Shulyak, Denis V.

[["dc.bibliographiccitation.artnumber","A14"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","537"],["dc.contributor.author","Krticka, J."],["dc.contributor.author","Mikulasek, Z."],["dc.contributor.author","Lueftinger, T."],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Zverko, J."],["dc.contributor.author","Ziznovsky, J."],["dc.contributor.author","Sokolov, N. A."],["dc.date.accessioned","2018-11-07T09:15:33Z"],["dc.date.available","2018-11-07T09:15:33Z"],["dc.date.issued","2012"],["dc.description.abstract","Context. The spectral energy distribution (SED) in chemically peculiar stars may be significantly affected by their abundance anomalies. The observed SED variations are usually assumed to be a result of inhomogeneous surface distribution of chemical elements, flux redistribution and stellar rotation. However, the direct evidence for this is still only scarce. Aims. We aim to identify the processes that determine the SED and its variability in the UV and visual spectral domains of the helium-weak star CU Vir. Methods. We used the TLUSTY model atmospheres calculated for the appropriate surface chemical composition to obtain the emergent flux and predict the rotationally modulated flux variability of the star. Results. We show that most of the light variations in the vby filters of the Stromgren photometric system are a result of the uneven surface distribution of silicon, chromium, and iron. Our models are only able to explain a part of the variability in the u filter, however. The observed UV flux distribution is very well reproduced, and the models are able to explain most of the observed features in the UV light curve, except for the region 2000-2500 angstrom, where the amplitude of the observed light variations is higher than predicted. The variability observed in the visible is merely a faint gleam of that in the UV. While the amplitude of the light curves reaches only several hundredths of magnitude in the visual domain, it reaches about 1 mag in the UV. Conclusions. The visual and UV light variability of CU Vir is caused by the flux redistribution from the far UV to near UV and visible regions, inhomogeneous distribution of the elements and stellar rotation. Bound-free transitions of silicon and bound-bound transitions of iron and chromium contribute the most to the flux redistribution. This mechanism can explain most of the rotationally modulated light variations in the filters centred on the Paschen continuum and on the UV continuum of the star CU Vir. However, another mechanism(s) has to be invoked to fully explain the observed light variations in the u filter and in the region 2000-2500 angstrom."],["dc.identifier.doi","10.1051/0004-6361/201117490"],["dc.identifier.fs","596777"],["dc.identifier.isi","000300416800014"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9584"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/27719"],["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","Modelling of the ultraviolet and visual SED variability in the hot magnetic Ap star CU Virginis"],["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.issue","8"],["dc.bibliographiccitation.journal","Nature Astronomy"],["dc.bibliographiccitation.volume","1"],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Engeln, A."],["dc.contributor.author","Malo, L."],["dc.contributor.author","Yadav, R."],["dc.contributor.author","Morin, J."],["dc.contributor.author","Kochukhov, O."],["dc.date.accessioned","2020-12-10T18:09:53Z"],["dc.date.available","2020-12-10T18:09:53Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1038/s41550-017-0184"],["dc.identifier.eissn","2397-3366"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/73791"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Strong dipole magnetic fields in fast rotating fully convective stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","4094"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","4104"],["dc.bibliographiccitation.volume","445"],["dc.contributor.author","Fossati, Luca"],["dc.contributor.author","Kolenberg, Katrien"],["dc.contributor.author","Shulyak, Denis V."],["dc.contributor.author","Elmasli, A."],["dc.contributor.author","Tsymbal, V."],["dc.contributor.author","Barnes, T. G."],["dc.contributor.author","Guggenberger, Elisabeth"],["dc.contributor.author","Kochukhov, Oleg"],["dc.date.accessioned","2018-11-07T09:31:09Z"],["dc.date.available","2018-11-07T09:31:09Z"],["dc.date.issued","2014"],["dc.description.abstract","The stellar parameters of RR Lyrae stars vary considerably over a pulsation cycle, and their determination is crucial for stellar modelling. We present a detailed spectroscopic analysis of the pulsating star RR Lyr, the prototype of its class, over a complete pulsation cycle, based on high-resolution spectra collected at the 2.7-m telescope of McDonald Observatory. We used simultaneous photometry to determine the accurate pulsation phase of each spectrum and determined the effective temperature, the shape of the depth-dependent microturbulent velocity, and the abundance of several elements, for each phase. The surface gravity was fixed to 2.4. Element abundances resulting from our analysis are stable over the pulsation cycle. However, a variation in ionization equilibrium is observed around minimum radius. We attribute this mostly to a dynamical acceleration contributing to the surface gravity. Variable turbulent convection on time-scales longer than the pulsation cycle has been proposed as a cause for the Blazhko effect. We test this hypothesis to