CoChat
Sign Up
Cited by 229Stellar, planetary, and galactic studiesAstronomy and Astrophysical ResearchHistory and Developments in Astronomy

Stellar winds on the main-sequence: II. The evolution of rotation and winds

Open access
Johnstone, C. P., Güdel, M., Brott, I., Lüftinger, T.·2015·Astronomy & Astrophysics
DOI 10.1051/0004-6361/201425301
Open this paper in CoChat — free accountOpen PDF

Abstract

Aims. We study the evolution of stellar rotation and wind properties for low-mass main-sequence stars. Our aim is to use rotational evolution models to constrain the mass loss rates in stellar winds and to predict how their properties evolve with time on the main-sequence.

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Integrity signals

Registry

Crossref · 10.1051/0004-6361/201425301

Cites

85 of 85 references verified0 citation errors · 0 not checkable

Statistics

Claims the paper makes

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Claims other papers make about this one

Each is checked against this paper’s own text: does it say what the citing paper says it does?

  • Upper limits on mass loss rates of young Sun-like stars from radio observations and rotation-rate considerations rule out the early Sun being more massive and luminous enough to solve the faint young Sun problem.

    “However, upper limits on the mass loss rates of young Sun-like stars from radio observations and considerations of how rapidly the rotation rates of Sun-like stars decrease with age rule out this solution (Gaidos et al. 2000; Johnstone et al. 2015; Fichtinger et al. 2017).”

    From The young Sun's XUV-activity as a constraint for lower CO2-limits in the Earth's Archean atmosphere (2021) · cites this paper as Johnstone et al. 2015

    Section 6.2 reports radio-derived upper limits on mass-loss rates for three young solar analogues, and its discussion of rotational evolution constrains models of the early solar wind (page not supplied). But the paper says its wind predictions are consistent with those radio limits; it does not conclude that these constraints rule out a more massive, more luminous early Sun as a solution to the faint young Sun problem. (LLM, conf=0.84)

    Experimental — accuracy not yet measured

  • During the Archean, the Sun emitted higher levels of X-ray, extreme ultraviolet, and far ultraviolet radiation than it does now.

    “During the Archean, the Sun emitted higher levels of X-ray ( < 10 nm), extreme ultraviolet (EUV; 10-91.2nm)), and far ultraviolet (FUV; 91.2 200 nm) radiation”

    From The young Sun's XUV-activity as a constraint for lower CO2-limits in the Earth's Archean atmosphere (2021) · cites this paper as Johnstone et al. 2015

    The Introduction says older stars have lower levels of high-energy radiation, and §6.2 discusses the Sun’s X-ray, EUV, and FUV emission evolving over time. But §6.2 emphasizes uncertainty about the Sun’s rotation history and allows a slow-rotator scenario in which EUV emission was not significantly above current levels after the zero-age main sequence. The paper therefore does not establish the categorical claim for all three bands throughout the Archean. (LLM, conf=0.86)

    Experimental — accuracy not yet measured

  • The early Sun's XUV evolution is not known, with the major uncertainty being its early rotation rate.

    “The early Sun's XUV evolution is not known, with the major uncertainty being its early rotation rate (Johnstone et al. 2015; Tu et al. 2015).”

    From The young Sun's XUV-activity as a constraint for lower CO2-limits in the Earth's Archean atmosphere (2021) · cites this paper as Johnstone et al. 2015

Self-check

Percentages, sums and reported differences re-computed from the paper’s own numbers.

The self-check needs the paper’s full text.

