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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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“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.”
Method
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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
Cited by
Sorted by citations
Items 201–300 of 467
Full compressible 3D MHD simulation of solar wind
Matsumoto, T. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3533 · Cited by 28
“In addition, Suzuki et al. (2013) suggested a theoretical interpretation for the saturation problem of stellar wind (Wood et al. 2005).”
BackgroundDust amorphization in protoplanetary disks
Glauser, A. M., Güdel, M., Watson, D. M., Henning, T. K., Schegerer, A., Wolf, S., Audard, M., & Baldovin-Saavedra, C. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912087 · Cited by 28
“Although we cannot observe the stellar wind directly, its flux and/or speed might be related to the X-ray luminosity, as shown for low X-ray fluxes by Wood et al. (2005) by comparing stellar mass loss rates with X-ray surface fluxes.”
BackgroundSTELLAR WIND INFLUENCE ON PLANETARY DYNAMOS
Heyner, D., Glaßmeier, K., & Schmitt, D. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/750/2/133 · Cited by 27
Coronal dimmings and what they tell us about solar and stellar coronal mass ejections
Veronig, A., Dissauer, K., Kliem, B., Downs, C., Hudson, H. S., Jin, M., Osten, R. A., Podladchikova, T., Prasad, A., Qiu, J., et al. (2025) · Living Reviews in Solar Physics · doi:10.1007/s41116-025-00041-4 · Cited by 40
Black widow formation by pulsar irradiation and sustained magnetic braking
Ginzburg, S., & Quataert, E. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3358 · Cited by 27
“Although it is too weak to evaporate the companion on a Gyr time-scale (Paper I), this ablated wind is still at least as strong as the measured spontaneous outflows from the sun and other solar-like stars (Wood et al. 2002, 2005).”
BackgroundOne Year in the Life of Young Suns: Data-constrained Corona-wind Model of κ 1 Ceti
Airapetian, V., Jin, M., Lüftinger, T., Saikia, S. B., Kochukhov, O., Güdel, M., Holst, B. V. D., & Manchester, W. B. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac081e · Cited by 27
The Solar Wind Environment in Time
Pognan, Q., Garraffo, C., Cohen, O., & Drake, J. J. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaaebb · Cited by 29
“Wood et al. (2005, 2014, 2015) indirectly measured the mass loss rates for cool main-sequence stars using absorption in high dispersion spectra of Lyα1215.”
BackgroundResultInfluentialTHE EFFECT OF MAGNETIC SPOTS ON STELLAR WINDS AND ANGULAR MOMENTUM LOSS
Cohen, O., Drake, J. J., Kashyap, V. L., & Gombosi, T. I. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/2/1501 · Cited by 27
“In principle, the dependency of the wind speed on the expansion rate, fs, could be fit to stellar wind observations such as those presented by Wood et al. (2005).”
BackgroundTHE INTERSTELLAR MEDIUM IN THEKEPLERSEARCH VOLUME
Johnson, M. C., Redfield, S., & Jensen, A. G. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/807/2/162 · Cited by 26
“Wood et al. (2005), however, measured the mass-loss rate Ṁ for several nearby stars and provided a scaling relation between Ṁ and the x-ray flux FX (for FX < 8× 105 ergs cm−2 s−1).”
BackgroundMethodResultInfluentialSelf-citationEvidence of a signature of planet formation processes from solar neutrino fluxes
Kunitomo, M., Guillot, T., & Buldgen, G. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244169 · Cited by 26
The Lunar Paleo‐Magnetosphere: Implications for the Accumulation of Polar Volatile Deposits
Garrick‐Bethell, I., Poppe, A. R., & Fatemi, S. (2019) · Geophysical Research Letters · doi:10.1029/2019gl082548 · Cited by 26
A Layered Debris Disk around M Star TWA 7 in Scattered Light
Ren, B. B., Choquet, É., Perrin, M. D., Mawet, D. P., Chen, C., Milli, J., Debes, J. H., Rebollido, I., Stark, C. C., Hagan, J., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac03b9 · Cited by 26
Non-thermal water loss of the early Mars: 3D multi-ion hybrid simulations
Boesswetter, A., Lammer, H., Kulikov, Y. N., Motschmann, U., & Simon, S. (2010) · Planetary and Space Science · doi:10.1016/j.pss.2010.10.003 · Cited by 26
Blocking Metal Accretion onto Population III Stars by Stellar Wind
Tanaka, S. J., Chiaki, G., Tominaga, N., & Susa, H. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7e2c · Cited by 25
“For example, a series of observations (Wood et al. 2001, 2002, 2005, 2014) in- dicates 0.1Ṁ < Ṁ?”
