Maximum Sunspot Numbers and Active Days

Journal of Astronomy and Space Sciences.
2013.
Sep,
30(3):
163-168

This is an open Access article distributed under the terms of theCreative Commons Attribution Non-Commercial License (http://creativecommons.org/licenses/by-nc/3.0/) which premits unrestrictednon-commercial use, distribution, and reproduction in any medium,provided the original work is properly cited.

- Received : May 19, 2013
- Accepted : June 19, 2013
- Published : September 15, 2013

Download

PDF

e-PUB

PubReader

PPT

Export by style

Share

Article

Metrics

Cited by

TagCloud

Parameters associated with solar minimum have been studied to relate them to solar activity at solar maximum so that one could possibly predict behaviors of an upcoming solar cycle. The number of active days has been known as a reliable indicator of solar activity around solar minimum. Active days are days with sunspots reported on the solar disk. In this work, we have explored the relationship between the sunspot numbers at solar maximum and the characteristics of the monthly number of active days. Specifically, we have statistically examined how the maximum monthly sunspot number of a given solar cycle is correlated with the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days for the corresponding solar cycle. We have calculated the linear correlation coefficient
r
and the Spearman rank-order correlation coefficient
r_{s}
for data sets prepared under various conditions. Even though marginal correlations are found, they turn out to be insufficiently significant (
r
~ 0.3). Nonetheless, we have confirmed that the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days is less steep when solar cycles belonging to the "Modern Maximum" are considered compared with rests of solar cycles. We conclude, therefore, that the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days is indeed dependent on the solar activity at its maxima, but that this simple relationship should be insufficient as a valid method to predict the following solar activity amplitude.
r
= 0.3 - 0.5). A significantly better correlation exists between the minimum activity level and the amplitude of the next maximum (Brown 1976, Hathaway et al. 1994). Note that in a more detailed study Solanki et al. (2002) find that the correlation coefficient of this relationship has steadily decreased during the course of the historical sunspot number record, while a significant negative correlation between the
i
-th cycle amplitude and (
i
-3)-th cycle length was also found. Another well-known relation between the amplitude and the duration of different phases of a solar cycle is the so-called Waldmeier relation (Dikpati, Gilman & de Toma 2008). In other words, there is a strong negative correlation between the duration of the ascending phase of a cycle and its amplitude (the cross-correlation coefficient is
r
≈ -0.83 including cycles up to 22nd). The reason for the weak negative relation between the amplitude and length of the solar cycle can be understood, together the Waldmeier effect, by the fact that the relation between the duration of the descending phase and the cycle amplitude is weakly positive (
r
≈ 0.41). Other relations, such as the solar North- South asymmetry, are suggested (e.g., Javaraiah 2008). It is also proposed to use the number of spotless days as a precursor of the amplitude of the upcoming sunspot maximum (Hamid & Galal 2006, Pesnell 2012). That is, correlation between the number of spotless days at the solar minimum and the level of activity in the upcoming solar maximum can be used in prediction.
In this present paper, the relationship between the sunspot numbers at solar maxima and the characteristics of the monthly number of active days (ADs) is studied. AD has been taken as a reliable indicator of solar activity, especially during periods of minimum activity (Harvey & White 1999, Usoskin, Mursula & Kovaltsov 2000, 2001, 2004, Vaquero, Trigo & Gallego 2012). Active days are basically days with sunspots reported on the solar disk. The monthly number of active days in percentage (%) is calculated by taking a ratio of the number of active days to that of observing days in a month. In general, it can be inferred that for years with a low AD value (i.e., AD < 50%) we ought to expect a very low number of sunspot groups observable on the solar disk. Thus, around the solar maxima the monthly number of active days is always 100%, while during the solar minima it is zero or very low (i.e., AD < 50%). There is practically a linear relationship between sunspot numbers and AD when AD < 30% (e.g., Hoyt & Schatten 1998). As stronger cycles are characterized by a steeper rise phase, due to a combination of the overlap of solar cycles with the Waldmeier effect, one may expect an anti-correlation between the level of activity in the following solar maximum and the slope of the linear relationship between sunspot numbers and AD. Simple line of reasoning is as follows. According to the observed Waldmeier relation, there is a strong negative correlation between the duration of the ascending phase of a cycle and its amplitude. What it means is that the sunspot appears somehow abruptly after a long period of the quiet sun, when a strong cycle is to be followed. On the contrary, when a relatively 'active' solar minimum period appears the slope of the active phase becomes less steep. Therefore, active days with weak solar activity consequently result in the first case we discussed. Here, we have attempted to examine whether this expectation is statistically valid.
