Evidence for magnetic flux cancelation leading to an ejective solar eruption observed by Hinode, TRACE, STEREO, and SoHO/MDI

A. C. Sterling; C. Chifor; H. E. Mason; R. L. Moore; P. R. Young

doi:10.1051/0004-6361/201014006

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Volume 521 (October 2010)

A&A, 521 (2010) A49

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Table 1:

Line list included in the ``CAM_ARTB_RHESSI'' observational sequence for EIS.
Ion	Wavelength (Å)	Log $T_{\rm max}$ ^* (K)	Note
Fe VIII	185.21	5.6	5.8, after Young et al. (2007a,b)
Fe XXIV	192.03	7.1
Ca XVII	192.82	6.7	EIS core line
Fe XII	195.12	6.1	EIS core line
Fe XIII	202.0, 203.8	6.2	density pair (10⁹-10¹¹ cm-3)
He II	256.32	4.8	EIS core line
Si X	258.37, 261.0	6.1	density pair (10⁷-10¹⁰ cm-3)
Fe XVI	262.98	6.4
Fe XXIII	263.76	7.1
Fe XIV	264.79, 274.2	6.2	density pair (10^8.5-10¹¹ cm^-3)
Mg VII	278.39, 280.75	5.8	density pair (10⁹-10¹¹ cm^-3)
Fe XV	284.16	6.3

Notes. ^(*) Temperature of the fractional ion population peak from Mazzotta et al. (1998).

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