Sunrise: Instrument, Mission, Data, and First Results

Solanki, S. K.; Barthol, P.; Danilović, S.; Feller, A.; Gandorfer, A.; Hirzberger, J.; Riethmüller, T. L.; Schüßler, M.; Bonet, J. A.; Pillet, V. Martı́nez; Iniesta, J. C. del Toro; Domingo, V.; Palacios, J.; Knölker, M.; González, N. Bello; Berkefeld, T.; Fränz, M.; Schmidt, Wolfgang; Title, A. M.

doi:10.1088/2041-8205/723/2/l127

Cited by 269 publications

(250 citation statements)

References 34 publications

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“…In total more than 33 h of science observation (23% of the total observing time) were obtained. Details on SuFI and IMaX observing modes, number of acquired images and duration of time series are given in Solanki et al (2010). The telescope aperture door was closed 93 times due to pointing errors exceeding 15 arcmin.…”

Section: Instrument In-flight Performancementioning

confidence: 99%

The Sunrise Mission

et al. 2010

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The first science flight of the balloon-borne Sunrise telescope took place in June 2009 from ESRANGE (near Kiruna/Sweden) to Somerset Island in northern Canada. We describe the scientific aims and mission concept of the project and give an overview and a description of the various hardware components: the 1-m main telescope with its postfocus science instruments (the UV filter imager SuFI and the imaging vector magnetograph IMaX) and support instruments (image stabilizing and light distribution system ISLiD and correlating wavefront sensor CWS), the optomechanical support structure and the instrument mounting concept, the gondola structure and the power, pointing, and telemetry systems, and the general electronics architecture. We also explain the optimization of the structural and thermal design of the complete payload. The preparations for the science flight are described, including AIV and ground calibration of the instruments. The course of events during the science flight is outlined, up to the recovery activities. Finally, the in-flight performance of the instrumentation is discussed.

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Section: Instrument In-flight Performancementioning

confidence: 99%

The Sunrise Mission

et al. 2010

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“…The Fe I line for the photospheric channel permits reliable photospheric vector magnetograms and detailed magnetic field investigations [e.g. 40]. The photospheric channel uses the same filtergraph as the chromospheric channel.…”

Section: Euv Imaging Polarimeter (Eip)mentioning

confidence: 99%

Solar magnetism eXplorer (SolmeX)

et al. 2011

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The magnetic field plays a pivotal role in many fields of Astrophysics. This is especially true for the physics of the solar atmosphere. Measuring the magnetic field in the upper solar atmosphere is crucial to understand the nature of the underlying physical processes that drive the violent dynamics of the solar coronathat can also affect life on Earth.SolmeX, a fully equipped solar space observatory for remote-sensing observations, will provide the first comprehensive measurements of the strength and direction of the magnetic field in the upper solar atmosphere. The mission consists of two spacecraft, one carrying the instruments, and another one in formation flight at a distance of about 200 m carrying the occulter to provide an artificial total solar eclipse. This will ensure high-quality coronagraphic observations above the solar limb SolmeX integrates two spectro-polarimetric coronagraphs for off-limb observations, one in the EUV and one in the IR, and three instruments for observations on the disk. The latter comprises one imaging polarimeter in the EUV for coronal studies, a spectro-polarimeter in the EUV to investigate the low corona, and an imaging spectro-polarimeter in the UV for chromospheric studies.SOHO and other existing missions have investigated the emission of the upper atmosphere in detail (not considering polarization), and as this will be the case also for missions planned for the near future. Therefore it is timely that SolmeX provides the final piece of the observational quest by measuring the magnetic field in the upper atmosphere through polarimetric observations.

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“…We estimated energy fluxes in shortperiod, acoustic waves of ∼3400 W m −2 at a height in the solar atmosphere of ∼250 km, and of 1730−2100 W m −2 at 450−600 km (see also Bello González et al 2010b). Most recently, from an analysis of high-resolution observations with the two-dimensional (2D) IMaX spectrometer (Martínez Pillet et al 2011) onboard the balloon-borne SUNRISE telescope (Barthol et al 2011;Solanki et al 2010), Bello González et al (2010c measured substantial flux in short-period waves, in the frequency range of 5.2−15 mHz, of ∼7000 W m −2 at a height of ∼200 km.…”

Section: Introductionmentioning

confidence: 99%

On acoustic and gravity waves in the solar photosphere and their energy transport

Kneer¹,

González

2011

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Aims. We study acoustic and atmospheric gravity waves in the quiet Sun to estimate their energy transport to the chromosphere. Methods. A two-dimensional time sequence from quiet Sun disc centre was analysed with simultaneous spectroscopic observations in Fe i 5576 Å and Fe i 5434 Å (both with Landé factor g = 0). We calculated response functions of the velocities for the line minimum shifts and atmospheric transmissions of waves for the two lines. For this, NLTE line formation in granular and intergranular model atmospheres from numerical simulations were performed. For the interpretation of the observed waves and for the estimates of energy fluxes, we assumed adiabatic propagation of plane waves in an isothermal model atmosphere. Fourier analyses of intensity and velocity fluctuations were carried out. They yield power, phase, and coherence as functions of frequency ν (from temporal Fourier transforms) and in the k h −ν plane (from three-dimensional transforms). The power spectra, together with the mass densities at velocity formation heights, give then the energy fluxes. Results. The rms velocities found here in the acoustic and gravity wave domains are lower by a factor ∼1.5 as in earlier work. We therefore admit a factor of 2 for an upward correction of the estimated fluxes. For acoustic waves we find: 1) upward propagating waves are present on the Sun with frequencies up to 14−15 mHz (periods U ≈ 70 s); 2) the approximation of plane adiabatic waves in an isothermal atmosphere appears adequate for estimating the energy fluxes; 3) the acoustic energy fluxes are in the same range as found in our earlier work from ground-based, two-dimensional spectroscopy, 1500−3100 W m −2 at an atmospheric height of ∼380 km and 1300−2700 W m −2 at 570 km. The energy flux carried by gravity waves is difficult to determine. We find: 1) phase and coherence spectra between continuum and velocity fluctuations show that convective overshoot and gravity waves are superimposed. We account for the convective flows using these coherence spectra. 2) At low frequencies, the vertical wavelength Λ z can be short ( 300 km), yielding large corrections for atmospheric transmissions (factors >100). We thus exclude from the flux estimates waves with |k z | > 20 Mm −1 and with vertical group velocities υ gr,z < 0.3 km s −1 . They are likely to be strongly reduced in amplitude by radiative damping. 3) With these caveats, the energy fluxes carried by gravity waves are found in the range of 4000−8200 W m −2 at 380 km and 700−1400 W m −2 at 570 km. Gravity waves thus also contribute to the energy transport into the chromosphere.

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Sunrise: Instrument, Mission, Data, and First Results

Cited by 269 publications

References 34 publications

The Sunrise Mission

The Sunrise Mission

Solar magnetism eXplorer (SolmeX)

On acoustic and gravity waves in the solar photosphere and their energy transport

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