@article{HermanussenLehmannScheffler2012, author = {Hermanussen, Michael and Lehmann, Andreas and Scheffler, Christiane}, title = {Sexuelle Reifeentwicklung \& Menarchealter : Bedeutung des psychosozialen Umfeldes damals und heute}, issn = {0179-9185}, year = {2012}, language = {de} } @article{DenzJurewiczSalzer2012, author = {Denz, Rebekka and Jurewicz, Grażyna and Salzer, Dorothea M.}, title = {Einblicke in die "British Jewish Studies"}, issn = {1614-6492}, year = {2012}, language = {de} } @article{DenzJurewiczSalzer2012, author = {Denz, Rebekka and Jurewicz, Grażyna and Salzer, Dorothea M.}, title = {Insight into "British Jewish Studies"}, issn = {1614-6492}, year = {2012}, language = {en} } @article{HermanussenLehmannScheffler2012, author = {Hermanussen, Michael and Lehmann, Andreas and Scheffler, Christiane}, title = {Psychosocial Pressure and Menarche A Review of Historic Evidence for Social Amenorrhea}, series = {Obstetrical \& gynecological survey}, volume = {67}, journal = {Obstetrical \& gynecological survey}, number = {4}, publisher = {Lippincott Williams \& Wilkins}, address = {Philadelphia}, issn = {0029-7828}, doi = {10.1097/OGX.0b013e31824c94ad}, pages = {237 -- 241}, year = {2012}, abstract = {Objective: The age of menarche is usually considered to be affected by nutritional, health-related, social, and economic factors and has significantly decreased since the mid-19th century. The present study was performed to investigate whether the timing of menarche paralleled the general acceleration of physical development, or whether this pattern differed. Study Design: In all, 30 German studies on menarcheal age (n = > 200) since 1848 were collected. Frequency distributions were analyzed. Results: During the second half of the 19th and the early 20th century, mean menarcheal age decreased from 18 to 12-13 years in Europe. Yet, the data fail to support the conventional hypothesis that menarcheal age mainly depends on nutritional, health, and economic factors. Conclusions: We suggest that later than usual menarche may not necessarily be regarded as a physical illness, but in view of the apparently physiological delay of menarche in the 19th century, may be viewed as "collective social amenorrhea." Target Audience: Obstetricians \& Gynecologists and Family Physicians. Learning Objectives: After participating in this CME activity, physicians should be better able to evaluate menarche as an indicator of developmental tempo in both historical and modern settings, compare menarche in healthy mid-19th century girls with menarche in average modern girls, and assess the marked sensitivity of full pubertal development to environmental circumstances.}, language = {en} } @misc{vFrankenbergSeidlSchultheissetal.2012, author = {v. Frankenberg, Jenny and Seidl, Rainer Ottis and Schultheiss, Corinna and Frank, Ulrike and Fuß, Sophia and Stefke, Michaela and Honekamp, Andrea and Winkler, Silke and J{\"a}ckel, Annemarie and Schindler, Wencke and Wenglarczyk, Anke and Weise, Stefanie and Heide, Judith and Stadie, Nicole and Schr{\"o}der, Astrid and Baer-Henney, Dinah and van de Vijver, Ruben and Sauerland, Uli and Yatsushiro, Kazuko and Sch{\"o}ppe, Doreen and Blatter, Kristine and Faust, Verena and J{\"a}ger, Dana and Artelt, Cordula and Schneider, Wolfgang and Stanat, Petra and Bruchm{\"u}ller, Wiebke and Sj{\"o}str{\"o}m, Saana and Sch{\"u}tz, Susann and Swietza, Romy and Zielina, Marie and Freymann, Marie and Hausmann, Nadin and K{\"o}ntopp, Isabelle and Liebig, Johanna and Schnell, Annemarie and Wegener, Viktoria and Heinemann, Steffi and Haensel, Diana and M{\"u}rbe, Dirk and Pomnitz, Patricia and Siegm{\"u}ller, Julia}, title = {Spektrum Patholinguistik = Schwerpunktthema: Schluck f{\"u}r Schluck: Dysphagietherapie bei Kindern und Erwachsenen}, number = {5}, editor = {Heide, Judith and Fritzsche, Tom and Meyer, Corinna B. and Ott, Susan}, publisher = {Universit{\"a}tsverlag Potsdam}, address = {Potsdam}, organization = {Verband f{\"u}r Patholinguistik e.V.