Reiners, Ansgar

[["dc.bibliographiccitation.firstpage","43"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","902"],["dc.contributor.author","Kochukhov, Oleg"],["dc.contributor.author","Reiners, Ansgar"],["dc.date.accessioned","2021-04-14T08:32:26Z"],["dc.date.available","2021-04-14T08:32:26Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.3847/1538-4357/abb2a2"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/83922"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1538-4357"],["dc.title","The Magnetic Field of the Active Planet-hosting M Dwarf AU Mic"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1039"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1046"],["dc.bibliographiccitation.volume","486"],["dc.contributor.author","Bean, Jacob L."],["dc.contributor.author","Benedict, G. Fritz"],["dc.contributor.author","Charbonneau, David"],["dc.contributor.author","Homeier, Derek"],["dc.contributor.author","Taylor, D. C."],["dc.contributor.author","McArthur, Barbara E."],["dc.contributor.author","Seifahrt, Andreas"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Reiners, Ansgar"],["dc.date.accessioned","2018-11-07T11:12:17Z"],["dc.date.available","2018-11-07T11:12:17Z"],["dc.date.issued","2008"],["dc.description.abstract","We present time series photometry for six partial transits of GJ 436b obtained with the Fine Guidance Sensor instrument on the Hubble Space Telescope (HST). Our analysis of these data yields independent estimates of the host star's radius R- = 0.505(-0.029) (+0.020) R-circle dot, and the planet's orbital period P = 2.643882(-0.000058)(+0.000060) d, orbital inclination i = 85.80 degrees(-0.25 degrees),(+ 0.21 degrees), mean central transit time T-c = 2 454 455.279241(-0.00025)(+0.00026) HJD, and radius Rp = 4.90(-0.33)(+ 0.45) R-circle plus. The radius we determine for the planet is larger than the previous findings from analyses of an infrared light curve obtained with the Spitzer Space Telescope. Although this discrepancy has a 92% formal significance (1.7s), it might be indicative of systematic errors that still influence the analyses of even the highest-precision transit light curves. Comparisons of all the measured radii to theoretical models suggest that GJ 436b has a H/ He envelope of similar to 10% by mass. We point out the similarities in structure between this planet and Uranus and Neptune and discuss possible parallels between these planets' formation environments and dynamical evolution. We also find that the transit times for GJ 436b are constant to within 10s over the 11 planetary orbits that the HST data span. However, the ensemble of published values exhibits a long-term drift and our mean transit time is 128 s later than that expected from the Spitzer ephemeris. The sparseness of the currently available data hinders distinguishing between an error in the orbital period or perturbations arising from an additional object in the system as the cause of the apparent trend. Assuming the drift is due to an error in the orbital period we obtain an improved estimate for it of P = 2.643904 +/- 0.000005 d. This value and our measured transit times will serve as important benchmarks in future studies of the GJ 436 system."],["dc.identifier.doi","10.1051/0004-6361:200810013"],["dc.identifier.fs","513377"],["dc.identifier.isi","000258326500046"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9395"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/53628"],["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","A Hubble Space Telescope transit light curve for GJ 436b"],["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","290"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Solar System Research"],["dc.bibliographiccitation.lastpage","310"],["dc.bibliographiccitation.volume","44"],["dc.contributor.author","Lammer, H."],["dc.contributor.author","Hanslmeier, A."],["dc.contributor.author","Schneider, J."],["dc.contributor.author","Stateva, I. K."],["dc.contributor.author","Barthelemy, M."],["dc.contributor.author","Belu, A."],["dc.contributor.author","Bisikalo, D. V."],["dc.contributor.author","Bonavita, M."],["dc.contributor.author","Eybl, Vera Theresa"],["dc.contributor.author","du Foresto, V. Coude"],["dc.contributor.author","Fridlund, M."],["dc.contributor.author","Dvorak, R."],["dc.contributor.author","Eggl, Siegfried"],["dc.contributor.author","Griessmeier, J.