FORECAST SOL: Moderate yellow MAG: Normal green ION: Normal green
HomeEducationalThe Sun and Solar ActivitySolar CycleSolar Cycle Number 22 (1986 - 1996) Monday, Jun 24 2024 03:56 UT
The Sun and Solar Activity

Solar Cycle Number 22 (1986 - 1996)

Cycle 22 certainly provided many highlights. Early in the cycle the smoothed sunspot number (determined by the number of sunspots visible on the Sun and used as the traditional measure of the cycle) climbed rapidly; in fact more rapidly than for any previous recorded cycle. This caused many to predict that it would eclipse Cycle 19 (peak sunspot number of 285) as the highest cycle on record. This was not to be as the sunspot number ceased climbing in 1989 and reached a maximum in November of that year. Whilst not of record amplitude, Cycle 22 still rated as 9th largest of the recorded cycles and continued a run of large solar cycles. (Cycles 18, 19 and 21 were all exceptional!) A very notable feature of Cycle 22 was that it had the 2nd shortest rise from minimum to maximum of all recorded cycles - just 38 months.

Sunspot Cycle Number Year of Minimum Minimum Sunspot Number Year of Maximum Maximum Sunspot Number Rise to Max (yrs) Fall to Min (yrs) Cycle Length (yrs)
14 Jan 1902 4.5 Feb 1906 107.1 4.1 7.4 11.5
15 Jul 1913 2.5 Aug 1917 175.7 4.1 6.0 10.1
16 Aug 1923 9.4 Apr 1928 130.2 4.7 5.4 10.1
17 Sep 1933 5.8 Apr 1937 198.6 3.6 6.8 10.4
18 Feb 1944 12.9 May 1947 218.7 3.3 6.9 10.2
19 Apr 1954 5.1 Mar 1958 285.0 3.9 6.6 10.5
20 Oct 1964 14.3 Nov 1968 156.6 4.1 7.3 11.4
21 Mar 1976 17.8 Dec 1979 232.9 3.8 6.8 10.5
22 Sep 1986 13.5 Nov 1989 212.5 3.2 6.5 9.7

The maximum phase brought some extraordinary intervals of activity. Prime amongst these was the March 1989 period which started on March 6th with the appearance of a large sunspot region (Space Environment Services Center, SESC #5395) on the eastern edge of the Sun. The next 14 days produced 11 "X class" flares (the largest category in X-ray emission) and 48 "M class" (still very large flares). However, the most outstanding feature of the interval occurred on March 13-14 with one of the largest geomagnetic storms in the last 50 years. This storm had an amazing list of effects on Earth and in space. Power systems in Canada and Sweden failed as large electric currents were induced in power lines and tripped protective relays. Increased atmospheric drag, resulting from the expansion of the Earth's outer atmosphere during the disturbance, altered the orbits of many satellites with the result that NASA lost track of some of them for a short period. Satellite navigation systems failed to operate and High Frequency (HF) communication systems were also out of action. Aurorae were sighted at quite equatorial latitudes. The southern regions of Australia were under cloud but numerous sightings were made into Queensland and even at Exmouth in Western Australia (which is north of the tropic of Capricorn). It was indeed an extraordinary period of time!

October 1989 was another interesting interval with a large proton event as a result of solar flares. These are periods of increased flux of charged particles from the Sun and they could have drastic consequences for astronauts away from the protective covering of the Earth's atmosphere. After October 1989 there was much speculation about the effects of a similar event during a manned mission to Mars and this has resulted in increased efforts to predict these events. The period also brought us a large (but not comparable with March 1989) geomagnetic storm again with sightings of aurorae. For Space Weather Services, the period was especially memorable as it coincided with a gathering of many of the world's leading solar-terrestrial forecasters at a workshop organised by ASWFC. As might be expected the large proton event gave the discussions a strong focus and an urgency not seen at previous meetings.

June 1991 was the most outstanding solar flare activity of this cycle, and probably the largest since the peak of the record Cycle 19. The interval from June 1st to June 17th was filled with numerous intense solar flares with one region (SESC #6659) producing five X12 and an X10 flares. An interesting indicator of the strength of this activity came from the US GOES satellites which measure the X-ray output of flares. X-ray detectors on GOES saturated during the five X12 flares over the period. Other flares have occasionally saturated the detectors but it was unique for more than one flare from a single region to achieve this feat. If saturation of the GOES detectors is a measure of strength as in old-time carnivals, then solar activity in June 1991 "rang the bell" like never before! In Australia, we were well placed to see the fireworks because, by pure chance, many of the large flares occurred during the middle of our day. This meant that local HF communications were badly disrupted by Sudden Ionospheric Disturbances (short-wave fadeouts) which cut circuits for many hours. An interesting side effect were the occurrence of several magnetic crochets during the month. These are abrupt changes in the terrestrial magnetic field which arise because of the rapid ionisation of the D-layer of the ionosphere during a large solar flare (this is the same effect which causes short-wave fadeouts when HF signals are absorbed in the highly ionised D-layer). Magnetic crochets are rarely observed because a flare must be both energetic in X-rays and also occur close to local midday. In Sydney at the ASWFC Space Forecast Centre we saw three in one week. June 1991 was quite remarkable and very memorable!

How can we compare the impressive June 1991 solar region with other regions observed over the previous twenty years beforehand? One method of comparison is to calculate the total output of X-ray flares by the region. This index, known as the X-ray flare index (XRI), adds together all the M and X class flares produced by the region with M1 flares counting as 0.1; M2 flares as 0.2; X1 flares as 1.0 and so on.

Patrick McIntosh a retired solar physicist from the NOAA Space Environment Laboratory in Boulder Colorado, compared the solar regions observed between August 1972 and 1991. The following table is based on his data and includes his estimate for the XRI of Region 6659.

Ranking of region Date of passage across centre of Sun SESC region number Latitude on Sun X-ray Flare Index (XRI)
1 09/06/1991 6659 N31 >86.5
2 12/03/1989 5395 N34 57.0
3 08/06/1982 3763 S08 42.4
4 03/07/1974 0433 S14 >=41.4
5 15/12/1982 4025 S06 36.7
6 23/03/1991 6555 S23 32.6
7 15/07/1982 3804 N14 31.6
8 14/07/1978 1203 N18 29.7
9 08/08/1989 5629 S17 >=26.8
10 04/08/1972 0331 N12 >=26.0
11 11/11/1980 2779 S11 25.9
12 17/05/1990 6063 N34 23.1
13 12/01/1989 5312 S31 22.4
14 28/04/1984 4474 S13 21.2
15 18/06/1982 3776 N13 18.8

This comparison indicates that Region 6659 in June 1991 easily heads the list of solar regions to 1991, surpassing even the March 1989 region. Solar cycle 22 is well represented with 6 out of the 15 regions in the list, including the top two regions!

The maximum phase of the cycle appeared to end rather abruptly in early 1992 when monthly values of sunspot number dropped significantly. The decline of Cycle 22 to its minimum in May 1996 was also remarkable because of the lack of major flare activity. The cycle had a multiple personality - malevolent in its first half and quite benign in its decline. This behaviour contrasts with Cycle 21 which was more active in its decline than during its rise or even its maximum.

The cycle was also less than 10 years in duration - a fair bit shorter than the "traditional" eleven year cycle.

There is an old saying that there is "nothing new under the Sun" - but this does not apply to the Sun itself! Cycle 22 proved to be a remarkable cycle by any measure.

Sunspot numbers based on Version 2.0 sunspot numbers published by SILSO

Material prepared by Richard Thompson

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