Viendo archivo del lunes, 3 marzo 2003
Informe actividad solar
Any mentioned solar flare in this report has a scaling factor applied by the Space Weather Prediction Center (SWPC). Because of the SWPC scaling factor, solar flares are reported as 42% smaller than for the science quality data. The scaling factor has been removed from our archived solar flare data to reflect the true physical units.
Informe de actividad Solar-Geofísica 2003 Mar 03 2200 UTCPreparado por NOAA © SWPC y procesado por SpaceWeatherLive.com
Informe conjunto USAF/NOAA de actividad Solar y Geofísica
SDF Número 062 Publicado el 2200Z a las 03 Mar 2003IA. Análisis de regiones solares activas y de actividad desde 02-2100Z hasta 03-2100Z Solar activity was at very low levels today. The
largest flare of the period was a B9.5 flare that occurred at
03/1830Z from Region 296 (N11E35). A slight growth in penumbral
coverage and an increase in magnetic complexity (beta-gamma) were
observed in this region today. The remainder of the active regions
were mostly quiescent throughout the period. Regions 298 (S08E18),
299 (N12E47), and 300 (N16E66) were newly assigned during the
interval.
IB. Pronóstico de la actividad solar
Solar activity is expected to be a low
levels. Region 296 has the potential of producing an isolated low
level M-class flare.
IIA. Resumen de la actividad geofísica 02-2100Z a 03-2100Z
The geomagnetic field was at unsettled to active levels. An increase
in the solar radial wind speed (approaching 500 km/sec at the time
of this writing) along with southward oscillations in the Bz
component of the interplanetary magnetic field allowed for the
active periods seen late in the period. The onset of a recurrent
coronal hole in the northwestern quadrant of the solar disk is
believed responsible for the increase in activity. The greater than
2 MeV electron fluxes at geosynchronous orbit reached high levels
today.
IIB. Pronóstico de la actividad geofísica
The geomagnetic field is
expected to be at unsettled to active levels. Isolated minor storm
conditions are possible due to a recurrent high speed stream coronal
hole through the first two days of the period. Day three should see
a return to predominantly unsettled levels.
III. Probabilidades del evento 04 Mar a 06 Mar
| Clase M | 30% | 30% | 30% |
| Clase X | 05% | 05% | 05% |
| Protón | 01% | 01% | 01% |
| PCAF | green | ||
IV. Penticton 10.7cm flujo
Observado 03 Mar 149 Previsto 04 Mar-06 Mar 150/155/155 Media de 90 Días 03 Mar 142
V. Índices Geomagnéticos A
Observado Afr/Ap 02 Mar 009/014 Estimado Afr/Ap 03 Mar 010/015 Previsto Afr/Ap 04 Mar-06 Mar 015/020-015/015-012/012
VI. Probabilidades de Actividad Geomagnética 04 Mar a 06 Mar
| A. Latitudes Medias | |||
|---|---|---|---|
| Activo | 35% | 35% | 25% |
| Tormenta Menor | 15% | 15% | 05% |
| Tormenta Mayor-Severa | 05% | 05% | 01% |
| B. Latitudes Altas | |||
|---|---|---|---|
| Activo | 45% | 40% | 30% |
| Tormenta Menor | 20% | 15% | 10% |
| Tormenta Mayor-Severa | 10% | 05% | 01% |
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