New Mass-Loss Measurements from Astrospheric Lyα Absorption
Open accessAbstract
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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Observations are unsupportive: fast mass loss only happens in the first ~200 Ma after Sun-like stars form.
“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]
Figure 3(b) and its accompanying discussion (page not provided) place the inferred weakening of the solar wind at about 0.7 Gyr when looking back toward younger ages. The paper therefore does not confine strong mass loss to the first ~200 million years; it suggests a different age pattern, with especially active, younger stars having weaker winds than the trend would predict. (LLM, conf=0.86)
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Cites
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MethodOn the Formation of Polar Spots in Sun‐like Stars
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Self-citationOn the Possibility of a Strong Magnetic Field in the Local Interstellar Medium
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Catling, D. C., & Zahnle, K. J. (2020) · Science Advances · doi:10.1126/sciadv.aax1420 · Cited by 568 · see citing works
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THE MUSCLES TREASURY SURVEY. I. MOTIVATION AND OVERVIEW*
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“Additionally, it is likely that the stellar mass-loss rates are higher earlier in their evolution (Wood et al. 2005a), increasing the potential planetary mass-loss.”
BackgroundSelf-citationHabitable planets around the star Gliese 581?
Selsis, F., Kasting, J. F., Levrard, B., Paillet, J., Ribas, I., & Delfosse, X. (2007) · Astronomy & Astrophysics · doi:10.1051/0004-6361:20078091 · Cited by 527 · see citing works
“Observational constraints on stellar winds exist (Wood et al. 2005), but their interpretation is still debated (Holzwarth & Jardine 2007).”
BackgroundM Stars as Targets for Terrestrial Exoplanet Searches And Biosignature Detection
Scalo, J., Kaltenegger, L., Segura, A., Fridlund, M. C., Ribas, I., Kulikov, Y. N., Grenfell, J. L., Rauer, H., Odert, P., Leitzinger, M., et al. (2007) · Astrobiology · doi:10.1089/ast.2006.0125 · Cited by 385 · see citing works
Emergence of a Habitable Planet
Zahnle, K., Arndt, N., Cockell, C., Halliday, A., Nisbet, E., Selsis, F., & Sleep, N. H. (2007) · Space Science Reviews · doi:10.1007/s11214-007-9225-z · Cited by 380 · see citing works
“Wood et al. (2005) have since characterized the winds of another half-dozen solar analogues.”
BackgroundWhat makes a planet habitable?
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Improved angular momentum evolution model for solar-like stars
Gallet, F., & Bouvier, J. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321302 · Cited by 373 · see citing works
“We therefore have to rely mainly on the results of numerical simulations of stellar winds, calibrated onto a few, mostly indirect, mass-loss measurements (e.g., Wood et al. 2002, 2005).”
MethodRedfield, S., & Linsky, J. L. (2008) · The Astrophysical Journal · doi:10.1086/524002 · Cited by 357 · see citing works
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“Similarly the majority of the valley networks are found almost exclusively in the highly cratered ancient southern highlands, which date back from the end of the heavy bombardment period some 3.5-3.8 Gyr ago (Fasset and Head, 2008).”
BackgroundInfluentialTESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS
Cranmer, S. R., & Saar, S. H. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/741/1/54 · Cited by 341 · see citing works
“If instead these values were used, our modeled mass loss rates would be in better agreement with the astrospheric observations of Wood et al. (2005a).”
MethodResultTHE MASS-DEPENDENCE OF ANGULAR MOMENTUM EVOLUTION IN SUN-LIKE STARS
Matt, S. P., Brun, A. S., Baraffe, I., Bouvier, J., & Chabrier, G. (2015) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/799/2/l23 · Cited by 304 · see citing works
“Despite significant progress in measurements of mass-loss rates of sun-like stars (Wood et al. 2005), theoretical predictions of wind properties (Suzuki et al. 2012; Cranmer & Saar 2011), mapping of surface magnetic fields (Donati & Landstreet 2009), and dynamo models (Miesch & Toomre 2009; Brun et…”
BackgroundSpitzer IRS Spectroscopy of IRAS ‐discovered Debris Disks
Chen, C. H., Sargent, B. A., Bohac, C., Kim, K. H., Leibensperger, E. M., Jura, M., Najita, J., Forrest, W. J., Watson, D. M., Sloan, G. C., et al. (2006) · The Astrophysical Journal Supplement Series · doi:10.1086/505751 · Cited by 299 · see citing works
“Changes in the field structure could precipitate changes in the stellar wind (Wood et al. 2005).”
