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","1294"],["dc.bibliographiccitation.issue","8"],["dc.bibliographiccitation.journal","Advances in Space Research"],["dc.bibliographiccitation.lastpage","1298"],["dc.bibliographiccitation.volume","40"],["dc.contributor.author","Burwitz, Vadim"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Greiner, J."],["dc.contributor.author","Rauch, T."],["dc.contributor.author","Suleimanov, V."],["dc.contributor.author","Walter, F. W."],["dc.contributor.author","Mennickent, R. E."],["dc.contributor.author","Predehl, P."],["dc.date.accessioned","2018-11-07T11:05:49Z"],["dc.date.available","2018-11-07T11:05:49Z"],["dc.date.issued","2007"],["dc.description.abstract","The transient luminous soft X-ray source RX J0513.9-6951 in the large magellanic cloud is a key object within the class of accreting binary supersoft X-ray sources. In this system, mass-transfer is thought to occur close to the Eddington limit of a solar mass white dwarf. The source switches quasi-periodically between two physically distinct states with anti-correlated X-ray and optical luminosities. We have obtained the first high-resolution X-ray spectrum of RX J0513.9-6951 on December 24, 2003 during an X-ray bright state as a 48 ks target of opportunity observation with the low energy transmission grating spectrograph (LETGS) on board Chandra. The X-ray observations were triggered using optical monitoring data obtained with ANDICAM on the 1.3-m telescope at Cerro Tololo, Chile of the SMARTS consortium. The X-ray spectrum deviates strongly from a smooth continuum and reveals complex structures which are probably a mixture of absorption and emission line patterns. Such features can be understood as a superposition of X-ray emission from a hot high-gravity stellar atmosphere and from an optically thin corona-like plasma enshrouding the system. Here, we present first results of our spectral analysis of the LETGS data using white dwarf atmosphere codes. (c) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved."],["dc.identifier.doi","10.1016/j.asr.2006.11.036"],["dc.identifier.isi","000253589900020"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/52152"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Elsevier Sci Ltd"],["dc.relation.issn","0273-1177"],["dc.title","First high-resolution Chandra LETGS spectrum of the transient supersoft x-ray source RX J0513.9-6951"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","143"],["dc.bibliographiccitation.issue","1-2"],["dc.bibliographiccitation.journal","New Astronomy Reviews"],["dc.bibliographiccitation.lastpage","148"],["dc.bibliographiccitation.volume","44"],["dc.contributor.author","Gansicke, B. T."],["dc.contributor.author","van Teeseling, A."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2018-11-07T11:25:18Z"],["dc.date.available","2018-11-07T11:25:18Z"],["dc.date.issued","2000"],["dc.description.abstract","Recent observational results on supersoft X-ray binaries are reviewed, with emphasis on the galactic source QR And and on the enigmatic LMC source RX J0439.8-6809. (C) 2000 Elsevier Science B.V. All rights reserved."],["dc.identifier.doi","10.1016/S1387-6473(00)00028-2"],["dc.identifier.isi","000090017800026"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/56592"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Elsevier Sci Ltd"],["dc.publisher.place","Oxford"],["dc.relation.conference","Cataclysmic Variables: a 60th Birthday Symposium in Honour of Brian Warner"],["dc.relation.eventlocation","OXFORD UNIV, OXFORD, ENGLAND"],["dc.relation.issn","1387-6473"],["dc.title","Supersoft X-ray binaries: an observational update"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","157"],["dc.bibliographiccitation.issue","6963"],["dc.bibliographiccitation.journal","Nature"],["dc.bibliographiccitation.lastpage","159"],["dc.bibliographiccitation.volume","426"],["dc.contributor.author","Greiner, J."],["dc.contributor.author","Klose, S."],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Schmid, H. M."],["dc.contributor.author","Sari, R."],["dc.contributor.author","Hartmann, D. H."],["dc.contributor.author","Kouveliotou, C."],["dc.contributor.author","Rau, A."],["dc.contributor.author","Palazzi, E."],["dc.contributor.author","Straubmeier, C."],["dc.contributor.author","Stecklum, B."],["dc.contributor.author","Zharikov, S. V."],["dc.contributor.author","Tovmassian, G."],["dc.contributor.author","Barnbantner, O."],["dc.contributor.author","Ries, C."],["dc.contributor.author","Jehin, E."],["dc.contributor.author","Henden, A. A."],["dc.contributor.author","Kaas, A. A."],["dc.contributor.author","Grav, T."],["dc.contributor.author","Hjorth, Johannes J. J."],["dc.contributor.author","Pedersen, H."],["dc.contributor.author","Wijers, RAMJ"],["dc.contributor.author","Kaufer, A."],["dc.contributor.author","Park, Hee-Soo"],["dc.contributor.author","Williams, G."],["dc.contributor.author","Reimer, O."],["dc.date.accessioned","2018-11-07T10:34:44Z"],["dc.date.available","2018-11-07T10:34:44Z"],["dc.date.issued","2003"],["dc.description.abstract","The association of a supernova with GRB030329(1,2) strongly supports the 'collapsar' model(3) of gamma-ray bursts, where a relativistic jet(4) forms after the progenitor star collapses. Such jets cannot be spatially resolved because gamma-ray bursts lie at cosmological distances; their existence is instead inferred from 'breaks' in the light curves of the afterglows, and from the theoretical desire to reduce the estimated total energy of the burst by proposing that most of it comes out in narrow beams. Temporal evolution of the polarization of the afterglows(5-7) may provide independent evidence for the jet structure of the relativistic outflow. Small-level polarization (similar to1-3 per cent)(8-17) has been reported for a few bursts, but its temporal evolution has yet to be established. Here we report polarimetric observations of the afterglow of GRB030329. We establish the polarization light curve, detect sustained polarization at the per cent level, and find significant variability. The data imply that the afterglow magnetic field has a small coherence length and is mostly random, probably generated by turbulence, in contrast with the picture arising from the high polarization detected in the prompt gamma-rays from GRB021206 (ref. 18)."],["dc.identifier.doi","10.1038/nature02077"],["dc.identifier.isi","000186517200036"],["dc.identifier.pmid","14614499"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44942"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Nature Publishing Group"],["dc.relation.issn","0028-0836"],["dc.title","Evolution of the polarization of the optical afterglow of the gamma-ray burst GRB030329"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","771"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","776"],["dc.bibliographiccitation.volume","481"],["dc.contributor.author","Beuermann, K."],["dc.contributor.author","El Kholy, E."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2019-07-09T11:55:00Z"],["dc.date.available","2019-07-09T11:55:00Z"],["dc.date.issued","2008-04-03"],["dc.description.abstract","Context. Polars (AM Herculis binaries) are a prominent class of bright soft X-ray sources, many of which were discovered with ROSAT. Aims. We present a homogenous analysis of all the pointed ROSAT PSPC observations of polars subdivided into two papers that discuss the prototype polar AM Her in detail and summarize the class properties of all other polars. Methods. We derive the high-state soft X-ray flux and short-term spectral variability of AM Her using a new detector response matrix and a confirmed flux calibration of the ROSAT PSPC below 0.28 keV. Results. The best-fit mean single-blackbody temperature and integrated bright-phase energy flux of AM Her in its April 1991 high state are 7.2\\pm1.0$ eV and \\times 10^{-9}$ erg cm-2 s-1, respectively. The total blackbody flux of a multi-temperature model that fits both the soft X-ray and the fluctuating far-ultraviolet components is \\mathrm{bb}=(4.5\\pm1.5)\\times 10^{-9}$ erg cm-2 s-1. The total accretion luminosity at a distance of 80 pc, \\mathrm{bb}=(2.1\\pm0.7)\\times 10^{33}$ erg s-1, implies an accretion rate of $\\dot M=(2.4\\pm0.8)\\times 10^{-10}$ \\odot\\,\\mathrm{yr}^{-1}$ for an 0.78 \\odot$ white dwarf. The soft X-ray flux displays significant variability on time scales down to 200 ms. Correlated spectral and count-rate variations are seen in flares on time scales down to 1 s, demonstrating the heating and cooling associated with individual accretion events. Conclusions. Our spectral and temporal analysis provides direct evidence for the blobby accretion model and suggests a connection between the soft X-ray and the fluctuating far-ultraviolet components."],["dc.identifier.doi","10.1051/0004-6361:20079335"],["dc.identifier.fs","513461"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9948"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60777"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["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","Soft X-ray spectral variability of AM Herculis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["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","199"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","212"],["dc.bibliographiccitation.volume","480"],["dc.contributor.author","Beuermann, K."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2019-07-09T11:54:35Z"],["dc.date.available","2019-07-09T11:54:35Z"],["dc.date.issued","2008"],["dc.description.abstract","Context. EXHya is one of the few double-lined eclipsing cataclysmic variables that allow an accurate measurement of the binary masses. Aims. We analyze orbital phase-resolved UVES/VLT high resolution (λ/Δλ 27 000) spectroscopic observations of EXHya with the aims of deriving the binary masses and obtaining a tomographic image of the illuminated secondary star. Methods. We present a novel method for determining the binary parameters by directly fitting an emission model of the illuminated secondary star to the phase-resolved line profiles of NaIλ8183/8195 in absorption and emission and CaIIλ8498 in emission. Results. The fit to the NaI and CaII line profiles, combined with the published K1, yields a white-dwarf mass M1 = 0.790 ± 0.026 M , a secondary mass M2 = 0.108 ± 0.008 M , and a velocity amplitude of the secondary star K2 = 432.4 ± 4.8 kms−1. The secondary is of spectral type dM5.5 ± 0.5 and has an absolute K-band magnitude of MK = 8.8. Its Roche radius places it on or very close to the main sequence of low-mass stars. It differs from a main sequence star by its illuminated hemisphere that faces the white dwarf. The secondary star contributes only 5% to the observed spin-phase averaged flux at 7500 Å, 7.5% at 8200 Å, and 37% in the K-band. We present images of the secondary star in the light of the NaI doublet and the CaII emission line derived with a simplified version of Roche tomography. Line emission is restricted to the illuminated part of the star, but its distribution differs from that of the incident energy flux. Conclusions. We have discovered narrow spectral lines from the secondary star in EXHya that delineate its orbital motion and allow us to derive accurate masses of both components. The primary mass significantly exceeds recently published values. The secondary is a low-mass main sequence star that displays a rich emission line spectrum on its illuminated side, but lacks chromospheric