Cites

Flagged first, then by citations

Research works printed but not linked: 79

  1. Aarnio, A. N., Matt, S. P., & Stassun, K. G. 2012, ApJ, 760, 9 · DOI
  2. Agüeros, M. A., Covey, K. R., Lemonias, J. J., et al. 2011, ApJ, 740, 110 · DOI
  3. Arge, C. N., & Pizzo, V. J. 2000, J. Geophys. Res., 105, 10465 · DOI
  4. Baines, E. K., & Armstrong, J. T. 2012, ApJ, 744, 138 · DOI
  5. Barnes, S. A. 2003, ApJ, 586, 464 · DOI
  6. Barnes, S. A. 2007, ApJ, 669, 1167 · DOI
  7. Barnes, S., & Sofia, S. 1996, ApJ, 462, 746 · DOI
  8. Belcher, J. W., & MacGregor, K. B. 1976, ApJ, 210, 498 · DOI
  9. Bouvier, J. 2008, A&A, 489, L53 · DOI
  10. Bouvier, J., Forestini, M., & Allain, S. 1997, A&A, 326, 1023 · DOI
  11. Bouvier, J., Matt, S. P., Mohanty, S., et al. 2014, Protostars and Planets VI, eds. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning (Tucson: University of Arizona Press), 433
  12. Brott, I., de Mink, S. E., Cantiello, M., et al. 2011a, A&A, 530, A115 · DOI
  13. Brott, I., Evans, C. J., Hunter, I., et al. 2011b, A&A, 530, A116 · DOI
  14. Cohen, O., Drake, J. J., Glocer, A., et al. 2014, ApJ, 790, 57 · DOI
  15. Cranmer, S. R., & Saar, S. H. 2011b, ApJ, 741, 54 · DOI
  16. Delorme, P., Collier Cameron, A., Hebb, L., et al. 2011, MNRAS, 413, 2218 · DOI
  17. Donahue, R. A., Saar, S. H., & Baliunas, S. L. 1996, ApJ, 466, 384 · DOI
  18. Drake, J. J., Cohen, O., Yashiro, S., & Gopalswamy, N. 2013, ApJ, 764, 170 · DOI
  19. Gaidos, E. J., Güdel, M., & Blake, G. A. 2000, Geophys. Res. Lett., 27, 501 · DOI
  20. Gallet, F., & Bouvier, J. 2013, A&A, 556, A36 · DOI
  21. Gregory, S. G., Donati, J.-F., Morin, J., et al. 2012, ApJ, 755, 97 · DOI
  22. Grießmeier, J.-M., Stadelmann, A., Penz, T., et al. 2004, A&A, 425, 753 · DOI
  23. Güdel, M., Guinan, E. F., & Skinner, S. L. 1997, ApJ, 483, 947 · DOI
  24. Guedel, M., Dvorak, R., Erkaev, N., et al. 2014, Protostars and Planets VI, eds. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning (Tucson: University of Arizona Press), 883
  25. Hartman, J. D., Gaudi, B. S., Holman, M. J., et al. 2008, ApJ, 675, 1233 · DOI
  26. Hartman, J. D., Gaudi, B. S., Pinsonneault, M. H., et al. 2009, ApJ, 691, 342 · DOI
  27. Hayashi, C., Nakazawa, K., & Mizuno, H. 1979, Earth Plan. Sci. Lett., 43, 22 · DOI
  28. Heger, A., Langer, N., & Woosley, S. E. 2000, ApJ, 528, 368 · DOI
  29. Holzwarth, V., & Jardine, M. 2007, A&A, 463, 11 · DOI
  30. Irwin, J., Hodgkin, S., Aigrain, S., et al. 2007, MNRAS, 377, 741 · DOI
  31. Irwin, J., Hodgkin, S., Aigrain, S., et al. 2008, MNRAS, 383, 1588 · DOI
  32. Irwin, J., Aigrain, S., Bouvier, J., et al. 2009, MNRAS, 392, 1456 · DOI
  33. Irwin, J., Berta, Z. K., Burke, C. J., et al. 2011, ApJ, 727, 56 · DOI
  34. Jeffries, R. D., Thurston, M. R., & Hambly, N. C. 2001, A&A, 375, 863 · DOI
  35. Kalirai, J. S., Fahlman, G. G., Richer, H. B., & Ventura, P. 2003, AJ, 126, 1402 · DOI
  36. Kawaler, S. D. 1988, ApJ, 333, 236 · DOI
  37. Kervella, P., Mérand, A., Pichon, B., et al. 2008, A&A, 488, 667 · DOI
  38. Khodachenko, M. L., Ribas, I., Lammer, H., et al. 2007, Astrobiology, 7, 167 · DOI
  39. King, R. R., McCaughrean, M. J., Homeier, D., et al. 2010, A&A, 510, A99 · DOI
  40. Kislyakova, K. G., Johnstone, C. P., Odert, P., et al. 2014, A&A, 562, A116 · DOI
  41. Kraft, R. P. 1967, ApJ, 150, 551 · DOI
  42. Lammer, H., Selsis, F., Ribas, I., et al. 2003, ApJ, 598, L121 · DOI
  43. Lammer, H., Selsis, F., Chassefière, E., et al. 2010, Astrobiology, 10, 45 · DOI
  44. Lammer, H., Stökl, A., Erkaev, N. V., et al. 2014, MNRAS, 439, 3225 · DOI
  45. Leitzinger, M., Odert, P., Greimel, R., et al. 2014, MNRAS, 443, 898 · DOI
  46. MacGregor, K. B., & Brenner, M. 1991, ApJ, 376, 204 · DOI
  47. Mamajek, E. E., & Hillenbrand, L. A. 2008, ApJ, 687, 1264 · DOI
  48. Meibom, S., Mathieu, R. D., & Stassun, K. G. 2009, ApJ, 695, 679 · DOI
