Aims. We investigate the role of convection in the formation of atomic and molecular lines in the atmosphere of a red giant star. For this purpose we study the formation properties of spectral lines that belong to a number of astrophysically important tracer elements, including neutral and singly ionized atoms (Li Ba ii, and Eu ii), and molecules (CH, CO, C 2 , NH, CN, and OH).Methods. We focus our investigation on a prototypical red giant located close to the red giant branch (RGB) tip (T eff = 3660 K, log g = 1.0, [M/H] = 0.0). We used two types of model atmospheres, 3D hydrodynamical and classical 1D, calculated with the CO 5 BOLD and LHD stellar atmosphere codes, respectively. Both codes share the same atmospheric parameters, chemical composition, equation of state, and opacities, which allowed us to make a strictly differential comparison between the line formation properties predicted in 3D and 1D. The influence of convection on the spectral line formation was assessed with the aid of 3D-1D abundance corrections, which measure the difference between the abundances of chemical species derived with the 3D hydrodynamical and 1D classical model atmospheres. Results. We find that convection plays a significant role in the spectral line formation in this particular red giant. The derived 3D-1D abundance corrections rarely exceed ±0.1 dex when lines of neutral atoms and molecules are considered, which is in line with the previous findings for solar-metallicity red giants located on the lower RGB. The situation is different with lines that belong to ionized atoms, or to neutral atoms with high ionization potential. In both cases, the corrections for high-excitation lines (χ > 8 eV) may amount to Δ 3D−1D ∼ −0.4 dex. The 3D-1D abundance corrections generally show a significant wavelength dependence; in most cases they are smaller in the near-infrared, at 1600-2500 nm.

We investigate the influence of convection on the formation of molecular spectral lines in the atmospheres of late-type giants. For this purpose we use the 3D hydrodynamical CO 5 BOLD and classical 1D LHD stellar atmosphere codes and synthesize a number of fictitious lines belonging to a number of astrophysically relevant molecules, C 2 , CH, CN, NH, OH. We find that differences between the abundances obtained from molecular lines using the 3D and 1D model atmospheres are generally small at [M/H]=0.0, but they quickly increase at sub-solar metallicities and may reach ∼ −0.9 dex at [M/H]=-3.0. The 3D-1D abundance corrections show a significant dependence on the spectral line parameters, such as wavelength and excitation potential. Our comparison, therefore, points to a complex interplay between the spectral line formation and convection that should be properly adressed in stellar abundance analysis. 11th Symposium on Nuclei in the Cosmos, NIC XI

Persistent idiopathic facial pain (PIFP) is an enigmatic condition presenting with variable features. Psychiatric comorbidities are speculated to influence PIFP. In this study, the authors evaluated patients with PIFP through the hospital anxiety and depression scale, facial expression analysis, and electrodermal activity. A total of 67 respondents enrolled as the experimental group and 28 participants as the control group. Pain scores were higher in the experimental group (5.24; SD 2.349) P < 0.001 depression (5.58 (SD 3.766) versus 3.07 (SD 2.418), P = 0.002) and anxiety scores (9.78 (SD 4.923) versus 6.75 (SD 4.097) P = 0.007) were higher in the experimental group. The experimental group expressed more negative episodes ( P = 0.024); Electrodermal Activity data in terms of peaks/min ( P = 0.872) and average peak amplitude ( P = 0.168) were not significantly different between the groups. It may be concluded that pain levels may be influenced by psychiatric comorbidity as PIFP patients showed insignificant physiological response to pain.

Abstract.We compare the abundances of various chemical species as derived with 3D hydrodynamical and classical 1D stellar atmosphere codes in a late-type giant characterized by T eff = 3640 K, log g = 1.0, [M/H]= 0.0. For this particular set of atmospheric parameters the 3D-1D abundance differences are generally small for neutral atoms and molecules but they may reach up to 0.3-0.4 dex in case of ions. The 3D-1D differences generally become increasingly more negative at higher excitation potentials and are typically largest in the optical wavelength range. Their sign can be both positive and negative, and depends on the excitation potential and wavelength of a given spectral line. While our results obtained with this particular late-type giant model suggest that 1D stellar atmosphere models may be safe to use with neutral atoms and molecules, care should be taken if they are exploited with ions.Keywords. Stars: late-type, stars: atmospheres, stars: abundances, convection Current 3-dimensional hydrodynamical codes have taken stellar atmosphere modeling to a new level of realism, making it possible to assess the influence of various nonstationary phenomena (e.g., convection) on the observable properties of various classes of stars. It has been recently demonstrated by Collet et al. (2007) that in the domain of latetype giants, which are important tracers of intermediate age and old stellar populations, the use of 1D classical and 3D hydrodynamical stellar atmosphere models may result in substantially different elemental abundances, especially at [M/H] −2.0. However, since Collet et al. (2007) have studied only stars located close to the base of RGB it is not clear whether similar conclusions would apply at lower effective temperatures and gravities.In this work we used a model of a considerably cooler late-type giant (T eff = 3640 K, log g = 1.0, [M/H]= 0.0) to assess the 3D-1D abundance differences at low effective temperatures. For this purpose we synthesized a number of artificial spectral lines at different wavelengths and with different excitation potentials, corresponding to various neutral atoms, ions and molecules. 3D and 1D stellar atmosphere models used in the spectral line synthesis were calculated with the CO 5 BOLD and LHD stellar atmosphere codes using identical atmospheric parameters (Freytag et al. 2002;Freytag et al. 2003;Wedemeyer et al. 2004). The CO 5 BOLD simulation was run on a Cartesian grid of 150x150x151 grid points (xyz, respectively). Both models shared identical equation of state and opacities. 209at https://www.cambridge.org/core/terms. https://doi