Sunrise overview

Sunrise: instrument, mission, data and first results

S. K. Solanki11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. 88affiliation: School of Space Research, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea , P. Barthol11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , S. Danilovic11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , A. Feller11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , A. Gandorfer11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , J. Hirzberger11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , T. L. Riethmüller11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , M. Schüssler11affiliation: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany. , J. A. Bonet22affiliation: Instituto de Astrofísica de Canarias, C/Via Láctea s/n, 38200 La Laguna, Tenerife, Spain. , V. Martínez Pillet22affiliation: Instituto de Astrofísica de Canarias, C/Via Láctea s/n, 38200 La Laguna, Tenerife, Spain. , J. C. del Toro Iniesta33affiliation: Instituto de Astrofísica de Andalucía (CSIC), Apdo. de Correos 3004, E-18080, Granada, Spain , V. Domingo44affiliation: Grupo de Astronomía y Ciencias del Espacio (Univ. de Valencia), E-46980, Paterna, Valencia, Spain , J. Palacios44affiliation: Grupo de Astronomía y Ciencias del Espacio (Univ. de Valencia), E-46980, Paterna, Valencia, Spain , M. Knölker55affiliation: High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder CO 80307-3000, USA.111HAO/NCAR is sponsored by the NSF , N. Bello González66affiliation: Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany. , T. Berkefeld66affiliation: Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany. , M. Franz66affiliation: Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany. , W. Schmidt66affiliation: Kiepenheuer-Institut für Sonnenphysik, Schöneckstr. 6, 79104 Freiburg, Germany. , and A. M. Title77affiliation: Lockheed-Martin Solar and Astrophysical Lab., Palo Alto, USA

The Sunrise balloon-borne solar observatory consists of a 1m aperture Gregory telescope, a UV filter imager, an imaging vector polarimeter, an image stabilization system and further infrastructure. The first science flight of Sunrise yielded high-quality data that reveal the structure, dynamics and evolution of solar convection, oscillations and magnetic fields at a resolution of around 100 km in the quiet Sun. After a brief description of instruments and data, first qualitative results are presented. In contrast to earlier observations, we clearly see granulation at 214 nm. Images in Ca ii H display narrow, short-lived dark intergranular lanes between the bright edges of granules. The very small-scale, mixed-polarity internetwork fields are found to be highly dynamic. A significant increase in detectable magnetic flux is found after phase-diversity-related reconstruction of polarization maps, indicating that the polarities are mixed right down to the spatial resolution limit, and probably beyond.

Subject headings:
Sun: photosphere — Sun: chromosphere — Sun: faculae, plages — techniques: photometric — techniques: polarimetric — techniques: spectroscopic

1. Introduction

In order to understand the processes that govern solar activity, we must disentangle how the magnetic field interacts with the solar plasma and guides the conversion of energy between its mechanical, magnetic, radiative, and thermal forms.

The photosphere represents the key interaction region: thermal, kinetic and magnetic energy all are of the same order of magnitude and transform most easily from one form into another. This interaction in turn leads to the creation of a rich variety of magnetic structures, from sunspots down to intense magnetic field concentrations on a length scale of 100 km or less. This structuring provides the need to obtain data with a homogeneous and constant resolution of such length scales. One possibility to fulfil this requirement is to fly a telescope carried by a stratospheric balloon.

Balloon missions aiming at high-resolution solar studies have a long history. An early highlight was the 12-inch Stratoscope, which flew multiple times in 1957 (Schwarzschild 1959) and 1959 (Danielson 1961). It produced high resolution images of solar granulation, the solar limb and of sunspot fine structure, which for many years represented the state of the art. A similar-sized instrument equipped with a spectrometer, the Spectrostratoscope, flew in 1975, but mainly obtained imaging data of solar granulation (Mehltretter 1976, 1978, Wittmann & Mehltretter, 1977). The Soviet Stratospheric Solar Station had multiple flights (e.g., Krat et al. 1970). The 50 cm telescope provided nearly diffraction limited broad-band images of solar granulation and a sunspot (Krat et al. 1972). These data led Karpinsky (1989) to propose large-scale restructuring of the solar granulation on a short time scale. The 80 cm diameter Flare Genesis telescope, equipped with a sophisticated Fabry-Pérot based vector magnetograph (Rust et al. 1996), flew in 1996 and in 2000, achieving a spatial resolution of roughly 0.5 arcsec (Georgoulis et al. 2002) during the second flight. This experiment resulted in the discovery of bipolar magnetic features moving towards a very young sunspot, which were interpreted as small U-loops (Bernasconi et al. 2002; Georgoulis et al. 2002).

