Galactic membership of BL Her type variable stars

As the RR Lyrae stars evolve on the Hertzsprung-Russell diagram they are believed to become short period Type II Cepheids, known as BL Her type (with a pulsation period from $1$ to $3-8$ days). Assuming that their mass is around $0.5 - 0.6 {\rm M}_{\odot}$, and that they are low metallicity objects, they were thought to belong to the halo of the Milky Way. We investigated seven Galactic short period Type II Cepheids (BL Her, SW Tau, V553 Cen, DQ And, BD Cas, V383 Cyg, and KT Com) in order to establish their membership within the Galactic structure using the kinematic approach. $Gaia$ should provide us with more data needed to conduct the study of the whole sample.Comment: 4 pages, 3 figure, proceedings of the RRL2015 - High-Precision Studies of RR Lyrae Stars conference, to appear in the Communications from the Konkoly Observator

First observations of W Virginis stars with K2: detection of period doubling

We present the first analysis of W Vir stars observed by the Kepler space telescope in the K2 mission. Clear cycle-to-cycle variation were detected in the light curves of KT Sco and the globular cluster member M80-V1. While the variations in the former star seems to be irregular on the short time scale of the K2 data, the latter appears to experience period doubling in its pulsation. Ground-based colour data confirmed that both stars are W Vir-type pulsators, while a comparison with historical photometric time-series data revealed drastic period changes in both stars. For comparison we reexamine ground-based observations of W Vir, the prototype of the class, and conclude that it shows period doubling instead of mode beating. These results support the notion that nonlinear dynamics plays an important role in the pulsation of W Virginis-type stars.Comment: 8 pages, 7 figures, accepted for publication in MNRA

Type II and anomalous Cepheids in the Kepler K2 mission

We present the results of the analysis of Type II and anomalous Cepheids using the data from the Kepler K2 mission. The precise light curves of these pulsating variable stars are the key to study the details of their pulsation, such as the period-doubling effect or the presence of additional modes. We applied the Automated Extended Aperture Photometry (autoEAP) to obtain the light curves of the targeted variable stars which were observed. The light curves were Fourier analyzed. We investigated twelve stars observed by the K2 mission, seven Type II and five anomalous Cepheids. Among the Type II Cepheids EPIC 210622262 shows period-doubling, and four stars have modulation present in their light curves which are different from the period-doubling effect. We calculated the high-order Fourier parameters for the short-period Cepheids. We also determined physical parameters by fitting model atmospheres to the spectral energy distributions. The determined distances using the parallaxes measured by the Gaia space telescope have limited precision below 16 mag for these types of pulsating stars, regardless if the inverse method is used or the statistical method to calculate the distances. The BaSTI evolutionary models were compared to the luminosities and effective temperatures. Most of the Type II Cepheids are modeled with low metallicity models, but for a few of them solar-like metallicity ([Fe/H]=0.06) model is required. The anomalous Cepheids are compared to low-metallicity single stellar models. We do not see signs of binarity among our sample stars.Comment: 21 pages, 13 figures, accepted for publication in MNRA

The role of emotional resilience, childhood parentification, and attachment style on antisocial behaviour in adulthood: a comparison of an offender and normative population

Purpose: Despite a robust link between poor caregiver attachment and antisociality, few studies have examined the influence of parentification and emotional resilience on delinquency in later life, in groups at differing risk for antisocial conduct. Methodology: This pilot study compared the influence of parentification, attachment style (avoidant or anxious) and emotional resilience on adulthood antisocial behaviour in an offender and normative sample. Of the 137 participants in this study, 66 were supervised by the National Probation Service (age M = 36.90, SD = 13.91), and 71 were recruited from community-dwelling and student populations (age M = 31.83, SD = 13.25). Findings: In partial support of the predictions, participants in the offender group reported significantly greater levels of attachment anxiety compared to the normative group. However, emotional resilience was positively associated with antisociality in the normative sample. Research implications: This small-scale investigation indicates value in exploring these specific variables in a larger, matched samples study, to enable clearer comparisons to be made between offender and normative groups. Practical implications: The preliminary findings suggest that attachment anxiety is associated with antisociality in offender populations, which indicate a therapeutic focus on attachment anxiety as part of correctional care and offender rehabilitation. Originality: This study is novel in its aim to examine the influence of childhood parentification, attachment deficits and emotional resilience on adulthood antisociality in participants from a high-risk offender sample and non-high-risk normative sample

