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In a radiation zone, energy is transported by radiation and conduction. Stellar convection consists of mass movement of plasma within the star which usually forms a circular convection current with the heated plasma ascending and the cooled plasma descending. The Schwarzschild criterion expresses the conditions under which a region of a star is ...
Stellar structure models describe the internal structure of a star in detail and make predictions about the luminosity, the color and the future evolution of the star. Different classes and ages of stars have different internal structures, reflecting their elemental makeup and energy transport mechanisms.
From 0.3 to 1.2 solar masses, the region around the stellar core is a radiative zone, separated from the overlying convection zone by the tachocline. The radius of the radiative zone increases monotonically with mass, with stars around 1.2 solar masses being almost entirely radiative. Above 1.2 solar masses, the core region becomes a convection ...
Convection zone; Radiative zone ... The geometry and width of the tachocline are thought to play an important role in models of the stellar dynamos by winding up the ...
Above this spherical radiation zone lies a small convection zone just below the outer atmosphere. At lower stellar mass , the outer convection shell takes up an increasing proportion of the envelope, and for stars with a mass of around 0.35 M ☉ (35% of the mass of the Sun) or less (including failed stars ) the entire star is convective ...
The stellar atmosphere is the outer region of the volume of a star, lying above the stellar core, radiation zone and convection zone. Overview The stellar atmosphere ...
The O-B stars, which do not have surface convection zones, have a strong X-ray emission. However these stars do not have coronae, but the outer stellar envelopes emit this radiation during shocks due to thermal instabilities in rapidly moving gas blobs. Also A-stars do not have convection zones but they do not emit at the UV and X-ray wavelengths.
Paul Ledoux (8 August 1914 – 6 October 1988 [2]) was a Belgian astrophysicist best known for his work on stellar stability and variability. With Theodore Walraven, he co-authored a seminal work on stellar oscillations. [3]