Asymmetries of solar coronal extreme ultraviolet emission lines

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Table 2:

Contribution of possible blends to Fe 15 at 284 Å.
	Rest	Relative	Modeled contribution [%] ^a
wavelength		shift^b		active	quiet	coronal
line	[Å]	[km s^-1]	flare	region	Sun	hole
Fe 17	284.010^c	-158	2.8	0.1	<0.1	0.0
Al 9	284.015^d	-152	0.2	0.6	2.1	83.7
Fe 15	284.160^e	0	97.0	99.3	97.8	16.3

Notes. ^(a) Contribution modeled using the Chianti atomic data base. ^(b) Doppler shift according to difference in rest wavelength. ^(c) From NIST atomic spectra data base (Ralchenko et al. 2008). ^(d) From NIST (as ^c); based on laboratory measurements by Valero & Goorvitch (1972), who estimate uncertainty to be $\pm$ 0.04 Å ( $\pm$ 40 km s^-1). ^(e) Based on solar observations as provided by Brown et al. (2008), uncertainty is given as $\pm$ 0.004 Å ( $\pm$ 4 km s^-1). Within errors consistent with NIST data base (observed and theoretical calculated values).

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