From stellar coronae to gyrochronology: A theoretical and observational exploration
Ahuir, J., Brun, A. S., & Strugarek, A. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936974 · Cited by 25
Imprint of planet formation in the deep interior of the Sun
Kunitomo, M., & Guillot, T. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141256 · Cited by 25
Linsky, J. L., Bushinsky, R., Ayres, T., & France, K. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/754/1/69 · Cited by 24
“…sunspots at the pole or at very high latitudes, ξ Boo A (G8 V), the solar-like star just to the right of the break in the mass flux-X-ray correlation (Wood et al. 2005), shows highlatitude spots (Toner & Gray 1988) and Zeeman-Doppler images (ZDI) show an inclined dipole and a large-scale toroidal…”
BackgroundSelf-citationThe Sun and stars as the primary energy input in planetary atmospheres
Ribas, I. (2009) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921309992298 · Cited by 29
“Recent results from the same team (Wood et al. 2005) have casted doubt on the validity of the results for the younger stars, with a break down of the relation for ages below ≈0.7 Gyr.”
ResultInfluentialAn Earth-like Stellar Wind Environment for Proxima Centauri c
Alvarado-Gómez, J. D., Drake, J. J., Garraffo, C., Cohen, O., Poppenhaeger, K., Yadav, R. K., & Moschou, S. P. (2020) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/abb885 · Cited by 23
“34X , Wood et al. 2005).”
From stellar coronae to gyrochronology: A theoretical and observational exploration
Ahuir, J., Brun, A. S., & Strugarek, A. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201936974/pdf · Cited by 23
Inhomogeneity within Local Interstellar Clouds*
Linsky, J. L., Redfield, S., Ryder, D., & Chasan-Taber, A. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac816b · Cited by 23
“Wood et al. (2005a) described their analysis of Lyα lines that take into account the extra absorption on the red side of the interstellar absorption from the heliospheric hydrogen wall and the extra absorption mostly on the blue side from the astrospheric hydrogen wall.”
BackgroundSelf-citationCatastrophic rotational braking among Sun-like stars
Gondoin, P. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629760 · Cited by 23
“I followed this second approach based on observational indications by Wood et al. (2005, 2014) that the mass-loss rate of Sun-like stars increases as a power law of their X-ray surface flux.”
MethodTransit Lyman-α signatures of terrestrial planets in the habitable zones of M dwarfs
Kislyakova, K. G., Holmström, M., Odert, P., Lammer, H., Erkaev, N. V., Khodachenko, M. L., Shaikhislamov, I. F., Dorfi, E., & Güdel, M. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833941 · Cited by 23
HUBBLE SPACE TELESCOPE CONSTRAINTS ON THE WINDS AND ASTROSPHERES OF RED GIANT STARS*
Wood, B. E., Müller, H., & Harper, G. M. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/829/2/74 · Cited by 23
“For mainsequence stars, the Mg II fluxes span a range of about a factor of 30 at a given spectral type, due to chromospheric and coronal emission being largely determined by rotation rate, which can vary greatly (e.g., Mathioudakis et al. 1995; Ribas et al. 2005; Wood et al. 2005b).”
