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","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","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"]]

[["dc.bibliographiccitation.firstpage","1099"],["dc.bibliographiccitation.issue","10"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","1102"],["dc.bibliographiccitation.volume","333"],["dc.contributor.author","Lutz, R."],["dc.contributor.author","Schuh, Sonja"],["dc.contributor.author","Silvotti, Roberto"],["dc.date.accessioned","2018-11-07T09:02:38Z"],["dc.date.available","2018-11-07T09:02:38Z"],["dc.date.issued","2012"],["dc.description.abstract","We review the status of the EXOTIME project (EXOplanet search with the TIming MEthod). The two main goals of EXOTIME are to search for sub-stellar companions to sdB stars in wide orbits, and to measure the secular variation of the pulsation periods, which are related to the evolutionary change of the stellar structure. Now, after four years of dense monitoring, we start to see some results and present the brown dwarf and exoplanet candidates V1636 Ori b and DW Lynb ((c) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)"],["dc.identifier.doi","10.1002/asna.201211793"],["dc.identifier.isi","000312541500049"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/24729"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.publisher.place","Weinheim"],["dc.relation.conference","ESF Conference The Modern Era of Helio- and Asteroseismology"],["dc.relation.eventlocation","Innsbruck, AUSTRIA"],["dc.relation.issn","1521-3994"],["dc.relation.issn","0004-6337"],["dc.title","EXOTIME: Searching for planets and measuring P in sdB pulsators"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","138"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.lastpage","143"],["dc.bibliographiccitation.volume","711"],["dc.contributor.author","Irrgang, Andreas"],["dc.contributor.author","Przybilla, Norbert"],["dc.contributor.author","Heber, Ulrich"],["dc.contributor.author","Nieva, M. Fernanda"],["dc.contributor.author","Schuh, Sonja"],["dc.date.accessioned","2018-11-07T08:45:11Z"],["dc.date.available","2018-11-07T08:45:11Z"],["dc.date.issued","2010"],["dc.description.abstract","Young, massive stars in the Galactic halo are widely supposed to be the result of an ejection event from the Galactic disk forcing some stars to leave their place of birth as so-called runaway stars. Here, we present a detailed spectroscopic and kinematic analysis of the runaway B star HIP 60350 to determine which runaway scenario-a supernova explosion disrupting a binary system or dynamical interaction in star clusters-may be responsible for HIP 60350's peculiar orbit. Based on a non-local thermodynamic equilibrium approach, a high-resolution optical echelle spectrum was examined to revise spectroscopic quantities and for the first time to perform a differential chemical abundance analysis with respect to the B-type star 18 Peg. The results together with proper motions from the Hipparcos Catalog further allowed the three-dimensional kinematics of the star to be studied numerically. The abundances derived for HIP 60350 are consistent with a slightly supersolar metallicity agreeing with the kinematically predicted place of birth similar to 6 kpc away from the Galactic center. However, they do not exclude the possibility of an alpha-enhanced abundance pattern expected in the case of the supernova scenario. Its outstanding high Galactic rest-frame velocity of 530 +/- 35 km s(-1) is a consequence of ejection in the direction of Galactic rotation and slightly exceeds the local Galactic escape velocity in a standard Galactic potential. Hence, IIIP 60350 may be unbound to the Galaxy."],["dc.identifier.doi","10.1088/0004-637X/711/1/138"],["dc.identifier.isi","000274417500012"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/20375"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","0004-637X"],["dc.title","THE NATURE OF THE HYPER-RUNAWAY CANDIDATE HIP 60350"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1164"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","1174"],["dc.bibliographiccitation.volume","348"],["dc.contributor.author","Reed, M. D."],["dc.contributor.author","Kawaler, Steven D."],["dc.contributor.author","Zola, S."],["dc.contributor.author","Jiang, X. J."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, S. L."],["dc.contributor.author","Deetjen, J. L."],["dc.contributor.author","Kalytis, R."],["dc.contributor.author","Meistas, E."],["dc.contributor.author","Janulis, Rimvydas"],["dc.contributor.author","Alisauskas, D."],["dc.contributor.author","Krzesinski, J."],["dc.contributor.author","Vuckovic, M."],["dc.contributor.author","Moskalik, P."],["dc.contributor.author","Ogloza, W."],["dc.contributor.author","Baran, A."],["dc.contributor.author","Stachowski, G."],["dc.contributor.author","Kurtz, D. W."],["dc.contributor.author","Perez, JMG"],["dc.contributor.author","Mukadam, A. S."],["dc.contributor.author","Watson, T. K."],["dc.contributor.author","Koen, C."],["dc.contributor.author","Bradley, P. A."],["dc.contributor.author","Cunha, M. S."],["dc.contributor.author","Kilic, M."],["dc.contributor.author","Klumpe, E. W."],["dc.contributor.author","Carlton, R. F."],["dc.contributor.author","Handler, G."],["dc.contributor.author","Kilkenny, D."],["dc.contributor.author","Riddle, R."],["dc.contributor.author","Dolez, N."],["dc.contributor.author","Vauclair, G."],["dc.contributor.author","Chevreton, M."],["dc.contributor.author","Wood, M. A."],["dc.contributor.author","Grauer, A."],["dc.contributor.author","Bromage, G."],["dc.contributor.author","Solheim, J. E."