This paper is organized as follows. We begin with brief descriptions of data and how the active days are defined in Section2. We present and discuss results based on the correlation between the maximum monthly solar sunspot number and the slope of the linear relationship between sunspot numbers and active days in Section 3. Finally, we summarize and conclude in Section 4.
^{1}
, which is the solar physics research department of the Royal Observatory of Belgium. The SIDC collects monthly observations from various stations worldwide in order to calculate the International Relative Sunspot Number (Berghmans et al. 2005, Vaquero 2007). The SIDC includes the World Data Center for the sunspot index and the International Space Environment Service Regional Warning Center Brussels for space weather forecasting. The entire sunspot dataset since 1818 is available as ASCII text files. Each file consists of records with information on individual sunspots for each day that sunspots were observed. Text files containing both monthly and yearly averages of the daily sunspot numbers are also available. In
Fig. 1
, we show yearly sunspot numbers from 1823 to 2008, which correspond to the beginning of solar cycle 7 and to the end
Yearly sunspot numbers from 1823 to 2008 as a function of time.
Monthly sunspot numbers as a function of the monthly number ofactive days (%). It should be noted that there is practically a linear relationshipbetween sunspot numbers and AD (%) when AD (%) is low, for example, ≤ 30.
of solar cycle 23, as a function of time. It should be noted that, besides the 11 year solar cycle a secular and long term variation is apparent.
In
Fig. 2
, we show monthly sunspot numbers as a function of the monthly number of active days (%), both of which are computed with daily sunspot numbers recorded from
The maximum monthly sunspot number of a given solar cycle as afunction of the slope of the linear relationship between monthly sunspotnumbers and the monthly number of active days for the corresponding solarcycle. The slope of the linear relationship between monthly sunspot numbersand the monthly number of active days is obtained using the methodof linear least squares for the part of AD < 30 %. In the upper panel, themaximum solar sunspot number (maximum SSN) of i-th cycle as a function ofthe slope of i-th cycle is shown. For comparisons, in the middle and bottompanels, the maximum SSN of (i -1)-th and (i +1)-th cycles as a function of theslope of i-th cycle are shown, respectively. The straight line in each panel isthe best fit obtained by the method of least squares.
1818 to 2008. Active days are defined as days with sunspots reported on the solar disk, as mentioned above. We calculated the monthly number of active days (%) by taking a ratio of the number of active days to that of observing days of that particular month. It is seen that there is practically a linear relationship between sunspot numbers and AD (%) when AD (%) is low, ≤ 30.
^{1} http://sidc.oma.be/sunspot-data/
Pearson correlation coefficient for AD < 30%. The second and third columns represent the linear correlation coefficients resulting from solar cycles defined by minimum to minimum and by maximum to maximum, respectively. See the text for the detailed discussion.
similar, ~ a couple of parts of hundreds. We would like to note that the solar cycle here is defined by minimum to minimum as commonly defined. For some active cycles, such as 19, the slope cannot be obtained since most of AD is hardly < 30%. In the upper panel, the maximum solar sunspot number (maximum SSN) of
i
-th cycle as a function of the slope of
i
-th cycle is shown. For comparisons, in the middle and bottom panels, the maximum SSN of (
i
-1)-th and (
i
+1)-th cycles as a function of the slope of
i
-th cycle are shown, respectively. The straight line in each panel is the best fit obtained by the method of least squares.
We have calculated a linear correlation coefficient
r
and the single-sided chance probability that |
r
| has an equal or larger value than its observed in the null hypothesis. The obtained correlation coefficients are listed in
Table 1
. The null probabilities are less than 10% for all cases. As to the obtained correlation coefficients there are only low anticorrelations found. The correlation coefficient resulting from the maximum SSN of (
i
-1)-th and the slope of
i
-th cycle particularly low. To examine additional statistical tests we also employ the Spearman rank-order correlation test, which returns a correlation value