  49. Meibom, S., Barnes, S. A., Latham, D. W., et al. 2011, ApJ, 733, L9 · DOI
  50. Moraux, E., Artemenko, S., Bouvier, J., et al. 2013, A&A, 560, A13 · DOI
  51. Morin, J., Donati, J.-F., Petit, P., et al. 2008, MNRAS, 390, 567 · DOI
  52. Parker, E. N. 1958, ApJ, 128, 664 · DOI
  53. Pevtsov, A. A., Fisher, G. H., Acton, L. W., et al. 2003, ApJ, 598, 1387 · DOI
  54. Reiners, A. 2012, Liv. Rev. Sol. Phys., 9, 1 · DOI
  55. Reiners, A. 2014, in IAU Symp., 302, 156 · DOI
  56. Reiners, A., Schuessler, M., & Passegger, V. M. 2014, ApJ, 794, 144 · DOI
  57. Ribas, I., Guinan, E. F., Güdel, M., & Audard, M. 2005, ApJ, 622, 680 · DOI
  58. Saar, S. H. 1996, in Stellar Surface Structure, eds. K. G. Strassmeier, & J. L. Linsky, IAU Symp., 176, 237 · DOI
  59. Saar, S. H. 2001, in 11th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, eds. R. J. Garcia Lopez, R. Rebolo, & M. R. Zapaterio Osorio, ASP Conf. Ser., 223, 292 · DOI
  60. Schatzman, E. 1962, Ann. Astrophys., 25, 18 · DOI
  61. Scholz, A., Irwin, J., Bouvier, J., et al. 2011, MNRAS, 413, 2595 · DOI
  62. See, V., Jardine, M., Vidotto, A. A., et al. 2014, A&A, 570, A99 · DOI
  63. Skumanich, A. 1972, ApJ, 171, 565 · DOI
  64. Soderblom, D. R., Hillenbrand, L. A., Jeffries, R. D., Mamajek, E. E., & Naylor, T. 2014, Protostars and Planets VI, eds. H. Beuther, R. S Klessen, C. P. Dullemond, & T. Henning (Tucson: University of Arizona Press), 219
  65. Spada, F., Lanzafame, A. C., Lanza, A. F., Messina, S., & Collier Cameron, A. 2011, MNRAS, 416, 447 · DOI
  66. Stauffer, J. R., Schultz, G., & Kirkpatrick, J. D. 1998, ApJ, 499, L199 · DOI
  67. Suzuki, T. K., Imada, S., Kataoka, R., et al. 2013, PASJ, 65, 98 · DOI
  68. Telleschi, A., Güdel, M., Briggs, K., et al. 2005, ApJ, 622, 653 · DOI
  69. Tóth, G. 1996, Astrophys. Lett. Comm., 34, 245 · DOI
  70. Tóth, G. 1997, J. Comput. Phys., 138, 981 · DOI
  71. van Leeuwen, F., Alphenaar, P., & Meys, J. J. M. 1987, A&AS, 67, 483 · DOI
  72. Vidotto, A. A., Jardine, M., Opher, M., Donati, J. F., & Gombosi, T. I. 2011, MNRAS, 412, 351 · DOI
  73. Vidotto, A. A., Jardine, M., Morin, J., et al. 2014b, MNRAS, 438, 1162 · DOI
  74. Wang, Y.-M., & Sheeley, Jr., N. R. 1990, ApJ, 355, 726 · DOI
  75. Weber, E. J., & Davis, Jr., L. 1967, ApJ, 148, 217 · DOI
  76. Wood, B. E., Linsky, J. L., Müller, H.-R., & Zank, G. P. 2001, ApJ, 547, L49 · DOI
  77. Wood, B. E., Müller, H.-R., Zank, G. P., & Linsky, J. L. 2002, ApJ, 574, 412 · DOI
  78. Wood, B. E., Müller, H.-R., Redfield, S., & Edelman, E. 2014, ApJ, 781, L33 · DOI
  79. Wright, N. J., Drake, J. J., Mamajek, E. E., & Henry, G. W. 2011, ApJ, 743, 48 · DOI

Cited by

Sorted by citations

Related

Authors
Johnstone, C. P., Güdel, M., Brott, I., & Lüftinger, T.
Affiliations
University of Vienna (AT)
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2015-04-27
Volume
577
Pages
A28
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361/201425301
OpenAlex
W4299966005
Cited by
229
References
85
Citations by year
2026: 11 · 2025: 18 · 2024: 14 · 2023: 16 · 2022: 15 · 2021: 22 · 2020: 28 · 2019: 34 · 2018: 22 · 2017: 22 · 2016: 17 · 2015: 10
FWCI
13.47
Type
journal article
Language
en
Open access
Locations
Astronomy and Astrophysics (publishedVersion)
Funders
Austrian Science Fund
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › History and Developments in Astronomy
Keywords
stellar winds, main-sequence stars, low-mass stars, stellar rotation, rotational evolution, mass loss rate, stellar evolution

About these checks

Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

Statistics and arithmetic are recomputed, not judged.

Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.

What counts as a claim ›How we measure confidence ›How we check this ›

Are you an author, or do you see a problem with this page? Request a review