Self-citationDetection Methods and Relevance of Exoplanetary Magnetic Fields
Grießmeier, J. ‐. (2014) · Astrophysics and space science library · doi:10.1007/978-3-319-09749-7_11 · Cited by 26
Attempts to Probe the Ozone Layer and the Ultraviolet-B Levels of the Past
Björn, L. O., & McKenzie, R. (2007) · AMBIO · doi:10.1579/0044-7447(2007)36[366:atptol]2.0.co;2 · Cited by 24
On the Effect of Magnetic Spots on Stellar Winds and Angular Momentum LossPreprint
Cohen, O., Drake, J. J., Kashyap, V. L., & Gombosi, T. I. (2012) · Cited by 23
A CATALOG OF STELLAR EVOLUTION PROFILES AND THE EFFECTS OF VARIABLE COMPOSITION ON HABITABLE SYSTEMS
Truitt, A., Young, P. A., Spacek, A., Probst, L., & Dietrich, J. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/804/2/145 · Cited by 21
“(Heightened early mass loss seen in some young stars Wood et al. 2005 is not included.)”
BackgroundThe winds of young Solar-type stars in the Hyades
Evensberget, D., Carter, B., Marsden, S. C., Brookshaw, L., & Folsom, C. P. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1696 · Cited by 22
Circumbinary habitability niches
Mason, P., Zuluaga, J. I., Cuartas-Restrepo, P. A., & Clark, J. M. (2014) · International Journal of Astrobiology · doi:10.1017/s1473550414000342 · Cited by 22
“Rapidly rotating stars are luminous XUV sources, due to intense chromospheric activity, and thereby undergo significant mass loss (Wood et al. 2005).”
BackgroundFinley, A. J., See, V., & Matt, S. P. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab12d2 · Cited by 22
Rossby waves and polar spots in rapidly rotating stars: implications for stellar wind evolution
Zaqarashvili, T. V., Oliver, R., Ballester, J. L., Carbonell, M., Khodachenko, M. L., Lammer, H., Leitzinger, M., & Odert, P. (2011) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201117122/pdf · Cited by 22
Liu, K., Kallio, E., Jarvinen, R., Lammer, H., Lichtenegger, H., Kulikov, Y. N., Terada, N., Zhang, T., & Janhunen, P. (2009) · Advances in Space Research · doi:10.1016/j.asr.2009.01.005 · Cited by 22
A Lyα Transit Left Undetected: the Environment and Atmospheric Behavior of K2-25b
Rockcliffe, K. E., Newton, E. R., Youngblood, A. A., Bourrier, V., Mann, A. W., Berta-Thompson, Z. K., Agüeros, M. A., Núñez, A., & Charbonneau, D. (2021) · The Astronomical Journal · doi:10.3847/1538-3881/ac126f · Cited by 21
Stellar Aspects of Habitability—Characterizing Target Stars for Terrestrial Planet-Finding Missions
Kaltenegger, L., Eiroa, C., Ribas, I., Paresce, F., Leitzinger, M., Odert, P., Hanslmeier, A., Fridlund, M. C., Lammer, H., Beichman, C., et al. (2010) · Astrobiology · doi:10.1089/ast.2009.0367 · Cited by 21
“…to the evolution of the radiation and plasma outflow of their host stars (which are much more intense compared to similar stars that are several billion years old) when the young stars arrive at the zero-age main sequence (Ayres, 1997; Wood et al., 2002, 2005; Ribas et al., 2005; Gu¨del, 2007).”
InfluentialCollisionless Damping of Fast Magnetohydrodynamic Waves in Magnetorotational Winds
Suzuki, T. K., Yan, H., Lazarian, A., & Cassinelli, J. P. (2006) · The Astrophysical Journal · doi:10.1086/500164 · Cited by 20
“A larger mass-loss rate, ṀE ¼ 2 ; 10 13 M yr 1, is employed than the present solar value, Ṁ ’ 2 ; 10 14 M yr 1, because young solar-mass stars are found to have a larger mass-loss rate (Wood et al. 2002, 2005), possibly as a result of their enhanced coronal activities or stellar rotation.”
