Voltage Across the Polar Cap / Convection Potential (Derived) This quantity also depends on IMF components measured by ACE/MAG. This affects the details of solar wind-magnetosphere interactions however, this is of tertiary importance compared to the IMF magnitude and polar angle. This quantity is the direction of the IMF perpendicular to the geomagnetic axis. Interplanetary Magnetic Field Azimuth (Derived) This quantity depends on IMF components measured by ACE/MAG. Under less severe conditions this radiation can still threaten polar orbiting spacecraft. In severe conditions this radiation can threaten high altitude aircraft in high latitude and polar regions. This process can also open the magnetosphere to solar energetic particle radiation. This process increases the transport of solar wind mass, momentum, and energy into the Earth's magnetosphere. When the IMF is southward, antiparallel fields near the magnetospheric subsolar point allow merging between the IMF and geomagnetic fields. This quantity is the angle between the IMF and the geomagnetic axis. Interplanetary Magnetic Field Polar Angle (Derived) This quantity is the strength of the interplanetary magnetic field (IMF) as measured by the ACE Magnetometer (MAG). Interplanetary Magnetic Field Magnitude (Measured) This quantity is the temperature of protons in the solar wind. The solar wind ram pressure depends on the solar wind speed and density. This is similar in concept to the force a surface wind exerts on a sail. This quantity is the solar wind ram pressure, the force per unit area required to stop the solar wind flow. This is the solar wind speed just as the bulk speed of air molecules is the wind speed we know here on the surface of the Earth.
This quantity is the average (bulk) speed of solar wind protons as measured by ACE/SWEPAM. This quantity is the number of solar wind protons per unit volume as measured by the ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM). This scheme is valid for all dials except the "Log" dial for which a different scheme applies. Yellow indicates that values in this range may contribute to disturbances, and Red indicates that values in this range are likely to drive disturbances. On the dial background color schemes, green indicates that values in this range are unlikely to disturb the near-Earth space environment. During times of outages in DSCOVR data or problems with the data, the data may then come from the NASA/ACE spacecraft. SWPC maintains the ability to instantaneously switch the spacecraft that provides the RTSW data. The NOAA/DSCOVR satellite became the operational RTSW spacecraft on Jat 1600UT (noon EDT, 10am MDT). Real-Time Solar Wind (RTSW) data refers to data from any spacecraft located upwind of Earth, typically orbiting the L1 Lagrange point, that is being tracked by the Real-Time Solar Wind Network of tracking stations. The real time space weather data uses the last good received set of measurements from the Real Time Solar Wind site at the Space Weather Prediction Center. This is designed to reduce shifts in status due to short-term spikes in the value of the potential. * The PCP status is changed to red only if the current 10-minute average exceeds 200 kV AND the previous 10-minute average exceeds 150 kV. This index is based on the most recent USAF/NOAA estimated planetary geomagnetic activity (Kp) 3-hour index:
0 kommentar(er)