BackgroundMethodInfluentialA Reappraisal of The Habitability of Planets around M Dwarf Stars
Tarter, J. C., Backus, P. R., Mancinelli, R. L., Aurnou, J. M., Backman, D. E., Basri, G. S., Boss, A. P., Clarke, A., Deming, D., Doyle, L. R., et al. (2007) · Astrobiology · doi:10.1089/ast.2006.0124 · Cited by 340 · see citing works
Khodachenko, M. L., Ribas, I., Lammer, H., Grießmeier, J. ‐., Leitner, M., Selsis, F., Eiroa, C., Hanslmeier, A., Biernat, H. K., Farrugia, C. J., et al. (2007) · Astrobiology · doi:10.1089/ast.2006.0127 · Cited by 275 · see citing works
Atmospheric Escape and Evolution of Terrestrial Planets and Satellites
Lammer, H., Kasting, J. F., Chassefière, E., Johnson, R. E., Kulikov, Y. N., & Tian, F. (2008) · Space Science Reviews · doi:10.1007/s11214-008-9413-5 · Cited by 275 · see citing works
“HST high-resolution spectroscopic observations of the hydrogen Lyman-α feature of several nearby main-sequence G and K stars by Wood et al. (2002, 2005) have revealed the absorption of neutral hydrogen associated with the interaction between the stars’ fully ionized coronal winds with the partially…”
BackgroundInfluentialWood, B. E., & Linsky, J. L. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/717/2/1279 · Cited by 265 · see citing works
“As mentioned in Section 1, ξ Boo has a measured wind strength of 5 Ṁ , but the measurement is for the combined wind of the system, and there is no way to tell from the observations the contribution of each star to this total (Wood et al. 2005a).”
BackgroundMethodResultInfluentialSelf-citationImpact of space weather on climate and habitability of terrestrial-type exoplanets
Airapetian, V. S., Barnes, R., Cohen, O., Collinson, G. A., Danchi, W. C., Dong, C., C, A. D. D. G., France, K., Garcia-Sage, K., Glocer, A., et al. (2019) · International Journal of Astrobiology · doi:10.1017/s1473550419000132 · Cited by 256 · see citing works
Self-citationMAVEN observations of the response of Mars to an interplanetary coronal mass ejection
JAKOSKY, B. M., Grebowsky, J. M., LUHMANN, J. G., Connerney, J. E. P., Eparvier, F. G., Ergun, R. E., Halekas, J. S., Larson, D. E., Mahaffy, P. R., McFadden, J., et al. (2015) · Science · doi:10.1126/science.aad0210 · Cited by 244 · see citing works
“Given the likely prevalence of ICMElike conditions earlier in solar-systemhistory (43), it is possible that ion escape rates at that time were dominated by storm events.”
Hillenbrand, L. A., Carpenter, J. M., Kim, J. S., Meyer, M. R., Backman, D. E., Moro‐Martín, A., Hollenbach, D. J., Hines, D. C., Pascucci, I., & Bouwman, J. (2008) · The Astrophysical Journal · doi:10.1086/529027 · Cited by 230 · see citing works
“There is still significant uncertainty in the appropriate values, however (e.g., Wood et al. 2005; Matt & Pudritz 2007), and so we do not consider further the details of this potentially relevant dust removal mechanism.”
BackgroundEvolution of protoplanetary discs with magnetically driven disc winds
Suzuki, T. K., Ogihara, M., Morbidelli, A., Crida, A., & Guillot, T. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628955 · Cited by 230 · see citing works
“Even after the accretion terminates, the mass flux of the stellar wind is expected to be still high because of the high magnetic activity (Wood et al. 2005; Cranmer & Saar 2011; Suzuki et al. 2013).”
BackgroundStellar winds on the main-sequence: II. The evolution of rotation and winds
Johnstone, C. P., Güdel, M., Brott, I., & Lüftinger, T. (2015) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201425301 · Cited by 229 · see citing works
“However, our results suggest a further M−3.36? dependence for the mass loss rate, and so the results could have been biased by the fact that the intermediate activity stars in the sample of Wood et al. (2005) were mostly K stars, whereas the low activity stars were mostly G stars.”
BackgroundResultInfluentialStrubbe, L. E., & Chiang, E. (2006) · The Astrophysical Journal · doi:10.1086/505736 · Cited by 212 · see citing works
“Nevertheless, it is unclear whether the measurements of Wood et al. (2005) apply to this highly variable, pre-main-sequence star.”
BackgroundPOSSIBLE DISINTEGRATING SHORT-PERIOD SUPER-MERCURY ORBITING KIC 12557548
Rappaport, S., Levine, A., Chiang, E., El Mellah, I., Jenkins, J., Kalomeni, B., Kite, E. S., Kotson, M., Nelson, L., Rousseau-Nepton, L., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/752/1/1 · Cited by 223 · see citing works
“This explains the well-known observation that the ionized gas tails of comets are swept anti-Sunward, in the direction of the Solar wind.”
The Mass-Dependence of Angular Momentum Evolution in Sun-Like Stars
Matt, S. P., Brun, A. S., Baraffe, I., Bouvier, J., & Chabrier, G. (2025) · Figshare · Cited by 213 · see citing works
van Saders, J. L., & Pinsonneault, M. H. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/776/2/67 · Cited by 211 · see citing works
“The mass loss rate is assumed proportional to Lx (Wood et al. 2005), and we adopt Lx/Lbol ∼ ω 2 (Pizzolato et al. 2003), again up to a saturation threshold.”
MethodNEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THESPITZER SPACE TELESCOPE
Plavchan, P., Werner, M. W., Chen, C. H., Stapelfeldt, K. R., Su, K. Y. L., Stauffer, J. R., & Song, I. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/698/2/1068 · Cited by 209 · see citing works
“However, at these ages of <700 Myr, X-ray activity is not a reliable proxy for stellar wind mass-loss rate as discovered in (Wood et al. 2005).”
InfluentialThe Sun in Time: Activity and Environment
Güdel, M. (2007) · Living Reviews in Solar Physics · doi:10.12942/lrsp-2007-3 · Cited by 205 · see citing works
“The only independent variable, the stellar age, then determines the rotation period and, through the internal magnetic dynamo, magnetic activity at all levels of the stellar atmosphere, probably including characteristics of the stellar wind (Wood et al., 2002, 2005; Kulikov et al., 2006).”
BackgroundMethodResultInfluentialFORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS
Carpenter, J. M., Bouwman, J., Mamajek, E. E., Meyer, M. R., Hillenbrand, L. A., Backman, D. E., Henning, T. K., Hines, D. C., Hollenbach, D. J., Kim, J. S., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/181/1/197 · Cited by 193 · see citing works
“However, given the uncertainties on the scaling of mass loss rates with stellar age (Wood et al. 2002, 2005), we do not consider wind drag effects.”
BackgroundHELIOSPHERIC STRUCTURE: THE BOW WAVE AND THE HYDROGEN WALL
Zank, G. P., Heerikhuisen, J., Wood, B. E., Pogorelov, N. V., Zirnstein, E. J., & McComas, D. J. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/763/1/20 · Cited by 186 · see citing works
“The precise methodology for synthesizing Lyα profiles from heliospheric models is described in detail elsewhere (Gayley et al. 1997; Wood et al. 2000, 2005b, 2007a).”
Self-citationPartially Ionized Plasmas in Astrophysics
Ballester, J. L., Alexeev, I. I., Collados, M., Downes, T. P., Pfaff, R. F., Gilbert, H. R., Khodachenko, M. L., Khomenko, E., Шайхисламов, И. Ф., Soler, R., et al. (2018) · Space Science Reviews · doi:10.1007/s11214-018-0485-6 · Cited by 183 · see citing works
“…absorption to that calculated by hydrodynamic codes made it possible to perform empirical estimation of the evolution of the stellar mass loss rate as a function of stellar age (Wood et al. 2002, 2005) and to conclude about 128 the dependence of nsw and vsw on the age of the stellar system.”
MethodImproved angular momentum evolution model for solar-like stars
Gallet, F., & Bouvier, J. (2013) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201321302/pdf · Cited by 173 · see citing works
A magnetic field evolution scenario for brown dwarfs and giant planets
Reiners, A., & Christensen, U. R. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014251 · Cited by 167 · see citing works
“…we parameterize the stellar mass-loss rates using the results from Wood et al. (2005) and use X-ray luminosities taken from the NEXXUS database1 (Schmitt & Liefke 2004) in analogy with Stevens (2005) but with the updated parameters from Wood et al. (2005) Ṁ⋆ Ṁ⊙ = ( R⋆ R⊙ )2 ( FX FX,⊙ )1.34 .”
BackgroundMethodInfluentialAlvarado‐Gómez, J. D., Drake, J. J., Cohen, O., Moschou, S. P., & Garraffo, C. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aacb7f · Cited by 166 · see citing works
“…generic field configuration driving the simulation, the resulting *Ṁ is comparable with the estimates from astrospheric Lyα absorption reported by Wood et al. (2005), for stars with commensurate large-scale magnetic field strengths (e.g., ξ Boo A, Morgenthaler et al. 2012; ò Eri, Jeffers et…”
BackgroundResultVidotto, A. A., Jardine, M., Morin, J., Donati, J. ‐., Opher, M., & Gombosi, T. I. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2265 · Cited by 165 · see citing works
“However, mass-loss rates of cool stars are notoriously difficult to observe (e.g. Wood et al. 2005).”
BackgroundPredicting low-frequency radio fluxes of known extrasolar planets
Grießmeier, J. ‐., Zarka, P., & Spreeuw, H. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20077397 · Cited by 164 · see citing works
“Comparing the measured absorption to that calculated by hydrodynamic codes, these measurements allowed the first empirical estimation of the evolution of the stellar mass loss rate as a function of stellar age (Wood et al., 2002; Wood, 2004; Wood et al., 2005).”
BackgroundMethodInfluentialPlanetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution
Lundin, R., Lammer, H., & Ribas, I. (2007) · Space Science Reviews · doi:10.1007/s11214-007-9176-4 · Cited by 161 · see citing works
IMPLICATIONS OF MASS AND ENERGY LOSS DUE TO CORONAL MASS EJECTIONS ON MAGNETICALLY ACTIVE STARS
Drake, J. J., Cohen, O., Yashiro, S., & Gopalswamy, N. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/764/2/170 · Cited by 160 · see citing works
“Wood et al. (2002) and Wood et al. (2005) estimated mass loss rates for a handful of stars of different activity level using astrospheric Lyα absorption.”
BackgroundResultInfluentialThe MUSCLES Treasury Survey. V. FUV Flares on Active and Inactive M Dwarfs* † ‡
Loyd, R. O. P., France, K. C., Youngblood, A. A., Schneider, C., Brown, A., Hu, R., Segura, A., Linsky, J. L., Redfield, S., Tian, F., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aae2bd · Cited by 155 · see citing works
Self-citationCarbon Deficiency in Externally Polluted White Dwarfs: Evidence for Accretion of Asteroids
Jura, M. A. (2006) · The Astrophysical Journal · doi:10.1086/508738 · Cited by 153 · see citing works
X-rays from solar system objects
Bhardwaj, A., Elsner, R. F., Gladstone, G. R., Cravens, T. E., Lisse, C. M., Dennerl, K., Branduardi-Raymont, G., Wargelin, B. J., Waite, J. H., Robertson, I. P., et al. (2007) · Planetary and Space Science · doi:10.1016/j.pss.2006.11.009 · Cited by 152 · see citing works
Magnetic moment and plasma environment of HD 209458b as determined from Lyα observations
Kislyakova, K. G., Holmström, M., Lammer, H., Odert, P., & Khodachenko, M. L. (2014) · Science · doi:10.1126/science.1257829 · Cited by 150 · see citing works
Faltering Steps Into the Galaxy: The Boundary Regions of the Heliosphere
Zank, G. P. (2015) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082214-122254 · Cited by 147 · see citing works
Self-citationAarnio, A. N., Matt, S. P., & Stassun, K. G. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/760/1/9 · Cited by 142 · see citing works
“…scaled-up solar-type winds and elevated solar-type Xray activity do not decline to present-day solar levels until approximately 1 Gyr (Wood 2004; Wood et al. 2005; Guedel et al. 1997), potentially affecting the ongoing evolution of the star’s angular momentum and the circumstellar environments…”
BackgroundChen, C. H., Mamajek, E. E., Bitner, M. A., Pecaut, M., Su, K. Y. L., & Weinberger, A. J. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/738/2/122 · Cited by 138 · see citing works
“Since that study was published, Wood et al. (2005) better quantify the relationship between stellar mass-loss rate and surface X-ray flux, finding a better fit with the power-law function, Ṁwind/A ∝ F 1.34±0.18x .”
InfluentialBackman, D. E., Marengo, M., Stapelfeldt, K. R., Su, K. Y. L., Wilner, D. J., Dowell, C. D., Watson, D. M., Stansberry, J., Rieke, G. H., Megeath, S. T., et al. (2008) · The Astrophysical Journal · doi:10.1088/0004-637x/690/2/1522 · Cited by 140 · see citing works
“Eri has been determined to be ∼3–4 × 1010 kg s−1 (Stevens 2005; Wood et al. 2005), about 20–30× the solar value.”
Ultra-wideband Detection of 22 Coherent Radio Bursts on M Dwarfs
Villadsen, J., & Hallinan, G. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf88e · Cited by 140 · see citing works
“…Lyman α absorption in the astrosphere of active M dwarf EV Lac indicate that it has a mass loss rate similar to the Sun (assuming isotropic mass loss; Wood et al. 2005), in contrast to the flare-based prediction of Osten & Wolk (2015) that it would be up to 500 times greater due to frequent CMEs.”
ResultThe evolution of the solar wind
Vidotto, A. A. (2021) · Living Reviews in Solar Physics · doi:10.1007/s41116-021-00029-w · Cited by 140 · see citing works
“4), Wood et al. (2005a) found that _M=R2 / F1:34 0:18X , with the fit being valid for FX.106 erg cm 2 s 1.”
BackgroundInfluentialKulikov, Y. N., Lammer, H., Lichtenegger, H. I. M., Penz, T., Breuer, D., Spohn, T., Lundin, R., & Biernat, H. K. (2007) · Space Science Reviews · doi:10.1007/s11214-007-9192-4 · Cited by 139 · see citing works
Magnetic field strengths of hot Jupiters from signals of star–planet interactions
Cauley, P. W., Shkolnik, E. L., Llama, J., & Lanza, A. F. (2019) · Nature Astronomy · doi:10.1038/s41550-019-0840-x · Cited by 139 · see citing works
New Observational Constraints on the Winds of M dwarf Stars*
Wood, B. E., Müller, H., Redfield, S., Konow, F. P., Vannier, H., Linsky, J. L., Youngblood, A. A., Vidotto, A. A., Jardine, M., Alvarado‐Gómez, J. D., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abfda5 · Cited by 138 · see citing works
Self-citationThe stellar wind cycles and planetary radio emission of the τ Boo system
Vidotto, A. A., Farès, R., Jardine, M., Donati, J. ‐., Opher, M., Moutou, C., Catala, C., & Gombosi, T. I. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21122.x · Cited by 134 · see citing works
“Other estimates were derived by Stevens (2005, Ṁ ≈ 83.4 Ṁ⊙ ≈ 1.67 × 10 −12 M⊙ yr −1) and Reiners & Christensen (2010, Ṁ ≈ 198.5 Ṁ⊙ ≈ 3.97 × 10−12 M⊙ yr −1), who adopted the empirically derived relation between Ṁ and the X-ray flux from Wood et al. (2002, 2005).”
