Publication Date:
2019-11-08
Description:
Small-scale ephemeral coronal holes may be a recurring feature on the solar disk but have received comparatively little attention. These events are characterized by compact structures and short total lifetimes, which are substantially less than a solar disk crossing. We present a systematic search for these events, using Atmospheric Imaging Assembly extreme ultraviolet image data from the Solar Dynamics Observatory, covering the time period of 20102015. Following strict criteria, this search yielded four clear examples of the ephemeral coronal hole phenomenon. The properties of each event are characterized, including their total lifetime, growth and decay rates, and areas. The magnetic properties of these events are also determined using Helioseismic and Magnetic Imager data. Based on these four events, ephemeral coronal holes experience rapid initial growth of up to 3000 Msq.m/hr, while the decay phases are typically more gradual. Like conventional coronal holes, the mean magnetic eld in each ephemeral coronal hole displays a consistent polarity, with mean magnetic ux densities generally 〈10 G. No evidence of a corresponding signature is seen in solar wind data at 1 au. Further study is needed to determine whether ephemeral coronal holes are under reported events or are truly rare phenomena.
Keywords:
Solar Physics
Type:
GSFC-E-DAA-TN73700
,
Astrophysical Journal (ISSN 0004-637X) (e-ISSN 1538-4357); 880; 2; 98
Format:
text
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