Sun · flares

A Sun that bursts

Flares are sudden releases of magnetic energy above active regions. The flashes in this view recall the classes of the strongest flares in the GOES catalogue (X, M); their positions are illustrative.

Latest catalogued flare

B7.5

2026-10-24 02:11 UTC

Strongest in the catalogue

X28

2003-11-04

X-class flares

558

1975 → 2026

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

Illustrative rendering: procedural prominence loops and flashes; classes from the GOES catalogue below.

Catalogued flares

94,033

1975 → 2026-10-24

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

X-class flares

558

7954 M-class

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

Latest catalogued flare

B7.5

2026-10-24 02:11 UTC · AR 14560

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

Strongest in the catalogue

X28

2003-11-04 18:29 UTC · S19W83

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

X- and M-class flares per year GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26 GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

Show the data as a table

Number of flares per calendar year in the GOES catalogue (NOAA). The current year is provisional; 2020 is marked “instrument change”: since December 2019 the flux is no longer reduced by the 0.7 factor, which raises classes by about 40%.

C-class flares per year GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

Show the data as a table

Detection of C-class flares depends on the background level, hence on the cycle phase and the instrument; these counts are less homogeneous than those of M and X classes.

Ten strongest flares (peak flux derived from the class)

#	Class	Start (UTC)	Peak	Peak flux (W/m²)	Position	Active region
1	X28	2003-11-04 18:29	18:50	3E-3	S19W83	10486
2	X20	1989-08-15 23:08	23:17	2E-3	S18W84	5629
3	X20	2001-04-02 19:32	19:51	2E-3	—	—
4	X17	2003-10-28 08:51	10:10	2E-3	—	10486
5	X17	2005-09-07 15:17	15:40	2E-3	S11E77	10808
6	X15	1989-03-06 12:54	13:10	2E-3	N35E69	5395
7	X14	2001-04-15 11:19	11:50	1E-3	S20W85	9415
8	X13	1984-04-24 21:56	22:01	1E-3	S12E43	4474
9	X13	1989-10-19 11:29	11:55	1E-3	S27E10	5747
10	X12	1982-06-06 14:30	14:54	1E-3	S09E25	3763

The peak flux (0.1–0.8 nm, W/m²) is derived from the published class, e.g. X28 = 28 × 10⁻⁴ W/m²; the GOES detectors saturated above X17 before 2003, so the 4 November 2003 flare is an estimate.

Filterable catalogue GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/24/26