InfluentialRotating models of young solar-type stars
Amard, L., Palacios, A., Charbonnel, C., Gallet, F., & Bouvier, J. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201527349 · Cited by 134 · see citing works
“Van Saders & Pinsonneault (2013) extended the application to more massive stars (1.1-1.5M⊙) by combining this prescription with the mass-loss rate of Wood et al. (2005).”
BackgroundInfluentialPOSSIBLE DISINTEGRATING SHORT-PERIOD SUPER-MERCURY ORBITING KIC 12557548
Chiang, E., Mellah, I. E., Jenkins, J. M., Kalomeni, B., Kite, E. S., Kotson, M. C., Nelson, L. A., Rousseau-Nepton, L., Tran, K., Rappaport, S., et al. (2012) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 131 · see citing works
Stellar winds on the main-sequence
Johnstone, C. P., Güdel, M., Lüftinger, T., Tóth, G., & Brott, I. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201425300 · Cited by 128 · see citing works
“Measurements using this technique are now available for several low-mass stars (Wood et al. 2002, 2005, 2014).”
BackgroundMethodInfluentialAtmospheric and water loss from early Venus
Kulikov, Y. N., Lammer, H., Lichtenegger, H. I. M., Terada, N., Ribas, I., Kolb, C., Langmayr, D., Lundin, R., Guinan, E. F., Barabash, S., et al. (2006) · Planetary and Space Science · doi:10.1016/j.pss.2006.04.021 · Cited by 146 · see citing works
Youngblood, A., France, K., Loyd, R. O. P., Brown, A., Mason, J. P., Schneider, P. C., Tilley, M. A., Berta-Thompson, Z. K., Buccino, A., Froning, C. S., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa76dd · Cited by 123 · see citing works
“Probing the astrosphere (analogous to the heliosphere) via high-resolution Lyαmeasurements allows for timeaveraged measurements of the stellar mass-loss rate (Wood et al. 2005a), which includes the accumulation of impulsive events (CMEs) and the quiescent stellar wind.”
BackgroundMethodInfluentialSelf-citationAstrospheres and Solar-like Stellar Winds
Wood, B. E. (2004) · Living Reviews in Solar Physics · doi:10.12942/lrsp-2004-2 · Cited by 121 · see citing works
Self-citationTime history of the Martian dynamo from crater magnetic field analysis
Lillis, R. J., Robbins, S. J., Manga, M., Halekas, J. S., & Frey, H. V. (2013) · Journal of Geophysical Research Planets · doi:10.1002/jgre.20105 · Cited by 123 · see citing works
“When the dynamo-driven global magnetic field disappeared, the early Mars atmosphere was thereafter exposed directly to the solar wind, which was likely substantially stronger than in recent times [Wood et al., 2005].”
ResultRamstad, R., Barabash, S., Futaana, Y., Nilsson, H., Wang, X., & Holmström, M. (2015) · Journal of Geophysical Research Planets · doi:10.1002/2015je004816 · Cited by 120 · see citing works
“, 2005] alongside an overall denser and more dynamic solar wind [Wood et al., 2005].”
BackgroundKite, E. S., Halevy, I., Kahre, M. A., Wolff, M. J., & Manga, M. (2012) · Icarus · doi:10.1016/j.icarus.2012.11.034 · Cited by 119 · see citing works
On the environment surrounding close-in exoplanets
Vidotto, A. A., Farès, R., Jardine, M., Moutou, C., & Donati, J. ‐. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv618 · Cited by 118 · see citing works
“The velocity and density structures are scaled with respect to the age of the system, based on the age relations found by Newkirk (1980) and Wood et al. (2005).”
BackgroundMethodThe history of the Solar system's debris disc: observable properties of the Kuiper belt
Booth, M., Wyatt, M. C., Morbidelli, A., Moro‐Martín, A., & Levison, H. F. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15286.x · Cited by 113 · see citing works
“For the change in stellar mass-loss rate with time, we have taken Ṁ (t) = Ṁ (t/4.5 Gyr)−2.33 for t > 700 Myr from the analysis of stellar mass-loss rates in Wood et al. (2005) and Ṁ (t) = 80 Ṁ for earlier times.”
