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Contrast of Coronal Holes and Parameters of Associated Solar Wind Streams

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Abstract

It is shown that the contrast of coronal holes, just as their size, determines the velocity of the solar wind streams. Fully calibrated EIT images of the Sun have been used. About 450 measurements in 284 Å have been analyzed. The time interval under examination covers about 1500 days in the declining phase of cycle 23. All coronal holes recorded for this interval in the absence of coronal mass ejections (CMEs) have been studied. The comparison with some other parameters (e.g. density, temperature, magnetic field) was carried out. The correlations with the velocity are rather high (0.70 – 0.89), especially during the periods of moderate activity, and could be used for everyday forecast. The contrast of coronal holes is rather small.

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Authors and Affiliations

  1. Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation (IZMIRAN), Russian Academy of Sciences, Troitsk, Russia

    V. N. Obridko, B. D. Shelting & I. M. Livshits

  2. Shemakha Astrophysical Observatory (ShAO), National Academy of Sciences of Azerbaijan Republic, Shemakha, Azerbaijan

    A. B. Asgarov

Authors
  1. V. N. Obridko
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  2. B. D. Shelting
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  3. I. M. Livshits
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  4. A. B. Asgarov
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Correspondence to V. N. Obridko.

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Obridko, V.N., Shelting, B.D., Livshits, I.M. et al. Contrast of Coronal Holes and Parameters of Associated Solar Wind Streams. Sol Phys 260, 191–206 (2009). https://doi.org/10.1007/s11207-009-9435-5

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  • DOI: https://doi.org/10.1007/s11207-009-9435-5

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