Redalyc.CHEMICAL ABUNDANCES for A-AND F-TYPE SUPERGIANT

Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Molina, R. E.; Rivera, H. CHEMICAL ABUNDANCES FOR A-AND F-TYPE SUPERGIANT STARS Revista Mexicana de Astronomía y Astrofísica, vol. 52, núm. 2, 2016, pp. 399-411 Instituto de Astronomía Distrito Federal, México

Available in: http://www.redalyc.org/articulo.oa?id=57150515016

How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México fselradceia vlto Lc ta.1998; al. et (Luck evolution chemical studies and in for stellar candidates luminous star suitable of visually of are area thus are and an objects galaxies is it These since surprising, galac- formation. not the is in events. plane objects tic supernova young massive and of winds existence interstel- The stellar the by to un- medium elements evolution lar chemical their rapid massive return nucleosynthesis their its of and process in of the through study objects changes dergo the These from stars. understood be can eit eiaad srnmı Astrof´ısica Astronom´ıa y de Mexicana Revista aoaoi eIvsiaio nFıiaAlcd optcoa,Univer Computacional, y F´ısica Investigación Aplicada en de Laboratorio HMCLAUDNE O -N -YESPRIN STARS SUPERGIANT F-TYPE A-AND FOR ABUNDANCES CHEMICAL h rcs fceia vlto nteGalaxy the in evolution chemical of process The olcńIpr uetd vltv opeesrdfiiosatisfactoriamente. definido ser puede no evolutivo estado su pero I Población ay hw yia bnacso ouainI u t vltoaysau cannot status Words: evolutionary Key con- its the but on defined. I, 180028, HD Population satisfactorily (post-1DU of region. be loop dredge-up abundances red-blue typical post-first the shows in the moving tary, in are they are abun- that that 224893 indicate and Their HD to phase, and population. seem diagram 194951 disc HD Hertzsprung-Russell thin the 45675, Alpha- HD the on Luck. to location by their belong and previously objects dances studied the reaffir 194951 We that HD 224893. indicate and HD elements 180028 and HD 45674 HD for for abundances analysis abundance the the of results first the –-yesprin tr D464 D102,H 991adH 22 HD and 194951 HD ( 180028, HD resolution high 45674, HD ing stars supergiant A–F-type aepseira rmrdaao(ot1U)ys uvne argńdel región la en la mueven en se encuentran y abundan- se (post-1DUP) Sus evolutivamente objetos indicarnos dragado ( los 224893 parecen HD primer rojo-azul galáctico. todos Hertzsprung-Russell y al lazo 194951 HD diagrama que disco posterior 194951 HD y el indican fase del 180028 45675, en nos población HD HD localización alfa su para la que elementos y abundancias a Los cias las pertenecen reafirman 45674 Luck. HD estudiados se para por abundancias y las calculadas de 224893, HD resultados primeros y los presentan Se ELODIE. utoojtsspriatsH 57,H 808 D145 D224 HD y ( resolución 194951 HD alta 180028, HD de 45674, HD espectros supergigantes usando objetos cuatro .INTRODUCTION 1. epeetteselrprmtr n lmna bnacso e of set a of abundances elemental and parameters stellar the present We eo fcud na´lssdtlaod a bnaca uıia de qu´ımicas abundancias las de detallado análisis un efectuado Hemos tr:audne tr:amshrs—sas vlto super- — evolution stars: — atmospheres giants stars: — abundances stars: e-leloop red-blue eevdMy921;acpe uy1 2016 11 July accepted 2016; 9 May Received R ≈ 42 .E oiaadH Rivera H. and Molina E. R. , 0)setatknfo LDElbay epresent We library. ELODIE from taken spectra 000) .H 808metaaudnistıia ela de t´ıpicas abundancias muestra 180028 HD ). Táchira, Venezuela , 52 ABSTRACT RESUMEN 9–1 (2016) 399–411 , R n hs a eaetdi eea ways. several in affected burn- be core can post-He phase the ing stars H massive 2011, in When exhausted al. therein). is references et and (Lyubimkov 1995a,1995b Venn states the evolutionary of discriminate to their abundances crucial been chemical have CNO The elements light evolved. erately e ssprin tr ihmse ewe to 5 between masses with stars 20 supergiant as fied 2003; 2001, 2000, al. 2004). et al. Venn et Kaufer 2006; al. et Smiljanic ≈ M oeo hs asv bet aebe classi- been have objects massive these of Some 42 ⊙ n -n- pcrltps hc r mod- are which types, spectral A-and-F and , , 0)tmdsd alibrer´ıa la de tomados 000) ia ainlEprmna del Experimental Nacional sidad 83us- 4893 893, P) m 399 © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México ihitreit ass(3 masses intermediate with 1991). 1976; (Stothers Chin unchanged & remain condi- abundances these stars CNO Under tions the phase. supergiant and blue the equilibrium in stay thermal is establish envelope to the develop able zone, they intermediate branch, convective fully giant a red the visiting without ( event. abun- (1DUP) CNO dredge-up altered first the an to shows due and dance layers in outer convection ther- the through resume equilibrium this to radiative In able and are mal re- supergiants phase. A–F supergiant supergiant the rapid red phase, blue a a them the towards in in cause expansion instabilities He thermal of but be- gion, and ignition sequence These the main the 1991). gun left Chin already & have Stothers objects 1992; al. et (Schaller a ealcte rdc htmsiesupergiants massive that predict ( metallicities lar 400 acsosre o uegatsasi h galactic the in the stars disc. that supergiant abun- for expected typical observed is the dances to It correspond derived 2004). abundances Kurucz the & (Castelli and (LTE) equilib- hy-rium thermodynamic geometry, local equilibrium, plane-parallel drostatic with mo- constructed atmospheric high- of dels employ set at- a we and their purpose spectroscopy ioniza- resolution this of For and determination excitation equilibrium. the tion from low- as assumption parameters well four the mospheric as of under 180028, HD LTE, 224893, of set HD 45674, HD and a 194951 HD supergiants: for A–F abundances latitude chemical of supergiants. of types to different us between allows discriminate objects such in in amount material changes The CNO-processed causing patterns. abundance event, CNO 1DUP observed the the the to by released of surface subsequently materials the are