Phase Dependent Spectroscopy of Mira Variable Stars

Spectroscopic measurements of Mira variable stars, as a function of phase, probe the stellar atmospheres and underlying pulsation mechanisms. For example, measuring variations in TiO, VO, and ZrO with phase can be used to help determine whether these molecular species are produced in an extended region above the layers where Balmer line emission occurs or below this shocked region. Using the same methods, the Balmer-line increment, where the strongest Balmer line at phase zero is H-delta and not H-alpha can be measured and explanations tested, along with another peculiarity, the absence of the H-epsilon line in the spectra of Miras when other Balmer lines are strong. We present new spectra covering the spectral range from 6200 Angstroms to 9000 Angstroms of 20 Mira variables. A relationship between variations in the CaII IR triplet and H-alpha as a function of phase support the hypothesis that H-epsilon's observational characteristics result from an interaction of H-epsilon photons with the CaII H line. New periods and epochs of variability are also presented for each star

Nestmate recognition in odorous house ants (Tapinoma sessile): Effects of social plasticity, urbanization, and laboratory maintenance

Odorous house ants (Tapinoma sessile) are a widespread North American ant species and common nuisance pest. In addition to their pest status, odorous house ants are of interest as a model system for understanding the factors that lead to variable queen number and nesting strategy across ants, as well as possible insight into common traits of exotic invasive (or “tramp”) ant species. While T. sessile is native to North America, in urban environments it forms large supercolonies with many queens and nest sites connected by trails, similar to a variety of exotic invasive ants, most of which are of tropical or subtropical origin. To determine the extent to which odorous house ants follow patterns of reduced conspecific aggression commonly found in other ant species with similar polygynous colony structures, a variety of behavioral assays were used to assess aggressive behavior between members of colonies from natural and urban environments. For all three assays, urban polygynous colonies were in fact the most aggressive, in contrast to my predictions. While the reasons for higher aggression in urban colonies are not clear, it is possible that the natural colonies of odorous house ants are simply too small to risk losses due to conflict. The extremely large worker populations of urban supercolonies may allow different competitive strategies that were previously impossible for T. sessile to utilize successfully. While a large proportion of the research on ant behavior and chemical ecology is performed within a laboratory setting, relatively few studies have directly examined the effects of laboratory maintenance on ants. Using a combination of methods from behavioral and chemical ecology, I compared workers that had been maintained in a lab over time to workers freshly collected from the field at a variety of time points. In contrast with previous research on the topic, this study had the added strength of taking several observations in a series over time, rather than simply comparing an initial and final time point. Contrary with those studies, I found no effect of lab maintenance on ant behavior. Cuticular hydrocarbon profiles were significantly altered by laboratory maintenance, however, this effect was small when compared to the differences in cuticular hydrocarbon profiles between colonies. However, given the likelihood of different responses for different species as well as the possibility of stronger effects with longer durations of laboratory maintenance, I encourage others to replicate my method with a broad variety of ant species and conditions. Taken together, these findings demonstrate that even for well-established patterns in ecology, any given species may deviate from the expectation for a variety of reasons. Continuing to test established theory with a wider range of organisms and conditions will ultimately strengthen our ability to create predictive theory for systems which are not currently as well understood

The formation process of the He I lambda 10830 line in cool giant stars

The Final Report on the formation process of the He I lambda 10830 line in cool giant stars is presented. The research involves observing a sample of cool giant stars with ROSAT. These stars were selected from the list of bright stars which display He I lambda 10830 in absorption or emission and lie on the cool side of the coronal dividing line. With measured x ray fluxes or upper limits measured by the Position Sensitive Proportional Counter (PSPC), the role x rays play in the formation of this important line was investigated using the non-LTE radiative transfer code PANDORA. Hydrodynamic calculations were performed to investigate the contributions of acoustic wave heating in the formation of this line as well

Spatially resolving the outer atmosphere of the M giant BK Vir in the CO first overtone lines with VLTI/AMBER

The mass-loss mechanism in normal K--M giant stars with small variability amplitudes is not yet understood, although they are the majority among red giant stars. We present high-spatial and high-spectral resolution observations of the 2.3 micron CO lines in the M7 giant BK Vir with a spatial resolution of 9.8 mas and a spectral resolution of 12000, using AMBER at the Very Large Telescope Interferometer (VLTI). The angular diameters observed in the CO lines are 12--31% larger than those measured in the continuum. We also detected asymmetry in the CO line-forming region. The data taken 1.5 months apart show possible time variation on a spatial scale of 30 mas (corresponding to 3 x stellar diameter) at the CO band head. Comparison of the observed data with the MARCS photospheric model shows that whereas the observed CO line spectrum can be well reproduced by the model, the angular sizes observed in the CO lines are much larger than predicted by the model. Our model with two additional CO layers above the MARCS photosphere reproduces the observed spectrum and interferometric data in the CO lines simultaneously. This model suggests that the inner CO layer at ~1.2 stellar radii is very dense and warm with a CO column density of ~10^{22} cm^{-2} and temperatures of 1900--2100K, while the outer CO layer at 2.5--3.0 stellar radii is characterized by column densities of 10^{19}--10^{20} cm^{-2} and temperatures of 1500--2100K. Our AMBER observations of BK Vir have spatially resolved the extended molecular outer atmosphere of a normal M giant in the individual CO lines for the first time. The temperatures derived for the CO layers are higher than or equal to the uppermost layer of the MARCS photospheric model, implying the operation of some heating mechanism in the outer atmosphere.Comment: 10 pages, 9 figures, accepted for publication in Astronomy and Astrophysic

