Nicklas, Harald E.

[["dc.bibliographiccitation.firstpage","1050"],["dc.bibliographiccitation.issue","10"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","1056"],["dc.bibliographiccitation.volume","337"],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Gomory, P."],["dc.contributor.author","Manrique, S. J. Gonzalez"],["dc.contributor.author","Kuckein, C."],["dc.contributor.author","Kavka, J."],["dc.contributor.author","Kucera, A."],["dc.contributor.author","Schwartz, P."],["dc.contributor.author","Vaskova, R."],["dc.contributor.author","Berkefeld, T."],["dc.contributor.author","Collados Vera, M."],["dc.contributor.author","Denker, C."],["dc.contributor.author","Feller, A."],["dc.contributor.author","Hofmann, Albrecht W."],["dc.contributor.author","Lagg, A."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Suarez, D."],["dc.contributor.author","Pastor Yabar, A."],["dc.contributor.author","Rezaei, R."],["dc.contributor.author","Schlichenmaier, R."],["dc.contributor.author","Schmidt, D."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Sigwarth, M."],["dc.contributor.author","Sobotka, M."],["dc.contributor.author","Solanki, Parth K."],["dc.contributor.author","Soltau, D."],["dc.contributor.author","Staude, J."],["dc.contributor.author","Strassmeier, K. G."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","von der Luhe, O."],["dc.contributor.author","Waldmann, T."],["dc.date.accessioned","2018-11-07T10:06:05Z"],["dc.date.available","2018-11-07T10:06:05Z"],["dc.date.issued","2016"],["dc.description.abstract","Arch filament systems occur in active sunspot groups, where a fibril structure connects areas of opposite magnetic polarity, in contrast to active region filaments that follow the polarity inversion line. We used the GREGOR Infrared Spectrograph (GRIS) to obtain the full Stokes vector in the spectral lines SiI lambda 1082.7 nm, He I lambda 1083.0 nm, and Ca I lambda 1083.9 nm. We focus on the near-infrared calcium line to investigate the photospheric magnetic field and velocities, and use the line core intensities and velocities of the helium line to study the chromospheric plasma. The individual fibrils of the arch filament system connect the sunspot with patches of magnetic polarity opposite to that of the spot. These patches do not necessarily coincide with pores, where the magnetic field is strongest. Instead, areas are preferred not far from the polarity inversion line. These areas exhibit photospheric downflows of moderate velocity, but significantly higher downflows of up to 30 km s(-1) in the chromospheric helium line. Our findings can be explained with new emerging flux where the matter flows downward along the field lines of rising flux tubes, in agreement with earlier results. (C) 2016 WILEY-VCH Verlag GmbH& Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201612432"],["dc.identifier.isi","000391297900010"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39025"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","12th Potsdam Thinkshop Conference on Dynamic Sun - Exploring the Many Facets of Solar Eruptive Events"],["dc.relation.eventlocation","Potsdam, GERMANY"],["dc.relation.issn","1521-3994"],["dc.relation.issn","0004-6337"],["dc.title","Spectropolarimetric observations of an arch filament system with the GREGOR solar telescope"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["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","28"],["dc.bibliographiccitation.issue","S327"],["dc.bibliographiccitation.journal","Proceedings of the International Astronomical Union"],["dc.bibliographiccitation.lastpage","33"],["dc.bibliographiccitation.volume","12"],["dc.contributor.author","Manrique, S. J. González"],["dc.contributor.author","Denker, C."],["dc.contributor.author","Kuckein, C."],["dc.contributor.author","Yabar, A. Pastor"],["dc.contributor.author","Collados, M."],["dc.contributor.author","Verma, M."],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Diercke, A."],["dc.contributor.author","Fischer, C. E."],["dc.contributor.author","Gömöry, P."],["dc.contributor.author","González, N. Bello"],["dc.contributor.author","Schlichenmaier, R."],["dc.contributor.author","Armas, M. Cubas"],["dc.contributor.author","Berkefeld, T."],["dc.contributor.author","Feller, A."],["dc.contributor.author","Hoch, S."],["dc.contributor.author","Hofmann, A."],["dc.contributor.author","Lagg, A."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Suárez, D. Orozco"],["dc.contributor.author","Schmidt, D."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Sigwarth, M."],["dc.contributor.author","Sobotka, M."],["dc.contributor.author","Solanki, S. K."],["dc.contributor.author","Soltau, D."],["dc.contributor.author","Staude, J."],["dc.contributor.author","Strassmeier, K. G."