MethodHydrogen 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) · Astrophysics and Space Science · doi:10.1007/s10509-011-0604-2 · Cited by 20
The critical binary star separation for a planetary system origin of white dwarf pollution
Veras, D., Xu, S., & Rebassa-Mansergas, A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2141 · Cited by 20
“The evolution of the Solar wind through time, t, is welldescribed by a power law with a exponent of t−2.33±0.55 (Wood et al. 2005), which is consistent with the t−2 dependence reported in equation 4 of Wood et al. (2002) and equation 9 of Zendejas et al. (2010).”
BackgroundResultInfluentialAn Orbital Window into the Ancient Sun’s Mass
Spalding, C., Fischer, W. W., & Laughlin, G. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aaf219 · Cited by 19
Atmospheric Escape and Evolution of Terrestrial Planets and Satellites
Lammer, H., Kasting, J. F., Chassefière, É., Johnson, R. E., Kulikov, Y. N., & Tian, F. (2008) · Space sciences series of ISSI · doi:10.1007/978-0-387-87825-6_11 · Cited by 28
Habitable Zones Exposed: Astrosphere Collapse Frequency as a Function of Stellar Mass
Smith, D. S., & Scalo, J. (2009) · Astrobiology · doi:10.1089/ast.2009.0337 · Cited by 20
“Observations of Wood et al. (2005) suggest b ¼ (cid:2) 2.33, but with use of the same relation between mass-loss rate and X-ray flux as Wood et al. (2005), the recent surveys of X-ray fluxes of dwarf M stars by Penz and Micela (2008) suggest b ¼(cid:2) 1.8.”
InfluentialRadiative levitation in carbon-enhanced metal-poor stars withs-process enrichment
Matrozis, E., & Stancliffe, R. J. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201628540 · Cited by 20
“While mass-loss rates in these stars are too small to be directly observable, indirect measurements based on the interaction of the wind with the interstellar medium yield values within about an order of magnitude of the solar mass-loss rate (Wood et al. 2002, 2005).”
BackgroundAn M Dwarf’s Chromosphere, Corona, and Wind Connection via Nonlinear Alfvén Waves
Sakaue, T., & Shibata, K. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac0e34 · Cited by 19
The winds of young Solar-type stars in Coma Berenices and Hercules-Lyra
Evensberget, D., Carter, B., Marsden, S. C., Brookshaw, L., Folsom, C. P., & Salmeron, R. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3557 · Cited by 19
The winds of young Solar-type stars in the Pleiades, AB Doradus, Columba, and β Pictoris
Evensberget, D., Marsden, S. C., Carter, B., Salmeron, R., Vidotto, A. A., Folsom, C. P., Kavanagh, R. D., Pineda, J. S., Driessen, F. A., & Strickert, K. M. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1650 · Cited by 19
Collisional modelling of the debris disc around HIP 17439
Schüppler, C., Löhne, T., Krivov, A. V., Ertel, S., Marshall, J. P., & Eiroa, C. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423523 · Cited by 19
“For moderately rotating K main sequence stars with radiusR⋆, Wood et al. (2005) found a correlation between the stellar Xray flux FX and the mass loss rate bẏM⋆/R2⋆ ∝ F 1.34±0.18 X as long asFX .”
BackgroundInfluentialHot grain dynamics by electric charging and magnetic trapping in debris disks
Kimura, H., Kunitomo, M., Suzuki, T. K., Robrade, J., Thébault, P., & Mitsuishi, I. (2018) · Planetary and Space Science · doi:10.1016/j.pss.2018.07.010 · Cited by 19
“(34) does not account for the evolution of stellar mass-loss rates observed for solar-type stars and thus might significantly overestimate or underestimate the mass-loss rates (cf. Wood et al. 2002, 2005).”
BackgroundMagnetic activity evolution on Sun-like stars
Gondoin, P. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201731541 · Cited by 19
Global trends in winds of M dwarf stars
Mesquita, A. L., & Vidotto, A. A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa798 · Cited by 19
“Another more successful method used to detect stellar winds is related to the study of stellar Ly-α line absorption when the stellar wind exchange charges with a neutral or partially neutral interstellar medium (Wood et al. 2002, 2005).”
