Table 6: A comparison of differential rotation parameters A, B, and C from Eq. (15) for coronal bright points (Tables 2-5) with other results. R - remark.

Tracer/method		 Time $A \pm M_A$ $-B \pm M_B$ $-C \pm M_C$ Source R

Coronal bright points		 1967 14.65 $\pm$ 0.2     Dupree & Henze (1972) 1
Coronal bright points 1973 14.6 $\pm$ 0.3     Golub et al. (1974) 2
Coronal bright points 1998-1999 14.530 $\pm$ 0.032 2.68 $\pm$ 0.13   present work, Table 4 3
Coronal bright points 1998-1999 14.677 $\pm$ 0.033 3.10 $\pm$ 0.14   present work, Table 5 4

Sunspots		 1921-1982 14.522 $\pm$ 0.004 2.84 $\pm$ 0.04   Howard et al. (1984) 5
Sunspots 1921-1982 14.393 $\pm$ 0.010 2.95 $\pm$ 0.09   Howard et al. (1984) 6
Sunspots 1874-1976 14.551 $\pm$ 0.006 2.87 $\pm$ 0.06   Balthasar et al. (1986) 7
Sunspots 1853-1996 14.531 $\pm$ 0.003 2.75 $\pm$ 0.05   Pulkkinen & Tuominen (1998) 8
Sunspots 1880-1976 14.37 $\pm$ 0.01 2.59 $\pm$ 0.16   Brajsa et al. (2002b) 9
H$\alpha $ filaments 1919-1929 14.48 2.16   d'Azambuja & d'Azambuja (1948) 10
H$\alpha $ filaments 1972-1973 14.45 1.43   Adams & Tang (1977) 11
H$\alpha $ filaments 1972-1987 14.45 $\pm$ 0.15 0.11 $\pm$ 0.90 3.69 $\pm$ 0.90 Brajsa et al. (1991) 12

Coronal bright points		 1998-1999 14.495 $\pm$ 0.026 1.89 $\pm$ 0.06 1.89 $\pm$ 0.06 present work, Table 2 13
Coronal bright points 1998-1999 14.454 $\pm$ 0.027 2.22 $\pm$ 0.07 2.22 $\pm$ 0.07 present work, Table 3 14

LTRs		 1979-1991 14.25 $\pm$ 0.06 1.25 $\pm$ 0.19 1.25 $\pm$ 0.19 Brajsa et al. (2000a) 15
LTRs 1979-1991 14.16 $\pm$ 0.06 1.41 $\pm$ 0.19 1.41 $\pm$ 0.19 Brajsa et al. (2000a) 16

Magnetic		 1967-1980 14.307 $\pm$ 0.005 1.98 $\pm$ 0.06 2.15 $\pm$ 0.11 Snodgrass (1983) 17
Magnetic 1975-1991 14.42 $\pm$ 0.02 2.00 $\pm$ 0.13 2.09 $\pm$ 0.15 Komm et al. (1993) 18
Magnetic 1997 14.00 $\pm$ 0.54 2.24 $\pm$ 1.22 1.78 $\pm$ 0.79 Deng et al. (1999) 19

Doppler		 1966-1968 13.76 1.74 2.19 Howard & Harvey (1970) 20
Doppler 1967-1984 14.05 1.49 2.61 Snodgrass (1984) 21
Doppler 1981-1982 13.99 $\pm$ 0.06     Küveler & Wöhl (1983) 22
Doppler 1983-1986 13.92 $\pm$ 0.12     Lustig & Wöhl (1989) 23
1. OSO-4, Mg X spectroheliograms;     2. Skylab, soft X-rays;     3. SOHO-EIT, automatic method, no height correction;
4. SOHO-EIT, automatic method, with height correction;     5. Mt. Wilson, sunspots;     6. Mt. Wilson, sunspot groups;
7. Greenwich, sunspot groups;     8. Extended Greenwich, sunspots and sunspot groups;
9. Greenwich, only stable recurrent sunspot groups;      10. Meudon;     11. Big Bear, with height correction;
12. Big Bear and Kanzelhöhe, with height correction;      13. SOHO-EIT, interactive method, no height correction;
14. SOHO-EIT, interactive method, with height correction;
15. Metsähovi, microwave low brightness temperature regions, no height correction;
16. Metsähovi, microwave low brightness temperature regions, with height correction;
17. Mt. Wilson, photospheric magnetic fields;     18. Kitt Peak, photospheric magnetic fields;
19. Huairou/Beijing, photospheric high-latitude magnetic fields;     20. Mt. Wilson, photosphere, spectroscopic;
21. Mt. Wilson, photosphere, spectroscopic;     22. Locarno, photosphere, spectroscopic;
23. Capri, photosphere, spectroscopic.


Source LaTeX | All tables | In the text