Schuh, Sonja

[["dc.bibliographiccitation.firstpage","1034"],["dc.bibliographiccitation.issue","9-10"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","1037"],["dc.bibliographiccitation.volume","331"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Randall, S. K."],["dc.contributor.author","Dhillon, V. S."],["dc.contributor.author","Marsh, T. R."],["dc.contributor.author","Savoury, C. D."],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Fontaine, Gilles"],["dc.contributor.author","Brassard, P."],["dc.date.accessioned","2018-11-07T08:36:00Z"],["dc.date.available","2018-11-07T08:36:00Z"],["dc.date.issued","2010"],["dc.description.abstract","V391 Peg (HS 2201+2610) is an extreme horizontal branch subdwarf B (sdB) star, it is an hybrid pulsator showing p- and g-mode oscillations, and hosts a 3.2/sin i M-Jup planet at an orbital distance of about 1.7 AU. In order to improve the characterization of the star, we measured the pulsation amplitudes in the u'g'r' Sloan photometric bands using ULTRACAM at the William Herschel 4.2m telescope and we compared them with theoretical values. The preliminary results presented in this article conclusively show that the two main pulsation periods at 349.5 and 354.1 s are a radial and a dipole mode respectively. This is the first time that the degree index of multiple modes has been uniquely identified for an sdB star as faint as V391 Peg (B = 14.4), proving that multicolor photometry is definitely an efficient technique to constrain mode identification, provided that the data have a high enough quality. C() 2010 WILEY-VCH Verlag GmbH&Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201011451"],["dc.identifier.isi","000285211700035"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/18206"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","4th HELAS International Conference"],["dc.relation.eventlocation","Canary Islands, SPAIN"],["dc.relation.issn","0004-6337"],["dc.title","V391 Peg: Identification of the two main pulsation modes from ULTRACAM u ' g ' r ' amplitudes"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","457"],["dc.bibliographiccitation.issue","3-4"],["dc.bibliographiccitation.journal","Astrophysics and Space Science"],["dc.bibliographiccitation.lastpage","464"],["dc.bibliographiccitation.volume","291"],["dc.contributor.author","O'Toole, S. J."],["dc.contributor.author","Falter, S."],["dc.contributor.author","Heber, Ulrich"],["dc.contributor.author","Jeffery, C. S."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, S. L."],["dc.date.accessioned","2018-11-07T10:52:04Z"],["dc.date.available","2018-11-07T10:52:04Z"],["dc.date.issued","2004"],["dc.description.abstract","We present the first results from the MultiSite Spectroscopic Telescope (MSST) observations of the sdBV star PG 1605+072. Pulsating sdB stars (also known as EC 14026 stars) offer the chance to gain new insights into the formation and evolution of extreme Horizontal Branch stars using the tools of asteroseismology. PG1605+072 is an outstanding object in its class, with the richest frequency spectrum, the longest periods, and the largest variations. The MSST campaign took place in May/June 2002 immediately following the Whole Earth Telescope Xcov22 run, which observed PG 1605+072 as an alternate target. We will first give an overview of the project and its feasibility, after which we will present the massive data set, made up of 399 h of photometry and 151 h of spectroscopy. The overall aims of the project are to examine light/velocity amplitude ratios and phase differences, changes in equivalent width/line index, and lambda-dependence of photometric amplitudes, and to use these properties for mode identification."],["dc.identifier.doi","10.1023/B:ASTR.0000044360.79737.38"],["dc.identifier.isi","000224389400041"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/49036"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Kluwer Academic Publ"],["dc.publisher.place","Dordrecht"],["dc.relation.conference","Meeting on sdB Stars"],["dc.relation.eventlocation","Keele Univ, Staffordshire, ENGLAND"],["dc.relation.issn","0004-640X"],["dc.title","MSST observations of the pulsating sdB star PG 1605+072"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","231"],["dc.bibliographiccitation.issue","1-2"],["dc.bibliographiccitation.journal","Astrophysics and Space Science"],["dc.bibliographiccitation.lastpage","242"],["dc.bibliographiccitation.volume","329"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Lutz, Ronny"],["dc.contributor.author","Loeptien, Bjoern"],["dc.contributor.author","Green, Elizabeth M."