eis meeting talk
TRANSCRIPT
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Solar magnetic field as seen from a balloon
Santiago Vargas Domínguez
UCL DEPARTMENT OF SPACE AND CLIMATE PHYSICSMULLARD SPACE SCIENCE LABORATORY
Fluex Emergence Workshop @ MSSL March 2010
A sneak peek at data from Sunrise
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Electronics box
Secondary mirror
InstrumentationGondola
Damping system
Solar panels
Swedish Solar Telescope
(SST)Observatory Roque de Los Muchachos (La Palma) @ 2400 mDiffraction
limited: ~ 0.1”
Ballon-borne 1-m solar telescope +CWS: Correlator and Wavefront Sensor
SUFI: Sunrise Filter Imager (high-res images visible & UV)IMaX: Imaging Magnetoraph eXperiment (2D maps of complete magnetic field vector, LOS velocity, white-light images
What is Sunrise ?
Aim at:
High-resolution Spectro-polarimetric observations of the solar atmosphere. Study magnetoconvection at fine scales
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What is Sunrise ?
QuickTimeª and a decompressor
are needed to see this picture.SST
FOV 16”x16”0.034 “/pix
118 images
Cadence: 10 s
Sunrise combinesstrengths of SST (aperture)
and Hinode (spectro-polarimetry
with stable image quality).
Images in UV down to 0.05”
Gband (λ430.5 nm)
1000 km
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QuickTimeª and a decompressor
are needed to see this picture.
QuickTimeª and a decompressor
are needed to see this picture.
Launched on 08/06/2009 from ESRANGE base Kiruna (Sweden)
Launching & flight
6 days
Altitude: 40 km
v ~ 50 km/h
140 m
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Back on Earth
Somerset island
A week after .....
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Fe 525.02 nm
FOV 7”x 7”
Small thumbnails 256x256 pixels and 0.22 arcsec/pix
FOV 50”x 50”
IMaX white-light
Post-facto image restoration (Phase Diversity)
Preliminary data
exp time: 1.5 s
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Preliminary data
Summer Schedule
July
1st week : Sunrise back home - Lindau (Germany)
2nd week : Sunrise data meeting - Lindau (Germany)
3rd week : IMaX data reduction meeting - somewhere (Spain)
August
September
Data reduction (first steps)
Spanish Solar Physics Meeting ( IMaX first results ? )
Data available for scientific community
in early 2010
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Science with Sunrise
Filter positions
388 nm (CN)397 nm (CaH)300 nm313 nm (OH)214 nm
PointingMeasure 3D-distribution of B vector, v, T
Polarization sensitive spectroscopy in photospheric/chromospheric line(s)
Coordinated ObservationsHinode, SOHO, TRACE SST, DOT, VTT, DST
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Science with Sunrise
Formation/destruction of intense magnetic elements
Quiet Sun
Convective collapse (Parker 1978). Convincing observation of the formation of intense flux tubes (~ KG)
Photospheric footpoints of chromospheric and TR loops
Dynamics of solar vortex flows (Bonet et al 2008) Coupling to the TR
Photospheric structure @ spatial resolution ~35 km (214 nm)
Magnetic landscape and coupling of the Polar Regions
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Science with Sunrise
Solar active regions Magnetoconvection
at small scales
Are umbral dots, light bridges and penumbral filaments intrusions of field-free plasma from beneath the sunspot ?
Internal structure and evolution of individual penumbral filaments(< dark cores, Scharmer et al 2002)
Those are still open questions generating an ongoing debate
1000 km
1000 km
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Science with Sunrise
Solar active regions Photospheric/Chromospheric drivers of penumbral microjets
Kaysukawa et al, 2007
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Science with Sunrise
Solar active regions
Relationship between Chromospheric and Photospheric EF
Photospheric/Chromospheric drivers of penumbral microjets
Flux emergence - Coupling to the TR
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Future plans
2nd Sunrise flight planned for 2011
The penguin in the logo will make sense then
From McMurdo baseAntarctica (9 - 12 days)
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Thank you