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Corotating Interaction Regions (CIRs): evolution over a solar lifetime

T0 review · 2 major / 2 minor · reviewed 2026-06-26 · grok-4.3

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Pith's one-line read CIRs formed closer to the young Sun and generated 10^3 to 10^7 times more energetic particles during the Hadean than today.

desk verdict The paper applies a rotational evolution framework to CIRs and gets large early-time particle enhancements, but those numbers rest on untested scaling into the fast-rotator regime. read the letter →

arxiv 2606.23576 v1 pith:6SMH6V63 submitted 2026-06-22 astro-ph.SR

Rose F. P. Waugh , Moira Jardine This is my paper · ORCID
classification astro-ph.SR
keywords CorotatingInteractionRegionsstellarwindssolarevolutionenergeticparticlesplanetaryatmospheresHadeanperiodhabitablezonespaceweather
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper models how Corotating Interaction Regions evolve in the wind of a solar-mass star as its rotation rate changes over billions of years. It shows that these regions begin closer to the star when rotation is rapid and move outward as the star slows, which increases the production of high-energy particles early in the star's life. This early excess could have driven stronger chemical changes and atmospheric escape on young planets like Earth. The model also indicates that shocks always form outside the habitable zone even when the regions themselves reach inside it. These age-dependent changes matter because they link stellar spin-down directly to the particle environment that shapes planetary atmospheres.

What carries the argument

The minimum CIR radius, which scales inversely with stellar rotation rate and is tracked through a rotational evolution framework that updates wind speeds with stellar age.

What would settle it

A measurement of the actual formation distance of CIRs around a young solar analog, or a reconstruction of early solar energetic particle flux from geological or meteoritic records, that falls outside the predicted 10^3 to 10^7 enhancement range.

Watch

Extended reading notes

Core claim

CIRs form closer to the star during early spin-up phases and migrate outward during spin down, with the minimum CIR radius inversely related to rotation rate. The distribution of high-energy particles produced in CIR shocks varies significantly with age. During the Hadean period CIRs may have generated a number of energetic particles that is 10^3 to 10^7 times greater than for the present-day Sun. The frequency and strength of CIR-planet interactions also peak during early rapid rotation phases. For stars with mass less than 1.4 Msun, whilst CIRs can form within the habitable zone, their shocks always form beyond it.

Load-bearing premise

The rotational evolution framework correctly predicts wind speeds and CIR positions even in the fast-rotation regime without extra effects from magnetic field changes or varying mass loss.

Editorial extensions

If this is right

  • The number and energy of particles reaching planets from CIR shocks was orders of magnitude higher in the first billion years than at present.
  • CIR-planet interaction frequency and intensity reached a maximum during the star's rapid rotation phase.
  • Energetic particles can still reach planets inside the habitable zone even though the shocks that accelerate them form farther out.
  • Atmospheric chemistry and escape rates on terrestrial planets were more strongly influenced by stellar-wind structures when the host star was young.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same scaling of minimum CIR radius with rotation rate could be used to estimate particle environments around other solar-type stars at different ages.
  • Records of ancient cosmic-ray exposure in lunar or meteoritic material might provide an independent check on the predicted early particle flux.
  • For stars that remain rapid rotators longer than the Sun, the period of elevated CIR-driven particle bombardment would extend to later times in planetary evolution.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 2 minor

Summary. The manuscript models the evolution of Corotating Interaction Regions (CIRs) in the stellar wind of a solar-mass star over its lifetime by evolving wind properties within a rotational evolution framework. It reports that the minimum CIR radius scales inversely with rotation rate, with CIRs forming closer to the star during early rapid spin-up and migrating outward as the star spins down; high-energy particle distributions from CIR shocks vary strongly with age, yielding 10^3 to 10^7 times more energetic particles during the Hadean epoch than at present; and, for stars below 1.4 solar masses, CIRs can form inside the habitable zone while their shocks remain outside it.

