Achim Gandorfer
Max Planck Institute for Solar System Researchon behalf of the Sunrise Team
Solar-C science meeting, Takayama, Nov.2013

Flying from Germany to Japan1929
LZ 127 „Graf Zeppelin“Launch of Sunrise in ESRANGE,Sweden• SEPARATE MOVIE

8th June 2009Sunrise
2009/2013

LZ127 „GrafZeppelin“ 1929

Who isSUNRISE?

S.K. Solanki (PI),P.Barthol (PM),A. Gandorfer (PS),
Max-Planck-Institut fürSonnensystemforschung,
Katlenburg-Lindau
M. Knölker (Co-I)
High Altitude Observatory,Boulder, USA
V. Martínez-Pillet (Co-I)
Instituto de Astrofísica deCanarias, Teneriffa, Spanien
und das IMaX TeamW. Schmidt (Co-I)
Kiepenheuer Institut fürSonnenphysik,Freiburg i. Br.
A.M. Title (Co-I)
Lockheed-Martin Solar andAstrophysics Laboratory,
Palo Alto, USA

What is Sunrise?
Sunrise• is a 1-m aperture telescope(biggest solar telescope to leavethe ground)• operates in the stratosphere• carries two science instruments
working in UV and visible• to provide UV images, Doppler
maps, and vectormagnetogramsof unprecedented quality

Barthol et al., 2011, Sol. Phys. 268,1

Sunrise balloon-borne
solar observatory• Gregory telescope, 1-m aperture(biggest solar telescope to leave theground) (Barthol et al. 2010)• 2 science instruments:– SUFI, UV filter imager(Gandorfer et al. 2010)– IMAX, Imaging Magnetograph Experiment:
vectormagnetograms in Fe I 525.02 nm(Landé g=3) (Martínez Pillet et al. 2010)– Both instruments observe simultaneously
thanks to clever light distribution unit

• Correlating wavefront sensor (Berkefeldet al. 2010)• Protective and stabilizing gondola

IMaX Imaging Magnetograph eXperiment(Martínez Pillet et al., 2011, Sol.Phys. 268, 57)
vectormagnetograms andDoppler maps in Fe I
525.02 nm (Landé g=3)
33s cadence
50“x50“ FoV
0.15“ resolution
S/N ~ 1000

SuFI Sunrise Filter Imager(Gandorfer et al. 2011,Sol.Phys. 268, 35)
214nm, 300nm, 312nm,
CN, Ca II H
1s max cadence (fixedwavelength)
8sec (all wvlgthsexcluding 214nm)
30sec including 214
14“x40“arcsec
0.15“

SuFI Sunrise Filter Imager

new for 2013 flight:
214nm, 300nm, Ca II H
(0.18nm), Ca II H
(0.11nm), Mg II k (0.48nm)
1s max cadence (fixedwavelength)
8sec (all wvlgthsexcluding 214nm and280nm)
60sec including 214
14“x40“arcsec
0.15“ except Mg II k

First flight path (duration ~6 days)

Somerset Island, Canada, 74o N
68o N Kiruna, Sweden

High-speed telemetry lost hours after launch. No images until recovery
Observatory was recovered with all major systems intact

Sunrise 1 Data

Sun was VERY quiet during first flight: no1. Quiet solar granulation: UV Intensity,
sunspots, no pores
dynamics, and morphology
 Sunrise 1 results all refer to quiet Sun

PD Reconstructed SUFI Images
λ=300nm

14 arcsec

λ=313nm

λ=388nm

λ=397nmComparison Sunrise with Hinode data
Sunrise: SUFI 388 nm (filterwidth 0.8 nm)
Hinode: BFI 388 nm (filterwidth 0.7 nm)
Same grey scale

Note that the two images
were not taken
simultaneously (differentgranules), but both refer toquiet Sun at µ = 1104 km

104 kmMTF curves (circular, unobscured entrance
apertures of different sizes)

Hinode-size (D=50cm); Sunrise-size (D=1m)
if both telescopes are perfect, the larger telescope will provide highercontrast images AT ALL SPATIAL FREQUENCIES!

Data: SuFI
300-388nm: granulation with BPs, 214nm: more structured granules, prominentBPs, 397nm: reversed granulation, waves, BPs; more diffuse than other WLs

SUFI RMS:
BP contrast:

31.8%
2.3x

24.2%
1.5x

23.8%
1.4x

21.5%
1.6x

25.6%
1.9x

MHD RMS:

?

25.5%

22.0%

20.0%

?

Hirzberger et al. 2010, ApJ 723, L154; Riethmüller et al. 2010, ApJ 723, L169

SUFI
CLV

214nm displays signs ofincreasing inverse granulation
away from disk centreGranules (or convectivefeatures at limb are distinclysmaller.  sub-structure ofgranules better visible at limb

Sunrise 1 Data

velocities, flows, and waves...

Vortices in granulation

Bonet et al., 2010, ApJ 723, L139

3.1 × 10−3 vortices Mm−2 minute−1, a factor of∼1.7 larger than previous estimates.

