Fe I and Fe II Abundances of Solar-Type Dwarfs in the Pleiades Open Cluster

We have derived Fe abundances of 16 solar-type Pleiades dwarfs by means of an equivalent width analysis of Fe I and Fe II lines in high-resolution spectra obtained with the Hobby - Eberly Telescope and High Resolution Spectrograph. Abundances derived from Fe II lines are larger than those derived from Fe I lines (herein referred to as over-ionization) for stars with Teff < 5400 K, and the discrepancy (deltaFe = [Fe II/H] - [Fe I/H]) increases dramatically with decreasing Teff, reaching over 0.8 dex for the coolest stars of our sample. The Pleiades joins the open clusters M 34, the Hyades, IC 2602, and IC 2391, and the Ursa Major moving group, demonstrating ostensible over-ionization trends. The Pleiades deltaFe abundances are correlated with Ca II infrared triplet and Halpha chromospheric emission indicators and relative differences therein. Oxygen abundances of our Pleiades sample derived from the high-excitation O I triplet have been previously shown to increase with decreasing Teff, and a comparison with the deltaFe abundances suggests that the over-excitation (larger abundances derived from high excitation lines relative to low excitation lines) and over-ionization effects that have been observed in cool open cluster and disk field main sequence (MS) dwarfs share a common origin. Star-to-star Fe I abundances have low internal scatter, but the abundances of stars with Teff < 5400 K are systematically higher compared to the warmer stars. The cool star [Fe I/H] abundances cannot be connected directly to over-excitation effects, but similarities with the deltaFe and O I triplet trends suggest the abundances are dubious. Using the [Fe I/H] abundances of five stars with Teff > 5400 K, we derive a mean Pleiades cluster metallicity of [Fe/H] = +0.01 +/- 0.02.Comment: 32 pages, 7 figures, 7 tables; accepted by PAS

The Reason for the Addled Egg

What is so rare as a ·good egg in in September or October! If ever there come perfect eggs, it seems my tough luck to miss them. This thought no doubt comes thru the mind of many a housewife as she breaks open a dozen or more high-priced eggs, and finds only a few that are usable

Colour perception changes with basic colour word comprehension

Recent work has investigated the origin of infant colour categories, showing pre-linguistic infants categorise colour even in the absence of colour words. These infant categories are similar but not identical to adult categories, giving rise to an important question about how infant colour perception changes with the learning of colour words. Here we present two novel paradigms in which 12- and 19-month-old participants learning English as their first language were assessed on their perception of colour, while data on their colour word comprehension were also collected. Results indicate that participants' perception of colours close to the colour category boundaries dramatically change after colour word learning. The results highlight the shift made from infant colour categories to adult-like linguistically mediated colour categories that accompanies colour word learning

A Case of Late-Onset Gemcitabine Lung Toxicity

Gemcitabine is a chemotherapeutic agent used for the treatment of a number of malignancies. Although its major dose-limiting side effect is myelosuppression, many pulmonary toxicities have been described with its use. Severe pulmonary toxicity is rare, but symptoms tend to be rapid in onset and potentially deadly. The average time from initiation of chemotherapy to onset of symptoms is less than two months. The most effective therapy is steroid administration, the efficacy of which has been variable. In this report, we describe a unique case of gemcitabine pulmonary toxicity in a patient who did not experience symptoms of pulmonary dysfunction until after 1 year of treatment. Her symptoms did not improve rapidly with steroids, nor did she rapidly decompensate as has been frequently described. To our knowledge, this is one of the first reported descriptions of late-onset gemcitabine lung toxicity

The Iowa Homemaker vol.1, no.7

Table of Contents The Yea and Nay of Newspaper Work for Women by Helen Easter, page 1 Facts About the Feeding of Young Children by Belle Lowe, page 2 An Inventory of Skill for the Honest Homewife by Elizabeth Storm, page 3 Who Waits on Your Table? by Beth Bailey, page 4 My First Flight in the Pursuit of Beauty by Eda Lord Murphy, page 4 A New Cure for the “Run-Down” Housewife by Carrie Plunkett, page 5 A Pattern in Hot Lunch Service for Rural Schools by Grace McIlrath, page 6 The Reason for the Addled Egg by C. H. Plunkett, page 7 Short Cuts in Sewing by Helen Easter, page 1

The Algebraic Bethe Ansatz and Tensor Networks

We describe the Algebraic Bethe Ansatz for the spin-1/2 XXX and XXZ Heisenberg chains with open and periodic boundary conditions in terms of tensor networks. These Bethe eigenstates have the structure of Matrix Product States with a conserved number of down-spins. The tensor network formulation suggestes possible extensions of the Algebraic Bethe Ansatz to two dimensions

An Asymmetric Cone Model for Halo Coronal Mass Ejections

Due to projection effects, coronagraphic observations cannot uniquely determine parameters relevant to the geoeffectiveness of CMEs, such as the true propagation speed, width, or source location. The Cone Model for Coronal Mass Ejections (CMEs) has been studied in this respect and it could be used to obtain these parameters. There are evidences that some CMEs initiate from a flux-rope topology. It seems that these CMEs should be elongated along the flux-rope axis and the cross section of the cone base should be rather elliptical than circular. In the present paper we applied an asymmetric cone model to get the real space parameters of frontsided halo CMEs (HCMEs) recorded by SOHO/LASCO coronagraphs in 2002. The cone model parameters are generated through a fitting procedure to the projected speeds measured at different position angles on the plane of the sky. We consider models with the apex of the cone located at the center and surface of the Sun. The results are compared to the standard symmetric cone model