Schüssler, Manfred

[["dc.bibliographiccitation.artnumber","A121"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","539"],["dc.contributor.author","Beeck, B."],["dc.contributor.author","Collet, R."],["dc.contributor.author","Steffen, M."],["dc.contributor.author","Asplund, M."],["dc.contributor.author","Cameron, R. H."],["dc.contributor.author","Freytag, B."],["dc.contributor.author","Hayek, W."],["dc.contributor.author","Ludwig, H.-G."],["dc.contributor.author","Schüssler, M."],["dc.date.accessioned","2019-07-09T11:54:44Z"],["dc.date.available","2019-07-09T11:54:44Z"],["dc.date.issued","2012-03-05"],["dc.description.abstract","Context. Radiative hydrodynamic simulations of solar and stellar surface convection have become an important tool for exploring the structure and gas dynamics in the envelopes and atmospheres of late-type stars and for improving our understanding of the formation of stellar spectra. Aims. We quantitatively compare results from three-dimensional, radiative hydrodynamic simulations of convection near the solar surface generated with three numerical codes (CO5BOLD, MURaM, and Stagger) and different simulation setups in order to investigate the level of similarity and to cross-validate the simulations. Methods. For all three simulations, we considered the average stratifications of various quantities (temperature, pressure, flow velocity, etc.) on surfaces of constant geometrical or optical depth, as well as their temporal and spatial fluctuations. We also compared observables, such as the spatially resolved patterns of the emerging intensity and of the vertical velocity at the solar optical surface as well as the center-to-limb variation of the continuum intensity at various wavelengths. Results. The depth profiles of the thermodynamical quantities and of the convective velocities as well as their spatial fluctuations agree quite well. Slight deviations can be understood in terms of differences in box size, spatial resolution and in the treatment of non-gray radiative transfer between the simulations. Conclusions. The results give confidence in the reliability of the results from comprehensive radiative hydrodynamic simulations."],["dc.format.extent","11"],["dc.identifier.doi","10.1051/0004-6361/201118252"],["dc.identifier.fs","596636"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9654"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60718"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/247060/EU//PEPS"],["dc.relation.euproject","PEPS"],["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","Simulations of the solar near-surface layers with the CO5BOLD, MURaM, and Stagger codes"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","680"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Journal of Geophysical Research: Space Physics"],["dc.bibliographiccitation.lastpage","688"],["dc.bibliographiccitation.volume","119"],["dc.contributor.author","Cameron, R. H."],["dc.contributor.author","Jiang, J."],["dc.contributor.author","Schüssler, M."],["dc.contributor.author","Gizon, L."],["dc.date.accessioned","2017-09-07T11:49:44Z"],["dc.date.available","2017-09-07T11:49:44Z"],["dc.date.issued","2014"],["dc.description.abstract","The level of solar activity varies from cycle to cycle. This variability is probably caused by a combination of nonlinear and random effects. Based on surface flux transport simulations, we show that the observed inflows into active regions and toward the activity belts provide an important nonlinearity in the framework of Babcock‐Leighton model for the solar dynamo. Inclusion of these inflows also leads to a reproduction of the observed proportionality between the open heliospheric flux during activity minima and the maximum sunspot number of the following cycle. A substantial component of the random variability of the cycle strength is associated with the cross‐equatorial flux plumes that occur when large, highly tilted sunspot groups emerge close to the equator. We show that the flux transported by these events is important for the amplitude of the polar fields and open flux during activity minima. The combined action of inflows and cross‐equatorial flux plumes provides an explanation for the weakness of the polar fields at the end of solar cycle 23 (and hence for the relative weakness of solar cycle 24)."],["dc.identifier.doi","10.1002/2013ja019498"],["dc.identifier.gro","3147411"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4997"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-393"],["dc.notes.status","final"],["dc.notes.submitter","chake"],["dc.relation.issn","2169-9380"],["dc.title","Physical causes of solar cycle amplitude variability"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]