some extent by using the derived variable depth-dependent microturbulent velocity profiles to estimate their effect on the stellar magnitude. These effects turn out to be wavelength dependent and much smaller than the observed light variations over the Blazhko cycle: if variations in the turbulent motions are entirely responsible for the Blazhko effect, they must surpass the scales covered by the microturbulent velocity. This work demonstrates the possibility of a self-consistent spectroscopic analysis over an entire pulsation cycle using static atmosphere models, provided one takes into account certain features of a rapidly pulsating atmosphere."],["dc.identifier.doi","10.1093/mnras/stu2044"],["dc.identifier.isi","000346963300058"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/31475"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Oxford Univ Press"],["dc.relation.issn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","An in-depth spectroscopic analysis of RR Lyr Variations over the pulsation cycle"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","3471"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","3478"],["dc.bibliographiccitation.volume","449"],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Sokoloff, D."],["dc.contributor.author","Kitchatinov, L."],["dc.contributor.author","Moss, D."],["dc.date.accessioned","2018-11-07T09:56:36Z"],["dc.date.available","2018-11-07T09:56:36Z"],["dc.date.issued","2015"],["dc.description.abstract","Recent progress in observational studies of magnetic activity in M dwarfs urgently requires support from ideas of stellar dynamo theory. We propose a strategy to connect observational and theoretical studies. In particular, we suggest four magnetic configurations that appear relevant to dwarfs from the viewpoint of the most conservative version of dynamo theory, and discuss observational tests to identify the configurations observationally. As expected, any such identification contains substantial uncertainties. However, the situation in general looks less pessimistic than might be expected. Several identifications between the phenomenology of individual stars and dynamo models are suggested. Remarkably, all models discussed predict substantial surface magnetic activity at rather high stellar latitudes. This prediction looks unexpected from the viewpoint of our experience observing the Sun (which of course differs in some fundamental ways from these late-type dwarfs). We stress that a fuller understanding of the topic requires a long-term (at least 15 years) monitoring of M dwarfs by Zeeman-Doppler imaging."],["dc.description.sponsorship","RFBR [12-02-00170-a, 13-02-00277]; [SFB 963]"],["dc.identifier.doi","10.1093/mnras/stv585"],["dc.identifier.isi","000355342000012"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/36994"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Oxford Univ Press"],["dc.relation.issn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","Towards understanding dynamo action in M dwarfs"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","2548"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","2557"],["dc.bibliographiccitation.volume","418"],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Seifahrt, Andreas"],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Kochukhov, Oleg"],["dc.contributor.author","Piskunov, Nikolai E."],["dc.date.accessioned","2018-11-07T08:49:03Z"],["dc.date.available","2018-11-07T08:49:03Z"],["dc.date.issued","2011"],["dc.description.abstract","Close M dwarf binaries and higher multiples allow the investigation of rotational evolution and mean magnetic flux unbiased from scatter in inclination angle and age since the orientation of the spin axis of the components is most likely parallel and the individual systems are coeval. Systems composed of an early-type (M0.0-M4.0) and a late-type (M4.0-M8.0) component offer the possibility to study differences in rotation and magnetism between partially and fully convective stars. We have selected 10 of the closest dM systems to determine the rotation velocities and the mean magnetic field strengths based on spectroscopic analysis of FeH lines of Wing-Ford transitions at 1 mu m observed with Very Large Telescope/CRIRES. We also studied the quality of our spectroscopic model regarding atmospheric parameters including metallicity. A modified version of the Molecular Zeeman Library (MZL) was used to compute Landeg-factors for FeH lines. Magnetic spectral synthesis was performed with the synmast code. We confirmed previously reported findings that less massive M dwarfs are braked less effectively than objects of earlier types. Strong surface magnetic fields were detected in primaries of four systems (GJ 852, GJ 234, LP 717-36 and GJ 3322), and in the secondary of the triple system GJ 852. We also confirm strong 2-kG magnetic field in the primary of the triple system GJ 2005. No fields could be accurately determined in rapidly rotating stars with nu sin i > 10 km s(-1). For slowly and moderately rotating stars, we find the surface magnetic field strength to increase with the rotational velocity nu sin i which is consistent with other results from studying field stars."],["dc.identifier.doi","10.1111/j.1365-2966.2011.19644.x"],["dc.identifier.isi","000298088100036"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/21363"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-blackwell"],["dc.relation.issn","0035-8711"],["dc.title","Rotation, magnetism and metallicity of M dwarf systems"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","811"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","823"],["dc.bibliographiccitation.volume","471"],["dc.contributor.author","Barnes, J. R."