The H-alpha radial velocities of an arch filament system in solar emerging flux region Shino Kawahara Rakutou High School KYOTO

On emerging flux region : EFR In H-alpha images, we can observe black bands between sun spots pair in early stage. In H-alpha images, we can observe black bands between sun spots pair in early stage. It is believed that these black bands are emerging flux tubes. It is believed that these black bands are emerging flux tubes. These tubes were These tubes were made in convection zone in solar interior, made in convection zone in solar interior, and rose to the surface. These areas are called These areas are called as emerging flux region (EFR), and black bands as arch filament system (AFS).

It is believed that there are flux tubes which move upward about 10km/s at the center, and the downward moving of about 30km/s to 50km/s at both ends of the arch. It is believed that there are flux tubes which move upward about 10km/s at the center, and the downward moving of about 30km/s to 50km/s at both ends of the arch. Then we examined distributions of velocity in AFS by means of Doppler shift measurements of H-alpha lines. Then we examined distributions of velocity in AFS by means of Doppler shift measurements of H-alpha lines.

Observation and Analysis Using the 70cm coelostat telescope and the high dispersion spectrogram, we observed the solar surface phenomena at Kwasan observatory on 10th and 11th of Aug. in Using the 70cm coelostat telescope and the high dispersion spectrogram, we observed the solar surface phenomena at Kwasan observatory on 10th and 11th of Aug. in We observed sunspots group NOAA0904. We observed sunspots group NOAA0904. We performed Doppler shift measurements of H-alpha lines We performed Doppler shift measurements of H-alpha lines of each AFSs. We derived the radial velocities of each AFSs from following formula We derived the radial velocities of each AFSs from following formula Δλ/λ V/c Δλ/λ V/c (Δλ: Doppler shift of H-alpha line center, (Δλ: Doppler shift of H-alpha line center, λ: H-alpha wave length, V: radial velocity, c: velocity of light)

Observing time of both figures is 2:25 on the 10 th of Aug. in 2006(UT) Fig.1 The spectral image of sun spotsNOAA0904 (left), H-alpha image of the slit mirror of the spectrogram right H-alpha image of the slit mirror of the spectrogram right Blue Red

Fig.2 The spectral trace was made from Fig1. Relative intensity H-α center Shortward (blue)Longward (red)Wavelength (in pixel units)

The three radial velocity observations obtained between 2:25 to 2:40 10th of Aug. show; The three radial velocity observations obtained between 2:25 to 2:40 10th of Aug. show; The eastward No observation. The eastward No observation. The center -14.5km/s -15.4km/s The center -14.5km/s -15.4km/s The westward +0.7km/s The westward +0.7km/s The mean radial velocities from 12 observations obtained between 0:42 to 1:56 11th of Aug. show ; The mean radial velocities from 12 observations obtained between 0:42 to 1:56 11th of Aug. show ; The eastward +2.1km/s (±1.13km/s The eastward +2.1km/s (±1.13km/s The center -13.1km/s(±2.8km/s The center -13.1km/s(±2.8km/s The westward -0.5km/s The westward -0.5km/s Results

The radial velocities of upward flux of central region are observed higher values among three regions. The other hand, the radial velocities of downward flux of each ends are observed not so high. Results Results The solar surface Mean value 2.1km/s Line of sight Sun spots Mean value 0.5km/s Mean value 13.1km/s AFS

Acknowledgment We thank Drs. Shibata, Kurokawa and Ishii, We thank Drs. Shibata, Kurokawa and Ishii, and staffs of Kwasan observatory. This work was supported by SPP/JST (2006).