In addition to achieving high resolution, stratospheric balloon flights also allow the Sun to be explored in near ultraviolet radiation that is strongly attenuated by the Earth’s atmosphere. In 1970 and 1971, a 20 cm telescope flew on a stratospheric balloon and recorded images between 200 nm and 460 nm (Hersé 1979). Later, the Rasolba balloon experiment, a 30 cm telescope with an ultraviolet spectrograph, obtained high resolution spectra in the wavelength range between 190 nm and 295 nm, which includes the Mg ii h and k lines (Samain and Lemaire 1985, Staath and Lemaire 1995).

Sunrise extends this tradition of telescopes carried by a stratospheric balloon in order to study the Sun. It combines high spatial resolution with sensitivity to ultraviolet radiation. At 1 m diameter, it is the largest solar telescope so far to leave the ground. It is equipped with sophisticated post-focus instruments, including a UV imager and a filter-based vector magnetograph.

2. Instrumentation and Mission

2.1. Instrument

The Sunrise stratospheric balloon-borne observatory is composed of a telescope, two post-focus science instruments (SuFI and IMaX, see below), an Image Stabilization and Light Distribution (ISLiD) unit, and a Correlating Wave-front Sensor (CWS), carried in a gondola, which possesses pointing capability.

2.1.1 Telescope

The telescope is a Gregory-type reflector with 1 m clear aperture and an effective focal length of close to 25 m. A heat-rejection wedge at the prime focus reflects 99% of the light from the solar disk off to the side, reducing the heat load on the post-focus instruments to approximately 10 W. The secondary mirror is actively controlled in three degrees of freedom to compensate for thermoelastic deformations of the telescope during flight. The post-focus instrumentation rests on top of the telescope. More details are given by Barthol et al. (2010).

2.1.2 SuFI

The Sunrise Filter Imager (SuFI) provides images at violet and near ultraviolet wavelengths. The wavelengths sampled by SuFI are: 214 nm at 10 nm bandwidth, 300 nm at 5 nm bandwidth, 312 nm at 1.2 nm bandwidth, 388 nm at 0.8 nm bandwidth and 396.8 nm (core of Ca ii H) at 0.18 nm bandwidth. A UV-enhanced CCD is employed, with a plate scale of 0.02 arcsec per pixel, on average (the plate scale is slightly wavelength dependent). In order to overcome aberrations due to thermoelastic deformations of the telescope and any remaining seeing, a phase-diversity technique (cf. Paxman et al. 1992; Löfdahl and Scharmer 1994) is used: a special optical arrangement in front of the detector delivers a nominally focused image on one half of the detector, while the other half receives an image with a defocus of one wave at 214 nm. Hence the field of view is arcsec. Both halves of the CCD together provide sufficient information for post-facto removal of low-order aberrations from the image.

A cadence of better than an image every 2 s can be achieved, depending on the exposure time, to either take rapid time series at a given wavelength or to switch wavelengths. Thus the 4 longer wavelengths can be cycled through within 8 s. Since the exposure time of the 214 nm was typically 30 s even at local noon, owing to residual ozone at and above float altitudes, the cadence was correspondingly lower whenever this wavelength was included.

A description of SuFI can by found in Gandorfer et al. (2010).

2.1.3 IMaX

The Imaging Magnetograph eXperiment (IMaX) operates in the Fe i 525.02 nm line (a Zeeman triplet with Landé factor ). Images in polarized light covering  arcsec are recorded at a spectral resolution of 85 mÅ, normally at 4 wavelengths within the spectral line and 1 in the nearby continuum. The full Stokes vector in these 5 wavelengths at a noise level of is obtained in 30 sec, which is the typical cadence for most of the observations. The number of wavelength points (between 3 and 12) and of polarization states can be varied to obtain a higher cadence, or a better rendering of the line profile shape.

The spectral resolution and sampling is achieved by using a thermally stabilized tunable solid-state Fabry-Pérot etalon in double pass together with a narrowband, prefilter with a full width at half maximum of 0.1 nm.

Polarization states are isolated with the help of two nematic liquid-crystal modulators operated at a frequency of 4 Hz, which are switched between four states for full Stokes vector polarimetry. A dual-beam approach is taken, with 2 synchronized 1kk CCD cameras. After every observing run, a plate is inserted into the light path in front of one of the cameras in order to obtain phase-diversity information for post-facto reconstruction. Detailed information on IMaX is provided by Martínez Pillet et al. (2010).

2.1.4 ISLiD

The Image Stabilization and Light Distribution (ISLiD) unit allows simultaneous observations with the two science instruments by distributing the radiation according to wavelength (200–400 nm to SuFI; 525 nm to IMaX; 500 nm to CWS), while preserving diffraction-limited performance as well as polarization information. ISLiD contains a rapid, piezo-driven tip-tilt mirror, which stabilizes the image on the science instrument foci by damping all vibrations and motions acting at frequencies up to 60 Hz. This mirror is controlled by CWS, which is optically stimulated by ISLiD. ISLiD is described by Gandorfer et al. (2010).