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Ulla, A."],["dc.contributor.author","Burleigh, M."],["dc.contributor.author","Good, S."],["dc.contributor.author","Hurkal, O."],["dc.contributor.author","Anderson, R."],["dc.contributor.author","Pakstiene, E."],["dc.date.accessioned","2018-11-07T10:50:20Z"],["dc.date.available","2018-11-07T10:50:20Z"],["dc.date.issued","2004"],["dc.description.abstract","Since pulsating subdwarf B (sdBV or EC14026) stars were first discovered, observational efforts have tried to realize their potential for constraining the interior physics of extreme horizontal branch stars. Difficulties encountered along the way include uncertain mode identifications and a lack of stable pulsation mode properties. Here we report on Feige 48, an sdBV star for which follow- up observations have been obtained spanning more than four years. These observations show some stable pulsation modes. We resolve the temporal spectrum into five stable pulsation periods in the range 340- 380 s with amplitudes less than 1 per cent, and two additional periods that appear in one data set each. The three largest amplitude periodicities are nearly equally spaced, and we explore the consequences of identifying them as a rotationally split l = 1 triplet by consulting a representative stellar model. The general stability of the pulsation amplitudes and phases allows us to use the pulsation phases to constrain the time- scale of evolution for this sdBV star. Additionally, we are able to place interesting limits on any stellar or planetary companion to Feige 48."],["dc.identifier.doi","10.1111/j.1365-2966.2004.07438.x"],["dc.identifier.isi","000220088100006"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/48630"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0035-8711"],["dc.title","Observations of the pulsating subdwarf B star Feige 48: Constraints on evolution and companions"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","489"],["dc.bibliographiccitation.issue","5"],["dc.bibliographiccitation.journal","Astronomische Nachrichten"],["dc.bibliographiccitation.lastpage","501"],["dc.bibliographiccitation.volume","331"],["dc.contributor.author","Schuh, Sonja"],["dc.date.accessioned","2018-11-07T08:42:25Z"],["dc.date.available","2018-11-07T08:42:25Z"],["dc.date.issued","2010"],["dc.description.abstract","The disciplines of asteroseismology and extrasolar planet science overlap methodically in the branch of high-precision photometric time series observations. Light curves are, amongst others, useful to measure intrinsic stellar variability due to oscillations, as well as to discover and characterize those extrasolar planets that transit in front of their host stars, periodically causing shallow dips in the observed brightness. Both fields ultimately derive fundamental parameters of stellar and planetary objects, allowing to study for example the physics of various classes of pulsating stars, or the variety of planetary systems, in the overall context of stellar and planetary system formation and evolution. Both methods typically also require extensive spectroscopic follow-up to fully explore the dynamic characteristics of the processes under investigation. In particularly interesting cases, a combination of observed pulsations and signatures of a planet allows to characterize a system's components to a very high degree of completeness by combining complementary information. The planning of the relevant space missions has consequently converged with respect to science cases, where at the outset there was primarily a coincidence in instrumentation and techniques. Whether space- or ground-based, a specific type of stellar pulsations can themselves be used in an innovative way to search for extrasolar planets. Results from this additional method at the interface of stellar pulsation studies and exoplanet hunts in a beyond-mainstream area are presented. (C) 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim"],["dc.identifier.doi","10.1002/asna.201011366"],["dc.identifier.isi","000278544900003"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/19699"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Wiley-v C H Verlag Gmbh"],["dc.relation.issn","0004-6337"],["dc.title","Pulsations and planets: The asteroseismology-extrasolar-planet connection Ludwig Biermann Award Lecture 2009"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]