The Internal Rotation of the Sun

By M. Thompson, J. Christensen-Dalsgaard, Mark S. Miesch, J. Toomre. 2003

334 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

PERSISTENT MAGNETIC WREATHS IN A RAPIDLY ROTATING SUN (2010, background): “Helioseismology revealed the internal rotation profile of the Sun and the presence of this important shear layer (e.g., Thompson et al. 2003).”
The Case for a Distributed Solar Dynamo Shaped by Near-Surface Shear (2005, background): “This is the layer where recent helioseismological inversions have shown marked negative radial shear (Howe et al. 2000a, Corbard & Thompson 2002, Thompson et al. 2003).”
Local Helioseismology: Three-Dimensional Imaging of the Solar Interior (2010, methodology): “A major achievement of global helioseismology is the inference of the angular velocity in the solar interior (e.g. Schou et al. 1998, Thompson et al. 2003).”
Evolution of Close Binary Systems (2005, background): “Especially in the last few years, the study of the Sun (Schou et al. 1998; Thompson et al. 2003) has broadened our views on the later type near–main-sequence stars that are involved in all of LTCBs, NCBs, and DCBs.”
Solar Differential Rotation Influenced by Latitudinal Entropy Variations in the Tachocline (2006, background): “Under these conditions, we may derive the following expression (Kitchatinov & Rüdiger 1995; Durney 1999; Elliott et al. 2000; Brun & Toomre 2002; Thompson et al. 2003; Miesch 2005): @hSi @ ¼ 2CP g r 2 sin 60 = : ¼ 2rCP g 60 = : v ; ð1Þ with S the specific entropy, (r, ) the mean angular velocity,…”
Simulations of Core Convection in Rotating A-Type Stars: Differential Rotation and Overshooting (2003, background): “…of orderly magnetic fields and cyclic activity is thought to depend sensitively on highly turbulent convection yielding strong differential rotation, including a tachocline of shear at the interface between the bottom of the convection zone and the radiative interior (e.g., Thompson et al. 2003).”
ROTATIONAL AND RADIAL VELOCITIES FOR A SAMPLE OF 761 HIPPARCOS GIANTS AND THE ROLE OF BINARITY (2007, background): “The idea that the cores of solar-mass stars spin rapidly is controversial (cf. Demarque et al. 2001; Thompson et al. 2003).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “As stars are not solid bodies, they undergo radial differential rotation (Thompson et al. 2003; Balbus et al. 2012) and also rotate at different angular velocities at different latitudes (Ruediger et al. 1998; Bonanno et al. 2007; Küker et al. 2011).”
Structure and Evolution of Giant Cells in Global Models of Solar Convection (2007, background): “The angular velocity profile is similar to the solar internal rotation profile inferred from helioseismic measurements (Thompson et al. 2003), although the variation is smaller and there is somewhat more radial shear within the convection zone.”
Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, neutral): “…rotation profile from the external outer convection zone to the inner radiative core using inversion techniques (Deheuvels et al. 2012, 2014; Beck et al. 2014), as is also commonly done for the Sun (e.g. Thompson et al. 2003; García et al. 2008b; Mathur et al. 2008; Eff-Darwich & Korzennik 2013).”
Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope (2004, background): “This value is close to the contrast of 22% inferred from helioseismic inversion of the solar profile (Thompson et al. 2003).”
Improved angular momentum evolution model for solar-like stars (2013, neutral): “All the models presented here yield a complete recoupling between the radiative core and the convective envelope by the age of the Sun, as requested by helioseismology results (Thompson et al. 2003).”
From solar-like to antisolar differential rotation in cool stars (2013, background): “…of the Sun: (i) the outer convective region exhibits significant latitudinal gradients of shear; (ii ) a strong radial differential rotation is observed at the bottom of the convective zone forming the tachocline; (iii ) and the radiative core rotates nearly uniformly (e.g.Thompson et al. 2003).”
Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields (2006, result): “The overall fast equator and slow pole behavior is in keeping with theQ profiles deduced from helioseismology (e.g., Thompson et al. 2003), but this model possesses more radial shear within the bulk of the convection zone than in the Sun.”
MAGNETIC CYCLES IN A CONVECTIVE DYNAMO SIMULATION OF A YOUNG SOLAR-TYPE STAR (2011, background): “DYNAMOS IN RAPIDLY ROTATING SUNS In order to accentuate and investigate the self-organization processes associated with helicity and rotational shear, we have conducted a series of simulations of solar-type stars rotating more rapidly than the Sun.”
Asteroseismology of Solar-Type and Red-Giant Stars (2013, background): “A notable exception is of course the Sun, where helioseismic analysis of the frequency splittings of non-radial p modes has provided a detailed picture of rotation in the solar interior (e.g., see Thompson et al. 2003, Howe 2009).”
CONSTRAINING THE AGE–ACTIVITY RELATION FOR COOL STARS: THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 5 LOW-MASS STAR SPECTROSCOPIC SAMPLE (2007, background): “…MD 21218 7 Department of Physics & Astronomy, Vanderbilt University, Nashville, TN 37235 the tachocline) creates a rotational sheer; the convective zone undergoes differential rotation, while the radiative zone rotates like a solid body (Parker 1993; Ossendrijver 2003; Thompson et al. 2003).”