Sulfur, manganese … in the Galaxy Mishenina T.V., Gorbaneva T.I., Paramonova O.P., Basak N.Yu., Kovtyukh V.V., Korotin S.A., Chekhonadskih F. +…… Odessa Astronomical Observatory +…. Preliminary plan 2014-2016 Workshop "Heavy elements nucleosynthesis and galactic chemical evolution". September 8 – September 11, 2013 Moscow, Russia

Aims (sulfur): Abundance of sulfur shows a larger scatter than other alpha-elements (Luck et al., 2011; Lemasle et al. 2013). This is certainly due to the fact that sulfer abundances are based on typically 2-4 lines in IR region of spectra, which are subject to significant NLTE departures. It would be very important to reduce the scatter and to ascertain the sulfur abundances in Cepheids and dwarfs in the Galactic disc. This would enable us a sulfur abundance gradient in the disk using Cepheids. The distribution of sulfur in the disc dwarfs allows to trace the evolution of sulfur (to estimate the different sources of S production) at all ages of the disc stars.

Aims (manganese): Manganese is an element of the iron peak The behavior of Mn is inverse to that of alpha-elements (Wallerstein, 1962, Gratton 1989) and differs from that of iron group elements. SN II and SN Ia in different proportion as the main sources of Mn production. The behavior of manganese in the thick and the thin disc of the Galaxy allows us to consider some sources of they production and to precise its contribution in manganese enrichment.

Preliminary results for Sulfur and Manganese The spectra of stars were obtained with S/N about 100-350 using the 1.93 m telescope at the Observatoire de Haute-Provence (OHP, France), equipped with the echelle-spectrograph s ELODIE (Barrane et al., 1996ж; a resolving power is R = 42 000) and SOPHIE (Perruchot et al., 2008), a resolving power is R = 75 000). The spectral processing was carried out using the processing codes (Katz et al., 1998; Galazutdinov, 1992). The parameters of the investigated stars were taken from our earlier studies ( e.g.Mishenina et al. 2013).

Sulfur abundance The abundances of sulfur were obtained for 27 dwarfs under the LTE approximations upon the synthetic spectrum method, taking into account the HFS and the oscillator strengths of lines by Korotin (2009). The Kurucz model of atmospheres (Kurucz, 1993) and the new version of the STARSP code by Tsymbal (1996) were used. We used for the sulfur and iron abundance determination the lines in the visual region (of 6743-6762 ÅÅ). The NLTE corrections for those lines did not exceed -0.1 dex (Korotin, 2009).

The observed and synthetic spectra fitting for star HD108954

The model predictions by Timmes, Woosley&Weaver (1995) and the data of other authors (our data – as asterisks, Clegg et al. 1981 – as triangles, Francois 1987, 1988 – as squares and circles). The production of all stable sulfur isotopes in the massive-star models is sufficient to explain the solar abundance (Timmes et al. 1995) ???

Sulfur for Cepheids 250 Cepheids VLT (ESO) + McDonald (USA) HFS + NLTE approximation using a 65-level model of the SI atom (Korotin S., 2009) (Visual + IR)

Manganese The observations from ELODIE and SOPHIE (1.93m, OHP, France) for 200 dwarfs of the thin and thick disk stars HFS from (Prochaska et al., 2000) LTE, the new version of the STARSP code by V. Tsymbal Maximum NLTE correction about +0.1 dex for solar metallicity (Bergemann & Gehren, 2007), the program DETAIL (Butler & Giddings 1985), the model atom - 245 and 213 levels for Mn I and Mn II, respectively 0.2-0.5 dex for low metallicity (-1 -- -2 dex) (Bergemann & Gehren, 2008).

The observed and synthetic spectra fitting

Thin disk – as magenta, thick disc –as black squares, Hercules stream - as green triangles

Comparison with the data of other authors: black circles (Reddy et al Comparison with the data of other authors: black circles (Reddy et al. 2006); triangles (Nissen 2011); open circles (Feltzing et al. 2007); and asterisks (our data).

Timmes et al. (1995): Inclusion of nucleosynthesis from Type Ia supernovae improves the fit to the solar abundance of Mn.???

Trend of [Mn/Fe] vs. [Fe/H] Different assumptions are invoked to explain the trends: 1)a Mn overproduction with respect to Fe in supernovae of type Ia (Prochaska & McWilliam 2000; Nissen et al. 2000; Sobeck et al. 2006); 2) metallicity dependent yields from type II supernovae (McWilliam et al. 2003) New Mn nucleosynthesis results and new models of the chemical evolution! .