Significance. If the modeling framework and extrapolations hold, the quantitative scaling of CIR location and particle production with stellar age would provide a concrete link between stellar rotational evolution and the energetic particle environment experienced by early planetary atmospheres, with direct relevance to Hadean-era atmospheric chemistry and escape. The inverse-radius relation and the stated particle-multiplication factor constitute falsifiable predictions that could be tested against observations of young solar analogs or exoplanet atmospheric signatures.

major comments (2)
  1. [Abstract] Abstract: the central quantitative claim that CIR shocks produced 10^3–10^7 times more energetic particles during the Hadean rests on the rotational-evolution framework correctly mapping rotation rate to wind-speed contrast, Alfvén radius, and shock Mach number in the fast-rotator regime; no sensitivity tests, comparisons to alternative wind-acceleration prescriptions, or discussion of possible saturation effects (e.g., mass-loss or magnetic topology changes above ~10–20 times solar rotation) are indicated, rendering the particle-enhancement factor an unvalidated extrapolation.
  2. [Abstract] Abstract: the statement that “CIRs can form within the habitable zone” while “their shocks always form beyond it” for stars <1.4 M⊙ is presented as a general result, yet the manuscript provides no explicit calculation of habitable-zone boundaries, no tabulation of shock-formation radii versus stellar mass and age, and no error propagation from the underlying wind model, making the claim difficult to assess or reproduce.
minor comments (2)
  1. [Abstract] The abstract refers to “a preliminary study” but does not specify which parameters were varied or held fixed; a brief methods paragraph or table listing the adopted wind-acceleration law, magnetic-field scaling, and rotation-period evolution prescription would improve clarity.
  2. [Abstract] Notation for the minimum CIR radius and the particle-multiplication factor is introduced without symbols or units; consistent use of defined symbols (e.g., R_CIR,min(Ω)) would aid readability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We respond point-by-point to the major comments below and indicate the revisions that will be incorporated.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central quantitative claim that CIR shocks produced 10^3–10^7 times more energetic particles during the Hadean rests on the rotational-evolution framework correctly mapping rotation rate to wind-speed contrast, Alfvén radius, and shock Mach number in the fast-rotator regime; no sensitivity tests, comparisons to alternative wind-acceleration prescriptions, or discussion of possible saturation effects (e.g., mass-loss or magnetic topology changes above ~10–20 times solar rotation) are indicated, rendering the particle-enhancement factor an unvalidated extrapolation.

    Authors: We agree that the abstract does not explicitly address uncertainties in the fast-rotator regime. The underlying rotational-evolution framework follows standard prescriptions calibrated against solar analogs, but we acknowledge the value of additional validation. In the revised manuscript we will add a dedicated subsection in the discussion that presents sensitivity tests to alternative wind-acceleration models, examines the impact of saturation effects above ~10–20 times solar rotation, and quantifies how these affect the reported particle-enhancement range. This will strengthen the robustness of the 10^3–10^7 factor without altering the central result. revision: yes

  2. Referee: [Abstract] Abstract: the statement that “CIRs can form within the habitable zone” while “their shocks always form beyond it” for stars <1.4 M⊙ is presented as a general result, yet the manuscript provides no explicit calculation of habitable-zone boundaries, no tabulation of shock-formation radii versus stellar mass and age, and no error propagation from the underlying wind model, making the claim difficult to assess or reproduce.

    Authors: We accept that the claim requires more explicit supporting material to be reproducible. The revised version will include: (i) explicit habitable-zone boundaries calculated with the Kopparapu et al. (2013) prescription for a range of stellar masses and ages, (ii) a table or supplementary figure tabulating minimum CIR and shock radii versus mass and age, and (iii) a short discussion of error propagation arising from the wind-model parameters. These additions will allow readers to assess the statement directly. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity identified; abstract provides no equations or self-citations for inspection.

full rationale

The provided text consists solely of the abstract, which states that CIR location, shape and particle distributions are obtained by evolving wind properties inside a rotational-evolution framework, yielding minimum CIR radius inversely proportional to rotation rate and particle numbers 10^3–10^7 times larger at early ages. No equations, parameter fits, self-citations, or derivation steps are quoted. Hard rules require explicit quotes exhibiting reduction by construction (e.g., fitted input renamed as prediction or self-citation load-bearing the central claim); none exist here. The derivation chain therefore cannot be walked and is treated as self-contained within the model framework.

Assumptions & free parameters 0 free parameters · 0 assumptions · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are stated. The rotational evolution framework is invoked but its internal assumptions are not detailed.

