1/25/2024 0 Comments Does mercury into sun corona![]() Coronal loops have a wide variety of temperatures along their lengths. Thus, sunspots tend to occur under coronal loops, and tend to come in pairs of opposite magnetic polarity a point where the magnetic field loop emerges from the photosphere is a North magnetic pole, and the other where the loop enters the surface again is a South magnetic pole.Ĭoronal loops form in a wide range of sizes, from 10 km to 10,000 km. These appear as dark spots on the Sun's surface, known as sunspots. Within each footpoint, the strong magnetic flux tends to inhibit the convection currents which carry hot plasma from the Sun's interior to the surface, so the footpoints are often (but not always) cooler than the surrounding photosphere. The strong interaction of the magnetic field with the dense plasma on and below the Sun's surface tends to tie the magnetic field lines to the motion of the Sun's plasma thus, the two footpoints (the location where the loop enters the photosphere) are anchored to and rotate with the Sun's surface. This is known as the frozen-in condition. Thus, the plasma within a coronal loop cannot escape sideways out of the loop and can only flow along its length. As a result, they can only move freely parallel to the magnetic field lines, tending to spiral around these lines. Within a coronal loop, the paths of the moving electrically charged particles which make up its plasma- electrons and ions-are sharply bent by the Lorentz force when moving transverse to the loop's magnetic field. A coronal loop occurs when a curved arc of the magnetic field projects through the visible surface of the Sun, the photosphere, protruding into the solar atmosphere. These magnetic fields are in the form of closed loops of magnetic flux, which are twisted and tangled by solar differential rotation (the different rotation rates of the plasma at different latitudes of the solar sphere). The number of coronal loops varies with the 11 year solar cycle.ĭue to a natural process called the solar dynamo driven by heat produced in the Sun's core, convective motion of the electrically conductive plasma which makes up the Sun creates electric currents, which in turn create powerful magnetic fields in the Sun's interior. Ĭoronal loops are often associated with the strong magnetic fields located within active regions and sunspots. They typically form and dissipate over periods of seconds to days and may span anywhere from 1 to 1,000 megametres (621 to 621,000 mi) in length. Coronal loops begin and end at two footpoints on the photosphere and project into the transition region and lower corona. In solar physics, a coronal loop is a well-defined arch-like structure in the Sun's atmosphere made up of relatively dense plasma confined and isolated from the surrounding medium by magnetic flux tubes. Dynamics of coronal loops observed by SDO
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