2.1.5 Cws

The Correlating Wavefront Sensor (CWS) is a Shack-Hartmann type wavefront sensor with a lenslet array in a pupil image that feeds a field-of-view of arcsec on a high-speed camera. It is used in two ways, as a fast correlation tracker to derive control signals for a tip-tilt mirror, and as a slow wavefront sensor (defocus and coma) for active alignment control of the telescope secondary mirror. The CWS is described by Berkefeld et al. (2010).

2.1.6 Gondola

The Sunrise gondola provides the housing for the telescope, instruments, power supply etc. In addition, it is responsible for the precision pointing of the telescope towards the Sun. Situated approximately 100 m below the drifting balloon, the gondola attitude control system nominally keeps the telescope orientation fixed to the Sun within a range of less than  arcsec. Within this range, ISLiD and CWS are able to compensate residual motions and allow continuous observations. Azimuthal control of the gondola is performed via a momentum transfer unit at its top.

Electrical power is provided by large photovoltaic arrays housed in two panels placed left and right of the telescope. On the rear side of the gondola, the instrument control electronics are mounted on two racks.

The two data storage containers collecting the science data are mounted well-secured inside one of the upper side trusses of the core framework, which provides protection and easy access for data recovery after landing. The complete payload has dimensions of 5.5 m in width and length, is about 6.4 m high and has a mass of 1919.6 kg (without CSBF equipment, ballast etc.). More information on the gondola is provided by Barthol et al. (2010).

2.2. Mission

Sunrise was flown on a zero-pressure stratospheric long-duration balloon, launched and operated by the Columbia Scientific Ballooning Facility (CSBF). It was launched on June 8, 2009 at 6:27 UT (08:27h local time) from ESRANGE (67.89°N, 21.10°E) near Kiruna in northern Sweden. It then floated westwards at a mean cruise altitude of 36 km and landed on Somerset island (northern Canada), suspended on a parachute, on June 13, 2009 at 23:47 UT. The payload remained in direct sunlight during the entire flight. Since at float altitudes the payload was above 99% of the Earth’s atmosphere, virtually seeing-free observations were possible all the time. Also, the balloon stayed above most of the ozone in the Earth’s atmosphere, allowing high-resolution imaging in the UV at 214 nm, 300 nm and 312 nm.

The loss of high-speed telemetry relatively soon after reaching float altitude (due to the failure of a rented commercial telemetry system), meant that no full images could be downloaded during the entire mission, so that instrument commissioning and operations had to be carried out practically blindly.

3. Overview of the data recorded during the 2009 flight of Sunrise

The total observation time was 130 hours, in which IMaX acquired 415 GB of data (480332 images) and SuFI recorded 790 GB (150288 images). 55685 of the SuFI images were acquired while the CWS control loop was closed. 16128 of these closed-loop images were collected near or at the solar limb (  0.5).

During 23% of the total time at float altitude the CWS loop was closed. We obtained continuous time series longer than 1 min during 22% and time series longer than 10 min during 10% of the total observation time. The longest time series of SuFI data is 34 min, but only 19 min for the SuFI mode that includes the shortest wavelength of 214 nm. This wavelength is by far the most sensitive to the airmass along the line-of-sight (LOS) and was only observed around local noon. The longest IMaX time series lasts 32 min.

During data reduction, different versions of SuFI Data are generated. Starting from the level-0 raw data, level-1 data are produced that are fully reduced, but not phase-diversity reconstructed. A first phase-diversity reconstruction using individual wavefronts for each image results in level-2 data. Finally, level-3 data are phase-diversity reconstructed employing an averaged wavefront (see Hirzberger et al. 2010b for more details on Sunrise/SuFI data reduction). A brief summary of the recorded SuFI data is given in Tables 1 and 2.

SuFI mode Fraction of
observing time
: 214, 300, 312, 388, 397 nm  8%
: 300, 312, 388, 397 nm 56%
: 300, 388, 397 nm  9%
: mostly 388, 397 nm 12%
: mostly 397 nm 15%
Table 1SuFI observing modes.
Central Exp. time Exp. time No. images No. images
  0.5   0.5   0.5   0.5
[nm] [ms] [ms]
214 30000 30000   409    33
300 100–500 200–800  8949  2649
312 100–500 200–800  7372  2662
388  60–150  65–210 11560  2992
396.8 250–1200 750–1500 11267  7792
39557 16128
Table 2SuFI Exposure times and numbers of images