}, isbn = {978-3-86956-199-8}, issn = {1866-9433}, doi = {10.25932/publishup-5866}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-59877}, year = {2012}, abstract = {Das Herbsttreffen Patholinguistik wird seit 2007 j{\"a}hrlich vom Verband f{\"u}r Patholinguistik e.V. (vpl) durchgef{\"u}hrt. Die Jubil{\"a}umsveranstaltung am 19.11.2011 in Potsdam war nicht nur die 5. Auflage der Veranstaltung, sondern auch ein Fest zum 10j{\"a}hrigen Bestehen des Verbandes. Das Thema lautete "Schluck f{\"u}r Schluck: Dysphagietherapie bei Kindern und Erwachsenen". Im vorliegenden Tagungsband finden sich die Artikel der Hauptvortr{\"a}ge sowie die Abstracts der Posterpr{\"a}sentationen.}, language = {de} } @article{GuerreroRuizHamannetal.2012, author = {Guerrero, Mart{\´i}n A. and Ruiz, N. and Hamann, Wolf-Rainer and Chu, Y.-H. and Todt, Helge Tobias and Sch{\"o}nberner, Detlef and Oskinova, Lidia M. and Gr{\"u}ndl, R. A. and Steffen, M. and Blair, William P. and Toala, Jes{\´u}s Alberto}, title = {Rebirth of X-Ray emission from the born-again planetary Nebula A30}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, volume = {755}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, number = {2}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {0004-637X}, doi = {10.1088/0004-637X/755/2/129}, pages = {15}, year = {2012}, abstract = {The planetary nebula A30 is believed to have undergone a very late thermal pulse resulting in the ejection of knots of hydrogen-poor material. Using multi-epoch Hubble Space Telescope images, we have detected the angular expansion of these knots and derived an age of 850(-150)(+280) yr. To investigate the spectral and spatial properties of the soft X-ray emission detected by ROSAT, we have obtained Chandra and XMM-Newton deep observations of A30. The X-ray emission from A30 can be separated into two components: a point source at the central star and diffuse emission associated with the hydrogen-poor knots and the cloverleaf structure inside the nebular shell. To help us assess the role of the current stellar wind in powering this X-ray emission, we have determined the stellar parameters and wind properties of the central star of A30 using a non-LTE model fit to its optical and UV spectra. The spatial distribution and spectral properties of the diffuse X-ray emission are highly suggestive that it is generated by the post-born-again and present fast stellar winds interacting with the hydrogen-poor ejecta of the born-again event. This emission can be attributed to shock-heated plasma, as the hydrogen-poor knots are ablated by the stellar winds, under which circumstances the efficient mass loading of the present fast stellar wind raises its density and damps its velocity to produce the observed diffuse soft X-rays. Charge transfer reactions between the ions of the stellar winds and material of the born-again ejecta have also been considered as a possible mechanism for the production of diffuse X-ray emission, and upper limits on the expected X-ray production by this mechanism have been derived. The origin of the X-ray emission from the central star of A30 is puzzling: shocks in the present fast stellar wind and photospheric emission can be ruled out, while the development of a new, compact hot bubble confining the fast stellar wind seems implausible.}, language = {en} } @article{LiermannHamannOskinova2012, author = {Liermann, A. and Hamann, Wolf-Rainer and Oskinova, Lidia M.}, title = {The Quintuplet cluster III. Hertzsprung-Russell diagram and cluster age}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {540}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {0004-6361}, doi = {10.1051/0004-6361/201117534}, pages = {9}, year = {2012}, abstract = {The Quintuplet, one of three massive stellar clusters in the Galactic center (GC), is located about 30 pc in projection from Sagittarius A*. We aim at the construction of the Hertzsprung-Russell diagram (HRD) of the cluster to study its evolution and to constrain its star-formation history. For this purpose we use the most complete spectral catalog of the Quintuplet stars. Based on the K-band spectra we determine stellar temperatures and luminosities for all stars in the catalog under the assumption of a uniform reddening towards