Kneer, Franz

[["dc.bibliographiccitation.artnumber","L177"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal Letters"],["dc.bibliographiccitation.volume","597"],["dc.contributor.author","Almeida, J. S."],["dc.contributor.author","Cerdena, I. D."],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2018-11-07T10:34:47Z"],["dc.date.available","2018-11-07T10:34:47Z"],["dc.date.issued","2003"],["dc.description.abstract","We present the first simultaneous infrared (IR) and visible spectropolarimetric observations of a solar internetwork region. The Fe I lines at 6301.5, 6302.5, 15648, and 15652 Angstrom were observed, with a lag of only 1 minute, using highly sensitive spectropolarimeters operated in two different telescopes (Vacuum Tower Telescope and THEMIS at the Observatorio del Teide). Some 30% of the observed region shows IR and visible Stokes V signals above noise. These polarization signals indicate the presence of kilogauss (kG) magnetic field strengths (traced by the visible lines) coexisting with sub-kG fields (traced by the infrared lines). In addition, one-quarter of the pixels with signal have visible and IR Stokes V profiles with opposite polarity. We estimate the probability density function of finding each longitudinal magnetic field strength in the region. It has a tail of kG field strengths that accounts for most of the (unsigned) magnetic flux of the region."],["dc.identifier.isi","000186433200023"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44949"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-637X"],["dc.title","Simultaneous visible and infrared spectropolarimetry of a solar internetwork region"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1078"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1086"],["dc.bibliographiccitation.volume","378"],["dc.contributor.author","Hirzberger, J."],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2018-11-07T11:25:56Z"],["dc.date.available","2018-11-07T11:25:56Z"],["dc.date.issued","2001"],["dc.description.abstract","The radial variation of the Evershed ow in two small sunspots (NOAA 8737 and NOAA 9145) is studied by means of two-dimensional spectrograms of high spatial resolution. We find a systematic decrease of the flow velocity with photospheric height and a shift of the velocity maximum towards larger penumbral radii in higher layers but no clear correlation between ow velocity and continuum intensity. At the outer penumbral boundaries the Evershed flow ceases abruptly and even downward directed flow velocities in the deepest probed photospheric layers were found. Furthermore, granules adjacent to the penumbral boundary show a systematic redshift of their spot-side parts which is attributed to fast, eventually supersonic, downflows between them and the penumbral boundary."],["dc.identifier.doi","10.1051/0004-6361:20011156"],["dc.identifier.isi","000171897200034"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9719"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/56742"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","2D-spectroscopy of the Evershed flow in sunspots"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A92"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","509"],["dc.contributor.author","Blanco Rodríguez, J."],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2019-07-09T11:54:46Z"],["dc.date.available","2019-07-09T11:54:46Z"],["dc.date.issued","2010-01-22"],["dc.description.abstract","Aims. This study extends earlier investigations on faculae and their small-scale magnetic fields near the solar poles (polar faculae – PFe) to measurements of the magnetically sensitive infrared (IR) lines at 1.5 μm, which provide more accurate information about the magnetic field than lines in the visible spectral range. Methods. PFe were observed with the Tenerife Infrared Polarimeter (TIP II) mounted at the Vacuum Tower Telescope/Observatorio del Teide/Tenerife. Several areas at various heliocentric angles were scanned. Faculae near the solar equator (equatorial faculae – EFe) were also observed for comparison with PFe. The full Stokes vector of the line pair at 1.5 μm was measured. The magnetic field properties were determined (1) from the centre of gravity (COG); (2) with the weak field approximation (WFA); (3) assuming the strong field regime (SFR); and (4) with inversions under the hypothesis of Milne-Eddington (ME) atmospheres. Line-of-sight (LOS) velocities were determined from the COG of I profiles and from the zero-crossing of the V profiles. Results. The main findings of this work can be divided in five parts: (1) the detected PFe do not harbour sufficient magnetic flux to account for the global flux observed with other methods. (2) Near the solar limb, the apparent, measured transversal field components are most times stronger than the longitudinal components by factors of up to 10 for both PFe and EFe, as found from observations with HINODE SOT. (3) Many PFe indeed harbour kilo-G magnetic fields. Of those, more than 85% possess the same magnetic polarity as the global field. The inclinations γ of the strong fields, G in the SFR, are compatible with their vertical emergence from the solar surface. (4) The results for weaker fields, G from ME inversions, indicate a random magnetic field