Changes in Solar Dynamics from 1995 to 2002

By S. Basu, H. M. Antia. 2002

157 citations recorded by the source corpus.

Data obtained by the GONG and MDI instruments over the last 7 years are used to study how solar dynamics—both rotation and other large scale flows—has changed with time. In addition to the well-known phenomenon of bands of faster and slower rotation moving toward the equator and pole, we find that the zonal flow pattern rises upward with time. Like the zonal flows, the meridional flows also show distinct solar activity-related changes. In particular, the antisymmetric component of the meridional flow shows a decrease in speed with activity. We do not see any significant temporal variations in the dynamics of the tachocline region where the solar dynamo is believed to be operating.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e1516ff80015ee0a13e60dc2ecdb32a2d3f86207

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In Astronomy and Astrophysics

1. Paul Charbonneau
2. Mark S. Miesch
3. J. Toomre
4. A. Brun
5. S. Solanki
6. D. Hathaway
7. N. Krivova
8. Matthias Rempel

Citations in the corpus

• Torsional Oscillation, Meridional Flows, and Vorticity Inferred in the Upper Convection Zone of the Sun by Time-Distance Helioseismology (2004, background): “…with f-mode analysis near the photosphere (Gizon 2003), and are in general agreement with findings from the ring-diagram analyses (Haber et al. 2002; Basu & Antia 2003) that the gradient of the near-equator meridional flows steepen with the development of the solar cycle toward the solar maximum.”
• Dynamo Models of the Solar Cycle (2005, background): “85 (Schou and Bogart, 1998; Braun and Fan, 1998), without significant departure from the poleward direction except locally and very close to the surface, in the vicinity of active region belts (Haber et al., 2002; Basu and Antia, 2003; Zhao and Kosovichev, 2004).”
• Solar Interior Rotation and its Variation (2009, background): “Basu and Antia (2003) found similar results in MDI and GONG data up to 2002, as seen in Figure 23.”
• Simulating and Predicting Solar Cycles Using a Flux-Transport Dynamo (2006, unknown): “For a solar-like surface flow speed as observed (Komm et al. 1993; Hathaway et al. 1996; Basu & Antia 2003) and for a return flow theoretically constructed from mass conservation (see Fig.”
• Solar Differential Rotation Influenced by Latitudinal Entropy Variations in the Tachocline (2006, background): “The meridional circulation near the surface of the Sun is generally poleward at latitudes<60 with an amplitude of 15– 20m s 1, but it fluctuates substantially over the course of months and years (Hathaway 1996; Snodgrass & Dailey 1996; Haber et al. 2002; Basu & Antia 2003; Zhao & Kosovichev 2004).”
• ON THE WEAKENING OF THE POLAR MAGNETIC FIELDS DURING SOLAR CYCLE 23 (2009, background): “…flow speeds have amplitudes in the range 10–20 m s−1 and are generally directed poleward (Komm et al. 1993; Hathaway 1996; Giles et al. 1997; Haber et al. 2002; Basu & Antia 2003; Gizon 2004; Zhao & Kosovichev 2004; González Hernández et al. 2006; Švanda et al. 2007; Meunier & Zhao 2009).”
• Sunspot Group Tilt Angles and the Strength of the Solar Cycle (2010, background): “…consist of a time-dependent component of the solar differential rotation (Howard & Labonte, 1980) called zonal flows, and a timedependent component in the meridional plane which has been observed by tracking magnetic features (Komm et al., 1993) and with helioseismology (Basu & Antia, 2003).”
• Predicting the strength of solar cycle 24 using a flux‐transport dynamo‐based tool (2006, methodology): “[14] The dashed curve in Figure 2b is obtained by repeating the above simulation with a steady meridional flow from cycle 12 through 22 and then continuing the simulation through the present to 2020 using observations [ Basu and Antia, 2003, Figures 10 and 11] that the meridional flow slowed down b”
• Diagnostics of Polar Field Reversal in Solar Cycle 23 Using a Flux Transport Dynamo Model (2004, background): “The flow pattern showed a systematic decrease in its speed in both hemispheres (Haber et al. 2002; Basu & Antia 2003) during the period 1996–2002.”