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Haswell, C. A."],["dc.contributor.author","Jones, H. R. A."],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Pavlenko, Ya. V."],["dc.contributor.author","Jenkins, J. S."],["dc.date.accessioned","2020-12-10T18:19:26Z"],["dc.date.available","2020-12-10T18:19:26Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1093/mnras/stx1482"],["dc.identifier.eissn","1365-2966"],["dc.identifier.issn","0035-8711"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/75245"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Surprisingly different star-spot distributions on the near equal-mass equal-rotation-rate stars in the M dwarf binary GJ 65 AB"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","318"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astrophysical Bulletin"],["dc.bibliographiccitation.lastpage","327"],["dc.bibliographiccitation.volume","70"],["dc.contributor.author","Valeev, A. F."],["dc.contributor.author","Antonyuk, K. A."],["dc.contributor.author","Pit, N. V."],["dc.contributor.author","Solovyev, V. Ya."],["dc.contributor.author","Burlakova, T. E."],["dc.contributor.author","Moskvitin, A. S."],["dc.contributor.author","Grauzhanina, A. O."],["dc.contributor.author","Gadelshin, D. R."],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Fatkhullin, T. A."],["dc.contributor.author","Galazutdinov, G. A."],["dc.contributor.author","Malogolovets, E. V."],["dc.contributor.author","Beskin, G. M."],["dc.contributor.author","Karpov, S. V."],["dc.contributor.author","Dyachenko, V. V."],["dc.contributor.author","Rastegaev, D. A."],["dc.contributor.author","Rzaev, A. Kh."],["dc.contributor.author","Valyavin, G. G."],["dc.date.accessioned","2018-11-07T09:54:55Z"],["dc.date.available","2018-11-07T09:54:55Z"],["dc.date.issued","2015"],["dc.description.abstract","We present the results of photometric observations of the weak magnetic white dwarf WD 0009+501. The observations were carried out for two years with the 1-m telescopes of the Special and Crimean Astrophysical Observatories. As a result of these observations, we detected regular V -band luminosity variations with a period of P a parts per thousand 8 hours. The amplitude of the variability is stable on timescales greater than two years and amounts to 11 +/- 1 mmag. The difference in the variability amplitude from observations with different telescopes is 1-3 mmag. The result is interpreted within the concept of a rotation-modulated variability of magnetic properties of the star's atmosphere. We also discuss a possible variability due to the presence of planetary companions around stars of this type. The results of monitoring were used to explore the capabilities of the telescopes for exoplanet investigation. We studied the dependences between the characteristic times of exposures, magnitudes of the objects, and a threshold level of the expected variability amplitudes for all the telescopes involved in our program. A program of exoplanet monitoring with the mentioned telescopes was drawn up for the next few years based on the results of the study."],["dc.identifier.doi","10.1134/S1990341315030104"],["dc.identifier.isi","000359742200010"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/36641"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Maik Nauka/interperiodica/springer"],["dc.relation.issn","1990-3421"],["dc.relation.issn","1990-3413"],["dc.title","Detection of regular low-amplitude photometric variability of the magnetic dwarf WD0009+501. on the possibility of photometric investigation of exoplanets on the basis of 1-meter class telescopes of the special and crimean astrophysical observatories"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A88"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","520"],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Ryabchikova, Tanya"],["dc.contributor.author","Kildiyarova, R."],["dc.contributor.author","Kochukhov, Oleg"],["dc.date.accessioned","2018-11-07T08:39:29Z"],["dc.date.available","2018-11-07T08:39:29Z"],["dc.date.issued","2010"],["dc.description.abstract","Aims. Among the known Ap stars, HD 101065 is probably one of the most interesting objects, demonstrating very rich spectra of rare-earth elements (REE). Strongly peculiar photometric parameters of this star can not be fully reproduced by any modern theoretical calculations, even those accounting for realistic chemistry of its atmosphere. In this study we investigate a role of missing REE line opacity and construct a self-consistent atmospheric model based on accurate abundance and chemical stratification analysis. Methods. We employed the LLMODELS stellar model atmosphere code together with DDAFIT and SYNTHMAG software packages to derive homogeneous and stratified abundances for 52 chemical elements and to construct a self-consistent model of HD 101065 atmosphere. The opacity in REE lines is accounted for in details, by using up-to-date extensive theoretical calculations. Results. We show that REE elements play a key role in the radiative energy balance in the atmosphere of HD 101065, leading to the strong suppression of the Balmer jump and energy redistribution very different from that of normal stars. Introducing new line lists of REEs allowed us to reproduce, for the first time, spectral energy distribution of HD 101065 and achieve a better agreement between the unusually