which mixes shell, zone supergiant H-burning red convective the the During phase, phase 2015). supergiant but al. blue et stage a (Walmswell objects supergiant into back These red evolve HRD. the eventually the ris- reached in is already line have and Hayashi even- the envelope has up convective star ing the a stage this developed In tually loop. blue the called emn h hmclaudne o h he stars three the for abundances de- chemical We the termine estimated. were parameters atmospheric the cietesml eeto.In selection. sample the scribe < M M oee,aohrseai spsil o objects for possible is scenario another However, nteohrhn,ls asv – supergiants A–F massive less hand, other the On tla vltoaymdl osrce o so- for constructed models evolutionary Stellar hsppri raie sflos In follows: as organized is paper This study detailed a is work this of goal main The ≥ 10 10 M M ⊙ ⊙ r ntepaeo eimcr burning core helium of phase the in are ) aeas ntae h ecr burning He-core the initiated also have ) ODFNEW < M pct distribution opacity § < epeethow present we 3 9 M ⊙ n tis it and ) § ede- we 2 OIA&RIVERA & MOLINA tr speetdin presented is stars in de- in number. arranged HD are the stars stars order This creasing sample lines. been dashed have The the by elements important indicated 224893. certain of HD of lines and of spectra 194951 locations HD Representative 180028, HD 45674, HD 1. Fig. .3 eecp oae nteHaute-Provence of region the 6800 and spectral 4000 the between in cover the They located means (OHP). in Observatory by placed telescope respectively ELODIE spectrograph 1999 1.93m echelle 07, 18, the December July on of on 2003; 26, and July on 1999 observed 1999; were 06, spectra The July 3.1 on (2007). version al. its et in Prugniel updated by and (2001) al. et Moultaka u eut,adfinally, and results, our h paper. the D102,H 991adH 283aetaken are ELODIE 224893 HD library the and from 194951 HD 180028, HD (1977; young Luck G–K from taken of 1978). I sample mean Population a of The the of supergiants for with plane. obtained objects galactic compared were the abundances are luminous in abundances located 224893) HD are derived II and they I and Classes because 194951 HD selected 180028, HD § 1 R h tla pcr ae o D45674, HD for taken spectra stellar The 45674, (HD analysis this for stars The http://atlas.obs-hp.fr/elodie/ .A niiulaayi faudne o each for abundances of analysis individual An 4. ≈ 200 h inlt-os ai SN for (S/N) ratio signal-to-noise The 42,000. 2.1 .OBSERVATIONS 2. apeSelection Sample . § 5. ,n aearsligpower resolving a have A,and ˚ § § ie h ocuin of conclusions the gives 7 1 sddctdt discuss to dedicated is 6 rgnlypbihdby published originally © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México G rnra -n -yesprin star. post- supergiant a F-type to by A-and candidate identified normal possible was or AGB a object around as last (1993) dust This Likewise,Bidelman of star. evidence central show excesses. the not ob- infrared does three indicate 224893 these other HD not for from do AKARI data and jects flux WISE VisieR like that re- the sources indicates A in also contained database microns. photometry from 100 available (SED) low distributions and the energy of spectral 60 are the of 25, fluxes view at IRAS (Q=1) in- their quality realiable since display excesses them respec- frared of 3410 none + 20252 IRAS although 0032, - 06262 tively), and (IRAS sources, 0557 + 19122 point IRAS IRAS as labeled spectra all respectively. for 5550 145 derived at and been library the has 82 in pixel 175, per 83, 224893 HD S/N be This and to 194951 HD reported 180028, is HD 45674, HD niaetepsto fsm bopinlnso el- of Y lines as absorption such some ements of lines position dotted the 180028, vertical HD The indicate 45674, HD 224893. HD stars and the 194951 HD for spectrum the of al .Ti al otisteH ubr the number, HD the apparent contains in the table shown coordinates, equatorial are This sample total 1. Table the for parameters basic ain hs auswr ae rmteSIMBAD the from ro- taken database. of were astronomical velocity values the These and excess tation. velocity, color radial the parallax, the the coordinates, galactic the nitude, E)o h elnsaencsaya ela mea- as well (log as data necessary atomic are widths lines of equivalent Fe surements the the of of (Ew) measurements accurate tmcdt o h Fe the for data atomic esrd omaueteE eue h task the used we Ew the range measure a To to restricted measured. m 200 were to values 10 Ew from The Barbuy Meléndez & (2009). and (2006) Wiese Führ & from 2 808FI 91 4+60 469 .3040.97 7.73 6.96 54 02 +06 44 14 19 F6Ib 180028 991FI 02 7+41 464 .4073.86 6.84 6.41 44 19 +34 07 27 20 F1II 194951 283AI 00 7+11 255 .4116.97 5.94 5.57 22 13 +61 37 01 00 A8II 224893 iue1sosarpeettv ag f50 of range representative a shows 1 Figure objects are 194951 HD and 180028 HD 45674, HD nodrt banteamshrcparameters atmospheric the obtain to order In http://simbad.u-strasbg.fr/simbad/ 57 1a0 847 28 06 F1Ia 45674 DSpT HD .AMSHRCPARAMETERS ATMOSPHERIC 3. ,adol o-lne ie were lines non-blended only and A, ˚ hms ( s) m (h II V b l B V δ α La , A. ˚ 2 I II n Fe and − Ti , 03 065 .0210.85 7.30 6.56 20 34 00 o LMNA BNACSI UEGAT 401 SUPERGIANTS IN ABUNDANCES ELEMENTAL ′ ” II g AI AAEESFRTESAMPLE THE FOR PARAMETERS BASIC mg mg ( (mag) (mag) ) II Fe , and ie eetaken were lines V I χ Ni y and e).The (eV)). B I The . mag- AL 1 TABLE A ˚ o ( ) SPLOT in widths 180028. equivalent HD and reduced 45674 HD and excitation potential o xiainptnil h ufc rvt a de- was gravity surface The the potential. of excitation independent low be to abundances requiring as- iron by derived the the i.e., ef- equilibrium, under the excitation of model, determined sumption best was the temperature the With fitted fective best stars. that and of model trial photosphere the a selected devel- on we been Based test, error has assumptions. ETL code under at- This the oped of determination parameters. the mospheric for 1973) (Sneden code qiiru LE n the and thermodynamic (LTE) geom- equilibrium local models plane-parallel equilibrium, These a hydrostatic with etry, (2003). constructed Kurucz been and have collec- Castelli the of from tion selected were determinations dance 8-10%. measure- about the is in Ew error of The ments profiles. line observed the i.2 needneo Fe of Independence 2. Fig. tion. − − − − 53 +18.4 05.30 02.39 02.34 01.07 o h tla topei oesfrteabun- the for models atmospheric stellar The eue h pae eso 21)o the of (2010) version updated the used We k s (km ) fthe of − − − 13.5 23.2 5.1 ± r ± ± ± − IRAF . -0.32 0.7 . 