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Leccia, Silvio"],["dc.contributor.author","Kim, Seung-Lee"],["dc.contributor.author","Fontaine, Gilles"],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Francoeur, Myriam"],["dc.contributor.author","Randall, Suzanna"],["dc.contributor.author","Rodriguez-Lopez, Cristina"],["dc.contributor.author","van Grootel, Valerie"],["dc.contributor.author","Odell, Andrew P."],["dc.contributor.author","Paparo, Margit"],["dc.contributor.author","Bognar, Zsofia"],["dc.contributor.author","Papics, Peter"],["dc.contributor.author","Nagel, Thorsten"],["dc.contributor.author","Beeck, Benjamin"],["dc.contributor.author","Hundertmark, Markus"],["dc.contributor.author","Stahn, Thorsten"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Hessman, Frederic V."],["dc.contributor.author","Dall'Ora, Massimo"],["dc.contributor.author","Mancini, Dario"],["dc.contributor.author","Cortecchia, Fausto"],["dc.contributor.author","Benatti, Serena"],["dc.contributor.author","Claudi, Riccardo"],["dc.contributor.author","Janulis, Rimvydas"],["dc.date.accessioned","2018-11-07T08:38:16Z"],["dc.date.available","2018-11-07T08:38:16Z"],["dc.date.issued","2010"],["dc.description.abstract","In 2007, a companion with planetary mass was found around the pulsating subdwarf B star V391 Pegasi with the timing method, indicating that a previously undiscovered population of substellar companions to apparently single subdwarf B stars might exist. Following this serendipitous discovery, the EXOTIME (http://www.na.astro.it/similar to silvotti/exotime/)) monitoring program has been set up to follow the pulsations of a number of selected rapidly pulsating subdwarf B stars on time scales of several years with two immediate observational goals: (1) determine (P)over dot of the pulsational periods P (2) search for signatures of substellar companions in O-C residuals due to periodic light travel time variations, which would be tracking the central star's companion-induced wobble around the centre of mass These sets of data should therefore, at the same time, on the one hand be useful to provide extra constraints for classical asteroseismological exercises from the P. ( comparison with \"local\" evolutionary models), and on the other hand allow one to investigate the preceding evolution of a target in terms of possible \"binary\" evolution by extending the otherwise unsuccessful search for companions to potentially very low masses. While timing pulsations may be an observationally expensive method to search for companions, it samples a different range of orbital parameters, inaccessible through orbital photometric effects or the radial velocity method: the latter favours massive close-in companions, whereas the timing method becomes increasingly more sensitive toward wider separations. In this paper we report on the status of the on-going observations and coherence analysis for two of the currently five targets, revealing very well-behaved pulsational characteristics in HS 0444+0458, while showing HS 0702+6043 to be more complex than previously thought."],["dc.identifier.doi","10.1007/s10509-010-0356-4"],["dc.identifier.isi","000282823200038"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7631"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/18728"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Springer"],["dc.relation.issn","0004-640X"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","EXOTIME: searching for planets around pulsating subdwarf B stars"],["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.artnumber","A130"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","570"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Green, E."],["dc.contributor.author","Fontaine, Gilles"],["dc.contributor.author","Telting, J. H."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","van Grootel, V."],["dc.contributor.author","Baran, A. S."],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Machado, L. Fox"],["dc.date.accessioned","2018-11-07T09:34:04Z"],["dc.date.available","2018-11-07T09:34:04Z"],["dc.date.issued","2014"],["dc.description.abstract","KIC 10001893 is one out of 19 subdwarf-B (sdB) pulsators observed by the Kepler spacecraft in its primary mission. In addition to tens of pulsation frequencies in the g-mode domain, its Fourier spectrum shows three weak peaks at very low frequencies, which is too low to be explained in terms of g modes. The most convincing explanation is that we are seeing the orbital modulation of three Earth-size planets (or planetary remnants) in very tight orbits, which are illuminated by the strong stellar radiation. The orbital periods are P-1 = 5.273, P-2 = 7.807, and P-3 = 19.48 h, and the period ratios P-2/P-1 = 1.481 and P-3/P-2 = 2.495 are very close to the 3.2 and 5:2 resonances, respectively. One of the main pulsation modes of the star at 210.68 mu Hz corresponds to the third harmonic of the orbital frequency of the inner planet, suggesting that we see, for the first time in an sdB star, g -mode pulsations tidally excited by a planetary companion. The extreme planetary system that emerges from the Kepler data is very similar to the recent discovery of two Earth-size planets orbiting the sdB pulsator KIC 05807616 (Charpinet et al. 2011a)."],["dc.identifier.doi","10.1051/0004-6361/201424509"],["dc.identifier.fs","609721"],["dc.identifier.isi","000344158500124"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/11403"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/32100"],["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.