MethodInfluentialEVIDENCE FOR A WEAK WIND FROM THE YOUNG SUN
Wood, B. E., Müller, H., Redfield, S., & Edelman, E. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/781/2/l33 · Cited by 115 · see citing works
“Our analysis follows procedures developed to study previous Lyα spectra (Wood et al. 2005b).”
BackgroundMethodResultInfluentialSelf-citationTarduno, J. A., Blackman, E. G., & Mamajek, E. E. (2014) · Physics of The Earth and Planetary Interiors · doi:10.1016/j.pepi.2014.05.007 · Cited by 113 · see citing works
“However, while there are only a few solar analogs for times older than 3.45 Ga whose mass loss is constrained by H I Lyman-α observations (e.g. Wood et al., 2005, 2014), the few that are available seem to define mass loss rates that deviate from the trend defined by older stars.”
BackgroundInfluentialThe quest for stellar coronal mass ejections in late-type stars
Vida, K., Leitzinger, M., Kriskovics, L., Seli, B., Odert, P., Kovács, O. E., Korhonen, H., & van Driel-Gesztelyi, L. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834264 · Cited by 113 · see citing works
“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…”
BackgroundAeronomical evidence for higher CO2 levels during Earth's Hadean epoch
Lichtenegger, H. I. M., Lammer, H., Grießmeier, J.-M., Kulikov, Y. N., von Paris, P., Hausleitner, W., Krauss, S., & Rauer, H. (2010) · Icarus · doi:10.1016/j.icarus.2010.06.042 · Cited by 109 · see citing works
Lee, C. O., Jakosky, B. M., Luhmann, J. G., Brain, D. A., Mays, M. L., Hassler, D. M., Holmström, M., Larson, D. E., Mitchell, D. L., Mazelle, C., et al. (2018) · Geophysical Research Letters · doi:10.1029/2018gl079162 · Cited by 107 · see citing works
“Disturbed time periods also provide a foothold for evaluating atmospheric escape at earlier epochs in Mars history, since the solar and solar wind inputs during such time periods are likely to have been more intense than the current quiescent conditions (e.g., Ribas et al., 2005; Wood et al., 2005).”
BackgroundExoplanetary radio emission under different stellar wind conditions
Grießmeier, J. ‐., Preusse, S., Khodachenko, M. L., Motschmann, U., Mann, G., & Rucker, H. O. (2006) · Planetary and Space Science · doi:10.1016/j.pss.2006.01.008 · Cited by 107 · see citing works
Earth's atmosphere – Hadean to early Proterozoic
Shaw, G. H. (2008) · Geochemistry · doi:10.1016/j.chemer.2008.05.001 · Cited by 83 · see citing works
“Suggestions that the necessary warm climate was due to a more massive early sun (Sackman and Boothroyd, 2003) have been countered by observations of limited mass loss from the sun and comparable stars (Wood et al., 2005; Minton and Malhotra, 2007).”
BackgroundThe effects of stellar winds on the magnetospheres and potential habitability of exoplanets
See, V., Jardine, M., Vidotto, A. A., Petit, P. M., Marsden, S. C., Jeffers, S. V., & do Nascimento, J.-D. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424323 · Cited by 102 · see citing works
“This is not feasible for stellar winds because of the lack of in situ measurements, although indirect detections do exist (Wood et al. 2005).”
BackgroundCould we identify hot ocean-planets with CoRoT, Kepler and Doppler velocimetry?
Selsis, F., Chazelas, B., Borde, P. J., Ollivier, M., Brachet, F., Decaudin, M., Bouchy, F., Ehrenreich, D., Grießmeier, J. ‐., Lammer, H., et al. (2007) · Icarus · doi:10.1016/j.icarus.2007.04.010 · Cited by 102 · see citing works
“In order to make an upper estimate of the possible losses, we used constant wind properties corresponding the highest mass loss measured by Wood et al. (2005).”
BackgroundMethodInfluentialTerada, N., Kulikov, Y. N., Lammer, H., Lichtenegger, H., Tanaka, T., Shinagawa, H., & Zhang, T. (2009) · Astrobiology · doi:10.1089/ast.2008.0250 · Cited by 101 · see citing works
“Such high EUV flux and solar wind density values are expected to have existed during the first (cid:2) 100–150 million years after the young Sun arrived at the ZAMS (Zahnle and Walker, 1982; Ayres 1997; Guinan and Ribas, 2002; Wood et al. , 2002, 2005; Ribas et al. , 2005; Lundin et al. , 2007).”