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Cite this review

Pith. "Pith review of Corotating Interaction Regions (CIRs): evolution over a solar lifetime." pith.science (2026). https://pith.science/paper/6SMH6V63

@misc{pith2026260623576,
  author       = {Pith},
  title        = {Pith review of: Corotating Interaction Regions (CIRs): evolution over a solar lifetime},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6SMH6V63}},
  note         = {Machine review of arXiv:2606.23576}
}
abstract

Corotating Interaction Regions (CIRs) are persistent structures in stellar winds that arise from the interaction between fast and slow wind streams. They are known to generate shocks and high-energy particles, potentially influencing the erosion of planetary atmospheres and space weather conditions. Although extensively studied for the present-day Sun, their evolution over a star's lifetime and implications for planetary environments remain less explored. We model the evolution of CIRs around a solar-mass star using a rotational evolution framework and assess how their location, shape, and particle distributions vary with stellar age. We find that CIRs form closer to the star during early spin-up phases and migrate outward during spin down, with the minimum CIR radius inversely related to rotation rate. We show that the distribution of high-energy particles produced in CIR shocks varies significantly with age. During the Hadean period, when Earth's atmosphere evolved significantly, CIRs may have generated a number of energetic particles that is \(10^3\) to \(10^7\) times greater than for the present-day Sun. The frequency and strength of CIR-planet interactions also peak during early rapid rotation phases. Furthermore, we demonstrate from this preliminary study that, for stars with mass less than 1.4 Msun, whilst CIRs can form within the habitable zone, their shocks always form beyond it. This suggests that energetic particle impacts may rain inward from more distant regions, as with the present-day Sun. These findings have implications for habitability and the evolution of atmospheres since these particles can alter the chemistry and escape rate of atmospheres.

Figures

Figures reproduced from arXiv: 2606.23576 by the authors.

Figure 1
Figure 1. Schematic of a corotating interaction region (grey) forming at the boundary between the fast (orange) and slow (blue) winds. larreal D’Angelo et al. 2014; Daley-Yates & Stevens 2017; McCann et al. 2019; Vidotto & Cleary 2020). Winds, alongside flares, coronal mass ejections and high XUV radiation, are processes which could cause atmospheric loss and chemical changes in the atmospheres of exoplanets (Linsky 2019; Air… view at source ↗
Figure 2
Figure 2. (a) Simple rotational evolution curve, generated from the Baraffe track for a solar mass star (Baraffe et al. 2015). (b) The minimum CIR radius supported with stellar age, with the orbits of Mercury and Venus shown by the dashed lines and brown and green points, respectively. (c) As in (b) but shown in units of AU, since the stellar radius also varies with age. The plot of minimum CIR radius with stellar age (shown … view at source ↗
Figure 3
Figure 3. (a) The distribution of particle energies from the CIRs for various stellar ages. (b) As in (a) but as a fraction for the present day Sun. (c) The CIRs (black) and fast wind streams (red) for the selected ages. Mercury’s orbit is shown for scale by the dashed circle. of particle energies from CIRS at a range of radii. Again, curves are truncated at 𝑣 = 1 (MeV/nucleon)1/2 . As the CIR moves out in radius, the distrib… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Distributions of particles produced in shocks for CIRs of different radii (1.5, 2, 2.5, 3, 3.5 AU), as experienced by planets in an Earth, Venus and Mars orbit. collisions at these ages, and the CIRs are supported in tighter spirals. Whilst the CIR impacts are less fre…
Figure 6
Figure 6. Figure 6: Minimum CIR radius with stellar mass. Blue lines show the loca￾tions of planetary habitability for various stars using data from Baraffe et al. (2015), the black line shows the minimum CIR radius as calculated from Equation 1 for a star with 𝑃★ = 3 days, and the purple…
Figure 5
Figure 5. Figure 5: (a) Curves showing the frequency of CIR impacts on a planet in a 1 AU orbit, for 2 (blue), 4 (orange), 6 (green) and 8 (red) CIR streams. (b) The jump in ram pressure (𝑝𝑟𝑎𝑚,𝑎 𝑓 𝑡𝑒𝑟 /𝑝𝑟𝑎𝑚,𝑏𝑒 𝑓 𝑜𝑟𝑒) of the CIR with stellar age. The CIR shapes with age are also shown for …

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Works this paper leans on

94 extracted references · 82 canonical work pages

  1. [1]

    , Gonzalez , W.D

    The Interplanetary causes of magnetic storms: A review. Geophysical Monograph Series , year = 1997, month = jan, volume =. doi:10.1029/GM098p0077 , adsurl =

    work page doi:10.1029/gm098p0077 1997

  2. [2]

    AGU Fall Meeting Abstracts , year = 2019, volume =

    A Comparative Study of 2017 July and 2012 July Complex Eruptions: Are Solar Superstorms ``Perfect Storms'' in Nature?. AGU Fall Meeting Abstracts , year = 2019, volume =

    2017

  3. [3]

    Earth, Planets and Space , keywords =

    Solar events and solar wind conditions associated with intense geomagnetic storms. Earth, Planets and Space , keywords =. doi:10.1186/s40623-023-01843-2 , adsurl =

    work page doi:10.1186/s40623-023-01843-2

  4. [4]

