Download Solar cycle according to mean magnetic field data V.N. Obridko1

Крупномасштабное поле Солнца
и активные долготы.
Обридко В.Н., Иванов Е.В., Чертопруд В.Е.
.
Pushkov Institute of Terrestrial Magnetism, Ionosphere, and
Radio Wave Propagation (IZMIRAN)
1
8.02.2010
Использованные данные
Гринвичские наблюдения площадей пятен (1976 2005)
Наблюдения крупномасштабного магнитного
Солнца в WSO (1976-2009).
Расчеты положения глобального магнитного
диполя по наблюдениям в WSO (1976-2005)
Наблюдения фоновых полей на SOHO MDI
(1998-2003)
It is evident that the
fields of different
polarities tend to
concentrate in
different regions
Low-resolution images only reveal these extended
unipolar regions, but if we superimpose a low-resolution
map on a high-resolution magnetogram, we shall readily
see the agreement of the polarities.
3
4
Из вариации центр-лимб обнаружено,
что сильные фоновые поля в основном
вертикальные, а слабые горизонтальные
30
120
1980
1985
1990
1995
2000
2005
 vert , T/R
140
3
120
100
 full ,  , T/R
3
60
120
110
100
90
80
70
60
50
40
30
20
10
0
1975
80
60
40
20
0
1975
1980
1985
1990
1995
2000
2005
1975
1980
1985
1990
1995
2000
2005
0
3
, °
90
-60
-90
200
W
150
100
50
80
60
40
20
0
0
1975
100
 horiz , T/R
-30
1980
1985
1990
1995
2000
2005
Time in years
Total magnetic moment of the dipole:
a) magnetic moment;
b) the inclination angle 
of dipole axis (latitude),
c) the monthly mean Wolf numbers.
Time in years
Time variation of the vertical vert (a)
and horizontal horiz (b) components
of the global magnetic dipole (blue lines).
The dot lines on both panels show
the total magnetic moment.
6
Position of the north pole of the magnetic dipole for three solar cycles.
The upper panels correspond to the northern hemisphere and the lower
ones, to the southern hemisphere.
The circles are the contour lines of the values cos  given on the scales
7
for each cycle.
SOHO/MDI. <B2> after time standardization. This procedure combines the fields of
both signs and increases the contribution of large background fields.
The 11-year cycle is manifested at all latitudes. The cycle maximum
moves from pole to pole for two years. Outside the equator,
the cycle variation in the background magnetic field energy has two maxima.
8
Активные долготы
Впервые обнаружены в 1897 году Вольфером.
Понятие активных долгот для разных индексов
Дискуссия – одна или две активных долготы.
Зависимость от скорости вращения, широты и
мощности индексов
Связь с крупномасштабным полем
9
The tendency of the solar cycle to appear at the preferred longitudes was found
by Benevolenskaya, Hoeksema., Kosovichev and Scherrer (1999)
and Bumba, Garcia, and Klvana (2000).
Left panel: Synoptic maps of the
solar magnetic field for CR 1911–
1934 derived from the SOHO/MDI
magnetograms during the activity
minimum between cycles 22 and
23. Values of the line-of-sight
component of the magnetic field
are represented in light and dark
for positive and negative polarities,
respectively.
Right panel: More detailed
synoptic magnetic maps for CR
1916–1923.
The magnetic flux of
the new cycle has a
tendency to reappear
in the active longitudinal
zones. Benevolenskaya,
2009
•
The sunspot occurrence data confirm the existence of two
preferred longitudes 180 apart, which migrate in any fixed
rotation frame but are persistent throughout 120 years
• The differential rotation is significantly different from the
differential rotation of individual spots. This implies that the
depth at which sunspots are formed (and affected by the nonaxisymmetric component of the field) is different from that
where developed sunspots are anchored (I.G. Usoskin, S.V.
Berdyugina and J. Poutanen (2005)
• The lifetime of the sunspot formation zones exceeds
significantly that of individual sunspots and may reach 15-20
rotations.
• The stability of the Active Longitudes is larger for the larger
spots (Ivanov, 2006)
Longitudinal distribution for major, medium-size
and small short-lived sunspots in the northern
hemisphere in cycle 20. (Ivanov, 2006)
11
Theoretical arguments
Alberto Bigazzi and Alexander Ruzmaikin (2003)
explained the Sun’s Preferred Longitudes as a Coupling of Magnetic
Dynamo Modes.