Spectroscopy of the massive interacting binary UU Cassiopeiae

Context. The eclipsing close binary UU Cas is an interacting massive double-periodic system with a gainer star partly hidden in an accretion disk. Aims. In order to study the physics of the accretion process in greater detail, along with the structure and dynamics of the circumstellar matter in the system, we supplement our previous results obtained from photometry with an analysis of the spectra of UU Cas. Methods. We collected all available spectra used in previous publications on UU Cas and we acquired new ones. The method of disentangling was applied to this set of spectra spanning the years 2008 2021. The orbital parameters were disentangled and a fit of the separated component spectra by synthetic ones has been used to determine the physical parameters of the component stars. We compared the results to models of the evolution of interacting binaries. Results. We found that in addition to the dominant role of the donor star and a weak contribution of the gainer, the line profiles are strongly influenced by the circumstellar matter. The absorption lines reveal a presence of a disk wind emanating above the orbital plane. The variability of Hα emission yields evidence of changes in the structure of the circumstellar matter on a timescale of several orbital periods. © ESO 2022.Grantová Agentura České Republiky, GA ČR: 22-34467S; Fondo Nacional de Desarrollo Científico y Tecnológico, FONDECYT: 1190621, ANID PIA/BASAL FB210003, AP08856419, IN102120; Bulgarian National Science Fund, BNSF: DN 18/13-12.12.2017; Ministry of Education and Science of the Russian Federation, Minobrnauka: 075-15-2020-780, 780-10, FEUZ-2020-0030; Ministry of Education and Science of the Republic of Kazakhstan; Ministarstvo Prosvete, Nauke i Tehnološkog Razvoja, MPNTR: 21202285, 451-03-68/2020-14/200002; Centro de Astrofísica y Tecnologías Afines, CATA: PFB–06/2007The authors highly appreciate valuable comments and suggestions by the referee Herman Hensberge, which helped to improve this paper. We acknowledge the allotment of observing time at San Pedro Mártir observatory, UNAM, Baja California, Mexico. We are also indebted to Drs. Gyula Szabó and his colleagues for obtaining the GAO spectra, Zlatan Zvetanov for the APO spectra, and Brankica Kubátová, Petr Kabáth and other colleagues from AI for the AIO spectra. P. Hadrava was supported by project RVO 67985815, M. Cabezas also by GAČR 22-34467S. G. Djurašević, J. Petrović and M. I. Jurkovic acknowledge the financial support from the Ministry of Education, Science and Technological Development of the Republic of Serbia through contract No. 451-03-68/2020-14/200002. J. Garcés acknowledges support by ANID project 21202285. S. Yu. Gorda was supported in part by the Ministry of Science and Higher Education of the Russian Federation (projects no. FEUZ-2020-0030 and no. 075-15-2020-780, contract 780-10). H. Markov acknowledges the support by Bulgarian National Science Fund under contract DN 18/13-12.12.2017. R. E. Mennickent acknowledges support by BASAL Centro de Astrofísica y Tecnologías Afines (CATA) PFB–06/2007, FONDECYT 1190621 and the grant ANID PIA/BASAL FB210003. S. Zharikov acknowledges PAPIIT grants IN102120 and grant no. AP08856419 of the Science Committee of the Ministry of Education and Science of the Republic of Kazakhstan.Acknowledgements. The authors highly appreciate valuable comments and suggestions by the referee Herman Hensberge, which helped to improve this paper. We acknowledge the allotment of observing time at San Pedro Mártir observatory, UNAM, Baja California, Mexico. We are also indebted to Drs. Gyula Szabó and his colleagues for obtaining the GAO spectra, Zlatan Zvetanov for the APO spectra, and Brankica Kubátová, Petr Kabáth and other colleagues from AI for the AIO spectra. P. Hadrava was supported by project RVO 67985815, M. Cabezas also by GACˇ R 22-34467S. G. Djurašević, J. Petrović and M. I. Jurkovic acknowledge the financial support from the Ministry of Education, Science and Technological Development of the Republic of Serbia through contract No. 451-03-68/2020-14/200002. J. Garcés acknowledges support by ANID project 21202285. S. Yu. Gorda was supported in part by the Ministry of Science and Higher Education of the Russian Federation (projects no. FEUZ-2020-0030 and no. 075-15-2020-780, contract 780-10). H. Markov acknowledges the support by Bulgarian National Science Fund under contract DN 18/13-12.12.2017. R. E. Mennickent acknowledges support by BASAL Centro de Astrofísica y Tecnologías Afines (CATA) PFB–06/2007, FONDECYT 1190621 and the grant ANID PIA/BASAL FB210003. S. Zharikov acknowledges PAPIIT grants IN102120 and grant no. AP08856419 of the Science Committee of the Ministry of Education and Science of the Republic of Kazakhstan.IRAF is distributed by the National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract to the National Science Foundation of the United States

Partial Wave Analysis of the Reaction p(3.5GeV)+p→pK+Λp(3.5 GeV)+p \to pK^+\Lambda to Search for the "ppK−ppK^-" Bound State

Employing the Bonn-Gatchina partial wave analysis framework (PWA), we have analyzed HADES data of the reaction $p(3.5GeV)+p\to pK^{+}\Lambda$. This reaction might contain information about the kaonic cluster "$ppK^-$" via its decay into $p\Lambda$. Due to interference effects in our coherent description of the data, a hypothetical $\overline{K}NN$ (or, specifically "$ppK^-$") cluster signal must not necessarily show up as a pronounced feature (e.g. a peak) in an invariant mass spectra like $p\Lambda$. Our PWA analysis includes a variety of resonant and non-resonant intermediate states and delivers a good description of our data (various angular distributions and two-hadron invariant mass spectra) without a contribution of a $\overline{K}NN$ cluster. At a confidence level of CL$_{s}$=95\% such a cluster can not contribute more than 2-12\% to the total cross section with a $pK^{+}\Lambda$ final state, which translates into a production cross-section between 0.7 $\mu b$ and 4.2 $\mu b$, respectively. The range of the upper limit depends on the assumed cluster mass, width and production process.Comment: 7 Pages, 5 Figure

Deep sub-threshold Ξ−\Xi^- production in Ar+KCl reactions at 1.76A GeV

We report first results on a deep sub-threshold production of the doubly strange hyperon $\Xi^-$ in a heavy-ion reaction. At a beam energy of 1.76A GeV the reaction Ar+KCl was studied with the High Acceptance Di-Electron Spectrometer (HADES) at SIS18/GSI. A high-statistics and high-purity $\Lambda$ sample was collected, allowing for the investigation of the decay channel $\Xi^- \to \Lambda \pi^-$. The deduced $\Xi^-/(\Lambda+\Sigma^0)$ production ratio of $(5.6 \pm 1.2 ^{+1.8}_{-1.7})\cdot 10^{-3}$ is significantly larger than available model predictions.Comment: 4 pages, including 4 figure