SPACE WEATHER SCIENCE
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THIS SITE IS UNDER CONSTRUCTION. ALL THE DATA USED HERE NOW ARE ONLY DUMMY AND FOR DEVELOPMENT AND REPRESENTATION PURPOSE ONLY. PLEASE DO NOT USE THIS DATA UNTIL THE SITE IS DECLARED ACTIVE.
CURRENT SPACE WEATHER
This page provides the information of the current and the most recent parameters related to the space weather.
The values are measured by satellites like SDO, ACE, DSCOVR etc. or by the ground based instruments like the magnetometers or the ionosondes.
The relevant tabs gives an organized demarcation of different parameters pertaining to the Sun, the solar wind, the magnetosphere or the ionosphere.
Data from the last one week or last one solar rotation are provided for different parameters.
All the data in one place and with well organized interface provides a very efficient and comprehensive representation of the current space weather.
SUN
SOLAR WIND
MAGNETOSPHERE
IONOSPHERE
The Sun is imaged with different filters, allowing lights of different frequencies, to pass and form the image. Different frequencies carry information from different dephts of the solar corona.
The current image of the Sun at 304 A.
The current image of the Sun at 131 A.
The current image of the Sun at 193 A.
The source of all Space Weather is the Sun and its activities. Therefore the following solar parameters, which act as the drivers for the space weather and immense important for understanding the existing weather and the extent of its potential effects
IMPORTANT PARAMETERS
Bertels Rotation Number: 2613
Start Date:
Current Date:
Solar Activity Cycle No. : 25
Start Year : 2019
End Year : 2030
Stage : 51%
Sunspot Number: 114
Active Region: AC1039
F10.7 : 094
SUNSPOT NUMBER
Sunspots are the relatively cooler dark areas on the Sun's surface
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Sunspot numbers reflects the intensity of the solar magnetic activity
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F10.7
This is the total solar flux at the 10.7 cm wavelength
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10.7cm represents the weighted mean of the all radiations by the Sun
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The following parameters represent the particle or wave emissions. They can directly affect the earth's atmosphere and ionosphere from within a few minutes to few hours interval from the time of their occurrences.r daily and weekly values are availavbe in the plots.
SOLAR PARTICALE FLUX
The amount of energetic particles and radiation emissions from the Sun
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- PFU: Proton Flux Unit;
- 1 PFU =
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SOLAR X-RAY FLUX
The amount of energetic particles and radiation emissions from the Sun
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X-Ray Flux Unit is W/m^2
X-Ray flux > 10^-4 : Class X flare
X-Ray Flux Unit is W/m^2
X-Ray flux > 10^-4 : Class X flare
CORONAGRAPH AND DOPPLER
Coronagraph provides the image of the Sun's corona (the outer atmosphere of Sun)
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The solar winds are the perennial flow of charged particles (plasma) emitted from the Sun. These hot plasma fills up the interplanetary space and flow downstream towards the edge of the heliosphere. The wind parameters are measured at a location near to the earth, mostly at the Lagrangian point, L1.
SOLAR WIND VELOCITY
The solar wind flows through interplanetary space with velocities of few hundreds of kmps
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SOLAR WIND DENSITY
Solar wind is mostly constituted by Hydrogen ions with varying density
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SOLAR WIND TEMPERATURE
Ion temperature of the solar wind particles represents their average kinetic energy
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The interplanetary magnetic field fills up the interplanetary space. These magnetic fields have their sources at the Sun and is carried into the interplanetary space by the hot plasma of the solar wind which remians frozen with it. These fields are measured with respect to a geocentric reference frame GSE.
IMF Bz
It is the strength and orientation of Bz that determines the disruption in magnetosphere
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IMF Bx
It is the X component of the IMF when measured in GSE reference.
IMF By
It is the Y component of the IMF when measured in GSE reference.
The derived parameters tells a lot about the behaviour of the Solar Wind. The Parker's angle and clock angle provides the relative orientation of the IMF with respect to the earth and its orbit. The ram pressure reveals the strength of the wind to disrupt the benign magnetospheric nature while the distribution of the fast and slow solar wind let us understand the dominant region of the sun that emits the wind.
PARKER'S AND CLOCK ANGLES
The Parkers angle is the angle made by the solar with the earth's orbit.
RAM PRESSURE
Ram pressure is the thrusht provided by the solar wind on the magnetospheric surface.
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FAST/SLOW WIND DISTRIBUTION
Slow and fast winds are dominant during high and low activity periods respectively
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The magnetosphere acts as a shield that rpotects Earth from the disruptions of the solar wind. However, the magnetospheric features change with the variation of the solar wind emitted from the Sun. Here we present the most salient features of the magnetosphere that are influenced by the impinging solar wind and the associated IMF.
MAGNETOSPHERIC RADIUS
The radial periphery of the magnetosphere measured in Re.
POLAR CAP POTENTIAL
The electric potential developed across the polar cap due to magnetospheric convection
CLOCK ANGLE
Although clock angle is an IMF parameter, it determines many magnetospheric conditions
There are different states of the geomagnetic fields which are determined by various direct and proxy indices. These indices are determined from measurements done on ground or obtained through various models.
Ae
Although Ae is an ionospheric current, it reveals various magnetospheric conditions
PLASMA SHEET STATE
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GEOMAGNETIC FIELDS
These are the magnetometers data that represents the North geomagnetic fields
The near-surface geomagnetic fields undergo severe perturbation when space weather event affects the magnetosphere and its elements. This inturn alters the behaviour of the ionosphere and results in geomagnetic storm and substorms.
Dst
Dst is the depreciation of northward geomagnetic field from the nominal value
Ap
Ap index is the global average of deviations of the midlatitude magnetic field in linear scale
Kp
Kp index is the global average of deviations of the midlatitude magnetic field in log scale
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Important: Plots are derived at spaceweathersci.com from data available at SWPC. These are for educational purpose only and the values may contain errors.
"Courtesy of NASA/SDO and the AIA, EVE, and HMI science teams."