An automated classification approach to ranking photospheric proxies of magnetic energy build-up

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Volume 579 (July 2015)

A&A, 579 (2015) A64

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Table 5

Comparison to related flare prediction methods.

Reference	ARs	Images	Flares^a	Magnitude	Window (h)	Temporal	TPR	TNR	TSS	HSS


Ours	2124	122 060	3432–19 086^b	≥C1.0	2–24	No	0.81	0.70	0.51	0.39


1	N/A^c	?^d	8498	≥C1.0	24	No	0.46^e	0.99^e	0.45^f	0.54^e
2	230	?^d	167	≥C1.0	24	No	0.33^g	0.92^g	0.25^g	0.29^g
3	870	48 344	8612	≥M1.0^h	48	Yes	0.90ⁱ	0.88ⁱ	0.78^f	0.66ⁱ
4	?^d	31 164	8510	≥M1.0^h	48	Yes	0.85^j	0.88^j	0.73^f	0.69^j
5	1010	55 582	9801	≥M1.0^h	48	Yes	0.95^k	0.92^k	0.87^f	0.77^k
6	46	2708	119 228^b	≥C1.0	6, 24	No	0.49^l	0.99^l	0.47^l	0.51^l
7	?^d	55	54	≥C1.0	24	No	0.75^m	0.93^m	0.68^m	0.69^m

Notes.

^(a)

Number of data points associated with a flare; multiple data points may include the same flare within the time window.

^(b)

The range of values is due to the range in time windows.

^(c)

Magnetic features are considered rather than ARs.

^(d)

This information was not readily apparent from the paper.

^(e)

From Table 5 in Ahmed et al. (2013).

^(f)

Computed from TPR and TNR.

^(g)

Compiled from Figs. 3–6 in Yuan et al. (2010).

^(h)

This magnitude specifies the total flare importance index.

⁽ⁱ⁾

From Fig. 5 in Huang et al. (2010).

^(j)

From Table 5, BN_F column in Yu et al. (2010b).

^(k)

From Table 5, MODWT_DB2_Red column in Yu et al. (2010a).

^(l)

Computed from Table 4, 24N FLCT in Welsch et al. (2009).

^(m)

Computed from Table 8, Model (7) in Song et al. (2009).

Reference. (1) Ahmed et al. (2013); (2) Yuan et al. (2010); (3) Huang et al. (2010); (4) Yu et al. (2010b); (5) Yu et al. (2010a); (6) Welsch et al. (2009); (7) Song et al. (2009).

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