r_{s}
and the single-sided probability P (
r_{s}
,N) that N pairs of uncorrelated variables would yield a value of
r_{s}
equally or more discrepant than the one obtained from the data set. We find again there are only low correlations found as in the linear correlation coefficient calculation. In order to check how our results depend on the fitting procedure in obtaining the slope, we have repeated the whole process with data sets of AD < 50% instead of AD < 30%. It has turned out that results are similar to those of AD < 30%.
In
Fig. 4
, we show similar plots to
Fig. 3
, which results from the solar cycle defined by maximum to maximum. Even though the conventional idea that a new cycle begins at the solar minimum is widely accepted, such a standard definition may not be the best in this kind of analysis in that low AD parts have contributions from both beginning and end of a given cycle when sunspot numbers are equally small. Therefore, perhaps one would like to ask a question whether the slope of AD in each intra-cycle interval should be looked for or in inter-cycle interval. In other words, while the analysis presented above corresponds to the former one
Similar plots to Fig. 3 , except that the solar cycles are defined bymaximum to maximum.
would like to look at ADs contributed from the end of the previous cycle and from the beginning of the current cycle, whose case corresponds to the latter. To test the idea of the latter, as a pilot test, we define the solar cycle by maximum to maximum and repeat the same analysis (cf. Mursula & Ulich 1998). For instance, the solar cycle 22 is defined to begin in July in 1989 (officially known as the maximum of solar cycle 22) and to end in March in 2000 (officially known as the maximum of solar cycle 23), instead of traditional duration from September in 1986 (officially known as the beginning of solar cycle 22) to May in 1996 (officially known as the end of solar cycle 22). Having defined the solar cycle as such, we obtained statistical parameters as listed in
Table 1
. Surprisingly, it is very hard to tell that any improvement can be seen. Once again, we also employed the Spearman rank-order correlation test and redo same calculations with data sets of AD < 50 %. General conclusions are same as in minimum to minimum case.
In
Fig. 5
, we show monthly sunspot numbers as a function of the monthly number of active days (%). In upper and bottom panels result from the observed sunspot numbers during the period from solar cycles 7 to 16 and during solar cycles 17 to 23, which correspond to "Modern Maximum", respectively. We would like to note that solar cycles 17 to 23 are markedly stronger than average and none is weaker than average. The slope of the linear relationship between monthly sunspot numbers and the monthly number of active days are 0.155 ± 0.007 and 0.105 ± 0.006, respectively, when data sets of AD < 30% are analyzed. For AD < 50% the
Monthly sunspot numbers as a function of the monthly number ofactive days (%). Upper and bottom panels result from the observed sunspotnumbers during the period from solar cycles 7 to 16 and during solar cycles17 to 23, respectively. Note that solar cycles 17 to 23 are markedly strongerand correspond to "Modern Maximum".
slope of the linear relationship between monthly sunspot numbers and the monthly number of active days are 0.169 ± 0.007 and 0.124 ± 0.008, respectively. Even though the correlation we have found is insufficiently high, as a result of
Fig. 5
, we find that the slope is indeed small for the strong period in a long timescale.
r
and the Spearman rank-order correlation coefficient
r_{s}
for data sets prepared under various conditions. Even though marginal correlations are found, they are insufficiently significant (
r
~ 0.3). This finding is insensitive to a way of obtaining the slope. In particular, the length of intervals of AD in the fitting procedure hardly changes results. We have also attempted to test how the definition of a solar cycle affects results. Solar cycles defined by maximum to maximum instead of minimum to minimum result in similar outcomes. Nonetheless, we have confirmed that the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days is less steep when solar cycles belonging to the "Modern Maximum" are considered compared with rests of solar cycles. According to the relation given in
Fig. 3
, we estimate the maximum of monthly sunspot number is about 120. We note that the current value of monthly sunspot number as of May 2013 is about 80. We are not in a position to discuss whether our method is not working or the solar maximum is yet to come. However, the value of 120 is not out of ranges researchers have predicted as the maximum value of the solar cycle 24. As a result, we conclude that the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days is indeed dependent on the solar activity at its maxima, but unfortunately that it is an inadequate parameter as a precursor.