D. Elstner and H. Korhonen (2005) .To explain this
phenomenon, a non-axisymmetric dynamo mode, giving rise
to two permanent active longitudes at opposite stellar
hemispheres, is needed together with an oscillating
axisymmetric magnetic field.
Axel Brandenburg and Petri J. K¨apyl¨a (2005)
solved a two-dimensional mean field dynamo model where
magnetic helicity conservation is fully included. The model
develops longitudinal variability with activity patches
travelling in longitude. These patches may be associated
with active longitudes.
However, there are objections to the existence
of two active longitudes
Losh (1938) found that there is one maximum and one minimum
per rotation, and that the phase of the maximum is stable over a
solar cycle.
Balthasar & Schüssler (1984) investigated sunspot numbers
and showed that the phase of the maximum remains more or
less the same for two solar cycles and then it changes by about
180◦.
Baltasar (2007) revealed only one maximum in the Fourier
spectrum, i.e., one active longitude.
13
Knaack & Stenflo (2005) and Knaack et al.
(2005) used magnetograms from Mt.Wilson and from Kitt Peak
and found that the dominant rotation periods are different for
cycles 21, 22 and 23.
Bouwer (1992) investigated various indicators of solar activity
and found that precise periods between 27 and 28 days persist
only for a short time, sometimes only for a few solar rotations.
J. Pelt, J.M. Brooke , M.J. Korpi, and I. Tuominen (2006)
strong and well substantiated evidence for an essential and
century-scale persistent nonaxisymmetry in the sunspot
distribution does not exist.
C. J. Henney, B. R. Durney, 2007 A surprisingly non-negligible
likelihood is found, approximately 1 in 3, that observed
periodicities from integrated full-disk solar parameters are a
chance occurrence for time series of the order of 20 years in
duration.
North
area
Carrington system
1980
1980
1985
1985
1990
1990
1995
1995
2000
2000
2005
number
North
2005
90
180
270 South
1980
1980
1985
1985
1990
1990
1995
1995
2000
2000
2005
90
180
270
90
180
270
2005
90
180
270
South
carrington system
0,08
0,08
area
0,07
0,06
South
area
North
0,06
0,05
0,04
0,04
0,03
0,02
0,08
0,02
0
50
100
150
200
250
300
350
0
50
100
150
200
250
300
350
100
150
200
250
300
350
number
number
0,07
0,08
0,07
0,06
0,06
0,05
0,05
0,04
0,04
0,03
0,03
0,02
0,02
0
50
100
150
200
250
300
350
0
50
longitude
17
18
Хейловская
граница
Антихейловская
граница
Цикл 23
Цикл 22
Цикл 22
Цикл 23
В гелиомагнитной системе координат
фиксированные долготы определяются точками
пересечения гелиомагнитного и гелиографического
экваторов (270 и 90 градусов). Их положение не зависит
от времени. Меняется только раствор («tilt»). В минимуме
эти координаты становятся неопределенными.
About 70% of the spots with the
area >500 m.p.h are located
at a distance <20 degrees
in longitude from the
Large Scale Neutral Line.
However, the longitude of
the axis of the effective solar
dipole (and the longitude of
the associated neutral line)
changes with the course of time
21
The longitude of the effective solar dipole shifts
by 20.2 degrees per year and by 360 degrees
for 18-20 years
300
Это, кстати,
объясняет,
почему
активные
долготы
в
керрингтоновской
системе
Shift of the longitudeразмываются
o
1.5 /rotation
за 2-3 года
200
20.2 /year
1000
900
800
Longitude
700
600
500
400
R=0.91
0
100
1975 1980 1985 1990 1995 2000 2005 2010
Years
North
area
Heliomagnetic system
Number
1980
1980
1985
1985
1990
1990
1995
1995
2000
2000
2005
90
180
270 South
2005
1980
1980
1985
1985
1990
1990
1995
1995
2000
2000
2005
90
180
270
2005
North
90
180
270
90
180
270
South
heliomagnetic system
0,08
0,08
area
North
0,07
0,07
0,06
0,06
0,05
0,05
0,04
0,04
0,03
0,03
0,02
South
area
0,02
0,08 0
50
100
150
200
250
300
350
number
50
0,08 0 number
0,07
0,07
0,06
0,06
0,05
0,05
0,04
0,04
0,03
0,03
0,02
100
150
200
250
300
350
100
150
200
250
300
350
0,02
0
50
100
150
200
250
300
350
0
heliomagnetic longitude
50
0,12
0,12
0,12
Cycle 22
North
Cycle 21
North
Cycle 23
0,10
0,10
0,10
0,08
0,08
0,08
0,06
0,06
0,06
0,04
0,04
0,04
0,02
350
300 250
200 150
100
50
0,12
0,02
350
0,09
Cycle 21
South
0,10
0,08
0,06
300 250
Cycle 22
200 150
100
50
South
0,08
0,07
0,06
0,02
350
0,10
300 250
Cycle 23
North
200 150
100
50
South
0,08
0,06
0,05
0,04
0,04
0,04
0,02
350 300 250 200 150 100 50
0,03
350 300 250 200 150 100 50
0,02
350 300 250 200 150 100 50
Выводы
• Составляющие магнитного поля Солнца
образуют единый организм, в то же
время циклические вариации и области
генерации составляющих могут
меняться в зависимости от мощности и
характерных размеров.
