Rotation rates of the coronal holes and their probable anchoring depths

Abstract

For the years 2001-2008, we use full-disk, SOHO/EIT 195 $\mathring{A}$ calibrated images to determine latitudinal and day to day variations of the rotation rates of coronal holes. We estimate the weighted average of heliographic coordinates such as latitude and longitude from the central meridian on the observed solar disk. For different latitude zones between $40^o$ north - $40^o$ south, we compute rotation rates, and find that, irrespective of their area, number of days observed on the solar disk and latitudes, coronal holes rotate rigidly. Combined for all the latitude zones, we also find that coronal holes rotate rigidly during their evolution history. In addition, for all latitude zones, coronal holes follow a rigid body rotation law during their first appearance. Interestingly, average first rotation rate ($\sim 438nHz$) of the coronal holes, computed from their first appearance on the solar disk, match with rotation rate of the solar interior only below the tachocline.

Accepted in Astrophysical Journal

References in corpus (4)

• Observation of High-speed Outflow on Plume-like Structures of the Quiet Sun and Coronal Holes with SDO/AIA
• SDO Observations of Magnetic Reconnection at Coronal Hole Boundaries
• Coronal hole boundaries at small scales: III. EIS and SUMER views
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Cited by in corpus (9)

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• Differential rotation of the solar corona: A new data-adaptive multiwavelength approach
• Accounting for Differential Rotation in Calculations of the Sun's Angular Momentum-loss Rate
• Study on the Temporal Evolution of the Radial Differential Rotation of Solar Corona Using Radio Emissions
• Long-term Evolution of the Solar Corona Using PROBA2 Data