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Kepler detection of a new extreme planetary system orbiting the subdwarf-B pulsator KIC 10001893"],["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","L31"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","L34"],["dc.bibliographiccitation.volume","445"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Huber, Johannes"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Heber, Ulrich"],["dc.contributor.author","O'Toole, S. J."],["dc.contributor.author","Green, Elizabeth M."],["dc.contributor.author","Fontaine, Gilles"],["dc.date.accessioned","2018-11-07T10:30:18Z"],["dc.date.available","2018-11-07T10:30:18Z"],["dc.date.issued","2006"],["dc.description.abstract","Context. The hot subdwarf B star HS 0702 0702+6043 is known as a large-amplitude, short-period p-mode pulsator of the EC 14026 type. Its atmospheric parameters place it at the common boundary between the empirical instability regions of the EC 14026 variables and the typically C cooler long-period g-mode pulsators of the PG1716 kind. Aims. We analyse and interpret the photometric var variability iability of HS 0702 0702+ 6043 in order to explore its asteroseismological potential. Methods. We report on rapid wide band CCD photometric observations to follow up on and confirm the serendipitous discovery of multiperiodic long- period luminosity variations with typical time scales of similar to 1 h in HS 0702 0702+6043, in addition to the two previously known pulsations at 363 s and 383 s. In particular, we isolate a relatively low-amplitude (similar to 4 mmag), long-period (3538 +/- 130 s) light variation. Results. We argue that the most likely origin for this luminosity variation is the presence of an excited g-mode pulsation. If confirmed, HS 0702 0702+6043 would constitute a rare addition to the very select class of pulsating stars showing sim lect simultaneously parts of their pressure and ultaneously gravity mode pulsation spectra. The asteroseismological potential of such stars is immense, and HS 0702 0702+6043 thus becomes a target of choice for future investigations. While our discovery appears consistent with the location of HS 0702 0702+6043 at the common boundary between the two families of pulsating sdB stars, it does challenge theory's current description of stability and driving mechanisms in pulsating B subdwarfs."],["dc.identifier.doi","10.1051/0004-6361:200500210"],["dc.identifier.fs","45041"],["dc.identifier.isi","000234404500003"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/7680"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43835"],["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","HS 0702+6043: a star showing both short-period p-mode and long-period g-mode oscillations"],["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","189"],["dc.bibliographiccitation.issue","7159"],["dc.bibliographiccitation.journal","Nature"],["dc.bibliographiccitation.lastpage","191"],["dc.bibliographiccitation.volume","449"],["dc.contributor.author","Silvotti, Roberto"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Janulis, Rimvydas"],["dc.contributor.author","Solheim, J.-E."],["dc.contributor.author","Bernabei, S."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Oswalt, T. D."],["dc.contributor.author","Bruni, I."],["dc.contributor.author","Gualandi, R."],["dc.contributor.author","Bonanno, A."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Reed, M."],["dc.contributor.author","Chen, C.-W."],["dc.contributor.author","Leibowitz, E. M."],["dc.contributor.author","Paparo, Margit"],["dc.contributor.author","Baran, A."],["dc.contributor.author","Charpinet, Stephane"],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Kawaler, Steven D."],["dc.contributor.author","Kurtz, D. W."],["dc.contributor.author","Moskalik, P."],["dc.contributor.author","Riddle, R."],["dc.contributor.author","Zola, S."],["dc.date.accessioned","2018-11-07T10:58:37Z"],["dc.date.available","2018-11-07T10:58:37Z"],["dc.date.issued","2007"],["dc.description.abstract","After the initial discoveries fifteen years ago(1,2), over 200 extrasolar planets have now been detected. Most of them orbit main-sequence stars similar to our Sun, although a few planets orbiting red giant stars have been recently found(3). When the hydrogen in their cores runs out, main-sequence stars undergo an expansion into red-giant stars. This expansion can modify the orbits of planets and can easily reach and engulf the inner planets. The same will happen to the planets of our Solar System in about five billion years and the fate of the Earth is matter of debate(4,5). Here we report the discovery of a planetary-mass body (Msini = 