MethodThe Changing Picture of Volatiles and Climate on Mars
JAKOSKY, B. M., Haberle, R. M., & Arvidson, R. E. (2005) · Science · doi:10.1126/science.1118031 · Cited by 19
Stellar Flares, Superflares, and Coronal Mass Ejections—Entering the Big Data Era
Vida, K., Kővári, Z., Leitzinger, M., Odert, P., Oláh, K., Seli, B., Kriskovics, L., Greimel, R., & Görgei, A. (2024) · Universe · doi:10.3390/universe10080313 · Cited by 23
“The total stellar mass-loss rates also include the mass-loss by CMEs, and therefore the modeled CME mass-loss rates from Odert et al. [192] should be below the observed total mass-loss rates [193,194].”
BackgroundMethodInfluentialGuinan, E. F., & Engle, S. G. (2008) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921309032050 · Cited by 18
“The Loss of the water inventory from Venus Using the XUV irradiance appropriate for the young Sun (from Ribas et al. 2005) and solar wind flux estimates from Wood et al. (2002, 2005), Kulikov et al. (2006) have studied the atmosphere and water loss from early Venus.”
MethodInfluentialDimmock, A. P., Alho, M., Kallio, E., Pope, S. A., Zhang, T., Kilpua, E. K. J., Pulkkinen, T. I., Futaana, Y., & Coates, A. J. (2018) · Journal of Geophysical Research Space Physics · doi:10.1029/2017ja024852 · Cited by 18
Revisiting the Biological Ramifications of Variations in Earth’s Magnetic Field
Lingam, M. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab12eb · Cited by 19
Revisiting the Space Weather Environment of Proxima Centauri b
Garraffo, C., Alvarado‐Gómez, J. D., Cohen, O., & Drake, J. J. (2022) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aca487 · Cited by 17
“34µ★ , Wood et al. 2005; Vidotto et al. 2014; Garraffo et al. 2015a, 2017) and therefore close-in planets are expected to experience stronger stellar winds for longer evolutionary timescales, which puts their atmospheres at risk of being stripped.”
BackgroundNumerical quantification of the wind properties of cool main sequence stars
Chebly, J., Alvarado‐Gómez, J. D., Poppenhaeger, K., & Garraffo, C. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2100 · Cited by 17
Planetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution
Lundin, R., Lammer, H., & Ribas, I. (2007) · Space sciences series of ISSI · doi:10.1007/978-0-387-74288-5_9 · Cited by 18
Modeling the Archean Atmosphere and Climate
Kasting, J. F. (2013) · Elsevier eBooks · doi:10.1016/b978-0-08-095975-7.01306-1 · Cited by 19
Namekata, K., Ikuta, K., Petit, P. M., Airapetian, V., Vidotto, A. A., Heinzel, P., Wollmann, J., Maehara, H., Notsu, Y., Inoue, S., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad85df · Cited by 21
“…the complete X-ray and ultraviolet radiation (e.g., Linsky et al. 2014; Johnstone et al. 2019; Namekata et al. 2023) and plasma environments (e.g., Wood et al. 2005) around stars; however, characterizing these environments is often challenging because stars cannot be spatially resolved and the…”
Episodic warm climates on early Mars primed by crustal hydration
Adams, D., Scheucher, M., Hu, R., Ehlmann, B. L., Thomas, T. B., Wordsworth, R., Scheller, E. L., Lillis, R. J., Smith, K., Rauer, H., et al. (2025) · Nature Geoscience · doi:10.1038/s41561-024-01626-8 · Cited by 17
Signatures of Star-Planet Interactions
Shkolnik, E. L., & Llama, J. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_20 · Cited by 16
“Observing the stellar winds of stars other than the Sun is difficult and there are very few observational constraints on the winds of low-mass stars (Wood et al. 2005).”
BackgroundAtri, D. (2020) · Scientific Reports · doi:10.1038/s41598-020-68715-7 · Cited by 18
Lammer, H., Scherf, M., Itō, Y., Mura, A., Vorburger, A., Guenther, E. W., Wurz, P., Erkaev, N. V., & Odert, P. (2022) · Space Science Reviews · doi:10.1007/s11214-022-00876-5 · Cited by 17
Wiegert, J., Liseau, R., Thébault, P., Olofsson, G., Mora, A., Bryden, G., Marshall, J., Eiroa, C., Montesinos, B., Ardila, D., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201321887 · Cited by 13
“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.”