InfluentialThe Formation and Evolution of Planetary Systems: Placing Our Solar System in Context withSpitzer
Meyer, M. R., Hillenbrand, L. A., Backman, D., Beckwith, S., Bouwman, J., Brooke, T., Carpenter, J., Cohen, M., Cortes, S., Crockett, N., et al. (2006) · Publications of the Astronomical Society of the Pacific · doi:10.1086/510099 · Cited by 99 · see citing works
Stellar Winds on the Main-Sequence II: the Evolution of Rotation and WindsPreprint
Johnstone, C. P., Güdel, M., Brott, I., & Lüftinger, T. (2015) · arXiv (Cornell University) · doi:10.48550/arxiv.1503.07494 · Cited by 99 · see citing works
“However, our results suggest a further M−3.36? dependence for the mass loss rate, and so the results could have been biased by the fact that the intermediate activity stars in the sample of Wood et al. (2005) were mostly K stars, whereas the low activity stars were mostly G stars.”
BackgroundResultInfluentialTurbulence‐driven Polar Winds from T Tauri Stars Energized by Magnetospheric Accretion
Cranmer, S. R. (2008) · The Astrophysical Journal · doi:10.1086/592566 · Cited by 98 · see citing works
“This stands in contrast to the observationally inferred power-law decrease for these stages, which is approximatelyṀwind ∝ t−2 (e.g., Wood et al. 2002, 2005).”
ResultThe HARPS search for southern extra-solar planets
Delfosse, X., Bonfils, X., Forveille, T., Udry, S., Mayor, M., Bouchy, F., Gillon, M., Lovis, C., Neves, V., Pepe, F. A., et al. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201219013 · Cited by 93 · see citing works
“…the intensity and frequency of CMEs for M dwarfs (which is poorly known, and may be much smaller that initialy claimed (van den Oord & Doyle 1997; Wood et al. 2005)), (2) the magnetic moment of the planet (a strong magnetosphere will protect the planet against CME-induced Ion Pick Up (Lammer et…”
BackgroundRhee, J. H., Song, I., & Zuckerman, B. (2008) · The Astrophysical Journal · doi:10.1086/524935 · Cited by 91 · see citing works
“More recent observation and analysis somewhat cloud quantitative representation of the wind strength as a function of time (Wood et al. 2005; Wood 2006).”
Ion Acceleration and Outflow from Mars and Venus: An Overview
Lundin, R. (2011) · Space Science Reviews · doi:10.1007/s11214-011-9811-y · Cited by 90 · see citing works
Fontenla, J. M., Linsky, J. L., Garrison, J., France, K. C., Buccino, A. P., Mauas, P. J. D., Vieytes, M., & Walkowicz, L. M. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/830/2/154 · Cited by 88 · see citing works
“…utilized for reconstructing the Ly-α line: (1) using the interstellar absorption profiles of the D I Ly-α and metal lines to infer the H I absorption (Wood et al. 2005), and (2) a self-consistent solution for the interstellar absorption parameters and the intrinsic stellar emission line that best…”
MethodSelf-citationTheoretical mass loss rates of cool main-sequence stars
Holzwarth, V., & Jardine, M. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20066486 · Cited by 89 · see citing works
“Crosses along the curves mark the transition between the regimes of slow and fast magnetic rotators, andsymbols show the values inferred by Wood et al. (2005a) for main-sequence (single and binary) stars of different spectral types.”
BackgroundMethodResultInfluentialDong, C., Lee, Y., Ma, Y., Lingam, M., Bougher, S., Luhmann, J., Curry, S., Tóth, G., Nagy, A., Tenishev, V., et al. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aac489 · Cited by 87 · see citing works
Turbulent Generation of Magnetic Switchbacks in the Alfvénic Solar Wind
Shoda, M., Chandran, B. D. G., & Cranmer, S. R. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abfdbc · Cited by 88 · see citing works
A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved withHerschel
Lestrade, J.-F., Matthews, B. C., Sibthorpe, B., Kennedy, G. M., Wyatt, M. C., Bryden, G., Greaves, J. S., Thilliez, E., Moro‐Martín, A., Booth, M., et al. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201220325 · Cited by 87 · see citing works
“The correlation between X-ray surface flux and mass loss rateof GKM-type stars (Wood et al. 2005) then yields the upper limit of 2 Ṁ⊙, where the solar mass loss rateṀ⊙ = 2×10−14 M⊙ yr−1.”
BackgroundStellar coronal mass ejections – I. Estimating occurrence frequencies and mass-loss rates
Odert, P., Leitzinger, M., Hanslmeier, A., & Lammer, H. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1969 · Cited by 87 · see citing works
“However, there is a surprisingly high number of non-detections of astrospheric Ly α absorption for many active stars (Wood et al. 2005a, 2014), which we also show in Fig.”
BackgroundMethodInfluentialHeliospheric Response to Different Possible Interstellar Environments
Müller, H., Frisch, P. C., Florinski, V., & Zank, G. P. (2006) · The Astrophysical Journal · doi:10.1086/505588 · Cited by 86 · see citing works
“With the possible exception of Oph, interstellar column densities toward stars within 35 pc of the Sun do not exceed 1019 cm 2 (e.g., Frisch 2004; Redfield & Linsky 2004a; Wood et al. 2005b).”