3.2M(Jupiter)) orbiting the star V 391 Pegasi at a distance of about 1.7 astronomical units (AU), with a period of 3.2 years. This star is on the extreme horizontal branch of the Hertzsprung-Russell diagram, burning helium in its core and pulsating. The maximum radius of the red-giant precursor of V 391 Pegasi may have reached 0.7 AU, while the orbital distance of the planet during the stellar main-sequence phase is estimated to be about 1 AU. This detection of a planet orbiting a post-red-giant star demonstrates that planets with orbital distances of less than 2 AU can survive the red-giant expansion of their parent stars."],["dc.identifier.doi","10.1038/nature06143"],["dc.identifier.isi","000249394500042"],["dc.identifier.pmid","17851517"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/50505"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Nature Publishing Group"],["dc.relation.issn","0028-0836"],["dc.title","A giant planet orbiting the 'extreme horizontal branch' star V391 Pegasi"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","649"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","U9"],["dc.bibliographiccitation.volume","410"],["dc.contributor.author","Schuh, S. L."],["dc.contributor.author","Handler, G."],["dc.contributor.author","Drechsel, H."],["dc.contributor.author","Hauschildt, P. H."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Medupe, R."],["dc.contributor.author","Karl, C."],["dc.contributor.author","Napiwotzki, R."],["dc.contributor.author","Kim, S. L."],["dc.contributor.author","Park, B. G."],["dc.contributor.author","Wood, M. A."],["dc.contributor.author","Paparo, Margit"],["dc.contributor.author","Szeidl, B."],["dc.contributor.author","Viraghalmy, G."],["dc.contributor.author","Zsuffa, D."],["dc.contributor.author","Hashimoto, O."],["dc.contributor.author","Kinugasa, K."],["dc.contributor.author","Taguchi, H."],["dc.contributor.author","Kambe, E."],["dc.contributor.author","Leibowitz, E. M."],["dc.contributor.author","Ibbetson, P."],["dc.contributor.author","Lipkin, Y."],["dc.contributor.author","Nagel, T."],["dc.contributor.author","Gohler, E."],["dc.contributor.author","Pretorius, M. L."],["dc.date.accessioned","2018-11-07T10:34:54Z"],["dc.date.available","2018-11-07T10:34:54Z"],["dc.date.issued","2003"],["dc.description.abstract","We report the discovery of a new eclipsing system less than one arcminute south of the pulsating DB white dwarf KUV 05134+2605. The object could be identified with the point source 2MASS J0516288+260738 published by the Two Micron All Sky Survey. We present and discuss the first light curves as well as some additional colour and spectral information. The eclipse period of the system is 1.29 d, and, assuming this to be identical to the orbital period, the best light curve solution yields a mass ratio of m(2)/m(1) = 0.11, a radius ratio of r(2)/r(1) approximate to 1 and an inclination of 74degrees. The spectral anaylsis results in a T-eff = 4200 K for the primary. On this basis, we suggest that the new system probably consists of a late K + Brown dwarf (which would imply a system considerably younger than approximate to 0.01 Gyr to have r(2)/r(1) approximate to 1), and outline possible future observations."],["dc.identifier.doi","10.1051/0004-6361:20031241"],["dc.identifier.isi","000185917300027"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44975"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-6361"],["dc.title","2MASS J0516288+260738: Discovery of the first eclipsing late K+ Brown dwarf binary system?"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","16"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","24"],["dc.bibliographiccitation.volume","328"],["dc.contributor.author","Israel, H."],["dc.contributor.author","Hessman, Frederic V."],["dc.contributor.author","Schuh, Sonja"],["dc.date.accessioned","2018-11-07T11:06:02Z"],["dc.date.available","2018-11-07T11:06:02Z"],["dc.date.issued","2007"],["dc.description.abstract","Difference imaging is a technique for obtaining precise relative photometry of variable sources in crowded stellar fields and, as such, constitutes a crucial part of the data reduction pipeline in surveys for microlensing events or transiting extra-solar planets. The Optimal Image Subtraction (OIS) algorithm of Alard & Lupton (1998) permits the accurate differencing of images by determining convolution kernels which, when applied to reference images with particularly good seeing and signal-to-noise (SIN), provide excellent matches to the point-spread functions (PSF) in other images of the time series to be analysed. The convolution kernels are built as linear combinations of a set of basis functions, conventionally bivariate Gaussians modulated by polynomials. The kernel parameters, mainly the widths and maximal degrees of the basis function model, must be supplied by the user. Ideally, the parameters should be matched to the PSF, pixel-sampling, and SIN of the data set or individual