The Rotation of Sun and Stars

1. Front Matter

   Pages I-IX

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2. The Sun: A Slowly Rotating Star

   • J.-P. Zahn

   Pages 1-14

3. What Is Coming: Issues Raised from Observation of the Shape of the Sun

   • J.-P. Rozelot

   Pages 15-43

4. Effects of Rotation on Stellar p-Mode Frequencies

   • M.J. Goupil

   Pages 45-99

5. Approaching the Low-Frequency Spectrum of Rotating Stars

   • M. Rieutord

   Pages 101-121

6. The Rotation of the Solar Core

   • S. Turck-Chièze

   Pages 123-137

7. Physics of Rotation in Stellar Models

   • G. Meynet

   Pages 139-169

8. Long Baseline Interferometry of Rotating Stars Across the HR Diagram: Flattening, Gravity Darkening, Differential Rotation

   • A. Domiciano de Souza

   Pages 171-194

9. Is the Critical Rotation of Be Stars Really Critical for the Be Phenomenon?

   • Ph. Stee, A. Meilland

   Pages 195-205

10. On the Rotation of A-Type Stars

    • F. Royer

    Pages 207-230

11. The Solar Magnetic Field: Surface and Upper Layers, Network and Internetwork Field

    • V. Bommier

    Pages 231-259

12. Back Matter

    Pages 261-263

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The Sun and stars rotate in di?erent ways and at di?erent 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 lessevolved objects, however, can have averydi?erent 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 m- sured thanks to visible features across the solar disk, such as sunspots, or via spectroscopy. In addition, several studies cast light on di?erential 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 ?eld is strongly linked to the matter motions in the solar plasma. The solar magnetic ?eld can be measured only at the surface or in theupperlayers.Itistheproductoftheinternaldynamoorofthelocaldynamos if they exist – in any case magnetic ?eld and rotation cannot thus be separated.

• asteroseismology
• solar
• solar magnetic field
• solar physics
• stellar rotation

• Dept. Fizeau, Université de Nice Sophia-Antipolis CNRS-OCA, Grasse, France

  Jean-Pierre Rozelot

• Observatoire de Paris Section de Meudon GEPI, Meudon CX, France

  Coralie Neiner

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