SOT Highlights on Photospheric
Magnetic Fields

Ted Tarbell
LMSAL

Solar-C Meeting, 20 Nov 2008

SOT observations, combined with 3-Dmodels, are answering many of ourlong-standing questions about themagnetic field in the photosphere

Solar-C Meeting, 20 Nov 2008

SOT Highlights & Discoveries•

Flux Emergence on Many Scales•

Turbulent and Transient Horizontal Magnetic Fields•

Convective Collapse•

Polar Magnetic Fields -- you have seen Tsuneta’s talk•Reconnections & Jets Everywhere•

Penumbral Structure•

Flux Budget of a Decaying Sunspot•

Fields, Currents & NLFF Extrapolations -- see Schrijver’s talkSolar-C Meeting, 20 Nov 2008

Flux Emergence on Many Scales

Solar-C Meeting, 20 Nov 2008

Flux Emergence on Many Scales

Solar-C Meeting, 20 Nov 2008

Flux Emergence Patterns
in Ephemeral Scale
Regions 	

10 arcseconds	

7.2 Mm	Solar-C Meeting, 20 Nov 2008

Flux Emergence Patterns in
Granulation Scale Regions	

6 arcseconds	

4.32 mm	Solar-C Meeting, 20 Nov 2008

Solar-C Meeting, 20 Nov 2008

Flux Emergence on Many Scales

Solar-C Meeting, 20 Nov 2008

Solar-C Meeting, 20 Nov 2008

View of Surface and - 5 Mm	Solar-C Meeting, 20 Nov 2008

Turbulent & Transient Horizontal Fields• R. Ishikawa, “Statistical Properties of Transient
Horizontal Fields,” 2nd Hinode Science Meeting,Boulder, Oct 2008
• B. Lites, “Is Flux Submergence an Essential aspect ofFlux Emergence”• J. Pietarila Graham, “The Solar Surface Dynamo”• O. Steiner, “The Horizontal Internetwork Field:
Numerical Simulations in Comparison toObservations with Hinode”

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Transient Horizontal Magnetic Fields

Solar-C Meeting, 20 Nov 2008

Convective Collapse to form Flux Tubes• S. Nagata, “Convective Instability and the Formationof Solar Magnetic Flux Tubes,” 2nd Hinode Science
Meeting, Boulder, Oct 2008
• C. Fischer, “Analysis of High Cadence Hinode SP
Quiet Sun Time Series”

Solar-C Meeting, 20 Nov 2008

Convective Collapse to form Flux Tubes

Solar-C Meeting, 20 Nov 2008

Convective Collapse to form Flux Tubes• Blah, blah, blah

Solar-C Meeting, 20 Nov 2008

Convective Collapse to form Flux Tubes

Solar-C Meeting, 20 Nov 2008

Convective Collapse to form Flux Tubes• From Nagata et al, Hinode 2 Talk

Solar-C Meeting, 20 Nov 2008

Reconnections & Jets Everywhere•••••K. Shibata, “Ubiquitous Magnetic Reconnection in the SolarAtmosphere,” 2nd Hinode Science Meeting, Boulder, Oct 2008
M. Shimojo, “The Relationship between the Magnetic Field andthe Coronal Activities in the Polar Region”
R. Kano et al, “Photospheric Magnetic Activities to Trigger
Micro-flares Observed with Hinode SOT and XRT”
Y. Katsukawa & J. Jurcak, “Chromospheric Activity at theSmallest Scales Obtained by Hinode: Small Scale Activities inPenumbrae”
T. Shimizu, “Hinode Observation of the Vector Magnetic Fieldsin a Sunspot Light Bridge Accompanied by Chromospheric
Plasma Ejections”

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Jets Everywhere?

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure• L. Bellot Rubio, “Sunspot Magnetic Fields near theDiffraction Limit: the Hinode View,” 2nd Hinode
Science Meeting, Boulder, Oct 2008
• K. Ichimoto, “Convective Nature of the Evershed
Observed by SOT/Hinode,” ibid.

Solar-C Meeting, 20 Nov 2008

Hinode/SP: full Stokes spectropolarimetry at 0.3"
Continuum intensity 630.2 nm

2006-11-14
Target: NOAA 10940
Heliocentric angle: 8º
Mode: normal map
Solar-C Meeting, 20 Nov 2008

Total (circular+linear) polarization Stokes V spectra

Exposure time:
Slit width and length:
Noise level:
Spatial resolution:

4.8 s/slit
0.16ʺ″, 164ʺ″
1.1 x 10-3 Ic
0.3ʺ″Horizontal interlacing of different magnetic components
Ichimoto et al., 2007, PASJ, 59, 593
Milne-Eddington inversion

Solar-C Meeting, 20 Nov 2008

At 0.3", two magnetic components show up
prominently in the field strength andinclination maps derived from ME inversions

Vertical interlacing of different magnetic components
Bellot Rubio et al., 2007, ApJ, 668, L91
Bright filaments in inner limbside penumbra

The NCP of spectral lines is not zeroand shows correlation with penumbral
filaments, confirming results of Tritchler
et al. (2007) and Ichimoto et al. (2008)

Solar-C Meeting, 20 Nov 2008

Bright filaments are distinct
structures (with flows) embedded
in ambient sunspot field

Multi-lobed Stokes V profiles reflect vertical interlacing
Bellot Rubio et al., 2007, ApJ, 668, L91
Limb-side penumbra, θ = 50°

Multi-lobed Stokes V profiles still occur, but now
it is less likely that they are due to horizontal
interlacing of different magnetic components

Magnetic components of opposite polarity exist along theLOS: one is strongly Doppler-shifted to the red
Solar-C Meeting, 20 Nov 2008

Penumbral field lines return back to solar surface
Sainz Dalda & Bellot Rubio, 2008, A&A, 481, L21
Hinode/NFI Fe I 630.2 nm, Δλ = -120 mÅ

Opposite-polarity field lines occur
everywhere in the mid and outerpenumbra
First time that they are imaged
directly (confirming earlier
inversion results….)

Solar-C Meeting, 20 Nov 2008

Supersonic Evershed flows occur in the penumbra
Stokes V signal at +343 mÅ (~12 km s-1)

Stokes I

Stokes V

NOAA 10973, θ ~ 5o, courtesy K. IchimotoDoppler shift of 9.5 km s-1!!

Patches with supersonic flows are observed everywhere in the middle andouter penumbra (as also reported by Shimizu et al. 2008)
Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Penumbral Field Structure

Solar-C Meeting, 20 Nov 2008

Flux Budget of a Decaying Sunspot• Kubo et al, “Magnetic Flux Loss & Flux Transport in aDecaying Active Region,” 2nd Hinode Science
Meeting, Boulder, Oct 2008

Solar-C Meeting, 20 Nov 2008

Flux Budget of a Decaying Sunspot

Solar-C Meeting, 20 Nov 2008

Flux Budget of a Decaying Sunspot

Solar-C Meeting, 20 Nov 2008

Flux Budget of a Decaying Sunspot

Solar-C Meeting, 20 Nov 2008

Flux Budget of a Decaying Sunspot

Solar-C Meeting, 20 Nov 2008

Fields, Currents and NLFF
Extrapolations
difference in free energy = 3 × 1032 erg

E/Epot=1.32 isosurface of |J| shown in red

E/Epot=1.14• Stay tuned for talk by K. Schrijver later this afternoon
Solar-C Meeting, 20 Nov 2008