Observations of emerging and submerging regions with ASP and Solar-B

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Presentation transcript:

Observations of emerging and submerging regions with ASP and Solar-B Masahito Kubo (University of Tokyo)

Introduction Emerging flux region Observations with high accurate photospheric vector magnetic field are important to understand the flux emergence processes We observed an evolving active region that have significant emerging flux with ASP We obtain vector magnetic properties of initial stages of emerging flux Submerging region A large-scale cancellation region was formed in our observed active region This is first observation of cancellation region with vector magnetic field

Emerging and Submerging region in NOAA9231 move clockwise around leading sunspot move to cancellation region SoHO/MDI bright loops appear and connect emerging bipole bright structure appear above the cancellation region Yohko/SXT pre-existing loop-like structures New connection appear

Observation of rapidly emerging bipole a few hours old after their first appearance their evolution during three hours was observed with ASP Emerging region 19-NOV-00 17:41:50UT

Evolution of emerging flux in early phase Magnetic flux Pre-existing magnetic flux hide the negative pair horizontal vertical(outward) vertical(inward) Filling factor • filling factor represent percentage of each pixel occupied by magnetic atmosphere black represent large quantities of magnetic atmosphere are contained in a pixel High filling factor (>80%) area appears between active emerging bipole.

Vector magnetic properties of high filling factor area Inclination（θ）[deg] vertical(inward) In high filling factor area, the direction of magnetic field is horizontal to solar surface 5″ horizontal vertical(outward) Magnetic field strength(|B|) [Gauss] Magnetic field strength in high filling factor area is weaker (500 Gauss) than surrounding horizontally oriented magnetic field (800Gauss). 500[Gauss] 1600[Gauss] 800[Gauss]

Doppler velocity(vLOS) [km/s] line of sight velocity of magnetic atmosphere upward upward velocity (~0.5 km/s) downward

Summary of emerging flux region High filling factor area appears between active emerging bipole with flux emergence horizontal to the solar surface Weak field strength (500Gauss) upward velocity (0.5 km/s) consistent with other ASP observations of newly emerging flux (Lites et al. 1998) • Another two active emerging bipoles were observed (One was after about 3 hours from their first appearance and another was after 12 hours) High filling factor areas were also located between both active emerging bioples Properties of magnetic fields in the high filling factor areas are almost same

Emerging and Submerging region in NOAA9231 move clockwise around leading sunspot move to cancellation region SoHO/MDI bright loops appear and connect emerging bipole bright structure appear above the cancellation region Yohko/SXT pre-existing loop-like structures New connection appear

Magnetic field between colliding poles magnetic flux map (ASP) (arrow:tangential component, green line: neutral line) vertical(inward) horizontal vertical(outward) Horizontally oriented magnetic fields increase during three days and they connect colliding poles.

Horizontal magnetic field with downward velocity Doppler velocity(vLOS) [km/s] Perpendicular motion extract horizontally oriented magnetic field (45°< θ <135°) upward 20-NOV-00 14:52:02(S24W24) + + －－ + + downward Horizontally oriented magnetic fields have downward velocity between colliding poles  submerging magnetic field

Field strength and filling factor in cancellation region 20-NOV-00 14:52:02 Magnetic field strength[Gauss] horizontally oriented magnetic field between colliding poles  400 – 1500 Gauss　>　typical horizontal magnetic field + － + Filling factor high filling factor (>80%) area exist high filling factor area is almost coincided with downward velocity area + A1 － +

Solar-B observation of cancellation region Reconnection model Corona (XRT, EIS) bright structures between colliding poles + － + － Photosphere (SOT) horizontally oriented magnetic field with downward velocity between colliding poles before reconnection corona Solar-B will be able to observe submerging motion of identical magnetic loop from corona to photosphere chromosphere photosphere + － + － after reconnection

Summary We obtain the vector magnetic properties of emerging and submerging (cancellation) region as follow; Emerging region Submerging region Doppler velocity upward (~0.5 km/s) downward (~0.5 km/s) Inclination horizontal　　　　 horizontal Field strength　　　　　 ~500[Gauss]　　　　　　 400 – 1500 [Gauss] Filling factor high (> 80 %) high (> 80%)