Horizontal vortices

numerical simulation
IMaX intensity and Doppler
data

Steiner et al., 2010, ApJ 723, L180

Khomenko et al. 2010, ApJ 723, L159

Where thegranular flows
bendIntergranular lanes show
large line width (bright)Small line width at thegranular/intergranularborders (dark lanes)

MHD simulations: lowwidth where granular
flows bend over (lowvelocity gradient)

Important: this narrowing of spectral
lines can only be seen if spatial
resolution is sufficiently highMHDSunrise

MHD <B>=30 G, mixed polarity

FWHM of FeI 5250 Stokes I,
binned to IMaX (afterrestoration) resolution

FWHM of FeI 6301 Stokes I,
degraded to HINODE
resolution

Dark lanes do not appear at HINODE resolution
Elena Khomenko, Instituto de Astrofisica de Canarias

IMAX data: velocity movie• LOS velocity
shows combinationof– granules,– p-modes– higher frequency
waves

Acoustic wave power and small-scale
eventsSunrise provided firstevidence that acoustic
wave power (l > 1000)
is enhanced prior to
granule splitting(exploding granules)and displays vortices
Movie shows wave
pattern overplotted on
intensity structure(granules)

Roth et al. 2010, ApJ 723, L 175

High acoustic wave flux above cutoff
W m-2

W m-2

Bello González et al. 2010, ApJ 723, L134

4500–14000 W m-2 needed to explain quiet chromosphere emission
Difference to earlier work may partly be due to different methods.
However, the difference to work of Bello González et al. (2009) byfactor of 2.2-2.5 is due to the higher quality of Sunrise data

High acoustic wave flux above cutoff
W m-2

W m-2

Required to explain quiet chromosphere: 4500 – 14000 W m-2
The “missing acoustic wave flux” seems to be hidden not athigh frequencies, but at small spatial scales (inter granules)

Sunrise 1 Data
polarization and magnetic fields

Sunrise 1 IMaX data:
Total linear polarization

Stokes VUbiquitous linear polarization featuresin quiet sun
A number of features show downflows only.
They cannot be emerging loops!

≈ 5000 features analyzed
Most associated with bipoles
Occurrate: 7*10-4 s-1 arcsec-2
 Order of magnitude morethan earlier estimates. E.g.
Ishikawa & Tsuneta (2009):
6.3*10-5 s-1 arcsec-2
Martinez Gonzalez & Bellot Rubio(2009): 5.6*10-6 s-1 arcsec-2
Lites et al. (1997):
2.8*10-5 s-1 arsec-2

Danilovic et al. 2010, ApJ 723, L149

Kilo Gauss fields resolved
 Inversions with different

codes & techniques give: kilo Gauss fields without

the need to introduce
magnetic filling factor
 temperature enhancementthat agrees with empiricalflux-tube models
 Sunrise finally resolved

magnetic elements evenin the quiet Sun
 Many magnetic elementsare ≈100 km in size (evenin QS internetwork)

Lagg et al. 2010, ApJLCa II dynamics andmagnetic field• Clearly distinguishbetween magnetic
and non-magnetic(waves) Ca brightfeatures• Magnetic Ca brightpts tend to have aballistic, rather
than a randomwalk trajectory
Dissertation of
Shahin Jafarzadeh

purely geometricaldeterminationof theinclination of fluxtubes
yields almost vertical fields
in contradiction todifferent inversion runs
establishes acomplementary method toindependently analyze
inclination of flux tubes

Dissertation of
Shahin Jafarzadeh

Other interesting studies“Supersonic Magnetic Upflows in Granular Cells”
first observed in IMaX data (Borrero et al. 2010, ApJ 723, L144)
later also found in Hinode/SP data as„Ubiquitous quiet-Sun jets” (Martinez Pillet et al., 2011, A&A, inpress„Emergence of an intermediate-scale bipole“ (Guglielmino et al.,submitted to ApJ) see talk on Tuesday“Unnoticed Magnetic Field Oscillations in the Very Quiet Sun”
(Martínez González et al., 2011, ApJ 730, L37“Mesogranulation and the Solar Surface Magnetic FieldDistribution” (Yelles Chaouche et al., 727, L30)

and many, many more to be expected......

Riethmüller et al., 2013, APJLRemarkable similarity between
Mg II k and Ca II h• Danilovic et al., submittedSummary• In spite of a number of issues (early loss of telemetry;extremely quiet Sun; only short time series) first Sunrise
science flight was highly successful, providing unique data
• A significant number of results have been obtained, almost
all of them were unexpected• A lot more exciting science is still hidden in these data
• Data of second flight 2013 not fully reduced so far, but firstdata are promising• first results of SUFI Mg II k data are publishedOutlook• Quality of Sunrise data is resounding, but they are notperfect– residual jitter– residual aberrations– photon noise in blue channels• Phase diversity can help, but cannot do magic– photon noise is dominant driver at larger apertures!
– becomes more and more severe when going to apertures larger than1m

On behalf of theSUNRISE team:Thank you verymuch for yourinterest!

Sunrise data access
http://star.mpae.gwdg.de/Sunrise/
The SuFI data are available on the web:
http://www.mps.mpg.de/data/projekte/sunrise/sufidata/level2/
http://www.mps.mpg.de/data/projekte/sunrise/sufidata/level3/
Please see the readme files:
http://www.mps.mpg.de/data/projekte/sunrise/sufidata/level2/readme.pdf
The IMaX data are available on the web:
http://www.mps.mpg.de/data/projekte/sunrise/imaxdata/level1/
http://www.mps.mpg.de/data/projekte/sunrise/imaxdata/level2/