small observed Stromgren c(1) index and the model predictions. Using combined photometric and spectroscopic approaches and based on the iterative procedure of abundance and stratification analysis we find effective temperature of HD 101065 to be T(eff) = 6400 K."],["dc.identifier.doi","10.1051/0004-6361/200913750"],["dc.identifier.fs","581149"],["dc.identifier.isi","000283064200095"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9685"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/19008"],["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","Realistic model atmosphere and revised abundances of the coolest Ap star HD 101065"],["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","428"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","441"],["dc.bibliographiccitation.volume","338"],["dc.contributor.author","Kochukhov, Oleg"],["dc.contributor.author","Petit, P."],["dc.contributor.author","Strassmeier, K. G."],["dc.contributor.author","Carroll, T. A."],["dc.contributor.author","Fares, R."],["dc.contributor.author","Folsom, C. P."],["dc.contributor.author","Jeffers, Sandra V."],["dc.contributor.author","Korhonen, H."],["dc.contributor.author","Monnier, J. D."],["dc.contributor.author","Morin, Julien"],["dc.contributor.author","Rosen, L."],["dc.contributor.author","Roettenbacher, R. M."],["dc.contributor.author","Shulyak, D."],["dc.date.accessioned","2018-11-07T10:24:19Z"],["dc.date.available","2018-11-07T10:24:19Z"],["dc.date.issued","2017"],["dc.description.abstract","Magnetic fields are essential ingredients of many physical processes in the interiors and envelopes of cool stars. Yet their direct detection and characterization is notoriously difficult, requiring high-quality observations and advanced analysis techniques. Significant progress has been recently achieved by several types of direct magnetic field studies on the surfaces of cool, active stars. In particular, complementary techniques of field topology mapping with polarization data and total magnetic flux measurements from intensity spectra have been systematically applied to different classes of active stars, leading to interesting and occasionally controversial results. In this paper, we summarize the current status of direct magnetic field studies of cool stars and investigations of surface inhomogeneities caused by the field, based on the material presented at the Cool Stars 19 splinter session."],["dc.identifier.doi","10.1002/asna.201713310"],["dc.identifier.isi","000400944700007"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/42634"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.relation.issn","1521-3994"],["dc.relation.issn","0004-6337"],["dc.title","Surface magnetism of cool stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A151"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","537"],["dc.contributor.author","Nesvacil, N."],["dc.contributor.author","Lueftinger, T."],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Obbrugger, M."],["dc.contributor.author","Weiss, W."],["dc.contributor.author","Drake, N. A."],["dc.contributor.author","Hubrig, S."],["dc.contributor.author","Ryabchikova, Tanya"],["dc.contributor.author","Kochukhov, Oleg"],["dc.contributor.author","Piskunov, Nikolai E."],["dc.contributor.author","Polosukhina, N."],["dc.date.accessioned","2018-11-07T09:15:34Z"],["dc.date.available","2018-11-07T09:15:34Z"],["dc.date.issued","2012"],["dc.description.abstract","Context. In atmospheres of magnetic main-sequence stars, the diffusion of chemical elements leads to a number of observed anomalies, such as abundance spots across the stellar surface. Aims. The aim of this study was to derive a detailed picture of the surface abundance distribution of the magnetic chemically peculiar star HD 3980. Methods. Based on high-resolution, phase-resolved spectroscopic observations of the magnetic A-type star HD 3980, the inhomogeneous surface distribution of 13 chemical elements (Li, O, Si, Ca, Cr, Mn, Fe, La, Ce, Pr, Nd, Eu, and Gd) has been reconstructed. The INVERS12 code was used to invert the rotational variability in line profiles to elemental surface distributions. Results. Assuming a centered, dominantly dipolar magnetic field configuration, we find that Li, O, Mg, Pr, and Nd are mainly concentrated in the area of the magnetic poles and depleted in the regions around the magnetic equator. The high abundance spots of Si, La, Ce, Eu, and Gd are located between the magnetic poles and the magnetic equator. Except for La, which is clearly depleted in the area of the magnetic poles, no obvious correlation with the magnetic field has been found for these elements otherwise. Ca, Cr, and Fe appear enhanced along the rotational equator and the area around the magnetic poles. The intersection between the magnetic and the rotational equator constitutes an exception, especially for Ca and Cr, which are depleted in that region. Conclusions. No obvious correlation between the theoretically predicted abundance patterns and those determined in this study could be found. This can be attributed to a lack of up-to-date theoretical models, especially for rare earth elements."],["dc.identifier.doi","10.1051/0004-6361/201117097"],["dc.identifier.fs","596778"],["dc.identifier.isi","000300416800151"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9586"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/27720"],["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","Multi-element Doppler imaging of the CP2 star HD 3980"],["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"]]