IMaX observed in various modes that differ in the number of Stokes parameters observed, the number of wavelength points and the number of integrations at each wavelength. They are designated by the following nomenclature: Letter L or V (L=longitudinal, i.e. only Stokes and are observed, V=vector, i.e. full Stokes vector observed) followed by the number of wavelength points (3, 5 and 12 were used on this flight) and the number of integrations per wavelength. The most widely used (”standard”) mode is V5-6, i.e., Stokes vector measured in 5 wavelengths (4 in the line and 1 in the continuum), with 6 images accumulated per wavelength point. The cadence of the observations, the achieved noise level and the amount of time for which each mode was observed is given in Table 3. Note that the noise level refers to the Stokes continuum and is given for the unreconstructed data. After reconstruction, the noise level increases by roughly a factor of 3. The effective spatial resolution of the reconstructed data at 0.15– arcsec, however, is considerably higher and results in the resolution of both, small-scale magnetic and convective features (Lagg et al. 2010, Khomenko et al. 2010).

The reduction of IMaX data and the various calibrations of the instrument are described by Martínez Pillet et al. (2010). Different versions of IMaX data are produced. These include level-0 raw data, level-1 fully reduced, but not reconstructed data and level-2 data, which were reconstructed by deconvolution using a modified Wiener filter and the point spread function (PSF) of the optical system derived from calibration applying phase diversity. The reconstruction of the IMaX data always makes use of an averaged wavefront, so that IMaX level-2 data correspond to SuFI level-3 data.

Date cadence noise Total
Mode [s] [] [min]
V5-6 33 553
V5-3 18 180
V3-6 20 13
L12-2 31 64
L3-2 8 42
Table 3Time spans and cadences of various IMaX modes

4. First results

The Sun was extremely quiet during the entire flight of Sunrise, so that almost all of the Sunrise data correspond to internetwork regions with occasional network elements.

4.1. Results from SuFI data

Figure 1.— a) Images of a patch of quiet Sun near disk centre recorded by the SuFI instrument in wavelength bands centred on 397 nm, 388 nm, 312 nm, 300 nm and 214 nm (from left to right). The grey scale has been individually set to cover 3 times the RMS range of each image. b) Same as panel a, but right at the solar limb. The Ca H image (397 nm) is plotted with an enhanced brightness scale for the off-limb parts in order to reveal spicules. Owing to the low light level, no 214 nm data are available at this position.

Images of the quiet Sun at disk centre in all 5 SuFI wavelengths are shown in Fig. 1a, whose grey scale is saturated at for each wavelength in order to allow a better intercomparison of the granulation, at the cost of overexposing the bright points (this figure shows the same solar scene as Fig. 13 of Gandorfer et al. 2010, but with a different brightness scaling). The brightness scale (see the gray-scale bars above the individual frames) already indicates the large rms contrasts of the imaged granulation (see Hirzberger et al., 2010a, for a quantitative analysis). The images at 300 nm, 312 nm and 388 nm display rather similar granulation patterns and prominent bright points (BPs), especially in the network feature near the centre of the frame. Even in the 214 nm image, granulation is well identified, although intergranular lanes are no longer that clearly visible. It cannot be completely ruled out, however, that this is due to a larger spatial smearing. In addition, the granules display more substructure in the 214 nm images. This is in contrast to the statement made by Hersé (1979) that “at nm we find only bright grains of a mean area of 4 arcsec and a mean contrast of 47%”. Hersé identified them with facular grains. The reason for the difference may partly lie in strong underexposure of the granulation (see his Figs. 4 and 5). There is a hint of granule-like structures in the lower right part of his Fig. 7 (only visible in the printed paper).

Bright points are particularly prominent at 214 nm (their contrasts are highest at this wavelength, see Riethmüller et al., 2010), but somewhat more diffuse. This may be due to image jitter accumulated during the 30 s exposure and the greater height of formation of this wavelength, combined with the expansion of magnetic features with height.

Ca ii H 397 nm displays a variety of features including reversed granulation, oscillations and waves, and magnetic bright points. The leftmost frame of Fig. 1a reveals that although many of the intergranular lanes are indeed bright, some appear as dark stripes with bright lanes on either side of them. Examples can be found extending between the coordinates and , from to , or from to . Time series of Ca ii H images (see the movie M1 in the supplementary electronic material) reveals that these dark Ca ii H lanes are rather short lived. Possibly they are a result of the interaction of the reversed granulation with waves.

At an intermediate heliocentric angle of of roughly 0.72 (not shown) the granulation appears very similar at 300, 312 and 388 nm. At 214 nm, however, structures intermediate between reversed and normal granulation appear, with bright lanes (on the centreward side) and darker granule bodies.

