Coronal hole boundaries evolution at small scales - II. XRT view. Can small-scale outflows at CHBs be a source of the slow solar wind?

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Table 1:

Description of the XRT data used in the present study.
Date	Remark	Observing period	Field-of-view	Exposure time
		of time (UT)	(arcsec)	(s)
09/11/07	ECH	06:35-14:59	$366\times366$	16
12/11/07	ECH	01:17-10:59	$374\times374$	16
14/11/07	ECH	00:12-11:11	$374\times374$	16
16/11/07	ECH	18:07-23:58	$370\times370$	16
16/12/08	PCH	10:02-17:52	$362\times337$	23
20/09/07	PCH	12:22-18:05	$1018\times291$	16
10/01/09	QS	11:30-17:27	$370\times370$	23
13/01/09	QS	11:22-17:41	$370\times370$	23
29/11/07	QS with TCH	18:17-23:59	$506\times506$	23

Notes. ECH - equatorial coronal hole, PCH - polar coronal hole, TCH - transient coronal hole.

Source LaTeX | All tables | In the text

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