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","von der Lühe, O."],["dc.contributor.author","Waldmann, T."],["dc.date.accessioned","2020-12-10T15:22:25Z"],["dc.date.available","2020-12-10T15:22:25Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1017/S1743921317000278"],["dc.identifier.eissn","1743-9221"],["dc.identifier.issn","1743-9213"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/73394"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Flows along arch filaments observed in the GRIS ‘very fast spectroscopic mode’"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","L13"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","L17"],["dc.bibliographiccitation.volume","386"],["dc.contributor.author","Israel, G. L."],["dc.contributor.author","Hummel, W."],["dc.contributor.author","Covino, S."],["dc.contributor.author","Campana, S."],["dc.contributor.author","Appenzeller, I."],["dc.contributor.author","Gassler, W."],["dc.contributor.author","Mantel, K. H."],["dc.contributor.author","Marconi, G."],["dc.contributor.author","Mauche, C. W."],["dc.contributor.author","Munari, U."],["dc.contributor.author","Negueruela, I."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Rupprecht, G."],["dc.contributor.author","Smart, R. L."],["dc.contributor.author","Stahl, O."],["dc.contributor.author","Stella, L."],["dc.date.accessioned","2018-11-07T10:30:45Z"],["dc.date.available","2018-11-07T10:30:45Z"],["dc.date.issued","2002"],["dc.description.abstract","We carried out optical observations of the field of the X-ray pulsator RX J0806.3+1527. A blue V = 21.1 star was found to be the only object consistent with the X-ray position. VLT FORS spectra revealed a blue continuum with no intrinsic absorption lines. Broad (v similar to 1500 km s(-1)), low equivalent width (similar to -1 divided by -6 Angstrom) emission lines from the HeII Pickering series were clearly detected. B, V and R time-resolved photometry revealed the presence of similar to15% pulsations at the similar to321 s X-ray period, confirming the identification. These findings, together with the period stability and absence of any additional modulation in the 1 min-5 hr period range, argue in favour of the orbital interpretation of the 321 s pulsations. The most likely scenario is thus that RX J0806.3+1527 is a double degenerate system of the AM CVn class. This would make RX J0806.3+1527 the shortest orbital period binary currently known and one of the best candidates for gravitational wave detection."],["dc.identifier.doi","10.1051/0004-6361:20020314"],["dc.identifier.isi","000175132100004"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43939"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.title","RX J0806.3+1527: A double degenerate binary with the shortest known orbital period (321s)"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","880"],["dc.bibliographiccitation.issue","9"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","893"],["dc.bibliographiccitation.volume","333"],["dc.contributor.author","Puschmann, K. G."],["dc.contributor.author","Denker, C."],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Al Erdogan, N."],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Bauer, S. M."],["dc.contributor.author","Beck, C."],["dc.contributor.author","Gonzalez, N. Bello"],["dc.contributor.author","Collados, M."],["dc.contributor.author","Hahn, T."],["dc.contributor.author","Hirzberger, J."],["dc.contributor.author","Hofmann, Albrecht W."],["dc.contributor.author","Louis, R. E."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Okunev, O."],["dc.contributor.author","Martinez Pillet, V."],["dc.contributor.author","Popow, E."],["dc.contributor.author","Seelemann, T."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","Wittmann, A. D."],["dc.contributor.author","Woche, M."],["dc.date.accessioned","2018-11-07T09:04:01Z"],["dc.date.available","2018-11-07T09:04:01Z"],["dc.date.issued","2012"],["dc.description.abstract","The GREGOR Fabry-Perot Interferometer (GFPI) is one of three first-light instruments of the German 1.5-meter GREGOR solar telescope at the Observatorio del Teide, Tenerife, Spain. The GFPI uses two tunable etalons in collimated mounting. Thanks to its large-format, high-cadence CCD detectors with sophisticated computer hard- and software it is capable of scanning spectral lines with a cadence that is sufficient to capture the dynamic evolution of the solar atmosphere. The field-of-view (FOV) of 50 ' x38 ' is well suited for quiet Sun and sunspot observations. However, in the vector spectropolarimetric mode the FOV reduces to 25 ' x38 '. The spectral coverage in the spectroscopic mode extends from 530-860 nm with a theoretical spectral resolution of R approximate to 250 000, whereas in the vector spectropolarimetric mode the wavelength range is at present limited to 580-660 nm. The combination of fast narrow-band imaging and post-factum image restoration has the potential for discovery science concerning the dynamic Sun and its magnetic field at spatial scales down to similar to 50 km on the solar surface. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201211734"],["dc.identifier.isi","000310799500015"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/25018"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.relation.issn","0004-6337"],["dc.title","The GREGOR Fabry-Perot Interferometer"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.subtype","letter_note"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1057"],["dc.bibliographiccitation.issue","10"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","1063"],["dc.bibliographiccitation.volume","337"],["dc.contributor.author","Manrique, S. J. Gonzalez"],["dc.contributor.author","Kuckein, C."],["dc.contributor.author","Pastor Yabar, A."],["dc.contributor.author","Collados, M."],["dc.contributor.author","Denker, C."],["dc.contributor.author","Fischer, C. E."],["dc.contributor.author","Gomory, P."],["dc.contributor.author","Diercke, A."],["dc.contributor.author","Gonzalez, N. Bello"],["dc.contributor.author","Schlichenmaier, R."],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Berkefeld, T."],["dc.contributor.author","Feller, A."],["dc.contributor.author","Hoch, S."],["dc.contributor.author","Hofmann, Albrecht W."],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Lagg, A."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Orozco Suarez, D."],["dc.contributor.author","Schmidt, D."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Sigwarth, M."],["dc.contributor.author","Sobotka, M."],["dc.contributor.author","Solanki, Parth K."],["dc.contributor.author","Soltau, D."],["dc.contributor.author","Staude, J."],["dc.contributor.author","Strassmeier, K. G."],["dc.contributor.author","Verma, M."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","von der Luhe, O."],["dc.contributor.author","Waldmann, T."],["dc.date.accessioned","2018-11-07T10:06:06Z"],["dc.date.available","2018-11-07T10:06:06Z"],["dc.date.issued","2016"],["dc.description.abstract","The new generation of solar instruments provides better spectral, spatial, and temporal resolution for a better understanding of the physical processes that take place on the Sun. Multiple-component profiles are more commonly observed with these instruments. Particularly, the He i 10830 triplet presents such peculiar spectral profiles, which give information on the velocity and magnetic fine structure of the upper chromosphere. The purpose of this investigation is to describe a technique to efficiently fit the two blended components of the He i 10830 triplet, which are commonly observed when two atmospheric components are located within the same resolution element. The observations used in this study were taken on 2015 April 17 with the very fast spectroscopic mode of the GREGOR Infrared Spectrograph (GRIS) attached to the 1.5-m GREGOR solar telescope, located at the Observatorio del Teide, Tenerife, Spain. We apply a double-Lorentzian fitting technique using Levenberg-Marquardt least-squares minimization. This technique is very simple and much faster than inversion codes. Line-of-sight Doppler velocities can be inferred for a whole map of pixels within just a few minutes. Our results show sub-and supersonic downflow velocities of up to 32 km s(-1) for the fast component in the vicinity of footpoints of filamentary structures. The slow component presents velocities close to rest. (C) 2016 WILEY-VCH Verlag GmbH& Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201512433"],["dc.identifier.isi","000391297900011"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39026"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","12th Potsdam Thinkshop Conference on Dynamic Sun - Exploring the Many Facets of Solar Eruptive Events"],["dc.relation.eventlocation","Potsdam, GERMANY"],["dc.relation.issn","1521-3994"],["dc.relation.issn","0004-6337"],["dc.title","Fitting peculiar spectral profiles in He I 10830 angstrom absorption features"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","796"],["dc.bibliographiccitation.issue","9"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","809"],["dc.bibliographiccitation.volume","333"],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","von der Luehe, O."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","Denker, C."],["dc.contributor.author","Solanki, Parth K."],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Gonzalez, N. Bello"],["dc.contributor.author","Berkefeld, Th."],["dc.contributor.author","Collados, M."],["dc.contributor.author","Fischer, A."],["dc.contributor.author","Halbgewachs, C."],["dc.contributor.author","Heidecke, F."],["dc.contributor.author","Hofmann, Albrecht W."],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Lagg, A."