1.31 0.9 . 1.00 2.0 . 1.06 2.0 1 ms mg k s (km (mag) (mas) ) otaewt asinfi to fit Gaussian a with software ± ± ± E π ± .10.382 0.51 .102020 0.230 0.41 .702440 0.244 0.27 .103623.3 0.346 0.51 I ODFNEW bnacsfo h low the from abundances ( B − pct distribu- opacity V ) sini v − 1 MOOG ) © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México ie yrqiigta h Fe the that requiring by rived 402 lrt hs bandfrteFe the for obtained those to ilar qiaetwdh lgEw/ (log widths equivalent ec eoiywsdtrie yrqiigta the microturbu- Fe that the requiring of Finally by abundances determined Ni. was ionization Cr, velocity two lence Ti, with Ca, elements can like other condition states to equilibrium extended the gravity, be the of value h bnacso Fe of abundances the oiyteema values. mean these at- satisfac- torily match their that parameters note for atmospheric We adopted value our estimated. mean was a parameters with measure mospheric objects one For than work. atmospheric more this the for and adopted also photometric parameters and from techniques authors spectroscopic different by mated equivalent 180028. HD reduced and 45674 the HD for of widths and potential excitation al it h topei aaeesesti- parameters atmospheric the lists 2 Table TOPEI AAEESDRVDI HSWR N HS OBTAINED THOSE AND WORK THIS IN DERIVED PARAMETERS ATMOSPHERIC 28374 .63.9 1.96 7340 224893 9917392 194951 80868 .5+.4W ta.(2011) al. et Wu +0.14 1.65 6287 180028 57 6020 01 ue l (2011) al. et Wu +0.16 2.05 7630 45674 HD I eidpneto h reduced the of independent be 7488 6349 6959 I 502040+.6Ti ok(adopted) Work This +0.16 4.0 2.0 7500 902.02 (2001) Soubiran 6950 & Prugniel +0.18 4.6 1.72 6280 1.95 7346 301028Adivk ta.(2002) 4.5 al. et Andrievsky 2.0 7500 2.8 1.0 6350 1.54 6531 5224 .1+.9Lc (2014) Luck (2014) Luck (2012) al. et (2002) Kovtyukh al. et Andrievsky +0.39 +0.26 +0.10 4.11 4.08 4.0 2.46 3.0 2.32 1.9 6502 1.3 6488 6307 6050 40214.8 2.1 6400 701.92 6760 7268 9722 .7+.1Lc (2014) Luck (2014) Luck +0.11 +0.08 3.87 3.93 2.21 2.22 6977 7019 00184.7 1.8 7000 K k s (km (K) T r needn ftelow the of independent are eff ± ± ± 0 2.00 200 7 1.84 171 4 1.87 341 λ .Fgr hw that shows 2 Figure ). I bnacsb sim- be abundances II ocnr the confirm To . log ± ± ± .7+0.17 0.07 .23.96 0.42 .03.53 0.50 ξ g RMTELITERATURE THE FROM OIA&RIVERA & MOLINA ± ± AL 2 TABLE t .9+0.14 0.59 0.64 − 1 ) es(20Ki T in parame- K atmospheric (+250 widths of equivalent ters model measured defined the the in (8–10%), errors of dances in e fhg cuayfrFe for accuracy val- high experimental of example, ues For element. to element o1%aeaalbefralrefato ftelines. the their of in fraction errors elements, large Fe-peak a other for For available are 10% to edo h ult ihwihte eederived. the were in they error de- which the and with short, systematic quality In the are on data pend atomic and rameters star. the and of (S/N) type ratio noise spectral position to the the signal as the because continuum, such random the factors, of several are on widths depend equivalent they to due rors − 0.01 ξ F/]Ref. [Fe/H] − − − − − − − − ecluae h ffcso h hmclabun- chemical the on effects the calculated We ncnrs,err u oteamshrcpa- atmospheric the to due errors contrast, In t ,adteaoi aa(log data atomic the and ), .4Ga ta.(2001b) al. et Gray 0.24 .9Ga ta.(2001b) al. et Gray 0.09 (2001b) al. et Gray 0.03 .6Ti ok(adopted) Work This 0.26 (2001) Soubiran & Prugniel 0.01 .6Ti ok(adopted) Work This 0.06 .3Luikve l (2011) al. et Lyubimkov 0.13 .5Ti ok(adopted) Work This 0.15 ± ± ± .1Ma Value Mean 0.01 .6Ma Value Mean 0.16 .2Ma Value Mean 0.12 3.1 netit nteAbundances the in Uncertainty . eff otuhe l (2007) al. et Kovtyukh 05i log in +0.5 , ol ta.(2010) al. et Hohle gf I vle a aisfrom varies can -values n Fe and gf g n 05k s km +0.5 and and II χ ewe 3% between e).Er- (eV)). gf -values − 1 © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México to neetv eprtr f20Kgnrtsa generates vari- K a 250 that of see temperature effective can We in making ation wings large inaccurate. strong not strengths develop spectra is to line lines temperature the the the stars for and enough these cleaner For much K. are 7500 i.e., perature, Ta- 3. in in displayed ble changes is The parameters to range. atmosphere abundances model 50% the derived to 10 the the el- of in capture sensitivity neutron- is For accuracy 25%. the to ements 10 from range may ESTVT FAUDNE OTEICRANISI H OE PARA MODEL THE IN INCERTAINTIES THE TO ABUNDANCES OF SENSITIVITY Eu Nd Ce La Ba Zr Y Zn Cu Ni Fe Fe Mn Cr V Cr Ti Ti Sc Ca Ca S Si Si Mg Na O N pce ∆T Species C D464adH 991hv h aetem- same the have 194951 HD and 45674 HD I I II II I I II I II I II II I II I II I II II I II II I II I I II I I 20K+. 05+0 20K+. 05+10% +0.5 +0.5 K +250 +10% +0.5 +0.5 K +250 − − − − − − − − − − − − − − − − − − − +0 − − +0 − − − · · · · · · · · · · · · · · · − · · · · · · · · · · · · · · · − · · · · · · · · · · · · · · · − · · · · · · · · · · · · · · · 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 W AGSO EPRTR PNIGORSML STARS SAMPLE OUR SPANNING TEMPERATURE OF RANGES TWO ...... 28 24 00 30 17 19 4+0 24 2+0 22 4+0 24 10 4+0 24 10 7+0 27 13 15 8+0 28 15 07 7+0 27 7+0 17 02 2+0 22 0+0 20 02 02 40 14 eff ∆log − − − − − − − − − − − − − 0 0 0 0 0 0 0 0 0 0 0 0 0 ...... LMNA BNACSI UEGAT 403 SUPERGIANTS IN ABUNDANCES ELEMENTAL 50 05 8+0 08 0+0 00 3+0 13 1+0 11 7+0 07 8+0 08 7+0 07 2+0 12 7+0 07 2+0 12 6+0 06 2+0 12 3+0 13 50 05 2+0 12 4+0 04 0+0 10 4+0 04 8+0 08 8+0 08 8+0 08 8+0 08 60 06 0+0 00 g D45674 HD 70 K) (7500 ∆ ...... ξ 00 00 01 05 05 03 10 01 10 01 03 04 02 05 03 02 08 00 07 30 03 05 02 16 08 01 01 00 01 t − − − − − − − − − − − − − − − − − − − − − ∆Ew 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 ...... 