Reinsch, Klaus

[["dc.bibliographiccitation.firstpage","671"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","681"],["dc.bibliographiccitation.volume","451"],["dc.contributor.author","Euchner, F."],["dc.contributor.author","Jordan, S."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Gansicke, B. T."],["dc.date.accessioned","2018-11-07T09:50:53Z"],["dc.date.available","2018-11-07T09:50:53Z"],["dc.date.issued","2006"],["dc.description.abstract","Aims. We analyse the magnetic field geometry of the magnetic DA white dwarf PG1015+014 with our Zeeman tomography method. Methods. This study is based on rotation-phase resolved optical flux and circular polarization spectra of PG1015+014 obtained with FORS1 at the ESO VLT. Our tomographic code makes use of an extensive database of pre-computed Zeeman spectra. The general approach has been described in Papers I and II of this series. Results. The surface field strength distributions for all rotational phases of PG1015+014 are characterised by a strong peak at 70 MG. A separate peak at 80MG is seen for about one third of the rotation cycle. Significant contributions to the Zeeman features arise from regions with field strengths between 50 and 90 MG. We obtain equally good simultaneous fits to the observations, collected in five phase bins, for two different field parametrizations: (i) a superposition of individually tilted and off-centred zonal multipole components; and (ii) a truncated multipole expansion up to degree l = 4 including all zonal and tesseral components. The magnetic fields generated by both parametrizations exhibit a similar global structure of the absolute surface field values, but differ considerably in the topology of the field lines. An effective photospheric temperature of T-eff = 10 000 +/- 1000 K was found. Conclusions. Remaining discrepancies between the observations and our best-fit models suggest that additional small-scale structure of the magnetic field exists which our field models are unable to cover due to the restricted number of free parameters."],["dc.identifier.doi","10.1051/0004-6361:20064840"],["dc.identifier.fs","45028"],["dc.identifier.isi","237272100027"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9385"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/35801"],["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","Zeeman tomography of magnetic white dwarfs - III. The 70-80 Megagauss magnetic field of PG1015+014"],["dc.title.original","9385"],["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","651"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","660"],["dc.bibliographiccitation.volume","442"],["dc.contributor.author","Euchner, F."],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Jordan, S."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Gansicke, B. T."],["dc.date.accessioned","2018-11-07T10:54:29Z"],["dc.date.available","2018-11-07T10:54:29Z"],["dc.date.issued","2005"],["dc.description.abstract","We report time-resolved optical flux and circular polarization spectroscopy of the magnetic DA white dwarf HE 1045- 0908 obtained with FORS1 at the ESO VLT. Considering published results, we estimate a likely rotational period of P-rot similar or equal to 2.7 h, but cannot exclude values as high as about 9 h. Our detailed Zeeman tomographic analysis reveals a field structure which is dominated by a quadrupole and contains additional dipole and octupole contributions, and which does not depend strongly on the assumed value of the period. A good fit to the Zeeman flux and polarization spectra is obtained if all field components are centred and inclinations of their magnetic axes with respect to each other are allowed for. The fit can be slightly improved if an offset from the centre of the star is included. The prevailing surface field strength is 16 MG, but values between 10 and similar to 75 MG do occur. We derive an effective photospheric temperature of HE 1045- 0908 of T-eff = 10 000 +/- 1000 K. The tomographic code makes use of an extensive database of pre-computed Zeeman spectra ( Paper I)."],["dc.identifier.doi","10.1051/0004-6361:20053038"],["dc.identifier.isi","232404400032"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9389"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/49572"],["dc.notes.intern","In goescholar not merged with http://resolver.sub.uni-goettingen.de/purl?gs-1/9853 but duplicate"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.rights","Goescholar"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Zeeman tomography of magnetic white dwarfs - II. The quadrupole-dominated magnetic field of HE 1045-0908"],["dc.title.original","9389"],["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","984"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","998"],["dc.bibliographiccitation.volume","382"],["dc.contributor.author","Eisenbart, S."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Gansicke, B. T."],["dc.date.accessioned","2018-11-07T10:32:03Z"],["dc.date.available","2018-11-07T10:32:03Z"],["dc.date.issued","2002"],["dc.description.abstract","We present phase-resolved infrared and optical spectrophotometry of the intermediate polar EXHya supplemented by archival ultraviolet data. The spin-modulated emission from the accretion funnel and the emission from the accretion disk or ring contain substantial optically thin components. The white dwarf dominates the unmodulated flux in the ultraviolet and is identified by numerous absorption lines. Metal absorption in the accretion curtain may add to the observed spectral features. The secondary star is of spectral type M4 +/- 1 and is detected by its ellipsoidal modulation. We derive a distance of 65 +/- 11 pc which makes EX Hydrae one of the closest cataclysmic variables with a known distance. The luminosity derived from the integrated overall spectral energy distribution is 3 x 10(32) erg s(-1). The accretion rate of 3 x 10(15) g s(-1) (for an 0.6 M-. white dwarf) is in reasonable agreement with the rates expected from angular momentum loss by gravitational radiation and from the observed spin-up of the white dwarf."],["dc.identifier.doi","10.1051/0004-6361:20011655"],["dc.identifier.fs","19124"],["dc.identifier.isi","000174182900024"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9722"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44255"],["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","Multi-wavelength spectrophotometry of EX Hydrae"],["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","635"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","645"],["dc.bibliographiccitation.volume","424"],["dc.contributor.author","Haberl, F."],["dc.contributor.author","Motch, C."],["dc.contributor.author","Zavlin, V. E."],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Gansicke, B. T."],["dc.contributor.author","Cropper, M."],["dc.contributor.author","Schwope, Axel D."],["dc.contributor.author","Turolla, R."],["dc.contributor.author","Zane, S."],["dc.date.accessioned","2018-11-07T10:45:46Z"],["dc.date.available","2018-11-07T10:45:46Z"],["dc.date.issued","2004"],["dc.description.abstract","We report on the analysis of new X-ray data obtained with XMM-Newton and Chandra from two ROSAT-discovered X-ray dim isolated neutron stars (XDINs). RXJ0806.4-4123 was observed with XMM-Newton in April 2003, 2.5 years after the first observation. The EPIC-pn data confirm that this object is an X-ray pulsar with 11.371 s neutron star spin period. The X-ray spectrum is consistent with absorbed black-body emission with a temperature kT = 96 eV and N-H = 4 x 10(19) cm(-2) without significant changes between the two observations. Four XMM-Newton observations of RXJ0420.0-5022 between December 2002 and July 2003 did not confirm the 22.7 s pulsations originally indicated in ROSAT data, but clearly reveal a 3.453 s period. A fit to the X-ray spectrum using an absorbed black-body model yields kT = 45 eV, the lowest value found from the small group of XDINs and N-H = 1.0 x 10(20) cm(-2). Including a broad absorption line improves the quality of the spectral fits considerably for both objects and may indicate the presence of absorption features similar to those reported from RBS1223, RXJ1605.3+3249 and RXJ0720.4-3125. For both targets we derive accurate X-ray positions from the Chandra data and present an optical counterpart candidate for RXJ0420.0-5022 with B = 26.6 +/- 0.3 mag from VLT imaging."],["dc.identifier.doi","10.1051/0004-6361:20040440"],["dc.identifier.isi","000224300800031"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9835"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/47583"],["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","The isolated neutron star X-ray pulsars RX J0420.0-5022 and RX J0806.4-4123: New X-ray and optical observations"],["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"]]