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Popow, E."],["dc.contributor.author","Puschmann, K. G."],["dc.contributor.author","Schmidt, D."],["dc.contributor.author","Sigwarth, M."],["dc.contributor.author","Sobotka, M."],["dc.contributor.author","Soltau, D."],["dc.contributor.author","Staude, J."],["dc.contributor.author","Strassmeier, K. G."],["dc.contributor.author","Waldmann, T."],["dc.date.accessioned","2018-11-07T09:03:59Z"],["dc.date.available","2018-11-07T09:03:59Z"],["dc.date.issued","2012"],["dc.description.abstract","The 1.5 m telescope GREGOR opens a new window to the understanding of solar small-scale magnetism. The first light instrumentation includes the Gregor Fabry Perot Interferometer (GFPI), a filter spectro-polarimeter for the visible wavelength range, the GRating Infrared Spectro-polarimeter (GRIS) and the Broad-Band Imager (BBI). The excellent performance of the first two instruments has already been demonstrated at the Vacuum Tower Telescope. GREGOR is Europes largest solar telescope and number 3 in the world. Its all-reflective Gregory design provides a large wavelength coverage from the near UV up to at least 5 microns. The field of view has a diameter of 150 '. GREGOR is equipped with a high-order adaptive optics system, with a subaperture size of 10 cm, and a deformable mirror with 256 actuators. The science goals are focused on, but not limited to, solar magnetism. GREGOR allows us to measure the emergence and disappearance of magnetic flux at the solar surface at spatial scales well below 100 km. Thanks to its spectro-polarimetric capabilities, GREGOR will measure the interaction between the plasma flows, different kinds of waves, and the magnetic field. This will foster our understanding of the processes that heat the chromosphere and the outer layers of the solar atmosphere. Observations of the surface magnetic field at very small spatial scales will shed light on the variability of the solar brightness. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201211725"],["dc.identifier.isi","000310799500005"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/25015"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-6337"],["dc.title","The 1.5 meter solar telescope GREGOR"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.subtype","letter_note"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1090"],["dc.bibliographiccitation.issue","10"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","1098"],["dc.bibliographiccitation.volume","337"],["dc.contributor.author","Verma, M."],["dc.contributor.author","Denker, C."],["dc.contributor.author","Boehm, F."],["dc.contributor.author","Balthasar, H."],["dc.contributor.author","Fischer, C. E."],["dc.contributor.author","Kuckein, C."],["dc.contributor.author","Gonzalez, N. Bello"],["dc.contributor.author","Berkefeld, T."],["dc.contributor.author","Collados, M."],["dc.contributor.author","Diercke, A."],["dc.contributor.author","Feller, A."],["dc.contributor.author","Manrique, S. J. Gonzalez"],["dc.contributor.author","Hofmann, Albrecht W."],["dc.contributor.author","Lagg, A."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Orozco Suarez, D."],["dc.contributor.author","Pator Yabar, A."],["dc.contributor.author","Rezaei, R."],["dc.contributor.author","Schlichenmaier, R."],["dc.contributor.author","Schmidt, D."],["dc.contributor.author","Schmidt, W."],["dc.contributor.author","Sigwarth, M."],["dc.contributor.author","Sobotka, M."],["dc.contributor.author","Solanki, Parth K."],["dc.contributor.author","Soltau, D."],["dc.contributor.author","Staude, J."],["dc.contributor.author","Strassmeier, K. G."],["dc.contributor.author","Volkmer, R."],["dc.contributor.author","von der Luhe, O."],["dc.contributor.author","Waldmann, T."],["dc.date.accessioned","2018-11-07T10:06:06Z"],["dc.date.available","2018-11-07T10:06:06Z"],["dc.date.issued","2016"],["dc.description.abstract","Improved measurements of the photospheric and chromospheric three-dimensional magnetic and flow fields are crucial for a precise determination of the origin and evolution of active regions. We present an illustrative sample of multi-instrument data acquired during a two-week coordinated observing campaign in August 2015 involving, among others, the GREGOR solar telescope (imaging and near-infrared spectroscopy) and the space missions Solar Dynamics Observatory (SDO) and Interface Region Imaging Spectrograph (IRIS). The observations focused on the trailing part of active region NOAA 12396 with complex polarity inversion lines and strong intrusions of opposite