BackgroundMüller, H.-R., Frisch, P. C., Fields, B. D., & Zank, G. P. (2008) · Space Science Reviews · doi:10.1007/s11214-008-9448-7 · Cited by 16
“For the purpose of calculating astrospheres around stars in the solar neighborhood that are still embedded in a partially ionized ISM, Wood et al. (2003, 2005) determine relative Star-ISM velocities for selected objects.”
Self-citationX-ray detection of astrospheres around three main-sequence stars and their mass-loss rates
Kislyakova, K. G., Güdel, M., Koutroumpa, D., Carter, J. A., Lisse, C. M., & Saikia, S. B. (2024) · Nature Astronomy · doi:10.1038/s41550-024-02222-x · Cited by 15
“The observation 0748010101 of ϵ Eri in large window had a non-standard background, namely, a large box far away from the central star.”
InfluentialHeinrich, M., Khare, B. N., & McKay, C. P. (2007) · Icarus · doi:10.1016/j.icarus.2007.05.017 · Cited by 17
Evolution of solar‐type stellar winds
Suzuki, T. K. (2013) · Astronomische Nachrichten · doi:10.1002/asna.201211751 · Cited by 15
“Observations of asterospheres of low-mass to intermediate-mass stars show that the mass loss rates of young stars are much larger up to∼ 100 times of the present solar value (Wood et al. 2002, 2005).”
BackgroundStatistical Fitting of Evolutionary Models to Rotation Rates of Sun-like Stars
Breimann, A. A., Matt, S. P., & Naylor, T. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abf0a3 · Cited by 15
“Although there are some methods of inferring stellar wind properties, such as measuring Lyα emission (Wood et al. 2005), measuring stellar winds is difficult, and very few measurements exist.”
Formulating Mass-loss Rates for Sun-like Stars: A Hybrid Model Approach
Shoda, M., Cranmer, S. R., & Toriumi, S. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acfa72 · Cited by 14
“…has resulted in a limited number of observed values, which are indirectly obtained through methods such as astrospheric Lyman-alpha absorption (Wood et al. 2002, 2005, 2014, 2021), slingshot prominences (Jardine & Collier Cameron 2019; Jardine et al. 2020), and planetary responses to the…”
MethodMeasuring the Local ISM along the Sight Lines of the Two Voyager Spacecraft with HST/STIS
Zachary, J., Redfield, S., Linsky, J. L., & Wood, B. E. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac017 · Cited by 14
“This equation allows us to compute a Voigt opacity profile, τλ, for H I based on various assumed values for hydrogen column density (Wood et al. 2005b).”
BackgroundMethodResultInfluentialSelf-citationStellar wind retention and expulsion in massive star clusters
Naiman, J., Ramirez-Ruiz, E., & Lin, D. N. C. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1198 · Cited by 14
Johnstone, C. P., Zhilkin, A. G., Pilat‐Lohinger, E., Бисикало, Д. В., Güdel, M., & Eggl, S. (2015) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201425134/pdf · Cited by 14
Fractionation of Solar Wind Minor Ion Precipitation by the Lunar Paleomagnetosphere
Poppe, A. R., Garrick‐Bethell, I., & Fatemi, S. (2021) · The Planetary Science Journal · doi:10.3847/psj/abea7d · Cited by 14
“For the former assumption, we first note that the solar wind flux is believed to have decreased by nearly 2 orders of magnitude over its lifetime (e.g., Wood et al. 2005; Airapetian & Usmanov 2016); thus, even the undisturbed flux of 36Ar to the Moon may have a strong time dependence.”
