Space Weather

Solar Images

�� 193 A 131 A 171 A 211 A 304 A ��

211 + 193 + 171

�� ?211 + 193 + 171? �� , �� 211 (��), 193 (��) � 171 ? (��). � �� , �� , � �� . �� (��, �� ) �� . �� ?211 + 193 + 171?.

193 A

Description

��, �� AIA � �� 193 ?. �� 193 ? �� Fe XII � XXIV, �� 1.6 � 20 ��. �� .

131 A

Description

��, �� AIA � �� 131 ?. �� 131 ? �� Fe VIII � XXI, �� ~ 0.4 � 10 ��. �� .

171 A

Description

��, �� AIA � �� 171 ?. �� 171 ? �� Fe IX, �� ~ 0.6 ��. �� .

211 A

Description

��, �� AIA � �� 211 ?. �� 211 ? �� Fe XIV, �� ~ 2 ��. �� .

304 A

Description

��, �� AIA � �� 304 ?. �� 304 ? �� II, �� ~ 0.05 ��, �� .

Corona

Description

LASCO (Large Angle and Spectrometric Coronagraph)- �� SOHO, �� , �� , �� , �� , �� . �� , � �� . �� , �� , �� . LASCO C2 �� 8.4 �� . LASCO C3- �� 40 �� .

Magnetogram

Description

HMI (Helioseismic and Magnetic Imager) - �� SDO, �� . �� HMI �� 6173 ? � �� 1 �� . HMI �� (�� ) �� 45 �� 10 �� ?4 ��.

Solar X-rays

Description

�� (�� ), �� GOES-15 � �� . �� ? �� .

Solar Wind on the ACE Orbit

Description

�� , �� , �� SWEPAM � EPAM � �� L1. �� .

Particles

Description

�� GOES13 � ��-�. �� ? �� . �� GOES13 � GOES15 �� .

Magnetospheric Conditions

Description

�� Dst �� .

Current Coronal Holes Location

SDO/AIA 193A; ��:
��

Description

��, �� (��) �� . �� -�� . �� , �� , �� , �� . ��

Coronal Holes Size

Solar wind velocity forecast

Solar Wind Dynamic Pressure on the Earth's Orbit and Magnetopause Standoff Distance

Description

The form and the location of the magnetospheric boundary are defined by pressure balance of the solar wind and geomagnetic field. Parameters of the interplanetary environment are subject to the considerable changes connected with active processes on the Sun. It leads to changes of the magnetospheric spatial dimensions, in particular, to stand-off distance fluctuations. Being under continuous influence of the solar wind, the magnetosphere of Earth reflects the variations of parameters of the interplanetary environment.

Earth's magnetosphere structure

Description

The magnetosphere of Earth is formed due to interaction of the magnetized solar wind with geomagnetic field. When the solar wind reaches Earth vicinities, it compresses dayside geomagnetic field. Thin current sheet (Earth?s magnetopause) separates the area which structure is defined by mainly geomagnetic field (Earth?s magnetosphere) from the area of solar wind flow. Under the influence of the solar wind there is a distortion of the geomagnetic dipole magnetic field and there is a specific magnetic configuration with the field lines in the night area, extended from Earth. In The magnetic field structure in the noon-midnight plane is presented in the Figure above, calculated by paraboloid model of the magnetosphere (A2000) for solar wind conditions at present time moment.

Dst Forecast

Description

�� Dst �� . �� . � �� , � �� Dst �� . ��