orientation. (5) The velocities from I profiles and V zero-crossings are in average ~0.3 km s-1 towards observer, for both PFe and EFe. The zero-crossings of V exhibit a large velocity dispersion, of up to 3 km s-1."],["dc.identifier.doi","10.1051/0004-6361/200811111"],["dc.identifier.fs","581110"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9670"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60722"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Faculae at the poles of the Sun revisited: infrared observations"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A4"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","596"],["dc.contributor.author","Franz, M."],["dc.contributor.author","Collados, M."],["dc.contributor.author","Bethge, C."],["dc.contributor.author","Schlichenmaier, R."],["dc.contributor.author","Borrero, J. M."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Lagg, A."],["dc.contributor.author","Solanki, S. K."],["dc.contributor.author","Berkefeld, T."],["dc.contributor.author","Kiess, C."],["dc.contributor.author","Rezaei, R."],["dc.contributor.author","Schmidt, Christian D."],["dc.contributor.author","Sigwarth, M."],["dc.contributor.author","Soltau, D."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","Luhe, O. von der"],["dc.contributor.author","Waldmann, T."],["dc.contributor.author","Orozco, D."],["dc.contributor.author","Pastor Yabar, A."],["dc.contributor.author","Denker, C."],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Staude, J."],["dc.contributor.author","Hofmann, A."],["dc.contributor.author","Strassmeier, K."],["dc.contributor.author","Feller, A."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Sobotka, M."],["dc.date.accessioned","2020-07-01T07:16:29Z"],["dc.date.available","2020-07-01T07:16:29Z"],["dc.date.issued","2016"],["dc.description.abstract","Context. A significant part of the penumbral magnetic field returns below the surface in the very deep photosphere. For lines in the visible, a large portion of this return field can only be detected indirectly by studying its imprints on strongly asymmetric and three-lobed Stokes V profiles. Infrared lines probe a narrow layer in the very deep photosphere, providing the possibility of directly measuring the orientation of magnetic fields close to the solar surface. Aims. We study the topology of the penumbral magnetic field in the lower photosphere, focusing on regions where it returns below the surface. Methods. We analyzed 71 spectropolarimetric datasets from Hinode and from the GREGOR infrared spectrograph. We inferred the quality and polarimetric accuracy of the infrared data after applying several reduction steps. Techniques of spectral inversion and forward synthesis were used to test the detection algorithm. We compared the morphology and the fractional penumbral area covered by reversed-polarity and three-lobed Stokes V profiles for sunspots at disk center. We determined the amount of reversed-polarity and three-lobed Stokes V profiles in visible and infrared data of sunspots at various heliocentric angles. From the results, we computed center-to-limb variation curves, which were interpreted in the context of existing penumbral models. Results. Observations in visible and near-infrared spectral lines yield a significant difference in the penumbral area covered by magnetic fields of opposite polarity. In the infrared, the number of reversed-polarity Stokes V profiles is smaller by a factor of two than in the visible. For three-lobed Stokes V profiles the numbers differ by up to an order of magnitude."],["dc.identifier.arxiv","1608.00513v2"],["dc.identifier.doi","10.1051/0004-6361/201628407"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/66810"],["dc.language.iso","en"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Magnetic fields of opposite polarity in sunspot penumbrae"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","790"],["dc.bibliographiccitation.issue","9"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","795"],["dc.bibliographiccitation.volume","333"],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2018-11-07T09:03:59Z"],["dc.date.available","2018-11-07T09:03:59Z"],["dc.date.issued","2012"],["dc.description.abstract","This contribution to the series of GREGOR inauguration articles addresses the history of the GREGOR telescope. It was obvious since a long time that the study of the atmospheric dynamics on the Sun needs telescopes with a large aperture. So the first plans to replace the 40 years old Gregory-Coude Telescope, with its 45 cm primary mirror, by a large, 1.5-meter telescope date back to 1997. After a positive review of the project by the Deutsche Forschungsgemeinschaft in 2000, the large financial support started in 2000. Unfortunately, the new technology of the Cesic mirrors was not yet ripe to produce the large primary mirror with this light-weight material. So, the project was much delayed. After recollecting for the reader several dates, I also go through some properties of GREGOR. I recall the aims of the project and discuss difficulties and ways to realise the intentions. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201211726"],["dc.identifier.isi","000310799500004"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/25014"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.relation.issn","0004-6337"],["dc.title","Hopes and expectations with GREGOR"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","741"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","757"],["dc.bibliographiccitation.volume","407"],["dc.contributor.author","Cerdena, I. D."],["dc.contributor.author","Almeida, J. S."],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2018-11-07T10:37:07Z"],["dc.date.available","2018-11-07T10:37:07Z"],["dc.date.issued","2003"],["dc.description.abstract","We analyze a time sequence of Inter-Network (IN) magnetograms observed at the solar disk center. Speckle reconstruction techniques provide a good spatial resolution (0.\"5 cutoff frequency) yet maintaining a fair sensitivity (some 20 G). Patches with signal above noise cover 60% of the observed area, most of which corresponds to intergranular lanes. The large surface covered by signal renders a mean unsigned magnetic flux density between 17 G and 21 G (1 G equivalent to 1 Mx cm(-2)). The difference depends on the spectral line used to generate the magnetograms (Fe I lambda6302.5 Angstrom or Fe I lambda6301.5 Angstrom). Such systematic difference can be understood if the magnetic structures producing the polarization have intrinsic field strengths exceeding 1 kG, and consequently, occupying only a very small fraction of the surface (some 2%). We observe both, magnetic signals changing in time scales smaller than 1 min, and a persistent pattern lasting longer than the duration of the sequence (17 min). The pattern resembles a network with a spatial scale between 5 and 10 arcsec, which we identify as the mesogranulation. The strong dependence of the polarization signals on spatial resolution and sensitivity suggests that much quiet Sun magnetic flux still remains undetected."],["dc.identifier.doi","10.1051/0004-6361:20030892"],["dc.identifier.isi","000184550300035"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9792"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/45486"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Inter-network magnetic fields observed with sub-arcsec resolution"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","373"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","378"],["dc.bibliographiccitation.volume","436"],["dc.contributor.author","Puschmann, K. G."],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2018-11-07T10:24:08Z"],["dc.date.available","2018-11-07T10:24:08Z"],["dc.date.issued","2005"],["dc.description.abstract","Our work is an attempt to fulfil one of the aims of astronomical imaging, that is, to obtain information at high angular resolution. Stars as point sources can be represented by Dirac delta-functions whose Fourier transforms contain information about the position and the (integrated) intensity at all angular frequencies. Thus, we can deconvolve unresolved images of star fields even at angular distances smaller than the diffraction limit of the telescope with which the observations are performed. We give an example of reconstruction of the image of two stars with an angular separation of a factor 2.5 less than alpha(Ra) = 1.22 x lambda/D. However, we find that super-resolution is feasible only for point sources. For extended objects the information about intensity fluctuations at angular frequencies u > u(max) = D/lambda = 1/alpha(min) is irretrievably lost. We discuss the impossibility of super-resolution for the Sun using a numerically simulated image of solar granulation. However, one can enhance the contrast of solar images, though without increasing angular resolution beyond the diffraction limit."],["dc.identifier.doi","10.1051/0004-6361:20042320"],["dc.identifier.fs","38260"],["dc.identifier.isi","000229265500035"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9858"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/42601"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","On super-resolution in astronomical imaging"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1151"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1158"],["dc.bibliographiccitation.volume","451"],["dc.contributor.author","Puschmann, K. G."],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Seelemann, T."],["dc.contributor.author","Wittmann, A. D."],["dc.date.accessioned","2019-07-09T11:54:35Z"],["dc.date.available","2019-07-09T11:54:35Z"],["dc.date.issued","2006"],["dc.description.abstract","Studies of small-scale dynamics and magnetic fields in the solar atmosphere require spectroscopy and polarimetry with high spatial resolution. For this purpose, spectrometers based on Fabry-Pérot interferometers (FPIs) have advantages over slit spectrographs. They possess a high throughput and allow fast two-dimensional, narrow-band imaging and image reconstruction of the data. In the present contribution we describe an upgrade, essentially renewal, of the Göttingen FPI spectrometer achieved during the first half of 2005. A new etalon from IC Optical Systems Ltd. (formerly Queensgate), England, with 70mm free aperture for high spectral resolution has been mounted. New CCD detectors from LaVision GmbH (Göttingen) with powerful computer hard- and software were implemented. We consider the product of signal-to-noise ratio, frame rate, and field of