-M."],["dc.contributor.author","Guedel, M."],["dc.contributor.author","Guenther, Eckhard"],["dc.contributor.author","Hausleitner, W."],["dc.contributor.author","Holmstrom, M."],["dc.contributor.author","Kallio, E."],["dc.contributor.author","Khodachenko, M. L."],["dc.contributor.author","Konovalenko, A. A."],["dc.contributor.author","Krauss, Sandra"],["dc.contributor.author","Ksanfomality, L. V."],["dc.contributor.author","Kulikov, Yu N."],["dc.contributor.author","Kyslyakova, K."],["dc.contributor.author","Leitzinger, M."],["dc.contributor.author","Liseau, R."],["dc.contributor.author","Lohinger, E."],["dc.contributor.author","Odert, P."],["dc.contributor.author","Palle, E."],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Rucker, H. O."],["dc.contributor.author","Sarda, Nicolas"],["dc.contributor.author","Seckbach, J."],["dc.contributor.author","Shematovich, V. I."],["dc.contributor.author","Sozzetti, A."],["dc.contributor.author","Tavrov, A."],["dc.contributor.author","Xiang-Gruess, M."],["dc.date.accessioned","2018-11-07T08:41:06Z"],["dc.date.available","2018-11-07T08:41:06Z"],["dc.date.issued","2010"],["dc.description.abstract","After the discovery of more than 400 planets beyond our Solar System, the characterization of exoplanets as well as their host stars can be considered as one of the fastest growing fields in space science during the past decade. The characterization of exoplanets can only be carried out in a well coordinated interdisciplinary way which connects planetary science, solar/stellar physics and astrophysics. We present a status report on the characterization of exoplanets and their host stars by reviewing the relevant space- and ground-based projects. One finds that the previous strategy changed from space mission concepts which were designed to search, find and characterize Earth-like rocky exoplanets to: A statistical study of planetary objects in order to get information about their abundance, an identification of potential target and finally its analysis. Spectral analysis of exoplanets is mandatory, particularly to identify bio-signatures on Earth-like planets. Direct characterization of exoplanets should be done by spectroscopy, both in the visible and in the infrared spectral range. The way leading to the direct detection and characterization of exoplanets is then paved by several questions, either concerning the pre-required science or the associated observational strategy."],["dc.identifier.doi","10.1134/S0038094610040039"],["dc.identifier.isi","000281685700003"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/19396"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Maik Nauka/interperiodica/springer"],["dc.relation.issn","0038-0946"],["dc.title","Exoplanet status report: Observation, characterization and evolution of exoplanets and their host stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A22"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","645"],["dc.contributor.author","Yan, F."],["dc.contributor.author","Wyttenbach, A."],["dc.contributor.author","Casasayas-Barris, N."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Pallé, E."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Mollière, P."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Nortmann, L."],["dc.contributor.author","Molaverdikhani, K."],["dc.contributor.author","Chen, G."],["dc.contributor.author","Snellen, I. A. G."],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Huang, C."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Cont, D."],["dc.contributor.author","Khalafinejad, S."],["dc.contributor.author","Khaimova, J."],["dc.contributor.author","López-Puertas, M."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Oshagh, M."],["dc.contributor.author","Pedraz, S."],["dc.contributor.author","Stangret, M."],["dc.date.accessioned","2021-04-14T08:30:14Z"],["dc.date.available","2021-04-14T08:30:14Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/202039302"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/83161"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Detection of the hydrogen Balmer lines in the ultra-hot Jupiter WASP-33b"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1034"],["dc.bibliographiccitation.issue","10"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","1036"],["dc.bibliographiccitation.volume","328"],["dc.contributor.author","Reiners, Ansgar"],["dc.date.accessioned","2018-11-07T10:57:54Z"],["dc.date.available","2018-11-07T10:57:54Z"],["dc.date.issued","2007"],["dc.description.abstract","Differential rotation can be detected in single line profiles of stars rotating more rapidly than about v sin i = 10 km s(-1) with the Fourier transform technique. This allows to search for differential rotation in large samples to look for correlations between differential rotation and other stellar parameters. I analyze the fraction of differentially rotating stars as a function of color, rotation, and activity in a large sample of F-type stars. Color and rotation exhibit a correlation with differential rotation in the sense that more stars are rotating differentially in the cooler, less rapidly rotating stars. Effects of rotation and color, however, cannot be disentangled in the underlying sample. No trend with activity is found. (c) 2007 WHEY VCH Verlag GmbH & Co. KGaA, Weinheim."],["dc.identifier.doi","10.1002/asna.200710853"],["dc.identifier.isi","000252230600012"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/50359"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","5th Potsdam Thinkshop on Meridional Flow, Differential Rotation, Solar and Stellar Activity"],["dc.relation.eventlocation","Potsdam, GERMANY"],["dc.relation.issn","1521-3994"],["dc.relation.issn","0004-6337"],["dc.title","Differential rotation in F