One interpretation of the different behaviour displayed by 214 nm data is that the radiation in this band is formed (on average) at a greater height. A rough estimate, made including line opacities, can be obtained from Fig. 1 of Vernazza et al. (1976). It shows that around 300 nm the radiation is formed roughly 50 km above , while at 214 nm it is formed around 250 km above . The true value at 214 nm is rather tricky to determine owing to the broad filter profile, the presence of the ionization edge of Aluminium within the filter range and the great density of spectral lines at these wavelengths. We speculate that 214 nm wavelength radiation is formed sufficiently high in the atmosphere that first signs of reversed granulation become visible at disk centre (e.g. filling in of intergranular lanes in Fig. 1a). As we move towards the limb the reversed granulation becomes more apparent.

Reversed granulation is seen clearly in Ca ii H, but many of the finer-scale features are lost. The intermediate nature of 214 nm is illustrated by the fact that the best correspondence of 397 nm is found with 214 nm (coherence values are a factor of 1.5 higher than those between, e.g., 300 nm and 397 nm).

Images at 4 SuFI wavelengths at the solar limb, in the general vicinity of the south solar pole are shown in Fig. 1b. Obviously the structures at the south limb, although reminiscent of granules, are considerably smaller than those further away from the limb, in qualitative agreement with earlier results (Sánchez Cuberes et al. 2003). This smaller size could be related to greater prominence of granular sub-structure at the limb. In addition, polar faculae are visible, e.g. around , 20 and 36. Fibrils can be seen emanating from the faculae at and spicules are clearly present off the solar limb (they became visible after the off-limb brightness was enhanced). Some of the spicule-like structures appear strongly inclined to the vertical and even slightly bent, so that they may actually be parts of quiet-Sun loops.

4.2. Results from IMaX data

Figure 2.— IMaX data. Clockwise from upper left: continuum intensity at 5250.4 Å, line-of-sight velocity, net linear polarization (see text for an exact definition), line-averaged Stokes , (see main text for a definition), obtained from Fe I 5250.2 Å. All images are based on reconstructed data except for the linear polarization image.

Figure 2 shows a snapshot of IMaX data products; clockwise from upper left: continuum intensity, LOS velocity, total net linear polarization averaged over the line, , and the similarly averaged Stokes , (see below). All quantities are based on reconstructed data, with the exception of , for which the unreconstructed data are shown (reconstruction increases the noise, so that a number of significant patches in the unreconstructed image are no longer sufficiently above the noise in the reconstructed data). and are defined as:

Here runs over the 4 wavelength points inside the spectral line, takes on values of for to 4 (see Martínez Pillet et al., 2010) and is the continuum intensity averaged over the FOV.

The RMS contrast of quiet-Sun granulation obtained from IMaX continuum data is around 13.5%, which is a mark of the outstanding quality of the IMaX images. Due to the longer wavelength at which IMaX observes, the contrast is lower than in the SuFI images. In particular, the bright points are less clearly visible, having a contrast comparable to that of granulation (see Riethmüller et al., 2010). The velocity images prominently display a network of sharp intergranular downflow lanes (appearing bright in the figure). Upflow velocities are often largest in small patches, corresponding to small, often bright granules or parts of larger granules, although there is no one-to-one relationship between upflow speed and brightness (e.g. Hirzberger 2001). In addition, a larger-scale velocity pattern composed of 5–10 patches superposed on the granulation reflects the -mode oscillations (see Roth et al., 2010, for a detailed analysis of the -modes, and Bello González et al., 2010, for a determination of the vertical energy flux transported by high frequency waves). These enhance the granular down- and upflows according to the oscillation phase, as can be seen from the time series displayed in the movie M2 (in the additional electronic material).

The largest patch of strong Stokes  near the bottom centre of the frame is a network element. Other network patches are also present in the frame, but are less prominent, e.g. at (23, 31) in Fig. 2. Most of the Stokes  signal, however, is due to internetwork fields. These are clearly composed of rather localized (point-like or crinkled line-like) mixed-polarity magnetic patches. The sizes of internetwork magnetic features deduced from Stokes  is typically below 1, with many having sizes lying close to the spatial resolution of roughly 0.15. The internetwork fields clearly outline cell-like structures with ”mesogranular” scale sizes (cf. de Wijn et al. 2005; 2008) that range from 2-3 in regions with strong internetwork flux to 5-15 in regions with particularly low flux. There are hints of smaller cells there, which, however, cannot be confirmed without an in-depth analysis. At many locations both magnetic polarities are located in close proximity to each other.

displays a meso- to supergranular scale pattern. The larger apparent scale of this pattern (compared to that displayed by Stokes ) may result from the fact that, on average, features have a lower S/N ratio than Stokes- patches, so that we are probably missing more features of the former. The spatial distribution is also different, with the most prominent Stokes- elements being absent in the linear polarization signal. The opposite is generally not the case. The more prominent patches of linear polarization are usually associated with (weaker) patches of Stokes (see Danilovic et al. 2010a).