Multiwavelength Study of Pulsation and Dust Production in Mira Variables Using Optical Interferometry for Constraints

Optical interferometry is a technique by which the diameters and indeed the direct pulsations of stars are routinely being measured. As a follow-on to a 7 year interferometric campaign to measure the pulsations of over 100 mira variables, our team has been using the Spitzer Space Telescope to obtain 95 mid-infrared spectra of 25 miras during their pulsations over one year while simultaneously ascertaining their near-infrared diameters using the Palomar Testbed Interferometer. These data will then be combined with modeling from NLTE and radiative transfer codes to place hard constraints on our understanding of these stars and their circumstellar environments. We present some initial results from this work and discuss the next steps toward fully characterizing the atmosphere, molecular photosphere and dust production in mira variables.Some of the work on this project was supported through a NASA grant to the PI and team associated with Spitzer program GO50717

Radiative transfer in the dynamic atmospheres of Mira-type variables

This NASA grant covers our ADP research program, which involved detailed radiative transfer calculations of hydrodynamic models of pulsating asymptotic giant branch stars. Synthetic spectra resulting from these calculations are compared with International Ultraviolet Explorer (IUE) observations of these stars to test the validity of the models

PAIRED COMPETITION ANALYSIS USING MIXED MODELS

Urban and rural colonies of odorous house ants (Tapinoma sessile) have very different social structures. Urban colonies are very large with hundreds of cohabiting queens, while rural colonies are small with only one queen. To investigate whether worker ant aggressiveness varies across these two colony types, an experiment was performed using an aggression assay, in which 50 ants from each of two colonies were placed in a petri dish and allowed to fight. The response was the total number of dead ants within 24 hours. Because the ants were all the same species and not marked by colony, the number of dead ants per colony could not be determined. A total of 138 colony pairings, involving six urban (U) and seven rural (R) colonies, were used in the experiment. Interest was in comparing the three types of pairings (UU, UR, and RR) to see if there is an ordering based on aggressiveness (e.g., μUU \u3c μUR \u3c μRR). A linear mixed model is proposed to account for the fact that multiple assays involve ants from the same colony (i.e., to account for between colony variation in aggressiveness). However, the incorporation of random colony factors is not feasible for this study because of the UU and RR assays. As a result, we perform this mixed model analysis by specifying the covariance matrix (i.e., using the LINEAR covariance structure). A simulation study is used to assess the Type I and Type II errors of this mixed model approach relative to the standard one-way ANOVA. We conclude with an analysis of the real data set

Blinded by the Lines: Mid-IR Spectra of Mira Variables Taken with Spitzer

We present preliminary analysis of mid-infrared spectra of M-type and C-type Mira variables. Due to the brightness of this sample, it is straightforward to monitor changes with phase in the infrared spectral features of these regular pulsators. We have spectra of 25 Mira variables, taken with phase, using the Spitzer Infrared Spectrograph (IRS) high-resolution module. Each star has multiple spectra obtained over a one-year period from 2008-09. This is a rich, unique data set due to multiple observations of each star and the high signal-to-noise ratio from quick exposure times to prevent saturation of the IRS instrument. This paper focuses on the 17.6 and 33.2 micron lines shared by M-types and C-types. These are mostly emission lines that change with phase. We discuss preliminary physical diagnostics for the atmospheres based on the lines, as well as possible line identifcations such as fuorescence of metal species

Climate change and ecological intensification of agriculture in sub-Saharan Africa-A systems approach to predict maize yield under push-pull technology

Assessing effects of climate change on agricultural systems and the potential for ecological intensification to increase food security in developing countries is essential to guide management, policy-making and future research. 'Push-pull' technology (PPT) is a poly-cropping design developed in eastern Africa that utilizes plant chemicals to mediate plant-insect interactions. PPT application yields significant increases in crop productivity, by reducing pest load and damage caused by arthropods and parasitic weeds, while also bolstering soil fertility. As climate change effects may be species-and/or context-specific, there is need to elucidate how, in interaction with biotic factors, projected climate conditions are likely to influence future functioning of PPT. Here, we first reviewed how changes in temperature, precipitation and atmospheric CO2 concentration can influence PPT components (i.e., land use, soils, crops, weeds, diseases, pests and their natural enemies) across sub-Saharan Africa (SSA). We then imposed these anticipated responses on a landscape-scale qualitative mathematical model of maize production under PPT in eastern Africa, to predict cumulative, structure-mediated impacts of climate change on maize yield. Our review suggests variable impacts of climate change on PPT components in SSA by the end of the 21st century, including reduced soil fertility, increased weed and arthropod pest pressure and increased prevalence of crop diseases, but also increased biological control by pests' natural enemies. Extrapolating empirical evidence of climate effects to predict responses to projected climate conditions is mainly limited by a lack of mechanistic understanding regarding single and interactive effects of climate variables on PPT components. Model predictions of maize yield responses to anticipated impacts of climate change in eastern Africa suggest predominantly negative future trends. Nevertheless, maize yields can be sustained or increased by favourable changes in system components with less certain future behaviour, including higher PPT adoption, preservation of field edge density and agricultural diversification beyond cereal crops

Pulsating Stellar Atmospheres

We review the basic concepts, the present state of theoretical models, and the future prospects for theory and observations of pulsating stellar atmospheres. Our emphasis is on radially pulsating cool stars, which dynamic atmospheres provide a general example for the differences with standard static model atmospheres.Comment: 9 pages, 2 figs, LaTex, in Proc. of IAU Symp 189, "Fundamental Stellar Properties...", eds. T. R. Bedding, A. J. Booth and J. Davis, Kluwer, p.253, 199