J. L., & Redfield, S.
- Affiliations
- Joint Institute for Laboratory Astrophysics (US)
- University of California, Riverside (US)
- McDonald Observatory (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2005-07-11
- Volume
- 628
- Issue
- 2
- Pages
- L143-L146
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W1867591249
- Cited by
- 467
- References
- 19
- Citations by year
- 2026: 20 · 2025: 19 · 2024: 20 · 2023: 11 · 2022: 20 · 2021: 22 · 2020: 23 · 2019: 25 · 2018: 27 · 2017: 25 · 2016: 29 · 2015: 21 · 2014: 18 · 2013: 19 · 2012: 20
- FWCI
- 15.11
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- 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 › Instrumentation › Astronomy and Astrophysical Research
- Keywords
- stellar mass loss, Lyman-alpha absorption, stellar winds, coronal activity, solar-type stars
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