00 00 10 01 10 01 20 02 10 01 00 00 00 00 10 01 10 01 10 01 10 01 10 01 10 01 20 02 20 02 10 01 00 00 10 01 10 01 20 02 10 01 10 01 10 01 10 01 10 01 AL 3 TABLE σ ...... tot 28 25 30 22 22 25 23 25 6+0 16 25 6+0 16 28 18 21 29 20 09 29 8+0 18 8+0 18 25 22 8+0 08 06 4+0 14 icn hne nteucranisdet changes to due sig- log Ba, observe uncertainties in like not the did lines in we contrary, ionized changes the nificant and On O Nd. N, and neu- Ce C, in except particularly lines lines, tral all in uncertainty greater iesrntssossniiiyol ocagsboth changes T to the in only K) sensitivity (6400 shows temperature strengths lower line a at However, cent. h qaero fteqartcsmo h random the of sum errors. quadratic systematic the and of root square the h oa error total The eff ∆T − − − − − − − − − − − − − − − − g 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 y20K n nlog in and K, 250 by · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · · eff ...... y0.5, by 11 10 08 08 10 03 04 08 13 08 08 02 08 03 12 03 14 04 07 04 13 03 14 03 10 07 ∆log − − − − − − − − − − − − − − − − − − − − − − − − − − ξ t 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 ...... y05k s km 0.5 by 5+0 15 80 18 5+0 15 6+0 16 0+0 10 6+0 16 6+0 16 5+0 05 4+0 04 4+0 04 4+0 04 5+0 15 4+0 04 6+0 16 4+0 04 6+0 16 4+0 04 6+0 16 2+0 02 1+0 11 5+0 15 3+0 03 4+0 04 3+0 03 50 05 11 σ g tot D180028 HD 60 K) (6400 o aheeeti ie by given is element each for − ∆ 0 . . 00 00 ...... ξ g 10 01 10 01 06 07 10 01 20 02 02 01 02 04 05 04 06 03 04 01 03 04 02 07 10 01 40 04 05 10 01 t y0.5. by − 1 n wb 0per 10 by Ew and EESFOR METERS − − − − − − − − − − − − − − − − ∆Ew 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 · · · · · · · · · ...... 00 00 00 00 20 02 00 00 00 00 10 01 10 01 10 01 10 01 10 01 10 01 20 02 10 01 10 01 10 01 10 01 10 01 10 01 10 01 00 00 00 00 10 01 00 00 0 0 0 σ ...... tot 19 17 20 19 15 16 17 10 14 09 10 16 10 17 13 17 15 17 08 12 21 04 15 07 11 13 © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México tv oio.Teaudne fteeeet in hy- to elements respect the log with scale of namely: logarithmic drogen, a abundances in rel- The are 4 abundances Table the iron. and to lines ative un- the identified their hydrogen, of and as to number star relative (2005), each abundances for the al. certainty, calculated et those Asplund as photospheric by well solar given the as species photosphere, abundances chemical the the contains seen in table be present This can 4. 224893 Table HD in and 194951 HD ele- 180028, the HD of dex. 0.09 most to for 0.04 few values between very i.e., solar found ments, the and Solar 1984) in the al. differences from et (Kurucz spectrum Atlas solar Flux the employed thors n rnaeepesda XH log = [X/H] as expressed are hydrogen to iron relative and elements the of abundances The ǫ hyue ieetsucsfor sources when different caused used differences they systematic the studied also and details). further Giridhar for Rao, 4 Table Sumangala (see (2012) by Lambert given those the are 2. of Table in sources adopted The models atmospheric the employ bandfo oiaineulbimbtenthe between Fe were of equilibrium parameters lines ionization atmospheric from The su- obtained normal A-and-F possible star. an a or pergiant as post-AGB a object to this candidate includes (1993) Bidelman [X mnsCO h abnaudnewsobtained was (4769 abundance lines two carbon from the CNO, ements 2. Table in by shown is obtained authors parameters different atmospheric the of pilation D145 n D249,rsetvl.W s the use We respectively. task 73 180028, 224893, HD HD and and 45674, 184 HD 194951 HD 116, in identified 176, lines of absorption widths equivalent the used 404 log et uha a i r rmwih∆=[X = ∆ which from Cr, ele- Ti, other con- Ca, of as was such ionization 45674 HD ments equilibrium the for from gravity firmed surface The tively. CH = [C/H] Xsnad[/e XH F/]respectively. [Fe/H] - [X/H] = [X/Fe] and (X)sun .DTRIAINO H ABUNDANCES THE OF DETERMINATION 4. I H s0.08, is /H] g h hmclaudne eie o D45674, HD for derived abundances chemical The uagl a,Grda n abr (2012) Lambert and Giridhar Rao, Sumangala h trH 57 a encasfida F1Ia. as classified been has 45674 HD star The ihrsett h bnacso h ih el- light the of abundances the to respect With o h eemnto fceia bnacswe abundances chemical of determination the For 2.0, = ABFIND .DSUSO FTEINDIVIDUAL THE OF DISCUSSION 5. − .0ad[/e = [C/Fe] and 0.20 I χ n Fe and t fthe of . n F/]=+.6dxrespec- dex +0.16 = [Fe/H] and 4.0 = − .2and 0.02 5.1 ABUNDANCES gf n 5380 and A ˚ ǫ II MOOG X o NX/() 12.0. + [N(X)/N(H)] log = (X) D45674 HD . vle o ieetelements different for -values ihvle of values with − oe(ndn17) We 1973). (Sneden code .5rsetvl.Acom- A respectively. 0.05 − .6 en(1995b) Venn 0.36. )tervle being values their A) ˚ gf vle.Teau- The -values. T ǫ Xsa log - (X)star eff 50K, 7500 = OIA&RIVERA & MOLINA II /H]– naudnei eie rmtolnsat lines two from derived and is i.e., Si The abundance respectively. Zn enhancements, +0.25 2006). = [S/Fe] 2003; and moderate +0.31 al. = [Si/Fe] show et abundances objects (Reddy for disk S typical thin is Ti, the Ca, of Si, Mg, from estimated and bnacsvr iia oslr n agsfrom ranges and solar, to − similar very abundances O-rich. is 45674 HD that indicates 0.32 n OF]= [O/Fe] and at ie.A hstmeaueannLEcreto of correction non-LTE a temperature about this At lines. 