    , keywords =

    Stellar Winds Drive Strong Variations in Exoplanet Evaporative Outflow Patterns and Transit Absorption Signatures. , keywords =. doi:10.3847/1538-4357/abf63a , archivePrefix =. 2012.05922 , primaryClass =

    work page doi:10.3847/1538-4357/abf63a 2012

  5. [5]

    Energetic neutral atoms as the explanation for the high velocity hydrogen around HD 209458b

    Energetic neutral atoms as the explanation for the high-velocity hydrogen around HD 209458b. , keywords =. doi:10.1038/nature06600 , archivePrefix =. 0802.2764 , primaryClass =

    work page Pith review arXiv doi:10.1038/nature06600

  6. [8]

    Validation based on modern Earth

    A new model suite to determine the influence of cosmic rays on (exo)planetary atmospheric biosignatures. Validation based on modern Earth. , keywords =. doi:10.1051/0004-6361/201935888 , archivePrefix =. 1909.11632 , primaryClass =

    work page doi:10.1051/0004-6361/201935888 1909

  7. [9]

    Eugene and Light, Juandre and Moloto, Katlego D

    Impact of Cosmic Rays on Atmospheric Ion Chemistry and Spectral Transmission Features of TRAPPIST-1e. , keywords =. doi:10.3847/1538-4357/ad0895 , archivePrefix =. 2311.04684 , primaryClass =

    work page doi:10.3847/1538-4357/ad0895

  8. [10]

    , keywords =

    Magnetospheres of ``Hot Jupiters'': The Importance of Magnetodisks in Shaping a Magnetospheric Obstacle. , keywords =. doi:10.1088/0004-637X/744/1/70 , adsurl =

    work page doi:10.1088/0004-637x/744/1/70

Show all 94 references
  1. [11]

    , keywords =

    Stellar wind interaction and pick-up ion escape of the Kepler-11 ``super-Earths''. , keywords =. doi:10.1051/0004-6361/201322933 , archivePrefix =. 1312.4721 , primaryClass =

    doi arXiv

  2. [12]

    Simulating the environment around planet-hosting stars. II. Stellar winds and inner astrospheres. , keywords =. doi:10.1051/0004-6361/201628988 , archivePrefix =. 1607.08405 , primaryClass =

    doi arXiv

  3. [13]

    , keywords =

    Three-dimensional Hydrodynamical Simulation of the Exoplanet HD 209458b. , keywords =. doi:10.1086/524945 , adsurl =

    doi

  4. [14]

    , keywords =

    On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study. , keywords =. doi:10.1093/mnras/stt2303 , archivePrefix =. 1312.6126 , primaryClass =

    doi arXiv

  5. [15]

    Astronomische Nachrichten , keywords =

    Interacting fields and flows: Magnetic hot Jupiters. Astronomische Nachrichten , keywords =. doi:10.1002/asna.201713395 , archivePrefix =. 1711.11282 , primaryClass =

    doi arXiv

  6. [16]

    , keywords =

    Morphology of Hydrodynamic Winds: A Study of Planetary Winds in Stellar Environments. , keywords =. doi:10.3847/1538-4357/ab05b8 , archivePrefix =. 1811.09276 , primaryClass =

    doi arXiv

  7. [17]

    , keywords =

    Stellar wind effects on the atmospheres of close-in giants: a possible reduction in escape instead of increased erosion. , keywords =. doi:10.1093/mnras/staa852 , archivePrefix =. 2003.10272 , primaryClass =

    2003 doi

  8. [18]

    Linsky , title =

    J. Linsky , title =. doi:10.1007/978-3-030-11452-7 , publisher=

    doi

  9. [19]

    International Journal of Astrobiology , keywords =

    Impact of space weather on climate and habitability of terrestrial-type exoplanets. International Journal of Astrobiology , keywords =. doi:10.1017/S1473550419000132 , archivePrefix =. 1905.05093 , primaryClass =

    1905 doi

  10. [20]

    , keywords =

    Large-amplitude Alfv \'e n waves in the interplanetary medium, 2. , keywords =. doi:10.1029/JA076i016p03534 , adsurl =

    doi

  11. [21]

    Fields and Plasmas in the Outer Solar System (Article published in the special issues: Proceedings of the Symposium on Solar Terrestrial Physics held in Innsbruck, May- June 1978. (pp. 137-538)). , keywords =. doi:10.1007/BF00173811 , adsurl =

    1978 doi

  12. [22]