images to be analysed. We have studied the dependence of the reduction outcome as a function of the kernel parameters using our new implementation of OIS within the IDL-based TRIPP package. From the analysis of noise-free PSF simulations of both single objects and crowded fields, as well as the test images in the ISIS OIS software package, we derive qualitative and quantitative relations between the kernel parameters and the success of the subtraction as a function of the PSF widths and sampling in reference and data images and compare the results to those of other implementations found in the literature. On the basis of these simulations, we provide recommended parameters for data sets with different SIN and sampling. (c) 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.200610703"],["dc.identifier.isi","000244047200004"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/52210"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.relation.issn","0004-6337"],["dc.title","Optimising optimal image subtraction"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","376"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","378"],["dc.bibliographiccitation.volume","329"],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Traulsen, Imke"],["dc.contributor.author","Nagel, T."],["dc.contributor.author","Reiff, E."],["dc.contributor.author","Homeier, Derek"],["dc.contributor.author","Schwager, H."],["dc.contributor.author","Kusterer, D.-J."],["dc.contributor.author","Lutz, R."],["dc.contributor.author","Schreiber, M. R."],["dc.date.accessioned","2018-11-07T11:16:20Z"],["dc.date.available","2018-11-07T11:16:20Z"],["dc.date.issued","2008"],["dc.description.abstract","Methods to measure masses of PG 1159 stars in order to test evolutionary scenarios are currently based on spectroscopic masses or asteroseismological mass determinations. One recently discovered PG 1159 star in a close binary system may finally allow the first dynamical mass determination, which has so far been analysed on the basis of one SDSS spectrum and photometric monitoring. In order to be able to phase future radial velocity measurements of the system SDSS J212531.92 circle dot 010745.9, we follow up on the photometric monitoring of this system to provide a solid observational basis for an improved orbital ephemeris determination. New white-light time series of the brightness variation of SDSS J212531.92 circle dot 010745.9 with the Tubingen 80 cm and Gottingen 50 cm telescopes extend the monitoring into a second season (2006), tripling the length of overall observational data available, and significantly increasing the time base covered. We give the ephemeris for the orbital motion of the system, based on a sine fit which now results in a period of 6.95573(5) h, and discuss the associated new amplitude determination in the context of the phased light curve variation profile. The accuracy of the ephemeris has been improved by more than one order of magnitude compared to that previously published for 2005 alone. (C) 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim."],["dc.identifier.doi","10.1002/asna.200710920"],["dc.identifier.isi","000256049000005"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/54561"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.relation.issn","0004-6337"],["dc.title","A new period determination for the close PG1159 binary SDSS J212531.92-010745.9"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","321"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","BALTIC ASTRONOMY"],["dc.bibliographiccitation.lastpage","325"],["dc.bibliographiccitation.volume","15"],["dc.contributor.author","Jeffery, C. S."],["dc.contributor.author","Heber, Ulrich"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","O'Toole, S. J."],["dc.contributor.author","Schuh, S. L."],["dc.contributor.author","Woolf, Vincent M."],["dc.contributor.author","Falter, S."],["dc.contributor.author","Nitta, A."],["dc.contributor.author","Kleinman, S."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Billeres, M."],["dc.date.accessioned","2018-11-07T10:30:35Z"],["dc.date.available","2018-11-07T10:30:35Z"],["dc.date.issued","2006"],["dc.description.abstract","The MultiSite Spectroscopic Telescope (MSST) campaign aimed to provide a detailed view of the short-period pulsating subdwarf B star PC 1605+ 072. We present results from the part of the campaign undertaken on 4 m telescopes in 2002 May and June."],["dc.identifier.isi","000237216400026"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43901"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Inst Theoretical Physics Astronomy"],["dc.publisher.place","Moletai"],["dc.relation.conference","2nd Meeting on Hot Subdwarf Stars and Related Objects"],["dc.relation.eventlocation","Santa Cruz de la Palma, SPAIN"],["dc.relation.issn","1392-0049"],["dc.title","The MSST campaign: 4 m spectroscopy of PG 1605+072"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]