|
SUNSPOTS
A
remarkable phenomenon that appears in the optic observation of the surface of
the sun is constituted from the "sunspots."
The sunspots are formations relatively dark on the solar surface with
temperatures around 3000° K if compared to the surrounding zones of 6000° K.
The
sunspots, whose nature is not still very clear, center of intense magnetic
fields, (up to 0,4Wb/ m2) change polarity at the change of the cycle
of 11 years and have polarity opposed according to the solar hemisphere in which
they are.
The
sunspots vary from a minimum to a maximum, until to a new least, in around 11
years, and the available data for the old cycles are illustrated in figure 1.
Figure
1– Trend of the
sunspots
between 1700
and 1960
(the
more ancient data are less homogeneous and less sure)
Note:
On this trend for a long time term has been hypothesized the possibility of an
also secular cycle superimposed to that of 11 years.
The
trend of the total flux of the sun and the number of the sunspots are between
them in synchronous relationship, and the atmospheric ionization varied in
proportion with them; for this proportionality, at the effects of the ionization,
is used the index of sunspot, rather than their number; the practical formula is:
R=
K (10 g + S)
where:
R =
number index of the sunspots
g =
groups of sunspot
S =
single sunspot
K =
empirical coefficient of proportionality.
The
value R
is called number of the sunspots, while would be defined like "number index
of the sunspots”.
Diagram
performed by I2MOV
from the data received by the beacon DK0WCY.
The
data of the beacon was listened every day in CW on the frequency of 10144 kHz.
The
monthly solar flux averages are from August
1997 to December 2011.
The
level of the sunspot R = 0 corresponds
about at solar flux
F = 65.
|