emission on its dark side."],["dc.identifier.doi","10.1051/0004-6361:20079010"],["dc.identifier.fs","513376"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9386"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60685"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["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","High-resolution spectroscopy of the intermediate polar EX Hydrae"],["dc.title.alternative","I. Kinematic study and Roche tomography"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1043"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1046"],["dc.bibliographiccitation.volume","457"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Kim, Y."],["dc.contributor.author","Beuermann, K."],["dc.date.accessioned","2019-07-09T11:54:56Z"],["dc.date.available","2019-07-09T11:54:56Z"],["dc.date.issued","2006-10-03"],["dc.description.abstract","Context. The first phase-resolved JHK light curves of the eclipsing polar (AM Herculis binary) V1309Ori are presented and interpreted. Aims. We separate the contributions from the secondary star and from other sources with the aim of determining a photometric distance. Methods. Simple model calculations show that the accretion stream and the cyclotron source on the accreting white dwarf are minor contributors to the infrared light, allowing an accurate determination of spectral type and absolute flux of the secondary star. Results. The unilluminated backside of the secondary star as seen in eclipse has spectral type dM0 to dM0+. Its dereddened magnitude is K = 13.58 at orbital phase φ = 0 (eclipse). Using the calibrated surface brightness of M-stars and the published mass of the secondary, M2 = 0.46 M , we obtain a distance d = 600 ± 25 pc which scales as M1/2 2 . The radius of the Roche-lobe filling secondary exceeds the main-sequence radius of an M0 star by 21+11 −6 %. Conclusions. The debated origin of the infrared light of V1309 Ori has been settled in favor of the secondary star as the main contributor and an accurate distance has been derived that will place estimates of the luminosity and synchronization time scale on a more secure basis."],["dc.identifier.doi","10.1051/0004-6361:20065655"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9879"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60760"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","The secondary star and distance of the polar V1309 Orionis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A41"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","543"],["dc.contributor.author","Beuermann, K."],["dc.contributor.author","Burwitz, V."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2019-07-09T11:54:43Z"],["dc.date.available","2019-07-09T11:54:43Z"],["dc.date.issued","2012-06-25"],["dc.description.abstract","We present a simple heuristic model for the time-averaged soft X-ray temperature distribution in the accretion spot on the white dwarf in polars. The model is based on the analysis of the Chandra LETG spectrum of the prototype polar AM Her and involves an exponential distribution of the emitting area vs. blackbody temperature a(T) = a0 exp(−T/T0). With one free parameter besides the normalization, it is mathematically as simple as the single blackbody, but is physically more plausible and fits the soft X-ray and far-ultraviolet spectral fluxes much better. The model yields more reliable values of the wavelength-integrated flux of the soft X-ray component and the implied accretion rate than reported previously."],["dc.format.extent","5"],["dc.identifier.doi","10.1051/0004-6361/201219217"],["dc.identifier.fs","596640"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9606"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60712"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["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","A new soft X-ray spectral model for polars with an application to AM Herculis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","L79"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","L82"],["dc.bibliographiccitation.volume","356"],["dc.contributor.author","Gansicke, B. T."],["dc.contributor.author","Fried, R. E."],["dc.contributor.author","Hagen, H. J."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Engels, D."],["dc.contributor.author","Hessman, Frederic V."],["dc.contributor.author","Nogami, D."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2018-11-07T10:37:35Z"],["dc.date.available","2018-11-07T10:37:35Z"],["dc.date.issued","2000"],["dc.description.abstract","We report on follow-up spectroscopy and photometry of the cataclysmic variable candidate HS 0907+1902 selected from the Hamburg Quasar Survey. B, V, and R photometry obtained during the first observed outburst of HS 0907+1902 (V approximate to 13) reveals deep eclipses (Delta V approximate to 2.1 - 2.8) and an orbital period P(orb) = 4.2 h with the eclipse depth decreasing to the red. The outburst eclipse profiles are symmetric, indicating an axisymmetrical brightness distribution in the accretion disc. We derive an inclination i approximate to 73 degrees - 79 degrees from the eclipse duration. The quiescent spectrum obtained with the Hobby-Eberly Telescope shows double peaked emission lines of H I, He I and Fe I,II and clearly identifies the system as a dwarf nova. Absorption features of the secondary star are detected at red wavelengths from which a spectral class M3 +/- 1.5 and a distance of d = 320 +/- 100 pc are derived."],["dc.identifier.isi","000087446700005"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/45601"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-6361"],["dc.title","HS 0907+1902: a new 4.2 hr eclipsing dwarf nova"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]