Detailed analysis of four stars with different metallicity Spectrograph SOPHIE (http://www.obs-hp.fr/www/guide/sophie/sophie-info.html R=75000, λλ 3872-6943 Å Å Now, we have redefined the parameters and focused our attention on the lines of the elements produced in the process of neutron captures WIDTH9 by Kurucz R. LTE approximation, EWs FeI, FeII, YII, ZrI, ZrII, LaII, CeII, PrII, NdII, SmII, GdII

Parameters of studied stars HD V Sp   S/N Teff (K) log g ξ (km s-1) [Fe/H] 6582 5.1 G5Vb Double or multiple star 321 5330 4.35 0.4 -0.86 19445 8.1 A4p Variable Star 102 5950 4.1 1.3 -1.99 84937 8.3 sdF5 High proper-motion Star 148 6200 3.8 1.6 -2.15 170153 3.6 F7V 317 6160 4.0 0.9 -0.57

Selection of lines ElEMENT Number of lines min max Fe I 475 846 Fe II 51 83 Y II 11 23 Zr I Zr II 9 19 La II 7 25 Ce II 5 57 Pr II 4 22 Nd II 73 Sm II 46 Gd II 1 12 Parameters of line from VALD (Piskunov et al. 1995; Kupka et al. 1999), for Ce II also from Lawler et al. (2009). Lawler J. E. et al.: 2009, Astrophys. J. Suppl., 182, 51.

Element abundances HD6582 HD19445 HD84937 HD170153 [X/H]  N lg [X/Fe] Fe I -0.86 0.1 846 6.64 -1.99 0.11 539 5.51 0  -2.15 475 5.35 -0.57 802 6.93 Fe II -0.87 0.07 63 6.63 -0.01 -2 0.13 55 5.5 -0.01  -2.14 51 5.36 0.01  -0.58 83 6.92 Y II 22 1.35 -2.07 11 0.14 -0.08 -2.2 12 0.01 -0.05 -0.66 23 1.55 -0.09 Zr I -0.75 0.06 1.83   -0.56 5 2.02 Zr II -0.71 0.05 19 1.87 0.15 -1.76 10 0.82 0.23 -1.93 9 0.65 0.22 -0.52 18 2.06 La II -0.76 0.34 -1.8 0.09 8 -0.7 0.19 -1.9 7 -0.8 0.25 -0.5 0.08 25 0.6 Ce II -0.83 57 0.75 0.03 -1.58 0.41 -1.79 -0.21 0.36 52 1.08 Pr II -0.72 -1.15 -0.43 0.84 -1.51 0.02 4 -0.79 0.64 -0.55 0.17 Nd II 72 0.66 -1.64 0.12 15 -0.22 0.35 -0.34 0.39 73 0.9 Sm II -0.65 46 0.31 0.21 -1.28 -0.32 0.71 -1.45 -0.49 0.7 -0.45 41 0.51 Gd II -0.62 0.45 0.24 -1.31 1 <-0.24 0.68 -1.53 3 <-0.46 0.62 -0.47

Behavior of the element abundances in the atmospheres of the Sun and of investigated stars

Plan (2014) Chekhonadskikh F., Korotin S.A, (Kovtyukh V.V.) Galactic abundance gradients from Cepheids: NLTE abundance of Sulphur.  Mishenina T.V., (Pignatari M., Gorbaneva T.I.) Determination of Mn abundances in the sample of thin and thick disk stars for study of the sources of Mn production and Mn Chemical evolution. Chekhonadskikh F., (Kovtyukh V.V.) Abundances of double-mode Cepheids from high-resolution echelle spectroscopy.  Korotin S.A. NLTE analysis of C, O, Na, Mg for 60 F supergiants . Andrievsky S.M., Korotin S.A, (Kovtyukh V.V.) Oxygen NLTE abundance distribution in the central part of the Galactic disc. Yushchenko V. The most detailed elemental abundance pattern in RM 1-667-stars of SMC Analysis of radioactive elements (Th). Mishenina T.V., (Basak N.Yu.) The detailed investigation of 10 stars as standard stars in the region of metallicity [Fe/H] from -0.8 to -3 dex.  

Plan (2015) Chekhonadskikh F., Korotin S.A, (Kovtyukh V.V.) Galactic abundance gradients from Cepheids: NLTE analyze of alpha-elements. Mishenina T.V., (Paramonova O.P.) Determination of Sulfur abundances in the thin and thick disk stars for study the sources of its production Chekhonadskikh F., (Kovtyukh V.V.) FGK Supergiants: elemental abundances and their implementation for the stellar and galactic evolution. Yushchenko V. Determination of the Th abundance in HD204543 by synthesis method.  Mishenina T.V., Korotin S.A., (Kovtyukh V.V.) Enrichment with alpha- and neutron capture elements of open cluster stars. Andrievsky S.M., Korotin S.A. Silicon abundance problem in B stars.

Plan (2016) Chekhonadskikh F., (Kovtyukh V.V.) Galactic abundance gradients from FGK supergiants: alpha-elements.  Mishenina T., (Kovtyukh V.V., Usenko I.) Light and heavy elements in the stars of the Southern sky (thick disk). Korotin S.A., Andrievsky S.M., (Kovtyukh V.V.) NLTE analysis of Ca for supergiants. Yushchenko V. Investigation of Ba-type stars.  Mishenina T.V., Korotin S.A., (Kovtyukh V.V.) Enrichment with alpha- and neutron capture elements of globular cluster stars. Andrievsky S.M., Korotin S.A. Europium NLTE abundance distribution in Galactic disc.

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