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

C1.5

2026-10-26 04:36 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) · 10/26/26

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

Catalogued flares

94,047

1975 → 2026-10-26

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

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) · 10/26/26 Current · provisional

Latest catalogued flare

C1.5

2026-10-26 04:36 UTC · AR 14561

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

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) · 10/26/26

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) · 10/26/26 Current · provisional

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) · 10/26/26 Current · provisional

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) · 10/26/26

Year

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Start (UTC)	Peak	End	Duration	Class	Peak flux (W/m²)	Position	Active region
1989-01-08 14:02	14:09	14:58	56 min	M1.1	1E-5	S27E17	5310
1989-01-08 11:28	11:47	12:35	67 min	M7.5	8E-5	S33E58	5312
1989-01-08 06:57	06:58	07:02	5 min	M2.4	2E-5	S34E55	5312
1989-01-07 20:44	21:57	22:59	135 min	M1.6	2E-5	—	—
1989-01-07 18:05	18:40	19:17	72 min	M1.3	1E-5	S35E66	5312
1989-01-07 17:29	17:30	17:38	9 min	M1.2	1E-5	S34E71	5312
1989-01-07 17:10	17:14	18:08	58 min	M1.1	1E-5	S18W77	5301
1989-01-07 16:00	16:28	16:44	44 min	M1.3	1E-5	S20W77	5301
1989-01-07 12:06	12:31	13:01	55 min	M1.8	2E-5	S19W79	5301
1989-01-07 03:12	03:36	03:44	32 min	X1.1	1E-4	S34E80	5312
1989-01-06 21:50	22:43	23:20	90 min	M1.1	1E-5	—	—
1989-01-06 18:14	18:20	18:32	18 min	M1.2	1E-5	S17W66	5301
1989-01-06 16:53	17:12	17:46	53 min	M8.9	9E-5	S31E78	5312
1989-01-06 03:59	04:08	04:26	27 min	M1.4	1E-5	—	—
1989-01-04 16:13	16:29	16:41	28 min	M1.4	1E-5	—	—
1989-01-04 15:03	16:53	18:28	205 min	M4.7	5E-5	S20W60	5303
1989-01-03 16:38	16:38	16:48	10 min	M1.5	2E-5	N24E67	5307
1989-01-03 12:44	12:46	13:10	26 min	M1.1	1E-5	S15W53	5297
1989-01-03 10:42	10:43	10:54	12 min	M1	1E-5	N24E70	5307
1989-01-03 09:10	09:23	09:35	25 min	M1.2	1E-5	—	—
1989-01-02 17:48	18:10	21:09	201 min	M2.2	2E-5	—	—
1989-01-02 09:17	09:47	09:57	40 min	M1.1	1E-5	S17W64	5292
1989-01-01 05:12	05:20	05:57	45 min	M1.4	1E-5	S21W53	5292
1988-12-30 16:25	17:16	18:48	143 min	X1.4	1E-4	S19W30	5292
1988-12-29 10:55	11:00	13:47	172 min	M2.2	2E-5	S21W17	5292
1988-12-28 22:42	22:43	22:58	16 min	M3.6	4E-5	N21W58	5285
1988-12-28 17:43	17:46	17:46	3 min	M1.4	1E-5	S17E24	5297
1988-12-28 13:25	13:31	14:03	38 min	M1.3	1E-5	S17E27	5297
1988-12-28 11:18	11:21	12:14	56 min	M2.2	2E-5	N20W50	5285
1988-12-28 07:25	07:43	08:15	50 min	M1.2	1E-5	S17E31	5297
1988-12-27 23:27	23:48	01:06	99 min	M2.1	2E-5	S18E08	5292
1988-12-27 06:12	06:36	08:11	119 min	M1.9	2E-5	—	—
1988-12-27 04:30	04:31	04:42	12 min	M1.3	1E-5	N20W35	5285
1988-12-26 19:18	19:42	20:14	56 min	M6.1	6E-5	S20E20	5292
1988-12-25 10:10	10:15	10:23	13 min	M1.1	1E-5	—	—
1988-12-24 15:56	16:01	16:28	32 min	M1.1	1E-5	S17E54	5292
1988-12-24 12:25	12:36	14:01	96 min	M1.5	2E-5	—	—
1988-12-24 01:01	01:07	01:25	24 min	M2.9	3E-5	—	—
1988-12-23 14:10	14:18	15:43	93 min	M1.9	2E-5	S33W90	5275
1988-12-23 07:48	07:53	08:02	14 min	M1.6	2E-5	S32W89	5275
1988-12-22 22:07	22:10	00:26	139 min	M5.3	5E-5	N26W41	5280
1988-12-22 14:55	14:59	15:12	17 min	M1	1E-5	S31W69	5275
1988-12-22 05:17	05:22	05:29	12 min	M1	1E-5	S35W80	5273
1988-12-21 14:53	14:58	15:05	12 min	M1.5	2E-5	S32W67	5273
1988-12-20 11:18	11:44	14:32	194 min	M7.3	7E-5	—	—
1988-12-20 07:56	08:03	08:23	27 min	M1	1E-5	N21E58	5285
1988-12-20 00:52	01:00	02:08	76 min	M1.9	2E-5	S31W53	5273
1988-12-19 17:43	17:48	18:29	46 min	M1.2	1E-5	N21E68	5285
1988-12-18 23:30	23:00	23:47	1457 min	M1.4	1E-5	N24W27	5279
1988-12-18 15:51	16:14	17:45	114 min	X1.1	1E-4	S31W40	5273

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 26, 2026 · SHA-256 d24560b7385e…
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