stars"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","852"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.lastpage","857"],["dc.bibliographiccitation.volume","707"],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Giampapa, Mark S."],["dc.date.accessioned","2018-11-07T11:21:07Z"],["dc.date.available","2018-11-07T11:21:07Z"],["dc.date.issued","2009"],["dc.description.abstract","We report the results of the analysis of high-resolution photospheric line spectra obtained with the UVES instrument on the VLT for a sample of 15 solar-type stars selected from a recent survey of the distribution of H and K chromospheric line strengths in the solar-age open cluster M67. We find upper limits to the projected rotation velocities that are consistent with solar-like rotation (i. e., v sin i less than or similar to 2-3 km s(-1)) for objects with Ca II chromospheric activity within the range of the contemporary solar cycle. Two solar-type stars in our sample exhibit chromospheric emission well in excess of even solar maximum values. In one case, Sanders 1452, we measure a minimum rotational velocity of v sin i = 4 +/- 0.5 km s(-1), or over twice the solar equatorial rotational velocity. The other star with enhanced activity, Sanders 747, is a spectroscopic binary. We conclude that high activity in solar-type stars in M67 that exceeds solar levels is likely due to more rapid rotation rather than an excursion in solar-like activity cycles to unusually high levels. We estimate an upper limit of 0.2% for the range of brightness changes occurring as a result of chromospheric activity in solar-type stars and, by inference, in the Sun itself. We discuss possible implications for our understanding of angular momentum evolution in solar-type stars, and we tentatively attribute the rapid rotation in Sanders 1452 to a reduced braking efficiency."],["dc.identifier.doi","10.1088/0004-637X/707/1/852"],["dc.identifier.isi","000272162900070"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/55696"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","0004-637X"],["dc.title","THE ORIGIN OF ENHANCED ACTIVITY IN THE SUNS OF M67"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","L31"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","813"],["dc.contributor.author","Yadav, Rakesh K."],["dc.contributor.author","Christensen, Ulrich R."],["dc.contributor.author","Morin, Julien"],["dc.contributor.author","Gastine, Thomas"],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Poppenhaeger, Katja"],["dc.contributor.author","Wolk, Scott J."],["dc.date.accessioned","2018-11-07T09:48:58Z"],["dc.date.available","2018-11-07T09:48:58Z"],["dc.date.issued","2015"],["dc.description.abstract","Despite the lack of a shear-rich tachocline region, low-mass fully convective (FC) stars are capable of generating strong magnetic fields, indicating that a dynamo mechanism fundamentally different from the solar dynamo is at work in these objects. We present a self-consistent three-dimensional model of magnetic field generation in low-mass FC stars. The model utilizes the anelastic magnetohydrodynamic equations to simulate compressible convection in a rotating sphere. A distributed dynamo working in the model spontaneously produces a dipole-dominated surface magnetic field of the observed strength. The interaction of this field with the turbulent convection in outer layers shreds it, producing small-scale fields that carry most of the magnetic flux. The Zeeman-Doppler-Imaging technique applied to synthetic spectropolarimetric data based on our model recovers most of the large-scale field. Our model simultaneously reproduces the morphology and magnitude of the large-scale field as well as the magnitude of the small-scale field observed on low-mass FC stars."],["dc.description.sponsorship","DFG [SFB 963/A17, SPP 1488]; NASA [GO4-15011X]"],["dc.identifier.doi","10.1088/2041-8205/813/2/L31"],["dc.identifier.isi","000365035000009"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/35418"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","2041-8213"],["dc.relation.issn","2041-8205"],["dc.title","Explaining the Coexistence of Large-Scale and Small-Scale Magnetic Fields in fully Convective Stars"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","2717"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","2731"],["dc.bibliographiccitation.volume","438"],["dc.contributor.author","Jeffers, Sandra V."],["dc.contributor.author","Barnes, J. R."],["dc.contributor.author","Jones, Hugh R. A."],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Pinfield, David J."],["dc.contributor.author","Marsden, S. C."],["dc.date.accessioned","2018-11-07T09:43:19Z"],["dc.date.available","2018-11-07T09:43:19Z"],["dc.date.issued","2014"],["dc.description.abstract","Theoretical predictions suggest that the distribution of planets in very young stars could be very different to that typically observed in Gyr old systems that are the current focus of radial velocity surveys. However, the detection of planets around young stars is hampered by the increased stellar activity associated with young stars, the signatures of which can bias the detection of planets. In this paper, we place realistic