98 ol edt bnacso OH = [O/H] of abundances to lead would 1998) atr lmnsso XF]audne iha +0.06 from with ranges and abundances values solar [X/Fe] towards tendency show elements capture Z/e = [Zn/Fe] fteti n hc ikpplto,i.e., population, disk thick a and thin the of n sotie rmthe from obtained is and surface. the to of brought products being and 1DUP CN-cycle the the initial through of N conversion into moder- a carbon involves the N are and of respec- C values enhancement of dex ate non-LTE deficiency +0.36 observed Our = [N/Fe] The and tively. region. dex +0.60 blue = [N/H] the in line niae hta eprtr f70 ,a equiv- an K, 7500 of of width alent temperature a at that indicated 40Kfrti tr hsi fAI ye h non- The type. at A9II N region of for is IR whis correction near star, LTE the this for in K (1995b) 7400 Venn by derived wo 01m 10.1 of Ew T orcinsol esalfrti line. this for non- small the into be that Taking should argue negatively correction can LTE lines. a we above with IR the and the consideration toward K 9600 value of increasing temperature a at o h lergo ryil ulr(01 found (2001) Butler of & correction non-LTE Przybilla a contrast, region By blue 8). the Figure for (see zero almost is correction e oa bnac f[/e = [C/Fe] of abundance an to led ac a bandfo the from obtained abun- this was fact, dance In +0.68). = ([N/Fe] enrichement ate ffcietmeaueo 50K hrfr onon- of value no A therefore neccesary. was K; 7500 correction LTE an of has 45674 temperature HD K. effective 7400 with of (F0Ib) temperature effective 36673 HD an supergiant the for abundance rdcsannLEcreto of correction non-LTE a predicts .2t 01 e.Te[ The dex. +0.18 to 0.22 − λ rnpa lmns(c ,C,N)so [X/Fe] show Ni) Cr, V, (Sc, elements Iron-peak h bnac sna oa [/e +0.03), = ([O/Fe] solar near is abundance O The eaotdavleof value a adopted We h bnac o D464soe moder- a showed 45674 HD for abundance N The .0dx(ed ta.20;20) Neutron- 2006). 2003; al. et (Reddy dex 0.30 4810 λ 4810 − .5(ae rmTkd Takada-Hidai & Takeda from (taken 0.15 a bandfo abye t (2015). at. et Barbuy from obtained was A ˚ − .Tevleo log of value The A. ˚ .3i oe hnepce o objects for expected than lower is 0.33 .AnnLEcreto of correction non-LTE A A. ˚ − ≈ .6rsetvl.TeCOrtoof ratio C/O The respectively. 0.36 0m 10 n log and A ˚ I yLc abr (1985) Lambert & Luck by − α .1dxfrN for dex 0.11 λ F]ratio /Fe] 6156.0 − ≈ λ gf g 4151.4 .,tenon-LTE the 2.0, = − = 0 0.69. and A ˚ − . − 8dxfrour for dex 08 .5frteline the for 0.25 .5i h C the in 0.25 iewt an with line A ˚ ≈ +0.10 I − − λ ( λ − ≈ .8was 0.28 6156.8 .5dex 0.25 λ 3830 4722 ± − 0.16, 0.12 0.20 A) ˚ A ˚ A ˚ © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México ailvlct a eotdb ieetauthors: different by reported − was velocity radial an as +0.45). = ([Zr/Fe] enriched ately Ba 95 and 1995) lgtywd niaigta trttswt veloc- a km with 23.3 rotates of appear it ity that lines indicating absorption wide Its slightly variability. present not rminzto qiiru ewe h ie fFe of Fe lines the and between equilibrium ionization from i i r aey∆=[X = as ∆ namely such Cr, elements from Ti, other confirmed Si, of was ionization equilibrium 180028 HD the for gravity surface o+.9dx fohreeet dnie,lk Y like identified, elements other Of dex. +0.19 to χ t Eu Nd Ce Ca Sc Ti La V N Ti Fe S Ba Ca Mn Y Cr C log Species Cr Cu O Zr Zn Si Mg Ni Fe Na Si Ni . km 6.0 . n F/]= [Fe/H] and 4.8 = I II I II I II I D102 a lsie saFI n cataloged and F6Ib a as classified was 180028 HD hi topei aaeeswr obtained were parameters atmospheric Their II I II II I II I II I II I II II II I II I II II I I II I I Ce , IRAS II − ihvle fT of values with , II 1 0.52 .5+0 1.45 .8+0 1.58 .0+0 4.90 .5+0 3.05 .0+0 4.90 .1+0 6.31 .9+0 5.39 .3+0 1.13 8.39 .0+0 4.00 .4+0 7.14 .5+0 7.45 .8+0 7.78 .7+0 2.17 .1+0 6.31 .1+0 2.21 .4+0 5.64 4.21 .4+0 5.64 .9+0 2.59 .6+0 8.66 4.60 .3+0 7.53 .1+0 7.51 6.23 .5+0 7.45 .7+0 6.17 .1+0 7.51 6.23 LMNA BNACSFRH 57,H 808 D145 N HD AND 194951 HD 180028, HD 45674, HD FOR ABUNDANCES ELEMENTAL − n Nd and Wlo 1953), (Wilson on ore(RS112+05) The 0557). + 19122 (IRAS source point ǫ . km 5.1 ⊙ − 1 − − − D eerse l 2002). al. et Medeiros (De 0 0 0 5.2 ...... XH XF][/]N[/e XH XF][/]N[X/Fe] N [X/H] [X/Fe] N [X/H] [X/Fe] N [X/H] [X/Fe] N [X/H] 22 33 27 34 29 24 14 20 22 41 12 68 35 16 11 13 18 61 03 17 08 06 47 20 50 II − 1 nyZr only , D180028 HD . ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± − .51+0 1 0.05 .43+0 3 0.14 .03+0 3 0.10 .49+0 9 0.04 .41 +0 14 0.14 .18+0 8 0.11 .13 0.01 .22 0.02 .21+0 1 0.02 .05+0 5 0.10 .060 0.10 .61+0 1 0.06 .71+0 1 0.07 .520 2 0.15 .05 0.10 .83 0.08 .27+0 7 0.12 .33+0 3 0.13 .12 0.01 .62 0.16 .94 0.19 .28 0.12 .32+0 2 0.13 .810 0.08 .04+0 4 0.10 Gncao 06 n does and 2006) (Gontcharov D464H 808H 991H 224893 HD 194951 HD 180028 HD 45674 HD .6dxrsetvl.The respectively. dex 0.06 II /H]–[X − eff LMNA BNACSI UEGAT 405 SUPERGIANTS IN ABUNDANCES ELEMENTAL . km 6.0 II 40K log K, 6400 = em ob moder- be to seems − − − − − − − − I 0 0 0 0 0 0 0 0 H s0.11, is /H] ...... 6+0 06 17 1+0 11 8+0 18 3+0 13 8+0 08 06 5+0 25 52 9+0 19 00 2+0 02 36 02 5+0 45 1+0 31 5+0 05 4+0 34 03 3+0 13 33 8+0 08 22 − 1 Dflte al. et (Duflot − − − − − − − − − − 0 0 0 0 0 0 0 0 0 0 ...... 13 29 15 25 05 07 38 23 11 19 10 06 05 37 07 19 12 08 06 26 06 28 11 11 38 09 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± g .92+0 2 0.09 .51+0 1 0.05 .61+0 1 0.06 .94+0 4 0.09 .04+0 4 0.10 .35+0 5 0.13 .93+0 3 0.09 .0sn+0 syn 0.10 .84+0 4 0.08 .43+0 3 0.14 .41+0 1 0.04 .41+0 1 0.04 .23+0 3 0.12 .42+0 2 0.04 .0sn+0 syn 0.10 .91+0 1 0.09 .0syn 0.10 .63 0.16 .356 0.13 .41 0.04 .68 0.16 .0syn 0.10 .33 0.13 .02 0.10 .31 0.03 .64 0.06 − 2.1, = 0.10 II AL 4 TABLE I , − − − − − − − − 0 0 0 0 0 0 0 0 h epa lmnsso oa rn.Teratio The trend. solar a dex. show +0.43 = elements [Na/Fe] Fe-peak i.e. in The higher, obtained slightly value enrich- is The work moderate this dex. a +0.28 = [Na/Fe] found analysis of sodium (2002) ment a al. From et value. Andrievsky solar the than lower 21) h / ai sabout is ratio C/O The Luck by obtained those (2014). than 3). higher Figure are (see values O spectrum, respectively These dex, The the +0.13 = region [O/Fe] and in the estimated. synthesizing 6140–60 bands by be at CN derived not was or could abundance lines abundances N so no are and n e oavleo CF]= [C/Fe] of value 1994) a (Takeda small to non- very the led was K and 6100 C of to correction temperature LTE a At respectively. [Fe/H]= adopted 2. Table the in and displayed authors are parameters different by obtained ters ysnhszn h iea 5380 at = [C/H] line of values the synthesizing by ...... 