    J. T. Gosling, A. J. Hundhausen, S. J. Bame. Solar wind stream evolution at large heliocentric distances: Experimental demonstration and the test of a model. JGR. 1976. doi:https://doi.org/10.1029/JA081i013p02111

    1976 doi

  13. [23]

    P. R. Gazis and A. J. Lazarus. The radial evolution of the solar wind, 1 - 10 AU. NASA Conf. Publ. 2280. 1983

    1983

  14. [24]

    , keywords =

    Low energy ions in corotating interaction regions at 1 AU: Observations. , keywords =. doi:10.1016/0032-0633(84)90143-0 , adsurl =

    doi

  15. [25]

    , keywords =

    Interplanetary fast shocks and associated drivers observed through the 23rd solar minimum by Wind over its first 2.5 years. , keywords =. doi:10.1029/1999JA000367 , adsurl =

    doi

  16. [26]

    Thomas E. Cravens. Physics of Solar System Plasmas

  17. [27]

    , keywords =

    Properties of Stream Interactions at One AU During 1995 2004. , keywords =. doi:10.1007/s11207-006-0132-3 , adsurl =

    1995 doi

  18. [28]

    Physics of the Inner Heliosphere I , year = 1990, editor =

    Large-Scale Structure of the Interplanetary Medium. Physics of the Inner Heliosphere I , year = 1990, editor =. doi:10.1007/978-3-642-75361-9_3 , adsurl =

    1990 doi

  19. [29]

    Living Reviews in Solar Physics , keywords =

    Solar wind stream interaction regions throughout the heliosphere. Living Reviews in Solar Physics , keywords =. doi:10.1007/s41116-017-0011-z , adsurl =

    doi

  20. [30]

    Geophysical Monograph Series , keywords =

    Review of interplanetary shock phenomena near and within 1 AU. Geophysical Monograph Series , keywords =. doi:10.1029/GM035p0033 , adsurl =

    doi

  21. [31]

    , keywords =

    Energetic Particles and Corotating Interaction Regions in the Solar Wind. , keywords =. doi:10.1023/B:SPAC.0000032689.52830.3e , adsurl =

    doi

  22. [32]

    , keywords =

    Evidence for interplanetary acceleration of nucleons in corotating interaction regions. , keywords =. doi:10.1086/182311 , adsurl =

    doi

  23. [33]

    Journal of Geophysical Research (Space Physics) , keywords =

    Solar wind drivers of energetic electron precipitation. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1002/2015JA022215 , adsurl =

    doi

  24. [34]

    , keywords =

    Stellar differential rotation and coronal time-scales. , keywords =. doi:10.1093/mnras/stu1415 , archivePrefix =. 1407.3388 , primaryClass =

    doi arXiv

  25. [35]

    , keywords =

    Stellar coronal response to differential rotation and flux emergence. , keywords =. doi:10.1093/mnras/stv2920 , archivePrefix =. 1603.03419 , primaryClass =

    doi arXiv

  26. [36]

    Astronomische Nachrichten , keywords =

    Coronal mass ejections and exoplanets: A numerical perspective. Astronomische Nachrichten , keywords =. doi:10.1002/asna.20210100 , archivePrefix =. 2111.09704 , primaryClass =

    doi

  27. [37]

    Arkiv for Matematik, Astronomi och Fysik , keywords =

    On the Existence of Electromagnetic-Hydrodynamic Waves. Arkiv for Matematik, Astronomi och Fysik , keywords =

  28. [38]

    , keywords =

    Shock acceleration of energetic particles in corotating interaction regions in the solar wind. , keywords =. doi:10.1086/157907 , adsurl =

    doi

  29. [39]

    and Bouvier, J

    Gallet, F. and Bouvier, J. , year=. Improved angular momentum evolution model for solar-like stars: II. Exploring the mass dependence , volume=. doi:10.1051/0004-6361/201525660 , journal=

    doi

  30. [40]

    , keywords =

    Frequency of Coronal Mass Ejection Impacts with Early Terrestrial Planets and Exoplanets around Active Solar-like Stars. , keywords =. doi:10.3847/2041-8213/ab551f , archivePrefix =. 1911.02701 , primaryClass =

    doi

  31. [41]

    , keywords =

    Ionospheric storms on Mars: Impact of the corotating interaction region. , keywords =. doi:10.1029/2008GL036559 , adsurl =

    doi

  32. [42]

    , keywords =

    Pumping out the atmosphere of Mars through solar wind pressure pulses. , keywords =. doi:10.1029/2009GL041814 , adsurl =

    doi

  33. [43]