Year

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Start (UTC)	Peak	End	Duration	Class	Peak flux (W/m²)	Position	Active region
2013-06-23 18:48	18:56	18:59	11 min	M2.9	3E-5	S15E62	11778
2013-06-21 00:30	01:14	01:43	73 min	M2.9	3E-5	S16E73	11777
2013-06-07 20:11	20:49	21:04	53 min	M5.9	6E-5	—	11762
2013-06-05 06:14	06:57	07:26	72 min	M1.3	1E-5	S32W51	11762
2013-05-31 17:52	18:00	18:06	14 min	M1	1E-5	N13E43	11760
2013-05-22 11:08	11:32	12:08	60 min	M5	5E-5	—	11745
2013-05-20 03:16	03:25	04:03	47 min	M1.7	2E-5	—	11755
2013-05-17 06:43	06:57	07:19	36 min	M3.2	3E-5	—	11748
2013-05-16 19:36	19:53	20:03	27 min	M1.3	1E-5	N13E41	11748
2013-05-14 23:25	23:48	23:58	33 min	X1.2	1E-4	N12E64	11748
2013-05-13 22:00	23:11	23:20	80 min	X3.2	3E-4	—	11748
2013-05-13 13:48	14:05	14:16	28 min	X2.8	3E-4	N11E85	11748
2013-05-13 09:57	10:03	10:09	12 min	M1.3	1E-5	—	11748
2013-05-12 23:53	00:17	00:32	39 min	X1.7	2E-4	—	11748
2013-05-12 20:37	20:44	20:52	15 min	M1.2	1E-5	—	11748
2013-05-12 18:17	18:32	19:03	46 min	M1.9	2E-5	—	11748
2013-05-10 10:37	10:56	11:04	27 min	M1.3	1E-5	—	11745
2013-05-09 22:44	22:57	23:08	24 min	M3.9	4E-5	—	11745
2013-05-05 15:42	15:56	15:58	16 min	M1.4	1E-5	N13E49	11739
2013-05-03 15:24	15:32	15:41	17 min	M5.7	6E-5	N16E81	11739
2013-05-03 14:39	14:55	15:22	43 min	M1.3	1E-5	N10W38	11731
2013-05-02 02:58	03:10	03:19	21 min	M1.1	1E-5	N10W26	11731
2013-04-22 08:22	08:29	08:31	9 min	M1	1E-5	—	11726
2013-04-12 17:52	18:38	18:46	54 min	M3.3	3E-5	—	11718
2013-04-11 04:55	05:16	05:29	34 min	M6.5	6E-5	N09E12	11719
2013-04-05 15:34	15:48	16:04	30 min	M2.2	2E-5	—	11719
2013-03-21 20:42	21:04	21:36	54 min	M1.6	2E-5	—	11692
2013-03-15 04:46	05:58	07:35	169 min	M1.1	1E-5	N11E12	11692
2013-03-05 06:47	06:54	06:59	12 min	M1.2	1E-5	S15W54	11686
2013-02-17 14:45	14:50	14:52	7 min	M1.9	2E-5	N12E22	11675
2013-01-13 07:35	07:38	07:40	5 min	M1.7	2E-5	—	11652
2013-01-12 23:45	23:50	23:52	7 min	M1	1E-5	—	11652
2013-01-11 13:51	14:07	14:24	33 min	M1	1E-5	—	11654
2013-01-11 07:43	08:11	08:17	34 min	M1.2	1E-5	—	11654
2013-01-05 08:26	08:31	08:34	8 min	M1.7	2E-5	—	11652
2012-11-28 20:20	20:36	20:48	28 min	M2.2	2E-5	S14W57	11620
2012-11-27 20:05	20:26	20:30	25 min	M1	1E-5	S14W41	11620
2012-11-27 14:52	14:57	15:03	11 min	M1.6	2E-5	N05W73	11618
2012-11-21 14:10	14:30	14:38	28 min	M3.5	4E-5	—	11618
2012-11-21 05:45	05:56	06:08	23 min	M1.4	1E-5	N06E10	11618
2012-11-20 18:21	18:28	18:32	11 min	M1.6	2E-5	N07E15	11618
2012-11-20 11:36	11:41	11:46	10 min	M1.7	2E-5	—	—
2012-11-14 02:59	03:04	03:07	8 min	M1.1	1E-5	—	11613
2012-11-13 19:50	19:54	19:57	7 min	M2.8	3E-5	S22E33	11613
2012-11-13 04:42	04:50	04:54	12 min	M2.5	2E-5	—	11613
2012-11-13 00:58	01:04	01:06	8 min	M6	6E-5	—	11613
2012-11-12 22:13	22:28	22:33	20 min	M2	2E-5	—	11613
2012-11-11 01:11	01:33	01:52	41 min	M1	1E-5	—	11614
2012-11-08 01:08	01:23	01:55	47 min	M1.7	2E-5	—	11611
2012-10-23 01:13	01:17	01:21	8 min	X1.8	2E-4	—	11598

Method and sources

The catalogue reproduces the NOAA (SWPC/NGDC) GOES event lists compiled yearly by the NASA GSFC Hesperia centre: start, peak and end (UT), class, heliographic position and active region when known. The class encodes the peak flux in the 0.1–0.8 nm band: C = 10⁻⁶ W/m², M = 10⁻⁵, X = 10⁻⁴, times the number (M2.3 = 2.3 × 10⁻⁵ W/m²).

Lines without an X-ray class (optical or sub-threshold events) are not imported. The last two years are re-read on each import; duplicates are rejected by start time and class. Yearly counts are computed from the imported catalogue.

Reading these data

Until December 2019 NOAA applied a 0.7 factor to the XRS-B flux of GOES 8 to 15; since GOES-16 became the primary satellite the raw flux is used. For the same physical flux, a class after 2020 is therefore about 1.4 times higher (Janssens et al., 2025). Counts before and after 2020 are not directly comparable.

SOURCES OF THIS PAGE

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC): NOAA SWPC/NGDC GOES X-ray flare event lists (1975–), yearly compilations by K. Tolbert, NASA GSFC Hesperia. Flare classes as reported by NOAA at the time: until December 2019 the XRS-B flux carried a 0.7 scaling factor (Janssens et al., 2025). · source page ↗
Licence : U.S. Government work, public domain (NOAA/NASA) · retrieved on Oct 24, 2026 · SHA-256 775bfeb19587…
Janssens (2025): Janssens, J., et al. (2025). Solar flare rates and probabilities based on the McIntosh classification: impacts of GOES/XRS rescaling and recalibration. Journal of Space Weather and Space Climate. · doi:10.1051/swsc/2025007
Licence : Published literature; cited

Solar flares GOES X-ray flare catalogue since 1975

A Sun that bursts