06 19 35 21 31 11 13 44 17 02 5+0 25 16 29 12 11 20 3+0 43 25 22 13 07 05 32 3+0 03 D102 xiisamtliiyna oslrof solar to near metallicity a exhibits 180028 HD − − − − − − − − − − − − − − − − − − − +0 .0rsetvl.Teamshrcparame- atmospheric The respectively. 0.00 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 ...... 01 18 09 10 11 21 03 18 13 17 03 21 12 11 20 12 21 16 10 25 34 20 − ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .6 h bnac fCwsobtained was C of abundance The 0.06. .41+0 1 0.04 .62+0 2 0.06 .02+0 2 0.00 .16+0 6 0.11 .72+0 2 0.17 .62 0.06 .46+0 6 0.14 .213 0.12 .71 +0 10 0.17 .172 0.11 .0sn+0 syn 0.10 .85 0.18 .92+0 2 0.19 .71+0 1 0.07 .55 0.15 .120 0.11 .95 0.09 .95 0.09 .02+0 2 0.00 .111 0.11 .35 0.13 .0syn 0.10 .Tevle r OH 00 dex +0.07 = [O/H] are values The A. ˚ − .8dxad[/e = [C/Fe] and dex 0.28 − − − − − − − − − 0 0 0 0 0 0 0 0 0 ...... 04 2+0 12 02 16 33 12 06 4+0 24 03 03 04 06 05 5+0 05 25 06 01 10 05 19 − − − − − − − − − − − − − − +0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 ...... 89 13 29 19 24 27 28 29 20 26 34 21 20 34 11 40 26 25 − ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .W obtained We A. ˚ .9dx There dex. 0.39 224893 .61+1 1 0.06 .52+0 2 0.05 .41+0 1 0.04 .51+0 1 0.05 .21+0 1 0.02 .119 0.11 .92 0.29 .34 0.03 .11 +0 13 0.11 .77 0.17 .02 0.10 .31+0 1 0.03 .94+0 4 0.09 .13 0.11 .02+0 2 0.10 .94+0 4 0.09 .310 1 0.03 .22+0 2 0.12 ≈ .3 hc is which 0.23, − .2dex 0.22 − − − − 0 0 0 0 ...... 00 02 15 39 02 03 55 08 06 05 06 45 08 15 14 01 © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México pciey o h bnac o-T cor- non-LTE a abundance O of the rection For spectively. ia 19)wsetmtd n h bnacsof abundances the and estimated, was (1998) Hidai i.3 bevd(le qae)adsnhtc(solid synthetic and O the squares) of (filled spectra Observed line) 3. Fig. 406 ie ( lines 4. Table in presented elements are the identified of abundances chemical The spectively. te lmns uha i r n i rmwhich from Ni, and of Cr, ionization [X Ti, = ∆ 194951 as equilibrium HD such of the elements, gravity other from surface The be confirmed can was 3. adopted Table we values in The seen tech- 2). various Table spectroscopic (see by and niques determined photometric phys- using been The authors have (1972). Morgan parameters by Bidel- ical by F1II F3II and al.(1960), (1957) et man Stock by F2Iab authors: La and Ba for s- enhanced. except modestlly The trend are solar which dex. a +0.44 = [S/Fe] show is i.e., elements Sulfur enriched, mod- be a dex. shows found +0.25 Mg = [Mg/Fe] while Ca enhancement, values Si, erate Individually, solar present disk. Ti thin and the to belongs object h ytei pcr orsodfo o obto to bottom and to +0.07 top +0.37, = from [O/H] correspond spectra synthetic The [ ovle f[/]= [C/H] of values to rsn n orcinof correction were a effects non-LTE and the present K 7000 of temperature a At and α F]o +0 of /Fe] h abnaudnewsdtrie rmfive from determined was abundance carbon The D145 a lsie sFtp ydifferent by F-type as classified was 194951 HD λ 6014.8 λ II 4769.9 /H]–[X − . ) eotie CH au of value [C/H] a obtained We A). ˚ . e ae rmTkd Takada- & Takeda from taken dex 0.1 18 A, ˚ I ± H s+.5 00 and +0.09 +0.05, is /H] 0 5.3 λ . 5dxsest niaeta this that indicate to seems dex 05 4775.8 I D194951 HD . − rpe nte6140–60 the in triplet .6ad[/e = [C/Fe] and 0.36 − .3dx respectively. dex, 0.23 A, ˚ − . e o abnled carbon for dex 0.2 λ 4932.0 O I O I A, ˚ λ − − region. A ˚ 5380.3 OIA&RIVERA & MOLINA .6re- 0.26 .9re- 0.09 − 0.16. A ˚ otoeotie yLc 21) h ieat line N The similar (2014). are values Luck abundance by λ O obtained and those C to These lar. OH = [O/H] serce,wt auso NH 06 and +0.60 = [N/H] of values with that +0.73 = found [N/Fe] enriched, they 194951 is HD and for N abundance spectra N high-resolution the using study (2011) to al. et able Lyubimkov were However, measured. be not nteNaudneapa ob u ovariations to in due 0.5 be changes and to few K very 250 appear that of abundance K note 6760 N we i.e., the 3 al., in Table et In Lyumbikov 1.92. by and used relative model gravity the surface to and temperature effective in h / .6rtoi rcial oa,bti san is it but solar, star. star. practically the O-rich is of ratio surface 0.46 = the C/O on The H- released the been from has material burning has processed CN-cycle that the and that place experienced taken indicates and have N C in of that enrichment deficiency type the The (1DUP). F dredge-up and first en- A the N of super- the in stars authors present giant characteristic the general to a According is affected richment being model. without the abundance N by this use can we S/e 03.Ohreeet uha c r Mn between [X/Fe] Cr, abundances Sc, show as Zn such i.e., and elements enrichment, Other moderate +0.33. = a [Si/Fe] The exhibits population. disk abundance thin Si the to belonging object an Hre 1937), (Harper aito.Dnie ae 17)rpr rota- a s report km 40 (1972) little of Faber velocity very tion & show Danziger values These variation. 2006). (Gontcharov l .Temtliiyo D249 smoderately Ta- is 224893 in HD shown of = ([Fe/H] are metallicity for deficient The abundances performed The was 4. ble elements time. 15 first of the total a includes e h ailvlct ndffrn pcs obtaining s km epochs, stud- different (in authors in values clas- Several velocity was radial A8II. it the giant, and ied bright 2) a Table as (see sified star this for rameters solar. average on is it ta.1953), al. et h -lmnsrne from ranges s-elements the n hc ik h naudnewsobtained was at abundance line Zn synthesized The the thin the from disk. of objects thick in and present those to similar +0.09, 4151.4 u topei oe iesb 4 n 0.12 and K 240 by differs model atmospheric Our h [ The nti ae naayi faudne which abundances of analysis an paper this In rye l 20b eemndamshrcpa- atmospheric determined (2001b) al. et Gray on o D464adH 283could 224893 HD and 45674 HD for found A ˚ − α .0ad[/e = [O/Fe] and 0.20 F]rtovleo 00 scnitn for consistent is +0.06 of value ratio /Fe] − 7(ernahe l 96 and 1996) al. et (Fehrenbach 27 ± − − .8respectively. 