Eis meeting talk
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Transcript of Eis meeting talk
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
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
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
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
Back on Earth
Somerset island
A week after .....
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
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
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
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
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
Science with Sunrise
Solar active regions Photospheric/Chromospheric drivers of penumbral microjets
Kaysukawa et al, 2007
Science with Sunrise
Solar active regions
Relationship between Chromospheric and Photospheric EF
Photospheric/Chromospheric drivers of penumbral microjets
Flux emergence - Coupling to the TR
Future plans
2nd Sunrise flight planned for 2011
The penguin in the logo will make sense then
From McMurdo baseAntarctica (9 - 12 days)
Thank you