view as a measure of the efficiency. At low light levels, e.g. in narrow-band speckle applications, this product has increased by a factor ∼60 compared to the old system. In addition, several spectral regions can now be scanned quasi-simultaneously. We present first results obtained with the upgraded spectrometer. The efforts are undertaken to provide an up-to-date post-focus instrument for the new German 1.5m GREGOR solar telescope presently under construction at the Observatorio del Teide on Tenerife."],["dc.identifier.doi","10.1051/0004-6361:20054487"],["dc.identifier.fs","45044"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9384"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60684"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","The new Göttingen Fabry-Pérot spectrometer for two-dimensional observations of the Sun"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","L51"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","L54"],["dc.bibliographiccitation.volume","472"],["dc.contributor.author","Sánchez-Andrade Nuño, B."],["dc.contributor.author","Centeno, R."],["dc.contributor.author","Puschmann, K. G."],["dc.contributor.author","Trujillo Bueno, J."],["dc.contributor.author","Blanco Rodríguez, J."],["dc.contributor.author","Kneer, F."],["dc.date.accessioned","2019-07-09T11:54:35Z"],["dc.date.available","2019-07-09T11:54:35Z"],["dc.date.issued","2007"],["dc.description.abstract","Aims. Off-the-limb observations with high spatial and spectral resolution will help us understand the physical properties of spicules in the solar chromosphere. Methods. Spectropolarimetric observations of spicules in the He i 10 830 Å multiplet were obtained with the Tenerife Infrared Polarimeter on the German Vacuum Tower Telescope at the Observatorio del Teide (Tenerife, Spain). The analysis shows the variation of the off-limb emission profiles as a function of the distance to the visible solar limb. The ratio between the intensities of the blue and the red components of this triplet (R = Iblue/Ired) is an observational signature of the optical thickness along the light path, which is related to the intensity of the coronal irradiation. Results. We present observations of the intensity profiles of spicules above a quiet Sun region. The observable R as a function of the distance to the visible limb is also given. We have compared our observational results to the intensity ratio obtained from detailed radiative transfer calculations in semi-empirical models of the solar atmosphere assuming spherical geometry. The agreement is purely qualitative. We argue that future models of the solar chromosphere and transition region should account for the observational constraints presented here."],["dc.identifier.doi","10.1051/0004-6361:20077936"],["dc.identifier.fs","297858"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9401"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60687"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Spicule emission profiles observed in He I 10 830 Å"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1157"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1162"],["dc.bibliographiccitation.volume","360"],["dc.contributor.author","Krieg, J."],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Koschinsky, M."],["dc.contributor.author","Ritter, Carsten"],["dc.date.accessioned","2018-11-07T10:34:50Z"],["dc.date.available","2018-11-07T10:34:50Z"],["dc.date.issued","2000"],["dc.description.abstract","We present observations of granular velocities and their relation to the granular intensity pattern from the disc center of the Sun. They were obtained in June 1997 with the Vacuum Tower Telescope at the Observatorio del Teide on Tenerife. High spatial resolution, 0.\" 4-0.\" 5 for the velocities, was achieved with speckle methods applied to two-dimensional narrow-band images in Na D-2 from the \"Gottingen\" Fabry-Perot interferometer. The velocity observations refer to a geometric height of 50-200 km (above tau(5) = 1). Velocity amplitudes of +/- 2.2 km s(-1) are seen. The high velocity regions are small-scale and the upflows coincide frequently with the bright borders of granules or with small-scale brightenings. A statistical analysis reveals only a rough consistency to the -5/3 or -17/3 law of log(power) vs. log(wavenumber) expected for isotropic turbulence (cf. Espagnet et al. 1993). We consider an agreement with such power laws as accidental since the intensity and velocity power spectra found here decrease smoothly from flat ones at low wavenumbers to steep ones at high wavenumbers. The coherence of velocity and intensity fluctuation stays above 0.5 up to horizontal wavenumbers k(h) approximate to 11 Mm(-1)(corresponds to 0.\" 8) and the phase difference between intensity and velocity stays stable down to structures of 0.\" 5. While the intensity pattern exhibits a clearly non-Gaussian distribution, the velocity distribution can be represented by a Gaussian with a \"macroturbulent\" velocity of 0.825 km s(-1)"],["dc.identifier.isi","000089494500036"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44959"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.title","Granular velocities of the Sun from speckle interferometry"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]