0.18 32(isn1953), (Wilson 23.2 1 of ) 5.4 − T .6dx.TeCabundance C The dex). 0.26 D224893 HD . eff − − 1 n log and 24(dm 1915), (Adams 22.4 . − .9t 00,ta is, that +0.01, to 0.09 λ − 4810.5 .0aena oso- to near are 0.10 g hsmasthat means This . − XF]of [X/Fe] . A ˚ 19(Bouigue 21.9 − .5and 0.15 − − 25.10 26.4 © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México andfrom tained − hc smdrtl nihdb 03 e.The dex. Sc, +0.39 except by values enriched ([ solar alpha-elements show moderately Mn is and which Cr V, as such value a has and 45674. HD O-rich to is similar 224893 0.26 HD = C/O that ratio abundance indicates The O enrichment. the moderate respec- that a of shows dex indicate values values +0.53 = [O/Fe] These to and tively. leads dex +0.35 1998) = [O/H] Takada-Hidai & Takeda NF]=+.5dxrsetvl.Teequivalent The of m 15.8 rection was line this respectively. of width dex +1.15 = [N/Fe] [/e 04) oee,annLEcorrection non-LTE a of However, +0.45). = ([O/Fe] 6158 at the and ev- CN-cycle shows the star event. undergone this 1DUP having 45674, of HD dex idence +0.99 Like = [N/Fe] and dex respectively. +0.81 = [N/H] were ues -lmns( n a bnacsrsml h solar the values. resemble abundances Ba) and (Y s-elements CH n CF]rahdvle of values reached [C/Fe] and [C/H] epciey rmteLEaayi edrvda of derived we [C/H] analysis of LTE value the From respectively. T orcinof correction LTE 21)a oa ealct Z=000.Lumi- 224893 HD and 0.020). 194951 = HD (Z 45674, HD metallicity for solar nosities at (2012) f5 n 9 masses and theoretical for 7 po- the rotation 5, their employed evo- without of We from theoretical tracks obtained using evolutionary tracks. HR-diagram be the lutionary can on These sition stars. by derived values mean authors. other the (within with consistent the uncertainties) are for the metallicity values and microturbu- adopted velocity gravity, our lence surface that temperature, atmospheric note val-effective of can two value We than more mean with ues. a objects take present those We are of parameters work 2. this Table in in adopted those and erature a bandfo h ie 4770.0 lines the from obtained was .9dxrsetvl.TeNaudne ob- abundances N The respectively. dex 0.19 − h bnacs[/e fteF-ekelements, Fe-peak the of [X/Fe] abundances The h bnac sdrvdfo h line the from derived is abundance O The eas siae h asso u sample our of masses the estimated also We lit- the from taken parameters atmospheric The .5dxa eprtr f70 (from K 7500 of temperature a at dex 0.15 n hw in foverabundance of signs shows and A ˚ − 6.1 .8dxaotda 50 h e val- new the 7500K at adopted dex 0.08 λ 4151.4 topei Parameters Atmospheric . M α .DISCUSSION 6. F]= /Fe] ⊙ − − 6.2 ae rmEsro tal. et Ekström from taken , ee[/]=+.9dxand dex +0.89 = [N/H] were A ˚ .1dx ytkn non- a taking By dex. 0.11 .6dx(en19b,both 1995b), (Venn dex 0.26 Masses . − .2dx;teZ n the and Zn the dex); 0.02 .Wt o-T cor- non-LTE a With A. ˚ LMNA BNACSI UEGAT 407 SUPERGIANTS IN ABUNDANCES ELEMENTAL n 4771.7 and A ˚ − .7dxand dex 0.37 A ˚ orcint h oo xes( excess pc. color 125 the of to scale-height correction a A assuming with from disc modelled was exponential estimated disc thin where a Galactic the 2011) was in Finkbeiner dust excess & the (Schlafly color map Schlafly’s the 45674 HD H 57) .1(D102) .0(D194951) (HD 0.30 180028), (HD 0.29 0.11 are uncertainties 45674), (HD these cor- Individually, parallaxes, bolometric the and rections. of extinctions uncertainties magnitudes, the luminosi- visual on the based of is uncertainty ties The HR-diagram. the in listed are 1. Table values of The column eleventh assumption. the last the with ie rmSroge htmtyb rye al. obtained et We Gray by (2001b). photometry Strömgren from rived tion a)etmtdb otuhe l 21) The magnitude, bolometric M solar a (2012). adopted we al. and et (2006) Masana al. from taken et were corrections Kovtyukh bolometric by estimated mag) n D249 eeotie using obtained were 224893 HD and V V a eie rmama au ( value mean a from derived was 2007). Leeuwen (van parallaxes from mated eecluae using calculated were 0.020. = Z vltoaytak ihu oainfrmse f5 7 5, theoretical of The masses 9 for rotation and HR-diagram. 194951 HD without the 180028, tracks HD on evolutionary 45675, HD 224893 HD of and Locations 4. Fig. 0 0 Bol = iue4sostepsto forsml tr on stars sample our of position the shows 4 Figure h oo xessfrH 808 D194951 HD 180028, HD for excesses color The o D102,hwvr h bouemagnitude absolute the however, 180028, HD For steitiscclu eie rmexpresion from derived colour intrinsic the is E V 4.73 = M ( − b ⊙ − 3 r ae rmEsro ta.(02 with (2012) al. et Ekström from taken are . y ± 1 0.78 = ) E .1(ry2005). (Gray 0.01 ( B − V E and ) M ( B V E − = ( B V D V Fri 97.For 1987). (Fernie ) 0 − stedsac esti- distance the is 5 + B V M − rmterela- the from ) − V V = o() where log(D), E a applied was ) − ( b 3.38 − y ± de- ) 0.16 © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México oLuikve l 21)tems osi unim- super- is A–F loss of (progenitors mass stars the B-type (2011) for According al. portant et envelope. associ- Lyubimkov convective dredge-up to deep the the and mix- with phase induced ated MS rotationally the the during ing loss, be mass in can processes severe material these the CN-cycle stars single of In presence surfaces. stellar the stars. to massive leads for Each enhancement nitrogen surface the super- stars. for giant (2006) bright al. and et giant & Smiljanic Luck and (1985), Venn (1995) Lambert (1995b), Wepfer & of Venn Luck (2003), enhancement by Przybilla This reported & also surfaces. was stellar nitrogen the ma- CN-cycle in of terial systematic presence the a indicating and have N C of objects increase of deficiency These systematic a abundance. shown N of enhancement NF]=+0.99 = [N/Fe] h bnac nH 991wspreviously +0.73 = [N/Fe] that was i.e., found enriched, who 194951 is (2011), HD nitrogen al. et in CN-cycle. Lyubimkov by the abundance studied of N efficiency we the The 180028, HD about es- in to argue nitrogen unable cannot of were abundance we been the Since has timate that surface. material the