Science with Hinode

First internal Hinode Meeting, MSSL, Sep 7th, 2009

Santiago Vargas Domínguez

I. Small magnetic elements from the photosphere to the low chromosphere

They are ubiquitous bright points of magnetic field concentration, spread all over the solar surface in:

Network: Nearly vertical magnetic field ~100 G AR and frontiers of supergranules

Inter-Network: Horizontal trend (20 G or less)

Diffraction limit and high cadence observations are important since these structures are tiny and highly dynamic.

Understanding the formation and structure is fundamental to figure out the role of these magnetic elements on solar irradiance.

Quiet Sun

Active region

Small magnetic elements from the photosphere to the low chromosphere

Small magnetic elements from the photosphere to the low chromosphere

These MBP represent a significant area, are highly dynamic and evolve through fragmentation, merging and cancellation.

Gband Magnetogram

MBP properties

Small magnetic elements from the photosphere to the low chromosphere

MagCN Gband

Small magnetic elements from the photosphere to the low chromosphere

Mag

Gband

CN

CaIIH

Photospheric vortex-type event evidenced by magnetic field rotation.

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Small whirlpools in the Sun, with a size similar to the terrestial hurricanes (~<0.5Mm)(Bonet et al. 2007)

1000 km

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~ 4000 km

Small magnetic elements from the photosphere to the low chromosphere

mag

Gband

CN

CaIIH

Understand how small-scale events can affect the upper layers.QuickTimeª and a

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~ 4000 km

- Reconnection with pre-existing magnetic fields.

- Twisting of emerging flux as affected by convective motions

II. Solar active regions and their interaction with the surrounding granulation

Magnetic field inhibits convectionTransition from pores into sunspots ?

Formation and decay of sunspots: Modalities ofinteraction between high ionized plasma and magnetic fields.

Not a consensus for sub-photospheric flows responsible for the formation of solar pores.

Solar active regions and their interaction with the surrounding granulation

Solar active regions and their interaction with the surrounding granulation

Solar active regions and their interaction with the surrounding granulation

Bipolar Moving Magnetic Features streaming out from the “naked spot”

Solar active regions and their interaction with the surrounding granulation

CaIIH reveals filamentary structure all around the spot.

Naked spot ??

LCT measures inward radial horizontal velocity components all around the spot.

Magnetic extrapolations

Full-atmosphere inversions: LILIA

To obtain physical quantities (mag. field strength/inclinationv LOS, microturbulence, temperature, .....)

To relate evolution of photospheric magnetic structures with phenomena in upper layers (i.e. reconnection)

Local Correlation Tracking

Applied to EIS data.