Of productive germs and the immortal soul : Friedrich Schlegel’s writings on language and early biological theory

Friedrich Schlegel's lasting contribution to linguistics is usually seen in the impact that his book "Über die Sprache und Weisheit der Indier" from 1808 left on comparative linguistics and on the study of Sanskrit. Schlegel was one of the first European scholars to have studied Sanskrit extensively and he made a number of translations of Sanskrit literature into German which make up one third of "Über die Sprache und Weisheit der Indier". Schlegel's book is widely regarded as a founding document both of comparative linguistics and of indology, a fact which is quite remarkable in light of the development of Schlegel's thought after this text. His interest in Indian studies ceased more or less directly with the publication of this work, while his thoughts on language became more and more suffused by transcendental philosophy

A new eclipsing binary system with a pulsating component detected by CoRoT

We report the discovery of CoRoT 102980178 (R.A.= 06:50:12.10, Dec.= -02:41:21.8, J2000) an Algol-type eclipsing binary system with a pulsating component (oEA). It was identified using a publicly available 55 day long monochromatic lightcurve from the CoRoT initial run dataset (exoplanet field). Eleven consecutive 1.26m deep total primary and the equal number of 0.25m deep secondary eclipses (at phase 0.50) were observed. The following light elements for the primary eclipse were derived: HJD_MinI= 2454139.0680 + 5.0548d x E. The lightcurve modeling leads to a semidetached configuration with the photometric mass ratio q=0.2 and orbital inclination i=85 deg. The out-of-eclipse lightcurve shows ellipsoidal variability and positive O'Connell effect as well as clear 0.01m pulsations with the dominating frequency of 2.75 c/d. The pulsations disappear during the primary eclipses, which indicates the primary (more massive) component to be the pulsating star. Careful frequency analysis reveals the second independent pulsation frequency of 0.21 c/d and numerous combinations of these frequencies with the binary orbital frequency and its harmonics. On the basis of the CoRoT lightcurve and ground based multicolor photometry, we favor classification of the pulsating component as a gamma Doradus type variable, however, classification as an SPB star cannot be excluded.Comment: 16 pages, 7 figures, 3 tables, accepted to Communications in Asteroseismolog

Why do some spotted stars become bluer as they become fainter?

Chromospherically active, spotted stars generally become redder as well as fainter when large starspots rotate into view on the stellar disc. However, the RS CVn system UX Ari (a triple-lined system), becomes bluer as it gets fainter. One possible explanation is that hot, bright facular regions accompany the cool, dark photospheric spots of the active component. The bluer flux of the hotter, inactive component does not appear to be sufficient to explain the observed behaviour. We have begun a search for additional chromospherically active stars with a similar relation between colour and brightness, to investigate whether these relations can be explained in the same way. Our results for V711 Tau are presented here, and we conclude that the faculae explanation holds also in this case.Comment: 3 pages, 1 figure, proceedings from the 13th Cambridge Workshop on cool stars, stellar systems, and the Sun, Hamburg, Germany, July 2004, ESA-SP, in pres

Medicare Part D: Simplifying the Program and Improving the Value of Information for Beneficiaries

Examines options for simplifying Medicare's prescription drug benefit, including streamlining benefit procedures and descriptions; further standardizing benefit parameters, especially cost-sharing rules; and modifying rules on plan formularies

Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I

We have embarked on a project, under the aegis of the Nearby Stars (NStars)/ Space Interferometry Mission Preparatory Science Program to obtain spectra, spectral types, and, where feasible, basic physical parameters for the 3600 dwarf and giant stars earlier than M0 within 40 parsecs of the sun. In this paper we report on the results of this project for the first 664 stars in the northern hemisphere. These results include precise, homogeneous spectral types, basic physical parameters (including the effective temperature, surface gravity and the overall metallicity, [M/H]) and measures of the chromospheric activity of our program stars. Observed and derived data presented in this paper are also available on the project's website at http://stellar.phys.appstate.edu/