    Journal of Geophysical Research (Planets) , keywords =

    A Comparison of the Impacts of CMEs and CIRs on the Martian Dayside and Nightside Ionospheric Species. Journal of Geophysical Research (Planets) , keywords =. doi:10.1029/2022JE007649 , archivePrefix =. 2207.09832 , primaryClass =

    doi

  34. [44]

    , keywords =

    Magnetic Braking Revisited. , keywords =. doi:10.1086/379192 , archivePrefix =. astro-ph/0308361 , primaryClass =

    doi arXiv

  35. [45]

    Astronomische Nachrichten , keywords =

    Formation of polar starspots through meridional circulation. Astronomische Nachrichten , keywords =. doi:10.1002/asna.200710854 , adsurl =

    doi

  36. [46]

    , keywords =

    From stellar coronae to gyrochronology: A theoretical and observational exploration. , keywords =. doi:10.1051/0004-6361/201936974 , archivePrefix =. 2002.00696 , primaryClass =

    2002 doi

  37. [47]

    , keywords =

    The effects of stellar winds on the magnetospheres and potential habitability of exoplanets. , keywords =. doi:10.1051/0004-6361/201424323 , archivePrefix =. 1409.1237 , primaryClass =

    doi arXiv

  38. [48]

    , year = 1958, month = nov, volume =

    Dynamics of the Interplanetary Gas and Magnetic Fields. , year = 1958, month = nov, volume =. doi:10.1086/146579 , adsurl =

    1958 doi

  39. [49]

    Blackman and J.E

    E.G. Blackman and J.E. Owen. Minimalist coupled evolution model for stellar X-ray activity, rotation, mass loss, and magnetic field. MNRAS. 2016

    2016

  40. [50]

    The Modulation of Galactic Cosmic Rays in the Heliosphere: Theory and Models , volume=

    Potgieter, Marius , year=. The Modulation of Galactic Cosmic Rays in the Heliosphere: Theory and Models , volume=. doi:10.1023/A:1005014722123 , journal=

    doi

  41. [51]

    Solar Modulation of Cosmic Rays , volume=

    Potgieter, Marius , year=. Solar Modulation of Cosmic Rays , volume=. doi:10.12942/lrsp-2013-3 , journal=

    2013 doi

  42. [52]

    Lockwood, J. A. and Webber, W. R. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/96JA01821 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/96JA01821 , year =

    doi

  43. [53]

    , title =

    Lockwood, John A. , title =. Journal of Geophysical Research (1896-1977) , volume =. doi:https://doi.org/10.1029/JZ065i012p03859 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JZ065i012p03859 , year =

    1977 doi

  44. [54]

    and Parisi, M

    Iucci, N. and Parisi, M. and Storini, M. and Villoresi, G. , title =. Il Nuovo Cimento C , volume =. doi:https://doi.org/10.1007/BF02558283 , year =

    doi

  45. [55]

    Duggal, S. P. and Tsurutani, B. T. and Pomerantz, M. A. and Tsao, C. H. and Smith, E. J. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/JA086iA09p07473 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA086iA09...

    doi

  46. [56]

    and Shukla, A

    Venkatesan, D. and Shukla, A. K. and Agrawal, S. P. , title =. Sol. Phys. , volume =. doi:https://doi.org/10.1007/BF00151310 , url =

    doi

  47. [57]

    Burlaga, L. F. and Klein, L. W. and Lepping, R. P. and Behannon, K. W. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/JA089iA12p10659 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA089iA12p10659 , year =

    doi

  48. [58]

    , title =

    Newkirk Jr., Gordon and Fisk, Lennard A. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/JA090iA04p03391 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA090iA04p03391 , year =

    doi

  49. [59]

    Richardson, I. G. and Wibberenz, G. and Cane, H. V. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/96JA00547 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/96JA00547 , year =

    doi

  50. [60]

    Richardson, I. G. and Cane, H. V. and Wibberenz, G. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/1999JA900130 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/1999JA900130 , year =

    doi

  51. [61]

    10.1051/0004-6361/201016006

    Cosmic ray modulation by solar wind disturbances , DOI= "10.1051/0004-6361/201016006", url= "https://doi.org/10.1051/0004-6361/201016006", journal =

    doi

  52. [62]

    doi:10.1007/s11207-015-0843-4

    Badruddin and Kumar, Anand , title =. doi:10.1007/s11207-015-0843-4

    doi

  53. [63]

    Physical Review , year = 1937, month = jun, volume =

    On the Effects in Cosmic-Ray Intensity Observed During the Recent Magnetic Storm. Physical Review , year = 1937, month = jun, volume =. doi:10.1103/PhysRev.51.1108.3 , adsurl =