limitations on the possibilities for detecting planets around young active G and K dwarfs. The models of stellar activity based on tomographic imaging of the G dwarf HD 141943 and the K1 dwarf AB Dor also include contributions from plage and many small random starspots. Our results show that the increased stellar activity levels present on young solar-type stars strongly impacts the detection of Earth-mass and Jupiter-mass planets and that the degree of activity jitter is directly correlated with stellar v sin i. We also show that for G and K dwarfs, the distribution of activity in individual stars is more important than the differences in induced radial velocities as a function of spectral type. We conclude that Jupiter-mass planets can be detected close-in around fast-rotating young active stars, Neptune-mass planets around moderate rotators and that Super-Earths are only detectable around very slowly rotating stars. The effects of an increase in stellar activity jitter by observing younger stars can be compensated for by extending the observational base-line to at least 100 epochs."],["dc.identifier.doi","10.1093/mnras/stt1950"],["dc.identifier.isi","000332038000001"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/34159"],["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","Is it possible to detect planets around young active G and K dwarfs?"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A13"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","522"],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Christensen, Ulrich R."],["dc.date.accessioned","2018-11-07T08:37:21Z"],["dc.date.available","2018-11-07T08:37:21Z"],["dc.date.issued","2010"],["dc.description.abstract","Very little is known about magnetic fields of extrasolar planets and brown dwarfs. We use the energy flux scaling law presented by Christensen et al. to calculate the evolution of average magnetic fields in extrasolar planets and brown dwarfs under the assumption of fast rotation, which is probably the case for most of them. We find that massive brown dwarfs of about 70 M(Jup) can have fields of a few kilo-Gauss during the first few hundred Million years. These fields can grow by a factor of two before they weaken after deuterium burning has stopped. Brown dwarfs with weak deuterium burning and extrasolar giant planets start with magnetic fields between similar to 100G and similar to 1 kG at the age of a few Myr, depending on their mass. Their magnetic field weakens steadily until after 10 Gyr it has shrunk by about a factor of 10. We use observed X-ray luminosities to estimate the age of the known extrasolar giant planets that are more massive than 0.3 M(Jup) and closer than 20 pc. Taking into account the age estimate, and assuming sun-like wind-properties and radio emission processes similar to those at Jupiter, we calculate their radio flux and its frequency. The highest radio flux we predict comes out as 700 mJy at a frequency around 150 MHz for tau Boo b, but the flux is below 60 mJy for the rest. Most planets are expected to emit radiation between a few Mhz and up to 100 MHz, well above the ionospheric cutoff frequency."],["dc.description.sponsorship","DFG [RE 1664/4-1]"],["dc.identifier.doi","10.1051/0004-6361/201014251"],["dc.identifier.fs","581128"],["dc.identifier.isi","000284153100019"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9673"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/18509"],["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","A magnetic field evolution scenario for brown dwarfs and giant planets"],["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","A50"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","640"],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Kaminski, A."],["dc.contributor.author","Rodríguez López, C."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Azzaro, M."],["dc.contributor.author","Stahl, O."],["dc.contributor.author","Kossakowski, D."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Becerril Jarque, S."],["dc.contributor.author","Rodríguez, E."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Seifert, W."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Schäfer, S."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Cortés-Contreras, M."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Hatzes, A."],["dc.contributor.author","Henning, T."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Kürster, M."],["dc.contributor.author","Lafarga, M."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Morales, J. C."],["dc.contributor.author","Schmitt, J. H. M. M."],["dc.contributor.author","Schweitzer, A."],["dc.contributor.author","Solano, E."],["dc.date.accessioned","2021-04-14T08:24:23Z"],["dc.date.available","2021-04-14T08:24:23Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/202038031"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/81267"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.title.alternative","Measuring precise radial velocities in the near infrared: The example of the super-Earth CD Cet b"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]