BackgroundJohnstone, C., Zhilkin, A., Pilat-Lohinger, E., Bisikalo, D., Gudel, M., & Eggl, S. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201425134 · Cited by 11
“Although there are indirect observational constraints on the winds of low-mass stars (e.g. Gaidos et al. 2000; Wood et al. 2005), due to our current inability to directly observe the winds of such stars, binary wind interactions in such systems are less interesting from an observational point of…”
BackgroundThe Science of Exoplanets and Their Systems
Lammer, H., Blanc, M., Benz, W., Fridlund, M. C., du Foresto, V. C., Güdel, M., Rauer, H., Udry, S., Bonnet, R. M., Falanga, M., et al. (2013) · Astrobiology · doi:10.1089/ast.2013.0997 · Cited by 14
“The most accurate method for the reconstruction of stellar Lyman-a emission was developed by Wood et al. (2005) and requires high-resolution spectra of the Lyman-a line and knowledge of the interstellar velocity structure based on high-resolution spectra of the deuterium Lyman-a and metal lines.”
Self-citationVarela, J., Brun, A. S., Strugarek, A., Réville, V., Zarka, P., & Pantellini, F. G. E. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2519 · Cited by 16
Role of Longitudinal Waves in Alfvén-wave-driven Solar Wind
Shimizu, K., Shoda, M., & Suzuki, T. K. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac66d7 · Cited by 13
“Hot coronae and stellar winds are also ubiquitously observed in low-mass main-sequence stars that possess a surface convection zone (Wood et al. 2005, 2021; Güdel et al. 2014; Vidotto 2021) In the framework of the thermally driven wind model, the energy source of the solar wind is the thermal…”
BackgroundScaling and Evolution of Stellar Magnetic Activity
Işık, E., van Saders, J. L., Reiners, A., & Metcalfe, Τ. S. (2023) · Space Science Reviews · doi:10.1007/s11214-023-01016-3 · Cited by 13
“For mass loss, authors commonly adopt either empirical (e.g. Wood et al. 2005, 2021) or theoretical scalings (Cranmer and Saar 2011), but the choice remains a significant uncertainty.”
MethodAmazo-Gómez, E. M., Alvarado‐Gómez, J. D., Poppenhaeger, K., Hussain, G. A. J., Wood, B. E., Drake, J. J., do Nascimento, J.-D., Anthony, F., Sanz‐Forcada, J., Stelzer, B., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2086 · Cited by 12
Self-citationMAGNETIC STRUCTURE OF RAPIDLY ROTATING FK COMAE-TYPE CORONAE
Cohen, O., Drake, J. J., Kashyap, V. L., Korhonen, H., Elstner, D., & Gombosi, T. I. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/719/1/299 · Cited by 12
“However, due to the lack of stellar wind observations, we choose to use of the solar wind input over the use of a few indirect observation and general scaling laws for stellar winds (Wood et al. 2004, 2005), which hold many other uncertainties.”
MethodParametric analysis of modeled ion escape from Mars
Manning, C. V., Ma, Y., Brain, D. A., McKay, C. P., & Zahnle, K. J. (2010) · Icarus · doi:10.1016/j.icarus.2010.11.028 · Cited by 12
Radio Observations as an Exoplanet Discovery Method
Lazio, T. J. W. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_9 · Cited by 12
Collisional modelling of the debris disc around HIP 17439
Schüppler, C., Löhne, T., Krivov, A. V., Ertel, S., Marshall, J. P., & Eiroa, C. (2014) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201423523/pdf · Cited by 12
Xu, Y., Alvarado‐Gómez, J. D., Tian, H., Poppenhaeger, K., Guerrero, G. A., & Liu, X. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad5845 · Cited by 11
“…the X-ray flux per unit surface of the star (denoted as F X ) and the mass loss rate of stellar winds per unit surface area (denoted as ˙ M ⋆ /A ⋆ ) is presented by estimating the stellar mass rate thorough Lyman-α absorption from observation (Wood et al. 2002, 2005; Wood 2018; Wood et al. 2021).”
