Polar coronal holes during cycles 22 and 23

被引:156
|
作者
Harvey, KL
Recely, F
机构
[1] Solar Phys Res Corp, Tucson, AZ 85718 USA
[2] NOAA, Space Environm Lab, Tucson, AZ 85718 USA
基金
美国国家科学基金会;
关键词
D O I
10.1023/A:1022469023581
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The National Solar Observatory/Kitt Peak synoptic rotation maps of the magnetic field and of the equivalent width of the He I 1083 nm line are used to identify and measure polar coronal holes from September 1989 to the present. This period covers the entire lifetime of the northern and southern polar holes present during cycles 22 and 23 and includes the disappearance of the previous southern polar coronal hole in 1990 and and formation of the new northern polar hole in 2001. From this sample of polar hole observations, we found that polar coronal holes evolve from high-latitude (similar to60degrees) isolated holes. The isolated pre-polar holes form in the follower of the remnants of old active region fields just before the polar magnetic fields complete their reversal during the maximum phase of a cycle, and expand to cover the poles within 3 solar rotations after the reversal of the polar fields. During the initial 1.2-1.4 years, the polar holes are asymmetric about the pole and frequently have lobes extending into the active region latitudes. During this period, the area and magnetic flux of the polar holes increase rapidly. The surface areas, and in one case the net magnetic flux, reach an initial brief maximum within a few months. Following this initial phase, the areas (and in one case magnetic flux) decrease and then increase more slowly reaching their maxima during the cycle minimum. Over much of the lifetime of the measured polar holes, the area of the southern polar hole was smaller than the northern hole and had a significantly higher magnetic flux density. Both polar holes had essentially the same amount of magnetic flux at the time of cycle minimum. The decline in area and magnetic flux begins with the first new cycle regions with the holes disappearing about 1.1-1.8 years before the polar fields complete their reversal. The lifetime of the two polar coronal holes observed in their entirety during cycles 22 and 23 was 8.7 years for the northern polar hole and 8.3 years for the southern polar hole.
引用
下载
收藏
页码:31 / 52
页数:22
相关论文
共 50 条
  • [21] Coronal Holes and the Polar Field Reversals
    P. Fox
    P. McIntosh
    P. R. Wilson
    Solar Physics, 1998, 177 : 375 - 393
  • [22] Outflow velocities in polar coronal holes
    Gabriel, A. H.
    Bely-Dubau, F.
    Lemaire, P.
    Antonucci, E.
    Stars as Suns: Activity, Evolution and Planets, 2004, 2004 (219): : 635 - 640
  • [23] Oxygen abundance in polar coronal holes
    Teriaca, L
    Poletto, G
    Falchi, A
    Doyle, JG
    SOLAR AND GALACTIC COMPOSITION, 2001, 598 : 65 - 70
  • [24] Coronal holes and the polar field reversals
    Fox, P
    McIntosh, P
    Wilson, PR
    SOLAR PHYSICS, 1998, 177 (1-2) : 375 - 393
  • [25] Evolution of Coronal Holes and Implications for High-Speed Solar Wind During the Minimum Between Cycles 23 and 24
    de Toma, G.
    SOLAR PHYSICS, 2011, 274 (1-2) : 195 - 217
  • [26] Evolution of Coronal Holes and Implications for High-Speed Solar Wind During the Minimum Between Cycles 23 and 24
    G. de Toma
    Solar Physics, 2011, 274 : 195 - 217
  • [27] Polar magnetic fields and coronal holes during the recent solar minima
    de Toma, Giuliana
    COMPARATIVE MAGNETIC MINIMA: CHARACTERIZING QUIET TIMES IN THE SUN AND STARS, 2012, (286): : 101 - 112
  • [28] Polar coronal holes during the past solar cycle: Ulysses observations
    von Steiger, Rudolf
    Zurbuchen, Thomas H.
    JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS, 2011, 116
  • [29] TEMPORAL EVOLUTION OF SOLAR WIND ION COMPOSITION AND THEIR SOURCE CORONAL HOLES DURING THE DECLINING PHASE OF CYCLE 23. I. LOW- LATITUDE EXTENSION OF POLAR CORONAL HOLES
    Ko, Yuan-Kuen
    Muglach, Karin
    Wang, Yi-Ming
    Young, Peter R.
    Lepri, Susan T.
    ASTROPHYSICAL JOURNAL, 2014, 787 (02):
  • [30] On Polar Magnetic Field Reversal in Solar Cycles 21, 22, 23, and 24
    Mykola I. Pishkalo
    Solar Physics, 2019, 294