Stokes- movies, such as that displayed in M2, reveal how dynamic the quiet Sun magnetic field is, with the weaker magnetic features, i.e., those in the internetwork, being particularly dynamic. Constant appearance and disappearance of patches of Stokes is observed along the edges of the “mesogranular scale” internetwork cells. As pointed out by de Wijn et al. (2008), weaker features often disappear and reappear close by. This could be an effect of features dropping below the noise level by weakening and appearing again as they get more concentrated. However, we also expect the emergence and submergence of magnetic flux to take place on timescales of minutes. This is supported by the analysis of . Strong patches of linear polarization are found to be rather short-lived and are often associated with bipolar magnetic features suggestive of small-scale loops (Danilovic et al. 2010a). Some of these are also associated with supersonic velocities, presumably in the form of upflows (Borrero et al. 2010). There are also locations at which fresh flux emerges in a complex patch of mixed polarities (e.g. Zhang et al. 1998), similar to the simulations of Cheung et al. (2008), but on a small scale. An example in our data is given at around (36, 18) around the middle of the time series.

The Sunrise/IMaX Stokes- movie displays qualitative similarities to movies of the vertical magnetic field in turbulent dynamo simulations (Vögler and Schüssler 2007), although both the spatial and the temporal scales are quite different. However, both display vortical motions of weak magnetic field patches (see Bonet et al. 2010 for a study of the vortices in these data; cf. Steiner et al. 2010). In the simulations, the mixed-polarity magnetic fields are distributed between granules. There the individual magnetic features live less than the granule lifetime. In the observations both size scales and lifetimes are significantly larger/longer. Quiet-Sun magnetic fields in both, the turbulent dynamo simulations and Hinode observations, display a self-similar (fractal) spatial distribution (Pietarila Graham et al. 2009). This supports the idea that structure and evolution over different scales (of our observations and the MHD simulations) are similar.

The unreconstructed Stokes map has a noise level of 3.0 G, with a conversion from Stokes  to following Martínez Pillet et al. (2010). Similarly, the reconstructed map has 9.8 G. The average above in the reconstructed and non-reconstructed maps (i.e. averaged over all pixels, but with the signal set to zero in all pixels with ), converted into LOS field component, , gives G above G and G for  G. The index “rec” implies reconstructed data, “nonrec” non-reconstructed. Thus, in spite of the more than 3 times higher noise, the reconstructed image displays almost twice the amount of magnetic flux. If we set the same limit for both maps, namely , then is reduced to 1.96 G. This means that 3.7 times more magnetic flux is found if the effective spatial resolution is increased by roughly a factor of 2. This difference persists also if the threshold is set higher, so that it cannot be due to contributions from pixels containing noise .

This strong increase in magnetic flux suggests that the magnetic polarities are mixed at very small scales approaching the resolution limit of the present data, so that even moderate additional smearing leads to a substantial decrease in the amount of visible flux. This dependence on resolution is much stronger than found for the quiet Sun at lower spatial resolution by Krivova and Solanki (2004), and seemingly also than found by Pietarila-Graham et al. (2009). Quantitative comparisons are difficult, however, since the reconstruction does not, strictly speaking, change the spatial resolution, but rather significantly enhances the MTF at frequencies below the cutoff.

The increase in magnetic field strength also implies a considerably higher magnetic energy in the chromosphere (Wiegelmann et al. 2010).

4.3. Combination of SuFI and IMaX data

Figure 3 displays a set of cotemporal and cospatial SuFI and IMaX data. Clearly, the prominent, small-scale photospheric bright points in the photospheric SuFI image (2nd frame from left) are all associated with brightenings in Ca ii H and with Stokes- signals, although in some cases these signals are not particularly strong (cf. Riethmüller et al. 2010). Note that in the internetwork these bright points are still very sharp also in Ca ii H, which distinguishes them from more wave-like features, which are in general not quite so concentrated. In the 525 nm continuum, however, they are barely detectable. After identifying them in the 300 nm image they can, however, be made out as points with a similar brightness as the surrounding granules.

The relationship between Ca ii H brightness and magnetic field is more complex. While some of the magnetic features are associated with Ca ii H brightenings, e.g. in the network feature near the bottom of the frame, or other magnetic features related to internetwork bright points, there are numerous magnetic features in the internetwork, e.g. at (3.5, 8.5) or between (7.5, 8.5) and (7.5, 11), which are not associated with Ca ii H brightenings. Such Ca-dark magnetic features often display mixed polarity and are closely related to patches of (one striking case is discussed by Danilovic et al. 2010b). Conversely, there are numerous Ca ii H brightenings which do not seem to have any magnetic counterpart in the photosphere. Examples are at (12, 14) and at (10, 22). Although some of them can appear relatively concentrated, on the whole they are clearly more diffuse than the brightenings due to magnetic features. These may correspond to H bright points (Rutten and Uitenbroek 1991), although without further spectral information we cannot be sure.

