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Cited by 853Stellar, planetary, and galactic studiesSolar and Space Plasma DynamicsAstronomy and Astrophysical Research

The DOI matches its Crossref record; 45 of the 45 references it cites were found in a registry or an index.

The stellar activity-rotation relationship revisited: Dependence of saturated and non-saturated X-ray emission regimes on stellar mass for late-type dwarfs

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Pizzolato, N., Maggio, A., Micela, G., Sciortino, S., Ventura, P.·2003·Astronomy & Astrophysics
DOI 10.1051/0004-6361:20021560
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Abstract

We present the results of a new study on the relationship between coronal X-ray emission and stellar rotation in late-type main-sequence stars. We have selected a sample of 259 dwarfs in the range 0.5–2.0, including 110 field stars and 149 members of the Pleiades, Hyades, α Persei, IC 2602 and IC 2391 open clusters. All the stars have been observed with ROSAT, and most of them have photometrically-measured rotation periods available. Our results confirm that two emission regimes exist, one in which the rotation period is a good predictor of the total X-ray luminosity, and the other in which a constant saturated X-ray to bolometric luminosity ratio is attained; we present a quantitative estimate of the critical rotation periods below which stars of different masses (or spectral types) enter the saturated regime. In this work we have also empirically derived a characteristic time scale, , which we have used to investigate the relationship between the X-ray emission level and an X-ray-based Rossby number : we show that our empirical time scale resembles the theoretical convective turnover time for , but it also has the same functional dependence on as in the color range . Our results imply that – for non-saturated coronae – the Lx – Prot relation is equivalent to the vs. Re relation.

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Crossref · 10.1051/0004-6361:20021560

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  • Saturation is typically seen around 3.2 ± 0.2, and this is expected for rotation periods less than about 3.5 days for K5 stars.

    “where saturation is typically seen around 3 : 2 0 : 2, and this is expected for rotation periods less than about 3.5 days for K5 stars (Pizzolato et al. 2003).”

    From A search for transiting companions in the J1407 (V1400 Cen) system (2021) · cites this paper as Pizzolato et al. 2003

    Table 4 reports a saturation threshold of 3.5 ± 1.5 days for its 1.07 < B−V < 1.35 color bin, consistent with the approximate period claimed. But the corresponding saturation level is −3.2 ± 0.2 for log(Lx/Lbol), not positive 3.2 ± 0.2; the paper also does not label that bin specifically as K5 stars. (LLM, conf=0.88)

    Experimental — accuracy not yet measured

  • A K5-type star with rotation period 3.20 days would be predicted to have soft X-ray emission around the saturation level (log(L_X/L_bol) = -3.2 +/- 0.3), perfectly consistent with the observed ROSAT X-ray flux (log(L_X/L_bol) = -3.2), and consistent with other Sco-Cen pre-MS stars.

    “A K5-type star with rotation period of 3.20 days would be predicted to have soft X-ray emission around the saturation level (log(L X /L bol ) -3.2 ± 0.3; Pizzolato et al. 2003), perfectly consistent with the observed ROSAT X-ray flux (log(L X /L bol ) -3.2), and consistent with other Sco-Cen pre-MS stars (Mamajek et al. 2002).”

    From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Pizzolato et al. 2003

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Citations

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Research works printed but not linked: 16

  1. Allain, 1997, MmSAI, 68, 899
  2. Beuermann, 1999, A&A, 348, 524
  3. Delfosse, 1998, A&A, 331, 581
  4. Hempelmann, 1995, A&A, 294, 515
  5. Jardine, 1999, A&A, 346, 883
  6. Marino, 2000, A&A, 353, 177
  7. Micela, 1999, A&A, 341, 751
  8. Pizzolato, 2000, A&A, 361, 614
  9. Prosser, C. F., & Grankin, K. N. 1997, CfA preprint, 4539
  10. Randich, 1995, A&A, 300, 134
  11. Randich, 1996, A&A, 305, 785
  12. Siess, 2000, A&A, 358, 593
  13. Stepien, 1994, A&A, 292, 191
  14. Ventura, 1998, A&A, 334, 953
  15. Vilhu, 1984, A&A, 133, 117
  16. Vilhu, 1987, A&A, 321, 958

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Metadata

Authors
Pizzolato, N., Maggio, A., Micela, G., Sciortino, S., & Ventura, P.
Affiliations
  • Osservatorio Astronomico di Palermo (IT)
  • Astronomical Observatory of Rome (IT)
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2002-12-11
Volume
397
Issue
1
Pages
147-157
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361:20021560
OpenAlex
W2098479840
Cited by
853
References
45
Citations by year
2026: 21 · 2025: 41 · 2024: 50 · 2023: 36 · 2022: 42 · 2021: 46 · 2020: 66 · 2019: 53 · 2018: 36 · 2017: 41 · 2016: 59 · 2015: 36 · 2014: 40 · 2013: 41 · 2012: 41
FWCI
8.88
Type
journal article
Language
en
Open access
Locations
  • Astronomy and Astrophysics (publishedVersion)
  • Springer Link (Chiba Institute of Technology) (submittedVersion)
Funders
  • Agenzia Spaziale Italiana
  • Ministero dell'Università e della Ricerca
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 X-ray emission, coronal X-ray emission, stellar rotation periods, stellar mass dependence, Rossby number, convective turnover time, open clusters, Pleiades, Hyades, IC 2602, IC 2391

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