science with hinode
DESCRIPTION
Hinode space satellite observing the Sun.TRANSCRIPT
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.
QuickTimeª and aYUV420 codec decompressorare needed to see this picture.
Small whirlpools in the Sun, with a size similar to the terrestial hurricanes (~<0.5Mm)(Bonet et al. 2007)
1000 km
QuickTimeª and a decompressor
are needed to see this picture.
~ 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
decompressorare needed to see this picture.
~ 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.