What coronal parameters determine solar wind speed M

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What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H.

What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory, Nagoya University K. Hakamada Department of Natural Science and Mathematics, Chubu University

In order to model the solar wind acceleration it is important to find a

In order to model the solar wind acceleration it is important to find a universal relation between the global properties of the solar wind and corona holes. However most coronal holes are at high latitudes where spacecraft cannot access, with the exception of the Ulysses. In this study we identify the relation between the wind velocity and the coronal magnetic condition using the IPS tomographic measurements, which can derive an unbiased solar wind velocity map over all latitudinal ranges, .

Freq.  327 MHz Aperture 2000 m 2

Freq.  327 MHz Aperture 2000 m 2

10 2 k 126 km m Four-station system for IPS 98 k 109 km

10 2 k 126 km m Four-station system for IPS 98 k 109 km m 13 m k 1

Interplanetary scintillation measures an integration of the solar wind speed V and density turbulent

Interplanetary scintillation measures an integration of the solar wind speed V and density turbulent level △Ne distributed along a line of sight. Radio source ☆ Earth

The IPS los integrations provide us with perspective views of 3 D SW structures

The IPS los integrations provide us with perspective views of 3 D SW structures at various different view angles using both the solar rotation and solar wind outward motion. Computer Assisted Tomography analysis This technique can retrieve not only unbiased solar wind parameters but also provides high spatial resolution.

1996 CT Analysis

1996 CT Analysis

 • Nolte et al. (1976)  the velocity depends on the coronal hole scale

• Nolte et al. (1976)  the velocity depends on the coronal hole scale size. • Wang and Sheeley (1990)  the flux expansion rate is inversely proportional to the solar wind speed. • Fisk et al. (1999)  reconnection of emerging magnetic fields in supergranules supplies Poynting flux to   accelerate the solar wind.

CH size vs. V

CH size vs. V

potential field neutral line ? ? after Kojima et al. , 1999

potential field neutral line ? ? after Kojima et al. , 1999

after Kojima et al. , 1999

after Kojima et al. , 1999

dependence on polar coronal hole scale size Oct. 1999 1991 2000

dependence on polar coronal hole scale size Oct. 1999 1991 2000

CH size vs. V Polar CH Equatorial CH polar CH

CH size vs. V Polar CH Equatorial CH polar CH

CH size B weak medium expansion B 10 G small expansion B weak small

CH size B weak medium expansion B 10 G small expansion B weak small expansion B 20 G large expansion

We investigate the relation between the solar wind velocity and the coronal magnetic condition

We investigate the relation between the solar wind velocity and the coronal magnetic condition for various kinds of coronal holes, which have different properties of magnetic field intensity B and flux expansion rate f. We make correlation analysis between the velocity V and a) the inverse of an expansion rate 1/f, b) photospheric magnetic field intensity B, and c) the ratio between these two parameters B/f.

V-map on the source surface from IPS tomography Potential magnetic field lines Coronal holes

V-map on the source surface from IPS tomography Potential magnetic field lines Coronal holes on the photosphere He. I, open B region Data from the National Solar Observatory (NSO) at Kitt Peak

Analysis 1 Data period: 1995 -1996

Analysis 1 Data period: 1995 -1996

Although the polar coronal hole extended to lower latitudes than 60 degrees, we examine

Although the polar coronal hole extended to lower latitudes than 60 degrees, we examine the coronal hole area at latitudes higher than 60 degrees because the boundary region has a complex structure. If there is a extension from a polar coronal hole toward the equator beyond a latitude of 40 degrees, it is treated as an independent mid-latitude coronal hole.

Flux expansion rate weak B strong B after Hirano et al. (2004)

Flux expansion rate weak B strong B after Hirano et al. (2004)

Magnetic field energy large expansion small expansion after Hirano et al. (2004)

Magnetic field energy large expansion small expansion after Hirano et al. (2004)

Flux expansion + B energy after Hirano et al. (2004)

Flux expansion + B energy after Hirano et al. (2004)

Analysis 3 Data period: 1990 -2001 1. CR 1830 : Jun. 11. 4556, 1990.

Analysis 3 Data period: 1990 -2001 1. CR 1830 : Jun. 11. 4556, 1990. 2. CR 1844 : Jun. 28. 2611, 1991. 3. CR 1855 : Apr. 23. 4361, 1992 4. CR 1870 : Jun. 6. 4778, 1993. 5. CR 1887 : Sep. 12. 9590, 1994. 6. CR 1898 : Jul. 10. 0910, 1995. 7. CR 1901 : Sep. 29. 8104, 1995. 8. CR 1909 : May 5. 2840, 1996. 9. CR 1925 : Jul. 15. 5059, 1997. 10. CR 1939 : Aug. 1. 3214, 1998. 11. CR 1950 : May 28. 5213, 1999. 12. CR 1964 : Jun. 13. 3296, 2000. 13. CR 1976 : May 6. 7222, 2001.

Mesh size:

Mesh size:

Solar minimum phase

Solar minimum phase

V=236. 7×B/f +473. 4

V=236. 7×B/f +473. 4

Solar maximum phase

Solar maximum phase

Bp≦15 G (High Latitude) V=163. 6×B/f +419. 9 Bp>15 G (Low Latitude) V=143. 1×B/f

Bp≦15 G (High Latitude) V=163. 6×B/f +419. 9 Bp>15 G (Low Latitude) V=143. 1×B/f +376. 5

Physical meaning of the parameter B/f • Energy supply ー B • Efficiency ー

Physical meaning of the parameter B/f • Energy supply ー B • Efficiency ー Flux expansion f CH size What is the role of theslower coronal hole size fast slower in determining the solar wind speed ? slow

Flux expansion + B energy after Hirano (2004)

Flux expansion + B energy after Hirano (2004)