the cluster. We find two groups in the resulting HRD: early-type OB stars and late-type KM stars, well separated from each other. By comparison with Geneva stellar evolution models we derive initial masses exceeding 8 M-circle dot for the OB stars. In the HRD these stars are located along an isochrone corresponding to an age of about 4 Myr. This confirms previous considerations, where a similar age estimate was based on the presence of evolved Wolf-Rayet stars in the cluster. We derive number ratios for the various spectral subtype groups (e.g. N-WR/N-O, N-WC/N-WN) and compare them with predictions of population synthesis models. We find that an instantaneous burst of star formation at about 3.3 to 3.6 Myr ago is the most likely scenario to form the Quintuplet cluster. Furthermore, we apply a mass-luminosity relation to construct the initial mass function (IMF) of the cluster. We find indications for a slightly top-heavy IMF. The late-type stars in the LHO catalog are red giant branch (RGB) stars or red supergiants (RSGs) according to their spectral signatures. Under the assumption that they are located at about the distance of the Galactic center we can derive their luminosities. The comparison with stellar evolution models reveals that the initial masses of these stars are lower than 15 M-circle dot implying that they needed about 15 Myr (RSG) or even more than 30 Myr (RGB) to evolve into their present stage. It might be suspected that these late-type stars do not physically belong to the Quintuplet cluster. Indeed, most of them disqualify as cluster members because their radial velocities differ too much from the cluster average. Nevertheless, five of the brightest RGB/RSG stars from the LHO catalog share the mean radial velocity of the Quintuplet, and thus remain highly suspect for being gravitationally bound members. If so, this would challenge the cluster formation and evolution scenario.}, language = {en} } @article{EvansHainichOskinovaetal.2012, author = {Evans, C. J. and Hainich, Rainer and Oskinova, Lidia M. and Gallagher, J. S. and Chu, Y.-H. and Gruendl, R. A. and Hamann, Wolf-Rainer and Henault-Brunet, V. and Todt, Helge Tobias}, title = {A rare early-type star revealed in the wing of the small megellanic cloud}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, volume = {753}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, number = {2}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {0004-637X}, doi = {10.1088/0004-637X/753/2/173}, pages = {10}, year = {2012}, abstract = {Sk 183 is the visually brightest star in the N90 nebula, a young star-forming region in the Wing of the Small Magellanic Cloud (SMC). We present new optical spectroscopy from the Very Large Telescope which reveals Sk 183 to be one of the most massive O-type stars in the SMC. Classified as an O3-type dwarf on the basis of its nitrogen spectrum, the star also displays broadened He I absorption, which suggests a later type. We propose that Sk 183 has a composite spectrum and that it is similar to another star in the SMC, MPG 324. This brings the number of rare O2- and O3-type stars known in the whole of the SMC to a mere four. We estimate physical parameters for Sk 183 from analysis of its spectrum. For a single-star model, we estimate an effective temperature of 46 +/- 2 kK, a low mass-loss rate of similar to 10(-7) M-circle dot yr(-1), and a spectroscopic mass of 46(-8)(+ 9) M-circle dot (for an adopted distance modulus of 18.7 mag to the young population in the SMC Wing). An illustrative binary model requires a slightly hotter temperature (similar to 47.5 kK) for the primary component. In either scenario, Sk 183 is the earliest-type star known in N90 and will therefore be the dominant source of hydrogen-ionizing photons. This suggests Sk 183 is the primary influence on the star formation along the inner edge of the nebula.