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Star at the centre of the Solar System
zone and the convective zone are separated by a transition layer, the tachocline. This is a region where the sharp regime change between the uniform rotation
Sun
Region of a star
The tachocline is the transition region of stars of more than 0.3 solar masses, between the radiative interior and the differentially rotating outer convective
Tachocline
Differential rotation of the Sun
J. & Thompson, M.J. (2007). The Solar Tachocline:Observational results and issues concerning the tachocline. Cambridge University Press. pp. 53–86.
Solar_rotation
Periodic change in the Sun's activity
and at the boundary of these two is the tachocline. However, brown dwarfs lack radiative cores and tachoclines. Their structure consists of a solar-like
Solar_cycle
Region of space dominated by the Sun
v t e The Sun Internal structure Core Radiative zone Tachocline Convection zone Atmosphere Photosphere Supergranulation Granule Faculae Sunspot Ellerman
Heliosphere
Study of the structure and dynamics of the Sun through its oscillation
differentially-rotating envelope. The boundary layer is now known as the tachocline and is thought to be a key component for the solar dynamo. Although it
Helioseismology
French astrophysicist and applied mathematician
earned her Ph.D. in 2001. Her dissertation, The dynamics of the solar tachocline, was jointly supervised by Douglas Gough and Nigel Weiss. After postdoctoral
Pascale_Garaud
Physical process that generates a star's magnetic field
to electric-magnetic energy. Currently, the geometry and width of the tachocline are hypothesized to play an important role in models of the solar dynamo
Solar_dynamo
Central region of the Sun
v t e The Sun Internal structure Core Radiative zone Tachocline Convection zone Atmosphere Photosphere Supergranulation Granule Faculae Sunspot Ellerman
Solar_core
Region of a star
a radiative zone, separated from the overlying convection zone by the tachocline. The radius of the radiative zone increases monotonically with mass, with
Radiative_zone
Region of a star
region between the convection zone and the radiation zone is called the tachocline. In red giant stars, and particularly during the asymptotic giant branch
Convection_zone
Phenomenon of convection
The layer between the Sun's convective and radiative zone is called the tachocline. Overshooting can have more pronounced effects on the evolution of stars
Convective_overshoot
Mechanism by which a celestial body generates a magnetic field
iron in the outer core, and in the solar dynamo is ionized gas at the tachocline. Dynamo theory of astrophysical bodies uses magnetohydrodynamic equations
Dynamo_theory
Structure extending off of the Sun's surface
v t e The Sun Internal structure Core Radiative zone Tachocline Convection zone Atmosphere Photosphere Supergranulation Granule Faculae Sunspot Ellerman
Solar_prominence
Variations in rotation rates
stellar surface. Solar differential rotation causes shear at the so-called tachocline. This is a region where rotation changes from differential in the convection
Differential_rotation
Indian astronomer
calculate interaction of tachocline latitudinal differential rotation with Rossby waves. 2015 - 2018: Discovered Tachocline Nonlinear Oscillations, which
Mausumi_Dikpati
Fluid instability that causes turbulence in accretion disks
Conducting Fluids. Cambridge: Cambridge Univ Ogilvie G., 2007, in The Solar Tachocline. ed. D. Hughes, R. Rosner, N. Weiss, p. 299. Cambridge: Cambridge Univ
Magnetorotational_instability
Force on magnetic flux tubes
January 2018). "Magnetic Buoyancy and Rotational Instabilities in the Tachocline". The Astrophysical Journal. 853 (1): 65. Bibcode:2018ApJ...853...65G
Magnetic_buoyancy
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