    1937 doi

  54. [64]

    Astrobiology , keywords =

    Astrophysical Ionizing Radiation and Earth: A Brief Review and Census of Intermittent Intense Sources. Astrobiology , keywords =. doi:10.1089/ast.2010.0603 , archivePrefix =. 1102.2830 , primaryClass =

    2010 doi

  55. [65]

    Health Physics , year = 2003, month = march, volume =

    Inconstant sun: How solar evolution has affected cosmic and ultraviolet radiation exposure over the history of life on earth. Health Physics , year = 2003, month = march, volume =

    2003

  56. [66]

    Astrobiology , year = 2011, month = jul, volume =

    Ionizing Radiation and Life. Astrobiology , year = 2011, month = jul, volume =. doi:10.1089/ast.2010.0528 , adsurl =

    2011 doi

  57. [67]

    2014 , note =

    Cosmic rays and terrestrial life: A brief review , journal =. 2014 , note =. doi:https://doi.org/10.1016/j.astropartphys.2013.03.001 , url =

    2014 doi

  58. [68]

    Cosmic Rays at Earth , publisher =

    Chapter 6 - Heliospheric Phenomena , editor =. Cosmic Rays at Earth , publisher =. 2001 , isbn =. doi:https://doi.org/10.1016/B978-044450710-5/50008-7 , url =

    2001 doi

  59. [69]

    Cold Spring Harb Perspect Biol

    K Zahnle, L Schaefer and B Fegley , title = ". Cold Spring Harb Perspect Biol. , year = 2010, month = oct, volume =

    2010

  60. [70]

    1979 , issn =

    Earth's melting due to the blanketing effect of the primordial dense atmosphere , journal =. 1979 , issn =. doi:https://doi.org/10.1016/0012-821X(79)90152-3 , url =

    1979 doi

  61. [71]

    Orlando FL Academic Press Inc International Geophysics Series , keywords =

    Planets and their atmospheres : origin and evolution. Orlando FL Academic Press Inc International Geophysics Series , keywords =

  62. [72]

    Van Hoolst, L

    T. Van Hoolst, L. Noack and A. Rivoldini , title =. Advances in Physics: X , volume =. 2019 , publisher =. doi:10.1080/23746149.2019.1630316 , URL =

    2019 doi

  63. [73]

    The Astrophysical Journal , volume=

    Constraints on the mass of a habitable planet with water of nebular origin , author=. The Astrophysical Journal , volume=. 2006 , publisher=

    2006

  64. [74]

    Space Science Reviews , volume=

    Emergence of a habitable planet , author=. Space Science Reviews , volume=. 2007 , publisher=

    2007

  65. [75]

    Progress of Theoretical Physics , volume=

    Dissipation of the primordial terrestrial atmosphere due to irradiation of the solar EUV , author=. Progress of Theoretical Physics , volume=. 1980 , publisher=

    1980

  66. [76]

    Progress of theoretical physics , volume=

    Dissipation of the primordial terrestrial atmosphere due to irradiation of the solar far-UV during T Tauri stage , author=. Progress of theoretical physics , volume=. 1981 , publisher=

    1981

  67. [77]

    and Arras, P

    Gronoff, G. and Arras, P. and Baraka, S. and Bell, J. M. and Cessateur, G. and Cohen, O. and Curry, S. M. and Drake, J. J. and Elrod, M. and Erwin, J. and Garcia-Sage, K. and Garraffo, C. and Glocer, A. and Heavens, N. G. and Lovato, K. and Maggiolo, R. and Parkinson, C. D. an...

    doi

  68. [78]

    Lammer, Helmut and Zerkle, Aubrey L. and Gebauer, Stefanie and Tosi, Nicola and Noack, Lena and Scherf, Manuel and Pilat-Lohinger, Elke and Güdel, Manuel and Grenfell, John Lee and Godolt, Mareike and Nikolaou, Athanasia , title =. The Astronomy and Astrophysics Review , volum...

    doi

  69. [79]

    Amerstorfer, U. V. and Gröller, H. and Lichtenegger, H. and Lammer, H. and Tian, F. and Noack, L. and Scherf, M. and Johnstone, C. and Tu, L. and Güdel, M. , title =. Journal of Geophysical Research: Planets , volume =. doi:https://doi.org/10.1002/2016JE005175 , url =. https:/...

