The Sun and stars rotate in different ways and at different velocity rates. The knowledge of how they rotate is important in understanding the formation and evolution of stars and their structure. The closest star to our Earth, the Sun, is a good laboratory to study in detail the rotation of a G star and allows to test new ideas and develop new techniques to study stellar rotation. More or less massive, more or less evolved objects, however, can have a very different rotation rate, structure and history. In recent years our understanding of the rotation of the Sun has greatly improved. The Sun has a well-known large-scale rotation, which can be measured thanks to visible features across the solar disk, such as sunspots, or via spectroscopy. In addition, several studies cast light on differential rotation in the convective zone and on meridional circulation in the radiative zone of the Sun. Even the rotation of the core of the Sun can now be studied thanks to various methods, such as dynamics of the gravitational moments and of course, helioseismology, through g-modes analysis. Moreover, the magnetic field is strongly linked to the matter motions in the solar plasma. The solar magnetic field can be measured only at the surface or in the upper layers. It is the product of the internal dynamo or of the local dynamos if they exist – in any case magnetic field and rotation cannot thus be separated.
- The Sun: A Slowly Rotating Star
- What Is Coming: Issues Raised from Observation of the Shape of the Sun
- Effects of Rotation on Stellar p-Mode Frequencies
- Approaching the Low-Frequency Spectrum of Rotating Stars
- The Rotation of the Solar Core
- Physics of Rotation in Stellar Models
- Long Baseline Interferometry of Rotating Stars Across the HR Diagram: Flattening, Gravity Darkening, Differential Rotation
- Is the Critical Rotation of Be Stars Really Critical for the Be Phenomenon?
- On the Rotation of A-Type Stars
- The Solar Magnetic Field: Surface and Upper Layers, Network and Internetwork Field
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