Figure 3.— Cotemporal SuFI and IMaX data showing the SuFI field of view. From left to right: continuum intensity at 525.04 nm (IMaX data), intensity in the 300 nm band (SuFI data), intensity in the Ca ii H line core (SuFI data), net circular polarization deduced from Fe I 525.02 nm (IMaX data), total net linear polarization (; IMaX data), line-of-sight velocity (IMaX). All images have been reconstructed except for the linear-polarization image.

5. Conclusion

The Sunrise observatory has provided high-quality, high-resolution images, Dopplergrams and vector magnetograms at different positions on the solar disk. The extremely low solar activity level at that time means that these data mainly enable new insights into the quiet Sun. Here we provided a qualitative description of these data and some of the features visible in them. This, together with the more quantitative analyses described in the following papers in this special issue, has already led to new insights into the magnetism, convection and oscillations and waves in the quiet Sun. Given the richness and quality of the data and the fact that so far only a very small fraction of them have been analyzed, we expect many more results to follow. A flight of Sunrise during a period of higher solar activity is greatly to be welcomed.

We thank R. Rutten for helpful discussions on the structure of the chromosphere. The German contribution to Sunrise is funded by the Bundesministerium für Wirtschaft und Technologie through Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), Grant No. 50 OU 0401, and by the Innovationsfond of the President of the Max Planck Society (MPG). The Spanish contribution has been funded by the Spanish MICINN under projects ESP2006-13030-C06 and AYA2009-14105-C06 (including European FEDER funds). The HAO contribution was partly funded through NASA grant number NNX08AH38G. This work has been partially supported by the WCU grant No. R31-10016 funded by the Korean Ministry of Education, Science & Technology.