• Глобальное магнитное поле
восстанавливает свою долготноширотную структуру через 22 года
• Активные долготы лучше проявляются в
мощных элементах активности.
• Активные долготы отражают вращение
глобального магнитного поля.
• В гелиомагнитной системе координат
активные долготы возникают в точках
пересечения гелиомагнитного и
гелиографического экваторов.
• В каждом цикле в каждом полушарии есть
только одна активная долгота
определяемая глобальным полем с учетом
Хейловских законов полярности
Спасибо за внимание
31
Fig. 5. Histogram distribution of recovered spot locations
with respect to the semi-annual averages of one active
longitude for solar cycles 12 to 22. Error bars correspond
to 1σ statistical error. The best-fit double Gaussian function
with peaks at phases 0.0 and 0.5 and the standard
deviation of about 0.11 is shown by solid lines
S. V. Berdyugina and I. G. Usoskin, 2003)
32
Fig. 1. Active longitudes and the flip-flop phenomenon
on cool active binary components: on the left, as observed in light
curves of Gem, and on the right, in Doppler images of II Peg. The
images on the left show the distribution of the spot filling factor on
the stellar surface obtained via inversions of the light
curves (plots in the middle). The II Peg images obtained from
inversions of spectral line profiles show the temperature distribution
on the stellar surface as seen from the pole. Flip-flops appear as a
switch of thedominant activity to the opposite longitude
S.V. Berdyugina (2007)
33
Greenwich data for 1879-2005 (cycles 12-23) are
used to study the longitude distribution of sunspot
group areas summed over a Carrington rotation
separately in the southern and northern hemispheres.
The active longitudes were studied in two reference
frames corresponding to the rotation periods
T=27.2753 and T=27.00 days.
The AL zones are shown to consist of a set of
individual narrow sunspot formation zones rotating
rigidly with the Carrington period T~27.2753 days.
The lifetime of the sunspot formation zones exceeds
significantly that of individual sunspots and may reach
15-20 rotations.
Besides the rigidly rotating active longitudes we have
revealed the active longitudes that migrate in the
Carrington reference frame at different (greater and
smaller than Carrington) angular velocities.
E.V. Ivanov , 2006
34
Fig. 1. Longitudinal distribution
of SCR (d,e,f) for major (s(CR)>2000 m.v.h.), medium-size
(100 m.v.h.<s(CR)<2000 m.v.h.), and small short-lived
sunspots (10 m.v.h.<s(CR)<100 m.v.h.)
in the northern hemisphere in cycle 20. (Ivanov, 2006)
35
Fig. 7. Time-longitude diagrams of the rotation-summed sunspot
areas s(CR) for sunspots with s(CR)>2000 m.v.h. over
the past 6 cycles (18-23) separately in the northern
and southern hemispheres.
36
• 1. Выявлено два периода вращения, для
которых явление активных долгот
превышает принятый уровень
статистической достоверности. Это
позволило сделать предположение о
существовании двух систем активных
долгот на Солнце.
• 2. Система активных долгот с Р ~ 27 сут.
доминирует в наиболее мощных 11-летних
циклах активности.
• 3. Система активных долгот с Р ~ 28 сут.
наиболее выражена в эпоху минимума
векового цикла
S.V. Olemskoy, L.L. Kitchatinov
37
0,20
Power
0,15
0,10
0,05
0,00
1
2
3
Period in Years
4