Magnetic Flux Ropes in the Solar Photosphere: The Vector Magnetic Field under Active Region Filaments B.W.Lites the Astrophysical Journal, 622:1275-1291,2005,

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Presentation transcript:

Magnetic Flux Ropes in the Solar Photosphere: The Vector Magnetic Field under Active Region Filaments B.W.Lites the Astrophysical Journal, 622:1275-1291,2005, April1 雑誌会　速報2005年10月3日 J. Kiyohara

Introduction & Abstract Where is the helicity of solar atmospheric structures generated ?  by sheering flows ( Pneuman1983, van Ballegooijen & Martens 1989 etc. )  by actions in the solar interior

Active Region Filaments :　　　 An Observational Diagnostic of Twisted Magnetic Fields In quiet regions - Most prominences reside at heights well above the photosphere. In the photosphere, strong magnetic fields are highly buoyant, and this buoyant force tends to align them with gravity. ( Martinez Pillet et al, 1997, Parker 1979, pp136-151 )

Active Region Filaments :　　　 An Observational Diagnostic of Twisted Magnetic Fields In active regions - Arch Filaments upward velocity at the apex of the arch downwards at the two ends of the arch roots on opposite sides of the polarity inversion line(PIL) - very narrow , low-lying filaments follow along the PIL This paper focus on filaments in active region plage well separated from sunspots. the telltale signature of a flux rope as measured in the vector magnetic field The concave geometry is a characteristic signature for a flux rope whose axis has emerged into the atmosphere.

3. Observational Requirements -- vector magnetic field measurements DLSP ( Sankarasubramanian et al. 2004 ) SOLIS ( Keller et al. 2003 ) POLIS ( Schmidt et al . 2003 ) TIP and LPSP ( Martinez Pillet et al. 1999 ) -- high angular resolution 1”-2” resolution to reveal concave geometry -- chromospheric diagnostic Ha Stokes spectra and slit-jaw images of the line core

CASE1: An evolving region with persistent concave field geometry NOAA 8948

CASE1: An evolving region with persistent concave field geometry NOAA 8948 White lines : separator between positive and negative polarity magnetic fields (the PIL). Yellow lines : spatially smoothed PIL. In the vicinity of the PIL, Field strengths are generally weaker (400-700G) and fill factors are larger than in the plage on either side ( 1000-1500G ). April 6-10 : the photospheric field is generally aligned with the PIL. April 6-9 : the concave geometry

CASE1: An evolving region with persistent concave field geometry NOAA 8948 April 7 White lines : separator between positive and negative polarity magnetic fields (the PIL). Yellow lines : spatially smoothed PIL. In the vicinity of the PIL, Field strengths are generally weaker (400-700G) and fill factors are larger than in the plage on either side ( 1000-1500G ). April 6-10 : the photospheric field is generally aligned with the PIL. April 6-9 : the concave geometry

Orientation of the horizontal component of the magnetic field vector relative to the local tangent of the PIL. convex geometry ( frel<0 ) concave-up geometry ( 0 < frel< 180deg. )

CASE2: An active filament in NOAA390

CASE2: An active filament in NOAA390

Discussion ・ The observation presented herein show a qualitatively different vector magnetic field structure at the PIL than is normally found in plage.  The magnetic system associated with low-lying filaments has a profound influence on the magnetic field at the photosphere.  The likely scenario is that the flux ropes are generated in the solar interior and buoyantly rise through the photophere into the corona. ・ This first study points to the need for more complete studies that will be facilitated by new instrumentation for observing solar vector magnetic fields.  not only the imaging of the chromophere and corona but also the velocity field in the photosphere and in the chromosphere, both for Doppler measurements and proper motions.