}, language = {en} } @article{HuenemoerderOskinovaIgnaceetal.2012, author = {H{\"u}nem{\"o}rder, David P. and Oskinova, Lidia M. and Ignace, Richard and Waldron, Wayne L. and Todt, Helge Tobias and Hamaguchi, Kenji and Kitamoto, Shunji}, title = {On the weak-wind problem in massive stars X-ray spectra reveal a massive hot wind in mu columbaea}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, volume = {756}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, number = {2}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {2041-8205}, doi = {10.1088/2041-8205/756/2/L34}, pages = {5}, year = {2012}, abstract = {mu Columbae is a prototypical weak-wind O star for which we have obtained a high-resolution X-ray spectrum with the Chandra LETG/ACIS instrument and a low-resolution spectrum with Suzaku. This allows us, for the first time, to investigate the role of X-rays on the wind structure in a bona fide weak-wind system and to determine whether there actually is a massive hot wind. The X-ray emission measure indicates that the outflow is an order of magnitude greater than that derived from UV lines and is commensurate with the nominal wind-luminosity relationship for O stars. Therefore, the "weak-wind problem"-identified from cool wind UV/optical spectra-is largely resolved by accounting for the hot wind seen in X-rays. From X-ray line profiles, Doppler shifts, and relative strengths, we find that this weak-wind star is typical of other late O dwarfs. The X-ray spectra do not suggest a magnetically confined plasma-the spectrum is soft and lines are broadened; Suzaku spectra confirm the lack of emission above 2 keV. Nor do the relative line shifts and widths suggest any wind decoupling by ions. The He-like triplets indicate that the bulk of the X-ray emission is formed rather close to the star, within five stellar radii. Our results challenge the idea that some OB stars are "weak-wind" stars that deviate from the standard wind-luminosity relationship. The wind is not weak, but it is hot and its bulk is only detectable in X-rays.}, language = {en} } @article{SurlanHamannKubatetal.2012, author = {Surlan, B. and Hamann, Wolf-Rainer and Kubat, Jirij and Oskinova, Lidia M. and Feldmeier, Achim}, title = {Three-dimensional radiative transfer in clumped hot star winds I influence of clumping on the resonance line formation}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {541}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {0004-6361}, doi = {10.1051/0004-6361/201118590}, pages = {11}, year = {2012}, abstract = {Context. The true mass-loss rates from massive stars are important for many branches of astrophysics. For the correct modeling of the resonance lines, which are among the key diagnostics of stellar mass-loss, the stellar wind clumping has been found to be very important. To incorporate clumping into a radiative transfer calculation, three-dimensional (3D) models are required. Various properties of the clumps may have a strong impact on the resonance line formation and, therefore, on the determination of empirical mass-loss rates. Aims. We incorporate the 3D nature of the stellar wind clumping into radiative transfer calculations and investigate how different model parameters influence the resonance line formation. Methods. We develop a full 3D Monte Carlo radiative transfer code for inhomogeneous expanding stellar winds. The number density of clumps follows the mass conservation. For the first time, we use realistic 3D models that describe the dense as well as the tenuous wind components to model the formation of resonance lines in a clumped stellar wind. At the same time, we account for non-monotonic velocity fields. Results. The 3D density and velocity wind inhomogeneities show that there is a very strong impact on the resonance line formation. The different parameters describing the clumping and the velocity field results in different line strengths and profiles. We present a set of representative models for various sets of model parameters and investigate how the resonance lines are affected. Our 3D models show that the line opacity is lower for a larger clump separation and shallower velocity gradients within the clumps. Conclusions. Our model demonstrates that to obtain empirically correct mass-loss rates from the UV resonance lines, the wind clumping and its 3D nature must be taken into account.}, language = {en} }