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