1. INTRODUCTION

The sunspot numbers form the longest directly observed index of solar activity allowing us to study its variations. The observed sunspot numbers depict well-known the 11-year cycle, namely the Schwabe cycle (Cho & Chang 2011, Kim & Chang 2011, Oh & Chang 2012, Chang & Oh 2012). It is evident that the sunspot cycle is rather irregular (for a comprehensive discussion, see Petrovay 2010). The mean length of a cycle (defined as lasting from minimum to minimum) is 11.02 years (median 10.7 years), with a standard deviation of 1.2 years. The mean amplitude is 113 (median 115), with a standard deviation of 40. It should also be noted that there is an extended interval of atypically strong activity, the so-called "Modern Maximum", covered by solar cycles 17 - 23. Excluding these cycles from the averaging, the mean, and median values of the cycle amplitude are very close to 100, with a standard deviation of 35. On the contrary, solar cycles 5, 6, and 7 are unusually weak, forming the so-called "Dalton Minimum". The long series of moderately weak cycles 12 - 16 can be seen too and occasionally referred to as the "Gleissberg Minimum". In addition, the 11-year solar cycle has an asymmetric shape with a shorter ascending (≈ 4-year on an average) and a longer (≈ 7-year) descending phase. The asymmetry is typically larger for shorter cycles. It is these variations, scientifically speaking, that make the prediction of the solar cycle such a challenging and intriguing issue. Furthermore, solar activity prediction has acquired in recent decades a more prominent status, mostly as a consequence of the potentially large impact of solar activity in human technological activity.
Precursor forecasts remain the most common of predictions (Kane 2007). Many precursor methods of predicting solar activity have made use of the sunspot number. In the most general sense, precursor methods rely on the value of some measure of solar activity at a given time to predict the activity of the following solar cycle. Specifically, correlations between some parameters relating to solar minima and sunspot numbers at solar maxima have been looked for. For instance, the relationships between the solar cycle amplitude and solar cycle length are well known (Solanki et al. 2002, Du 2006, Vaquero & Trigo 2008, Tlatov 2009). There is indeed a marginal correlation, but the correlation coefficient is insufficiently significant (
2. DATA AND ACTIVE DAY

The analysed data are the daily sunspot number obtained from the Solar Influences Data Analysis Center (SIDC)
Lager Image

Lager Image

Lager Image

3. RESULTS AND DISCUSSION

In
Fig. 3
, we show the maximum monthly sunspot number of a given solar cycle as a function of the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days for the corresponding solar cycle. Using the method of linear least squares we obtain for the part of AD < 30%, from similar plots as
Fig. 1
for each solar cycle, the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days. When we calculate the slope of AD, we check the standard deviation. We note the standard deviation of different solar cycles is somewhat
Pearson correlation coefficient for AD < 30%. The second and third columns represent the linear correlation coefficients resulting from solar cycles defined by minimum to minimum and by maximum to maximum, respectively. See the text for the detailed discussion.

Lager Image

Lager Image

Lager Image

4. SUMMARY AND CONCLUSION

Parameters associated with solar minimum have been studied to relate them to solar activity at solar maximum so that one could possibly predict behaviors of an upcoming solar cycle. In this work, we have explored the relationship between the sunspot numbers at solar maximum and the characteristics of the monthly number of active days. Specifically, we have statistically examined how the maximum monthly sunspot number of a given solar cycle is correlated with the slope of the linear relationship between monthly sunspot numbers and the monthly number of active days for the corresponding solar cycle. We have calculated the linear correlation coefficient
Acknowledgements

HYC was supported by the National Research Foundationof Korea Grant funded by the Korean government (NRF-2011-0008123) and also thanks the anonymous referees forcritical comments and helpful suggestions which greatlyimprove the original version of the manuscript.

Berghmans D
,
van der Linden RAM
,
Vanlommel P
,
Warnant R
,
Zhukov A
(2005)
Solar Activity: Nowcasting andForecasting at the SIDC
AnGeo
23
3115 -
3128

Brown GM
(1976)
What Determines Sunspot Maximum
MNRAS
174
185 -
189

Chang HY
,
Oh SJ
(2012)
Does Correction Factor Vary with SolarCycle?
JASS
29
97 -
101
** DOI : 10.5140/JASS.2012.29.2.097**

Cho IH
,
Chang HY
(2011)
Latitudinal Distribution of SunspotsRevisited
JASS
28
1 -
7
** DOI : 10.5140/JASS.2011.28.1.001**

Dikpati M
,
Gilman PA
,
de Toma G
(2008)
The Waldmeier Effect: AnArtifact of the Definition of Wolf Sunspot Number?
ApJ
673
L99 -
L101
** DOI : 10.1086/527360**

Du ZL
(2006)
Relationship Between Solar Maximum Amplitudeand Max-Max Cycle Length
AJ
132
1485 -
1489
** DOI : 10.1086/506474**

