SOLAR ROTATION RATE DURING THE CYCLE 24 MINIMUM IN ACTIVITY

Journal Article · Wed Sep 01 04:00:00 EDT 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/720/1/494· OSTI ID:21460128

Antia, H M ^[1]; Basu, Sarbani ^[2]

---

1. Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005 (India)
2. Department of Astronomy, Yale University, P.O. Box 208101, New Haven CT 06520-8101 (United States)

The minimum of solar cycle 24 is significantly different from most other minima in terms of its duration as well as its abnormally low levels of activity. Using available helioseismic data that cover epochs from the minimum of cycle 23 to now, we study the differences in the nature of the solar rotation between the minima of cycles 23 and 24. We find that there are significant differences between the rotation rates during the two minima. There are differences in the zonal-flow pattern too. We find that the band of fast rotating region close to the equator bifurcated around 2005 and recombined by 2008. This behavior is different from that during the cycle 23 minimum. By autocorrelating the zonal-flow pattern with a time shift, we find that in terms of solar dynamics, solar cycle 23 lasted for a period of 11.7 years, consistent with the result of Howe et al. (2009). The autocorrelation coefficient also confirms that the zonal-flow pattern penetrates through the convection zone.

• OSTI ID: 21460128
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 720; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CONVECTION
ENERGY TRANSFER
EQUATOR
HEAT TRANSFER
MAIN SEQUENCE STARS
MASS TRANSFER
MOTION
ROTATION
SOLAR CYCLE
STARS
SUN