... waves in
the radiative zone
6 Towards a 3D Integrated Model of the Sun
Coupling nonlinearly the convection zone with the radiative interior is the key to
understand the solar global dynamo and inner ... sign, depending
on the sense of rotation (orientation of the field vector). The magnitudes of these
two effects depend on the competition between the Larmor prec...
... missing is the almost horizontal passage through the very
thin annulus occupying the space between its deepest penetration level and that of
the second wave: the space between the second and third ... reflected
beneath, rather than at, the surface of the Sun, one cannot know the structure of the
Sun all the way to the surface. So how can one proceed? And ho...
... hole
1
http://www.lmsal.com/solarsoft/
Coronal Mass Ejections from Sunspot and Non-Sunspot Regions 30 3
4.2 Implications to the Flare: CME Connection
The difference in the latitude distributions of CMEs (no butterfly diagram) and
flares ... al.
correlation was found between the flaring rate and sunspot number during the maxi-
mum phase. This result further confirms the close...
... Connection 33 3
is universal among cool stars, the Sun appears to be at the lower end of the observed
activity scale, and only few (cool) stars output even less X-ray emission than the
Sun. The ... 3: 9 /3 1 Ä Ä 3: 9
Set 4 – 1 Ä Ä 3: 9 /6 1 Ä Ä 3: 9
Set 5 ` D 2, n D 31 Ä Ä 3: 9 1 Ä Ä 3: 9
Set 6 ` D 1 2, n D1 to 10 1 Ä Ä 3: 9 1 Ä Ä 3: 9
The S...
... 0.50 and 90:16% for sunspot numbers;
(2) 0.42 and 82:12% for group sunspots; (3) 0 .31 and 67 :3% for sunspot areas;
and (4) 0 .33 and 41%for10:7 cm radio flux. The results for sunspot numbers
and ... sketches and magnetic field strengths of all sunspots and strong
pores. These were used to evaluate the magnetic configurations associated with the
sunspots.
3 Results...
... light on the constitution of
the Sun. In 1885, the Royal Society, London, constituted the Indian Observatories
Committee comprised of the Astronomer Royal, and a few Fellows of the Royal and
Royal ... showed
the CN bands and the C2 Swan bands in the head, while the tail showed bands due
to CO. He was ably assisted in the observations by his wife Mary.
Contents i...
... in the upper layers of the photosphere and the chromosphere
and consequently no substantial coupling between waves and the magnetic field
would occur in these layers. On the other hand, if there ... 30
Arcseconds
50
0
5
10
15
20
25
30
10
Arcseconds
15 20 25 30
0
630 0.0
630 1.9
630 3.7
630 5.6
5
10
15
20
25
30
Arcseconds
0
−1.50.0 1.5
5
10
15
20
25
30
Fig. 1...
... the sunspot (item 9), and it is conceivable that it continues within the
sunspot.
The existence of small scale convective upflows and downflows does not contra-
dict the systematic upward motions ... differences between the monolith and cluster models are
that in the cluster model the weak-field gaps are permanent and are connected to
the field-free plasma surrounding t...
... destabilization. The cusp-shaped magnetic
field in the main phase of the second flare and its evolution in correlation with ribbon
separation provide evidence for the cause of the CME eruption. The propagation ... T
e
, the effec-
tive ion temperatures and non-thermal motions, the plume cross-section relative to
the size of the coronal hole, and the plasma bulk speed...
... reactions in
the proto -Sun. Such resonances may expedite the onset of nuclear ignition in the
proto -Sun and the redistribution and loss of the proto -Sun s angular momentum.
1 Introduction
To ... equal to the
respective light-travel times and with amplitudes consistent with PPN expressions
for the accelerations used in the standard ephemeris.
The standard theory of...