Schuh, Sonja

[["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","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","445"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.lastpage","450"],["dc.bibliographiccitation.volume","607"],["dc.contributor.author","Reed, M. D."],["dc.contributor.author","Green, Elizabeth M."],["dc.contributor.author","Callerame, K."],["dc.contributor.author","Seitenzahl, I. R."],["dc.contributor.author","White, B. A."],["dc.contributor.author","Hyde, E. A."],["dc.contributor.author","Giovanni, M. K."],["dc.contributor.author","Ostensen, Roy H."],["dc.contributor.author","Bronowska, A."],["dc.contributor.author","Jeffery, E. J."],["dc.contributor.author","Cordes, O."],["dc.contributor.author","Falter, S."],["dc.contributor.author","Edelmann, H."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schuh, S. L."],["dc.date.accessioned","2018-11-07T10:48:53Z"],["dc.date.available","2018-11-07T10:48:53Z"],["dc.date.issued","2004"],["dc.description.abstract","A new class of pulsating subdwarf B stars has recently been announced by Green and coworkers. Here we present a follow-up paper describing our observations and the pulsation structure of the class prototype PG 1716+426. The oscillations are multiperiodic with periods between 0.8 and 1.4 hr (180-340 muHz) and semiamplitudes less than 0.2%. We also observe that the periods and amplitudes appear variable, making the pulsation structure of PG 1716 complicated. The periods are an order of magnitude longer than those seen in EC 14026 (sdBV) stars, implying that they are gravity modes rather than pressure modes. As such, they represent a new class of variable star."],["dc.identifier.doi","10.1086/383260"],["dc.identifier.isi","000221523900038"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/48308"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-637X"],["dc.title","Discovery of gravity-mode pulsators among subdwarf B stars: PG 1716+426, the class prototype"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]