Figure 3 - uploaded by Bhola Dwivedi
Content may be subject to copyright.
The solar corona and polar coronal holes observed from EIT and SUMER instruments on SOHO. The 'zoomed-in' or 'close-up' region in the image shows a Doppler velocity map of million degree gas at the base of the corona where the solar wind originates. Blue represents blue shifts or outflows and red represents red shifts or downflows. The blue regions are inside a coronal hole or open magnetic field region, where the high-speed solar wind is accelerated. Superposed are the edges of 'honeycomb'shaped patterns of magnetic fields at the surface of the Sun, where the strongest flows (dark blue) occur. (Image Credit: Science, 1999, 283, 810, SUMER/SOHO, EIT/SOHO, ESA/NASA).
Source publication
Figure 1. Image showing a famous view of the full tail of Halley recorded from the Mount Wilson Observatory. Figure 2. The Sun's atmosphere is threaded with magnetic fields (yellow lines). Areas with closed magnetic fields give rise to slow, dense solar wind (short, dashed, red arrows), while areas with open magnetic fields (coronal holes) yield fa...
Context in source publication
Context 1
... there was little additional direct observational evidence to support this view. Hassler et al. 5 found the Ne VIII emission blue shifted in the north polar coronal hole along the mag- netic network boundary interfaces com- pared to the average quiet-Sun flow (cf., Figure 3). These Ne VIII observations reveal the first two-dimensional coronal images showing velocity structure in a coronal hole, and provide strong evidence that coronal holes are indeed the source of the fast solar wind. ...