MethodConstraints on the early luminosity history of the Sun: applications to the Faint Young Sun problem
Basinger, C., Pinsonneault, M. H., Bastelberger, S., Gaudi, B. S., & Domagal-Goldman, S. D. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2280 · Cited by 12
Magnetic confinement of dense plasma inside (and outside) stellar coronae
Waugh, R. F. P., & Jardine, M. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1698 · Cited by 11
Wood, B. E., Linsky, J. L., & Güdel, M. (2014) · Astrophysics and space science library · doi:10.1007/978-3-319-09749-7_2 · Cited by 11
Self-citationWyman, K., & Redfield, S. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/773/2/96 · Cited by 11
“Observations of other solar type stars suggest that the historical solar wind may have been ∼50× stronger than it is today (Wood et al. 2005).”
BackgroundSelf-citationCHANDRA CHARACTERIZATION OF X-RAY EMISSION IN THE YOUNG F-STAR BINARY SYSTEM HD 113766
Lisse, C. M., Christian, D. J., Wolk, S. J., Günther, H. M., Chen, C., & Grady, C. A. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/153/2/62 · Cited by 11
“The constant C is determined by scaling from the solar result with = ´F 3.7 10x,Sun 4 erg cm −2 s−1 (Mamajek et al. 2002; Wood et al. 2002, 2005).”
BackgroundMethodInfluentialWood, S. R., Mussack, K., & Guzik, J. A. (2018) · Solar Physics · doi:10.1007/s11207-018-1334-1 · Cited by 10
Electric sails are potentially more effective than light sails near most stars
Lingam, M., & Loeb, A. (2019) · Acta Astronautica · doi:10.1016/j.actaastro.2019.12.013 · Cited by 11
Slingshot prominences: a hidden mass loss mechanism
Waugh, R. F. P., Jardine, M., Morin, J., & Donati, J. ‐. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1709 · Cited by 11
THE IMPACT OF STELLAR ABUNDANCE VARIATIONS ON STELLAR HABITABLE ZONE EVOLUTION
Young, P. A., Liebst, K., & Pagano, M. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/755/2/l31 · Cited by 11
“(Heightened early mass loss seen in some young stars (Wood et al. 2005) is not included.)”
BackgroundNonthermal Emission from the Interaction of Magnetized Exoplanets with the Wind of Their Host Star
Wang, X., & Loeb, A. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab108d · Cited by 11
“Planetary emission can be used to discover new planets or set constraints on the properties of the interplanetary medium around stars (Wood et al. 2005).”
BackgroundMars environment and magnetic orbiter model payload
Langlais, B., Leblanc, F., Fouchet, T., Barabash, S., Breuer, D., Chassefière, É., Coates, A. J., Dehant, V., Forget, F., Lammer, H., et al. (2008) · Experimental Astronomy · doi:10.1007/s10686-008-9101-1 · Cited by 10
“The past EUV flux is thought to have been up to 10 times larger 4.1 Gyr ago [30], whereas the solar wind flux may have been up to 100 times larger at the same epoch [ 36 ].”
InfluentialPlanetary 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 sciences series of ISSI · doi:10.1007/978-0-387-74288-5_10 · Cited by 11
The Impact of Stellar Abundance Variations on Stellar Habitable Zone EvolutionPreprint
Young, P. A., Liebst, K., & Pagano, M. D. (2016) · Cited by 13
Réville, V., Jasinski, J. M., Velli, M., Strugarek, A., Brun, A. S., Murphy, N., Regoli, L., Rouillard, A. P., & Varela, J. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8132 · Cited by 10
“The indirect observations of stellar winds using the Lyman-α (Ly α ) absorption signatures of the astrospheres (Wood et al. 2005) provides a power law relating the X-ray power of the corona and the mass loss rate of cool stars.”
The Wind‐ISM Interaction of α Tauri
Wood, B. E., Harper, G. M., Müller, H., Heerikhuisen, J., & Zank, G. P. (2007) · The Astrophysical Journal · doi:10.1086/510404 · Cited by 10
“If the astrospheric interpretation is correct, the Mg ii absorption feature is then somewhat analogous to the astrospheric H i Ly absorption that has previously been detected for many cool mainsequence stars (Wood et al. 2005b).”
Self-citation
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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