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A rendering of the magnetic field lines of the magnetosphere of the Earth. In astronomy and planetary science, a magnetosphere is a region of space surrounding an astronomical object in which charged particles are affected by that object's magnetic field. [1] [2] It is created by a celestial body with an active interior dynamo.
Venus lacks an internal dynamo, and its weakly induced magnetosphere is caused by atmospheric interactions with the solar wind. Internal heat escapes through active volcanism, resulting in resurfacing instead of plate tectonics. Venus is one of two planets in the Solar System, the other being Mercury, that have no moons.
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Venus only has an induced magnetosphere formed by the Sun's magnetic field carried by the solar wind. [46] This process can be understood as the field lines wrapping around an obstacle—Venus in this case. The induced magnetosphere of Venus has a bow shock, magnetosheath, magnetopause and magnetotail with the current sheet. [46] [47]
Using data from two Japanese scientists, it is possible to make an artificial magnetosphere around Venus by building a system of refrigerated latitudinal superconducting rings. Using this, scientists could build an artificial magnetosphere around Venus to prevent the loss of hydrogen from its atmosphere.
The magnetosheath is the region of space between the magnetopause and the bow shock of a planet's magnetosphere.The regularly organized magnetic field generated by the planet becomes weak and irregular in the magnetosheath due to interaction with the incoming solar wind, and is incapable of fully deflecting the highly charged particles.
Bow shock occurs when the magnetosphere of an astrophysical object interacts with the nearby flowing ambient plasma such as the solar wind. For Earth and other magnetized planets, it is the boundary at which the speed of the stellar wind abruptly drops as a result of its approach to the magnetopause .
This opening is called the dayside reconnection and occurs on the side of the magnetosphere facing the solar wind source. In the second stage, the flux travels in the direction of the solar wind across the magnetosphere. In the third stage, at the magnetotail, reconnection closes the open flux, allowing for a new cycle to begin. This ...