6. References


  • Barthol et al. (2010) Barthol, P., Gandorfer, A., Solanki, S. K., Schüssler, M., Chares, B., et al. 2010, Solar Phys., submitted
  • Bello González et al. (2010) Bello González, N., Franz, M., Martínez Pillet, V., Bonet, J. A., del Toro Iniesta, J. C., et al. 2010, ApJL, this issue
  • Berkefeld et al. (2010) Berkefeld, T., Schmidt, W., Soltau, D., Bell, A., Doerr, H. P., et al. 2010, Solar Phys., submitted
  • Bernasconi et al. (2002) Bernasconi, P. N., Rust, D. M., Georgoulis, M. K., & Labonte, B. J. 2002, Sol. Phys., 209, 119
  • Bonet et al. (2010) Bonet, J. A., Márquez, I., Sánchez Almeida, J., Palacios, J., Martínez Pillet, V., et al. 2010, ApJ, this issue
  • Borrero et al. (2010) Borrero, J. M., Martínez Pillet, V., Schlichenmaier, R., Solanki, S. K., Bonet, J. A., et al. ApJ, this issue
  • Cheung et al. (2008) Cheung, M. C. M., Schüssler, M., Tarbell, T. D., & Title, A. M. 2008, ApJ, 687, 1373
  • Danielson (1961) Danielson, R. E. 1961, ApJ, 134, 275
  • Danilovic et al. (2010a) Danilovic, S., Beeck, B., Pietarila, A., Martínez Pillet, V., Schüssler, M., et al. 2010a, ApJ, this issue
  • Danilovic et al. (2010b) Danilovic, S., Pietarila, A., Riethmüller, T. L., Lagg, A., Schüssler, M., et al. 2010b, ApJ, this issue
  • Gandorfer et al. (2010) Gandorfer, A., Grauf, B., Barthol, P., Riethmüller, T. L., Solanki, S. K., et al. 2010, Solar Phys., submitted
  • Georgoulis et al. (2002) Georgoulis, M. K., Rust, D. M., Bernasconi, P. N., & Schmieder, B. 2002, ApJ, 575, 506
  • Herse (1979) Hersé, M. 1979, Sol. Phys., 63, 35
  • Hirzberger et al. (2001) Hirzberger, J., Koschinsky, M., Kneer, F., & Ritter, C. 2001, A&A, 367, 1011
  • Hirzberger et al. (2010a) Hirzberger, J., Feller, A., Riethmüller, T. L., Schüssler, M., Borrero, J. M., et al. 2010a, ApJ, this issue
  • Hirzberger et al. (2010b) Hirzberger, J., Feller, A., Riethmüller, T. L., Gandorfer, A., Solanki, S. K., et al. 2010b, A&A, to be submitted
  • Karpinsky (1989) Karpinsky, V. N. 1989, Nature 341, 311
  • Khomenko et al. (1970) Khomenko, E., Martínez Pillet, V., Solanki, S. K., del Toro Inhiesta, J. C., Gandorfer, A., et al. 2010, ApJ, this issue
  • Krat et al. (1970) Krat, V. A., Dulkin, L. Z., Karpinsky, V. N., Majorov, E. P., Motenko, B. N., et al. 1970, Astron. Circ. 597, 1
  • Krat et al. (1972) Krat, V. A., Karpinsky, V. N., & Pravdjuk, L. M. 1972, Sol. Phys., 26, 305
  • Krivova & Solanki (2004) Krivova, N. A., & Solanki, S. K. 2004, A&A, 417, 1125
  • Lagg et al. (2010) Lagg, A., Solanki, S. K., Riethmüller, T. L., Martínez Pillet, V., Hirzberger, J., et al. 2010, ApJ, this issue
  • Lites et al. (2004) Lites, B. W., Scharmer, G. B., Berger, T. E., & Title, A. M. 2004, Sol. Phys., 221, 65
  • Löfdahl (2004) Löfdahl M. G. & Scharmer, G. B. 1994, Astron. Astrophys. Suppl. 107, 243
  • Martínez Pillet et al. (2010) Martínez Pillet, V., del Toro Iniesta, J. C., Álvarez-Herrero, A., Domingo, V., Bonet, J.A., et al. 2010, Solar Phys., submitted
  • Mehltretter (1976) Mehltretter, J. P. 1976, Sterne und Weltraum, 15, 44
  • Mehltretter (1978) Mehltretter, J. P. 1978, A&A, 62, 311
  • Paxman (1978) Paxman, R. G. and Schulz, T. J. , & Fienup, J. R. 1992, J. Optical Soc. America A, 9, 1072
  • Pietarila Graham et al. (2009) Pietarila Graham, J., Danilovic, S., & Schüssler, M. 2009, ApJ, 693, 1728
  • Riethmueller et al. (2010) Riethmüller, T. L., Solanki, S. K., Martínez Pillet, V., Hirzberger, J., Feller, A., et al. 2010, ApJ, this issue
  • Roth et al. (2010) Roth, M., Franz, M., Bello-González, N., Martínez Pillet, V., Bonet, J. A., et al. 2010, ApJL, this issue
  • Rust et al. (1996) Rust, D. M., Murphy, G., Strohbehn, K., & Keller, C. U. 1996, Sol. Phys., 164, 403
  • Rutten & Uitenbroek (1991) Rutten, R. J., & Uitenbroek, H. 1991, Sol. Phys., 134, 15
  • Samain & Lemaire (1985) Samain, D., & Lemaire, P. 1985, Ap&SS, 115, 227
  • Sánchez Cuberes et al. (2003) Sánchez Cuberes, M., Vázquez, M., Bonet, J. A., & Sobotka, M. 2003, A&A, 397, 1075
  • Schwarzschild (1959) Schwarzschild, M. 1959, ApJ, 130, 345
  • Staath & Lemaire (1995) Staath, E., & Lemaire, P. 1995, A&A, 295, 517
  • Steiner et al. (2010) Steiner, O., Franz, M., Bello-Gonzáles, N., Nutto, Ch., Rezaei, R., et al. 2010, ApJ, this issue
  • Vernazza et al. (1976) Vernazza, J. E., Avrett, E. H., & Loeser, R. 1976, ApJS, 30, 1
  • Vögler & Schüssler (2007) Vögler, A., & Schüssler, M. 2007, A&A, 465, L43
  • Wiegelmann et al. (2005) Wiegelmann, T., Solanki, S. K., Borrero, J. M., Danilovic, S., Hirzberger, J., et al. 2010, ApJ, this issue
  • de Wijn et al. (2005) de Wijn, A. G., Rutten, R. J., Haverkamp, E. M. W. P., Sütterlin, P. 2005, A&A, 441, 1183
  • de Wijn et al. (2008) de Wijn, A. G., Lites, B. W., Berger, T. E., Frank, Z. A., Tarbell, T. D., & Ishikawa, R. 2008, ApJ, 684, 1469
  • Wittmann & Mehltretter (1977) Wittmann, A., & Mehltretter, J. P. 1977, A&A, 61, 75
  • Zhang et al. (1998) Zhang, J., Lin, G., Wang, J., Wang, H., & Zirin, H. 1998, A&A, 338, 322

Appendix A Electronic supplementary material

Movie M1: Timeseries of Ca ii H images recorded by SuFI on Sunrise. The movie runs for 19 min solar time (see counter at the top). The brightness scale (grey scale at the right) is given relative to the brightness averaged over the time series.

Movie M2: Continuum intensity, line-of-sight velocity, linear polarization , and circular polarization deduced from IMaX measurements in the Fe I 525.02 nm line (clockwise from top left). See the main text (Sect. 4.2) for the definitions of and . The movie shows a region around arcsec in size. The edges have been slightly cut-off, since they are reduced by the reconstruction (this can partly still be seen in the various plotted quantities).

Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description