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

B4.3

2026-10-25 03:33 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) · 10/25/26

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

Catalogued flares

94,036

1975 → 2026-10-25

GOES X-ray flare lists (NOAA SWPC/NGDC events, yearly compilations by NASA GSFC) · U.S. Government work, public domain (NOAA/NASA) · 10/25/26 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) · 10/25/26 Current · provisional

Latest catalogued flare

B4.3

2026-10-25 03:33 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) · 10/25/26

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) · 10/25/26

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) · 10/25/26 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) · 10/25/26 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) · 10/25/26

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Start (UTC)	Peak	End	Duration	Class	Peak flux (W/m²)	Position	Active region
2003-06-11 08:51	09:09	09:32	41 min	M1.4	1E-5	—	10375
2003-06-11 08:28	08:33	08:35	7 min	M1.1	1E-5	N09W61	10375
2003-06-11 01:01	01:06	01:13	12 min	M1.8	2E-5	N14W56	10375
2003-06-10 21:19	22:02	22:12	53 min	X1.3	1E-4	N10W40	10375
2003-06-10 20:04	20:13	20:21	17 min	M1	1E-5	N14W50	10375
2003-06-10 16:08	16:15	16:26	18 min	M5.6	6E-5	—	10375
2003-06-10 14:28	14:30	14:32	4 min	M3.9	4E-5	—	10375
2003-06-10 14:20	14:24	14:27	7 min	M1	1E-5	N13W36	10375
2003-06-10 12:08	12:36	12:42	34 min	M2.2	2E-5	N10W45	10375
2003-06-10 10:44	11:00	11:17	33 min	M2.2	2E-5	N12W44	10375
2003-06-10 08:55	09:12	09:15	20 min	M5.1	5E-5	N11W45	10375
2003-06-10 06:34	06:37	06:40	6 min	M2.7	3E-5	N12W44	10375
2003-06-10 00:48	00:54	01:01	13 min	M2	2E-5	N13W41	10375
2003-06-09 20:19	20:31	20:42	23 min	M1.4	1E-5	—	10375
2003-06-09 19:31	19:39	19:43	12 min	X1.7	2E-4	—	10375
2003-06-09 09:21	09:28	09:33	12 min	M4.7	5E-5	—	10375
2003-06-08 14:05	14:11	14:15	10 min	M4	4E-5	S19E62	10380
2003-06-06 21:31	21:38	21:58	27 min	M1	1E-5	—	10375
2003-06-02 15:22	15:33	15:40	18 min	M1.8	2E-5	N10E70	10375
2003-06-02 11:13	11:17	11:22	9 min	M1	1E-5	—	10365
2003-06-02 06:12	06:37	06:52	40 min	M3.9	4E-5	S07W89	10365
2003-06-01 22:07	22:22	22:43	36 min	M6.5	6E-5	S06W90	10365
2003-06-01 18:58	19:05	19:10	12 min	M1	1E-5	—	—
2003-06-01 14:43	14:52	14:59	16 min	M1.4	1E-5	S08W80	10365
2003-06-01 10:39	10:50	10:56	17 min	M1	1E-5	—	10375
2003-06-01 05:01	05:11	05:22	21 min	M1	1E-5	—	10375
2003-06-01 00:23	01:06	02:00	97 min	M1.4	1E-5	—	10375
2003-05-31 00:13	00:24	00:40	27 min	M9.3	9E-5	S07W65	10365
2003-05-29 17:28	17:37	17:43	15 min	M2.8	3E-5	S35W13	10368
2003-05-29 00:09	00:18	00:24	15 min	M1.5	2E-5	S37E03	10368
2003-05-28 22:51	23:05	23:12	21 min	X1.2	1E-4	S06W37	10365
2003-05-27 22:17	22:27	22:39	22 min	X3.6	4E-4	—	—
2003-05-27 20:56	21:07	21:13	17 min	X1.3	1E-4	S07W17	10365
2003-05-27 03:06	04:26	05:16	130 min	M1.6	2E-5	S07W14	10365
2003-05-27 00:40	01:06	01:21	41 min	M1.4	1E-5	S07W03	10365
2003-05-26 14:22	14:37	14:51	29 min	M1	1E-5	—	10365
2003-05-26 03:34	03:50	04:02	28 min	M1.9	2E-5	S09E12	10365
2003-05-02 00:47	01:08	01:44	57 min	M1	1E-5	S15W22	10345
2003-04-29 02:32	02:59	03:10	38 min	M1.1	1E-5	S12W55	10337
2003-04-27 13:27	13:32	13:35	8 min	M1.7	2E-5	N21W85	10338
2003-04-26 21:37	21:40	21:42	5 min	M2.5	2E-5	—	10338
2003-04-26 06:01	06:07	06:09	8 min	M7	7E-5	—	10338
2003-04-26 01:01	01:06	01:12	11 min	M2.1	2E-5	—	10338
2003-04-25 22:51	22:58	23:00	9 min	M2.1	2E-5	N20W65	10338
2003-04-25 03:23	03:40	03:58	35 min	M1.2	1E-5	N14E79	10346
2003-04-24 10:45	10:53	11:03	18 min	M3.3	3E-5	N21W39	10338
2003-04-23 13:36	13:56	14:11	35 min	M2	2E-5	N20W22	10338
2003-04-22 22:39	23:06	23:15	36 min	M5.1	5E-5	N22W25	10338
2003-04-21 10:54	11:07	11:14	20 min	M2.8	3E-5	N18E02	10338
2003-04-18 17:50	17:58	18:02	12 min	M1.1	1E-5	—	10337

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 25, 2026 · SHA-256 a1d99f7354e3…
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