Hamid R
,
Galal A
(2006)
Preliminary Prediction of the Strength ofthe 24th 11-year Solar Cycle. In: Bothmer, V, Hady, AA(eds.) Solar Activity and Its Magnetic Origin, Proc. IAU Symp. 233
Cambridge Univ. Press
Cambridge
413 -
416

Harvey KL
,
White OR
(1999)
What is Solar Cycle Minimum?
JGR
104
19759 -
19764
** DOI : 10.1029/1999JA900211**

Hathaway DH
,
Wilson RM
,
Reichmann EJ
(1994)
The Shape of theSunspot Cycle
Sol. Phys.
151
177 -
190
** DOI : 10.1007/BF00654090**

Hoyt DV
,
Schatten KH
(1998)
Group Sunspot Numbers: A NewSolar Activity Reconstruction
Sol. Phys.
179
189 -
219
** DOI : 10.1023/A:1005007527816**

Javaraiah J
(2008)
Predicting the Amplitude of a Solar Cycle Usingthe North-South Asymmetry in the Previous Cycle: II.An improved Prediction for Solar Cycle 24
Sol. Phys.
252
419 -
439
** DOI : 10.1007/s11207-008-9269-6**

Kane RP
(2007)
Solar Cycle Predictions Based on Extrapolation ofSpectral Components: An update
Sol. Phys.
243
205 -
217
** DOI : 10.1007/s11207-007-0475-4**

Kim BY
,
Chang HY
(2011)
Alternating Sunspot Area and HilbertTransform Analysis
JASS
28
261 -
265
** DOI : 10.5140/JASS.2011.28.4.261**

Mursula K
,
Ulich Th
(1998)
A New Method to Determine the SolarCycle Length
Geophys. Res. Lett.
25
1837 -
1840
** DOI : 10.1029/98GL51317**

Oh SJ
,
Chang HY
(2012)
Change of Sunspot Groups Observed from2002 to 2011 at ButterStar Observatory
JASS
29
245 -
251
** DOI : 10.5140/JASS.2012.29.3.245**

Pesnell WD
(2012)
Solar Cycle Predictions
Sol. Phys.
281
507 -
532

Petrovay K
(2010)
Solar Cycle Prediction
LRSP
7
6 -
64

Solanki SK
,
Krivova NA
,
Schüssler M
,
Fligge M
(2002)
Search fora Relationship between Solar Cycle Amplitude andLength
A&A
396
1029 -
1035

Tlatov AG
(2009)
The Minimum Activity Epoch as a Precursor ofthe Solar Activity
Sol. Phys.
260
465 -
477
** DOI : 10.1007/s11207-009-9451-5**

Usoskin IG
,
Mursula K
,
Kovaltsov GA
(2000)
Cyclic Behaviour ofSunspot Activity during the Maunder Minimum
A&A
354
L33 -
L36

Usoskin IG
,
Mursula K
,
Kovaltsov GA
(2001)
Heliosphericmodulation of cosmic rays and solar activity duringthe Maunder minimum
JGR
106
16039 -
16046
** DOI : 10.1029/2000JA000105**

Usoskin IG
,
Mursula K
,
Kovaltsov GA
(2004)
An Upper Limit onSunspot Activity During the Maunder Minimum
Sol. Phys.
224
95 -
101
** DOI : 10.1007/s11207-005-3997-7**

Vaquero JM
(2007)
Historical Sunspot Observations: A Review
AdSpR
40
929 -
941

Vaquero JM
,
Trigo PM
(2008)
Can the Solar Cycle Amplitude BePredicted Using the Preceding Solar Cycle Length?
Sol. Phys.
250
199 -
206
** DOI : 10.1007/s11207-008-9211-y**

Vaquero JM
,
Trigo RM
,
Gallego MC
(2012)
A Simple Method toCheck the Reliability of Annual Sunspot Number in theHistorical Period 1610- 847
Sol. Phys.
277
389 -
395
** DOI : 10.1007/s11207-011-9901-8**

Citing 'Maximum Sunspot Numbers and Active Days
'

@article{ OJOOBS_2013_v30n3_163}
,title={Maximum Sunspot Numbers and Active Days}
,volume={3}
, url={http://dx.doi.org/10.5140/JASS.2013.30.3.163}, DOI={10.5140/JASS.2013.30.3.163}
, number= {3}
, journal={Journal of Astronomy and Space Sciences}
, publisher={The Korean Space Science Society}
, author={Chang, Heon-Young}
, year={2013}
, month={Sep}