BackgroundSelf-citationDust in the solar system and in extra-solar planetary systems
Mann, I. B., Köhler, M., Kimura, H., Cechowski, A., & Minato, T. (2006) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-006-0028-0 · Cited by 83 · see citing works
Angular momentum and mass evolution of contact binaries
Gazeas, K., & Stȩpień, K. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13844.x · Cited by 83 · see citing works
The Upper Edge of the Neptune Desert Is Stable Against Photoevaporation
Vissapragada, S., Knutson, H., Greklek-McKeon, M., Oklopčić, A., Dai, F., dos Santos, L. D., Jovanovic, N., Mawet, D., Millar-Blanchaer, M., Paragas, K., et al. (2022) · Astronomical Journal · doi:10.3847/1538-3881/ac92f2 · Cited by 46 · see citing works
“We can use the aforementioned X-ray fluxes along with the Wood et al. (2005) relation to estimate the stellar mass-loss rate for WASP-80.”
BackgroundMethodSaturation of StellarWinds from Young Suns
Suzuki, T. K., Imada, S., Kataoka, R., Kato, Y., Matsumoto, T., Miyahara, H., & Tsuneta, S. (2013) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/65.5.98 · Cited by 82 · see citing works
“We use Ṁ⊙ =2×10−14M⊙ yr−1 and v⊙ =400 km s−1 as the normalizations in Figure 12 according to Wood et al. (2002; 2005).”
BackgroundMethodResultInfluentialIs the Faint Young Sun Problem for Earth Solved?
Charnay, B., Wolf, E. T., Marty, B. M., & Forget, F. (2020) · Space Science Reviews · doi:10.1007/s11214-020-00711-9 · Cited by 83 · see citing works
Khodachenko, M. L., Alexeev, I. I., Belenkaya, E. S., Lammer, H., Grießmeier, J. ‐., Leitzinger, M., Odert, P., Zaqarashvili, T. V., & Rucker, H. O. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/744/1/70 · Cited by 78 · see citing works
“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. (2007a) estimated the time dependence of the stellar wind velocity and density at 1 AU (e.g., nsw(t, d = 1 AU) and vsw(t, d = 1…”
BackgroundResultThe Impact of Metallicity on the Evolution of the Rotation and Magnetic Activity of Sun-like Stars
Amard, L., & Matt, S. (2020) · Astrophysical Journal · doi:10.3847/1538-4357/ab6173 · Cited by 46 · see citing works
Simulating the environment around planet-hosting stars
Alvarado‐Gómez, J. D., Hussain, G. A. J., Cohen, O., Drake, J. J., Garraffo, C., Grunhut, J., & Gombosi, T. I. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628988 · Cited by 75 · see citing works
“This evidence is not only given directly by the astrospheric detections of ξ Boo A and π1 UMa (Wood et al. 2014), but also indirectly, by similar UV observations of a considerable number of active stars yielding non-detections (Wood et al. 2005b).”
BackgroundInfluentialHistory of water loss and atmospheric O2 buildup on rocky exoplanets near M dwarfs
Tian, F. (2015) · Earth and Planetary Science Letters · doi:10.1016/j.epsl.2015.09.051 · Cited by 72 · see citing works
Lammer, H., Güdel, M., Kulikov, Y. N., Ribas, I., Zaqarashvili, T. V., Khodachenko, M. L., Kislyakova, K. G., Gröller, H., Odert, P., Leitzinger, M., et al. (2012) · Earth Planets and Space · doi:10.5047/eps.2011.04.002 · Cited by 72 · see citing works
Ion Acceleration and Outflow from Mars and Venus: An Overview
Lundin, R. (2011) · Space sciences series of ISSI · doi:10.1007/978-1-4614-3290-6_9 · Cited by 72 · see citing works
Magnetospheric Emissions from the Planet Orbiting τ Bootis: A Multiepoch Search
Lazio, T. J. W., & Farrell, W. M. (2007) · The Astrophysical Journal · doi:10.1086/519730 · Cited by 71 · see citing works
“It now seems that stellar mass-loss rates change character at a characteristic X-ray flux of about 8 ; 105 erg cm 1 s 1 (Wood et al. 2005).”
BackgroundPlanetary Magnetic Dynamo Effect on Atmospheric Protection of Early Earth and Mars
Dehant, V., Lammer, H., Kulikov, Y. N., Grießmeier, J. ‐., Breuer, D., Verhoeven, O., Karatekin, Ö., Hoolst, T. V., Korablev, O., & Lognonné, P. H. (2007) · Space Science Reviews · doi:10.1007/s11214-007-9163-9 · Cited by 71 · see citing works
“However, recent observations of the absorption signature of the astrosphere of the ∼500 Myr old solar-type G star ‘ξ Boo’ imply that there exists, possibly, a high-activity cutoff time regarding the mass loss in the radiation activity relation (Wood et al. 2005; Lundin et al. 2007).”
BackgroundInfluential
- 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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