polarity flux. The GREGOR Infrared Spectrograph (GRIS) provided Stokes IQUV spectral profiles in the photospheric Si i.1082.7 nm line, the chromospheric He I lambda 1083.0 nm triplet, and the photospheric Ca I lambda 1083.9 nm line. Carefully calibrated GRIS scans of the active region provided maps of Doppler velocity and magnetic field at different atmospheric heights. We compare quick-look maps with those obtained with the \" Stokes Inversions based on Response functions\" (SIR) code, which furnishes deeper insight into the magnetic properties of the region. We find supporting evidence that newly emerging flux and intruding opposite polarity flux are hampering the formation of penumbrae, i.e., a penumbra fully surrounding a sunspot is only expected after cessation of flux emergence in proximity to the sunspots. (C) 2016 WILEY-VCH Verlag GmbH& Co.KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201612447"],["dc.identifier.isi","000391297900016"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39027"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","12th Potsdam Thinkshop Conference on Dynamic Sun - Exploring the Many Facets of Solar Eruptive Events"],["dc.relation.eventlocation","Potsdam, GERMANY"],["dc.relation.issn","1521-3994"],["dc.relation.issn","0004-6337"],["dc.title","Flow and magnetic field properties in the trailing sunspots of active region NOAA 12396"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","L69"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal Letters"],["dc.bibliographiccitation.volume","564"],["dc.contributor.author","Ziegler, Bodo L."],["dc.contributor.author","Bohm, A."],["dc.contributor.author","Fricke, K. J."],["dc.contributor.author","Jager, Kitty J."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Bender, R."],["dc.contributor.author","Drory, N."],["dc.contributor.author","Gabasch, A."],["dc.contributor.author","Saglia, R. P."],["dc.contributor.author","Seitz, Sebastian"],["dc.contributor.author","Heidt, J."],["dc.contributor.author","Mehlert, D."],["dc.contributor.author","Mollenhoff, C."],["dc.contributor.author","Noll, S."],["dc.contributor.author","Sutorius, E."],["dc.date.accessioned","2018-11-07T10:32:36Z"],["dc.date.available","2018-11-07T10:32:36Z"],["dc.date.issued","2002"],["dc.description.abstract","We present the B-band Tully-Fisher relation (TFR) of 60 late-type galaxies with redshifts 0.1-1. The galaxies were selected from the FORS Deep Field with a limiting magnitude of. Spatially resolved rotation curves R p 23 were derived from spectra obtained with FORS2 at the Very Large Telescope. High-mass galaxies with v(max) greater than or similar to 150 km s(-1) show little evolution, whereas the least massive systems in our sample are brighter by similar to1-2 mag compared with their local counterparts. For the entire distant sample, the TFR slope is flatter than for local field galaxies (-5.77+/-0.45 vs. -7.92+/-0.18). Thus, we find evidence for the evolution of the slope of the TFR with redshift on the 3 sigma level. This is still true when we subdivide the sample into three redshift bins. We speculate that the flatter tilt of our sample is caused by the evolution of luminosities and an additional population of blue galaxies at zgreater than or similar to0.2. The mass dependence of the TFR evolution also leads to variations for different galaxy types in magnitude-limited samples, suggesting that selection effects can account for the discrepant results of previous TFR studies on the luminosity evolution of late-type galaxies."],["dc.identifier.doi","10.1086/338962"],["dc.identifier.isi","000173167300003"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44387"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-637X"],["dc.title","The evolution of the Tully-Fisher relation of spiral galaxies"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.volume","324"],["dc.contributor.author","Kneer, F."],["dc.contributor.author","Al, N."],["dc.contributor.author","Hirzberger, J."],["dc.contributor.author","Nicklas, H."],["dc.contributor.author","Puschmann, K. G."],["dc.date.accessioned","2018-11-07T10:41:57Z"],["dc.date.available","2018-11-07T10:41:57Z"],["dc.date.issued","2003"],["dc.format.extent","302"],["dc.identifier.doi","10.1002/asna.200310102"],["dc.identifier.isi","000183506400009"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/46663"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","Workshop on From the Gregory-Coude Telescope to GREGOR - A Development from Past to Future"],["dc.relation.eventlocation","GOTTINGEN UNIV, III PHYS INST, GOTTINGEN, GERMANY"],["dc.relation.issn","0004-6337"],["dc.title","A Fabry-Perot spectrometer for high-resolution observation of the Sun"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]