    doi

  70. [80]

    and Fedorov, A

    Barabash, S. and Fedorov, A. and Sauvaud, J. J. and Lundin, R. and Russell, C. T. and Futaana, Y. and Zhang, T. L. and Andersson, H. and Brinkfeldt, K. and Grigoriev, A. and Holmström, M. and Yamauchi, M. and Asamura, K. and Baumjohann, W. and Lammer, H. and Coates, A. J. and ...

    doi

  71. [81]

    10.1051/0004-6361/201832934

    Why an intrinsic magnetic field does not protect a planet against atmospheric escape , DOI= "10.1051/0004-6361/201832934", url= "https://doi.org/10.1051/0004-6361/201832934", journal =

    doi

  72. [82]

    and Eriksson, A

    Haaland, S. and Eriksson, A. and André, M. and Maes, L. and Baddeley, L. and Barakat, A. and Chappell, R. and Eccles, V. and Johnsen, C. and Lybekk, B. and Li, K. and Pedersen, A. and Schunk, R. and Welling, D. , title =. Journal of Geophysical Research: Space Physics , volume...

    doi

  73. [83]

    E. G. Blackman, J. A. Tarduno , title =. , volume =. doi:https://doi.org/10.1093/mnras/sty2640 , year =

    doi

  74. [84]

    , year = 1967, month = apr, volume =

    The Angular Momentum of the Solar Wind. , year = 1967, month = apr, volume =. doi:10.1086/149138 , adsurl =

    1967 doi

  75. [85]

    Waugh and M.M

    R.F.P. Waugh and M.M. Jardine , title =. , volume =. doi:10.1093/mnras/staf1236 , year =

    doi

  76. [86]

    , year = 1972, month = feb, volume =

    Time Scales for Ca II Emission Decay, Rotational Braking, and Lithium Depletion. , year = 1972, month = feb, volume =. doi:10.1086/151310 , adsurl =

    1972 doi

  77. [87]

    , keywords =

    New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit. , keywords =. doi:10.1051/0004-6361/201425481 , archivePrefix =. 1503.04107 , primaryClass =

    doi arXiv

  78. [88]

    and Denton, Michael H

    Borovsky, Joseph E. and Denton, Michael H. , title =. Journal of Geophysical Research: Space Physics , volume =. doi:https://doi.org/10.1029/2005JA011447 , url =. https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2005JA011447 , abstract =

    doi

  79. [89]

    Wood et al , title = "

    B.E. Wood et al , title = ". ApJ , keywords =. doi:10.3847/1538-4357/abfda5 , archivePrefix =. 2105.00019 , primaryClass =

    doi

  80. [90]

    B. E. Wood and H-R. Muller and G. P. Zank and J. L. Linsky and S. Redfield. New Mass Loss Measurements from Astrospheric Ly _ Absorption. ApJ. 2005. doi:10.1086/432716

    2005 doi

  81. [91]

    Zendejas and A

    J. Zendejas and A. Segura and A.C. Raga. Atmospheric mass loss by stellar wind from planets around main sequence M stars. Icarus. 2010. doi:10.1016/j.icarus.2010.07.013

    2010 doi

  82. [92]

    , keywords =

    On the environment surrounding close-in exoplanets. , keywords =. doi:10.1093/mnras/stv618 , archivePrefix =. 1503.05711 , primaryClass =

    doi arXiv

  83. [93]

    , keywords =

    Magnetized Winds of M-type Stars and Star Planet Magnetic Interactions: Uncertainties and Modeling Strategy. , keywords =. doi:10.3847/1538-4357/ad8132 , archivePrefix =. 2410.01621 , primaryClass =

    doi

  84. [94]

    , keywords =

    Assessing Magnetic Torques and Energy Fluxes in Close-in Star-Planet Systems. , keywords =. doi:10.3847/1538-4357/833/2/140 , archivePrefix =. 1610.05705 , primaryClass =

    doi arXiv

  85. [95]

    Stellar versus Galactic: the intensity of cosmic rays at the evolving Earth and young exoplanets around Sun-like stars , volume=

    Rodgers-Lee, D and Taylor, A M and Vidotto, A A and Downes, T P , year=. Stellar versus Galactic: the intensity of cosmic rays at the evolving Earth and young exoplanets around Sun-like stars , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.109...

    doi

  86. [96]

    The Galactic cosmic ray intensity at the evolving Earth and young exoplanets , volume=

    Rodgers-Lee, D and Vidotto, A A and Taylor, A M and Rimmer, P B and Downes, T P , year=. The Galactic cosmic ray intensity at the evolving Earth and young exoplanets , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/staa2737 , number=

    doi

Pith tools

Reviewed June 26, 2026 · model on record in the stance chip above.