to processed brought CN of signs show D464adH 283 h auswith values The +0.36 = [N/Fe] 224893. HD are corrections NLTE and 45674 HD we n 7.5 and 7 tween ecudetmt htH 808hsams of mass a has 7 180028 HD and position 5 that their between estimate to could According we 224893). (HD 0.21 and 408 iyol n irgnln ( line nitrogen one only tify al. et Silva da (2014); oxygen al. the et our (2015). of Bensby general, by objects In in studied tendency disc observed bi-cycle. the show CNO values the probably to a +0.45) = due has ([O/Fe] contrast, enhancement by moderate 224893, HD respectively. +0.53, inywt o-T orcin .. hyrange they i.e., defi- correction, elements show non-LTE from light 224893 a HD the with and 45674, HD ciency to for 194951 HD abundances respect C 180028, the HD With that note we CNO, 4. shown is the Table summary A reflects in stars. composition the inside their process mixing since status tionary o h bnac of abundance values O show the 224893 HD for and 194951 HD 180028, HD he rcse aebe ugse oexplain to suggested been have processes Three an show 224893 HD and 194951 HD 45674, HD o h oa apew eeal oiden- to able were we sample total the For N bnacsaekyt eueteevolu- the deduce to key are abundances CNO plignnLEcretos D45674, HD corrections, non-LTE Applying − .4to 0.04 6.3 − ± M .9dex. 0.69 .4dx epciey ohobjects Both respectively. dex, 0.14 vltoayStatus Evolutionary . M ⊙ ⊙ n D249 faot9 about of 224893 HD and , D464adH 991be- 194951 HD and 45674 HD , − .6 +0.02, 0.36, λ ± 4145.4 .1dxand dex 0.11 ± − .8dex. 0.18 .0and 0.10 OIA&RIVERA & MOLINA )for A) ˚ M ⊙ . h oe sdb ybmo ta.(01.From (2011). al. et Lyubimkov by used model the vltoaymdl o assbten9-120 between masses for models evolutionary nta eoiyo 0 ms km 300 (with of rotating velocity calculate initial (2000) a Maeder & Meynet ok ee ems mhsz htormodel our that in emphasize this K 240 must in by estimated we et differs abundance Here, Lyubimkov C by the work. derived and abundance (2011) al. N the from (2006). al. DPaddrn h lelo hs o tr of stars for phase loop blue the 9 the during after rotation and with 1DUP dex +1.15 = ro- [N/C] without and dex tation +0.72 = [N/C] predict authors These sapoiaey[/]=+.0dxfrsaswith 15 stars and for 2 dex between (1992) +0.60 masses = ratio. al. [N/C] et [N/C] approximately Schaller the the is by know prediction through to post-1DUP passed necessary The is already event have 1DUP 224893 HD and companion. evolved an due from be transfer can enhancement mass binary this to contrary, In the the on stars. that differ stars, non-rotating might fact and event rotating observational 1DUP between found the an during be is process might mixing it processes e.g., two coupled, other the contrast, ins ihmse agn ewe 4–15 between ranging masses with giants) viewed be can figure color abun- The CNO online. data sources. mean represent different color and and from Symbols 1978) (2014). Luck (1977; by the dances Luck with supergiants young from [X/H] G–K of taken abundances sample our a for of abundances mean Comparison 5. Fig. M o D145,te[/]rtocudb obtained be could ratio [N/C] the 194951, HD For nodrt eiywehrH 57,H 194951 HD 45674, HD whether verify to order In ⊙ o oedtisseFgr 4i mlai et Smiljanic in 14 Figure see details more For . T eff n y01 nlog in 0.12 by and M ⊙ − nteohrhand, other the On . 1 n non-rotating and ) M g ⊙ By . from M ⊙ . © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México al ecnseta hr r ml differences small are there that see of can we 3 Table ol ei gemn ihterslsfrnon- for results 9 of the masses with with agreement stars rotating in be would o tr ihmse rm6t 13 to 6 occur from masses loops with red-blue stars Claret for extensive area. that loop suggests red-blue can the (2004) inside objects only post-1DUP located post-1DUP be the in Evolutionarily, are and already phase. event have 1DUP 224893 HD the experienced and 194951 HD 45674, HD a ocueta ihnterneo assof masses of range (5–9 the objects within our that conclude may D464adH 283w eemnda[/]ra- +0.88 [N/C] a of determined tio we 224893 HD and 45674 HD es h en[/]rtofrtesml tr is stars pro- sample the mixing for efficient ratio +0.90 an [N/C] = [N/C] mean of The that signs indicate cess. show values these stars that both also note We tively. aigmdl.Orma au +0.90 value mean Our (ro- dex dex +1.15 model). non-rotating 0.3-0.4 between and tating i.e., the between model) (2000), (non-rotating Maeder of factor dex & +0.72 those Meynet a by above of by model slightly (1992) are and Schaller al. by obtained values et the than larger are ratios ti osbet s h irgnaudnede- +0.81 = abun- [N/C] abundance C is our nitrogen value with This (2011) the al. dance. use et Hence, Lyubimkov to by abun- (2011). rived possible N al. is the et Lyubimkov it affect by not derived do dance differences small These oae ihnteetne e-lergo with region red-blue be extended to M the right, appear within 224893 be HD located and to 194951 HD luminosities 45674, HD and temperature fective 2011). al. et Lyubimkov in 12 Figure be ihrgr oH 808 suigams of mass a assuming 180028, unreli- 5 HD is to regard status With evolutionary able. lu- their the that in so change minosity appreciable an cause uncertainties ntecnrr,i easm aso 7 of mass a assume phase). we (post-1DUP if region contrary, loop the red-blue On the in it xeso ssilamte fcnrvry(see controversy of matter a still is extension n oigfrtefis ietwrsterdgi- red the towards time phase). first (post-MS region phase gap the ant/supergiant Hertzsprung for the moving on and located be to would D249,rsetvl.I sblee htthe dredge-up that first believed the to is related It is enrichment sodium and respectively. 194951 HD 180028, 224893, HD HD 45675, +0.24 HD +0.43, for +0.34, +0.55 and of [Na/Fe] i.e., abundances, Na M − 7 = nsot u eut o igeadma [N/C] mean and single for results our short, In nteohrhn,i ecnie h ef- the consider we if hand, other the On norsml efudamdrt nihetof enrichment moderate a found we sample our In ⊙ .2(in 0.02 t rbbeeouinr ttswudplace would status evolutionary probable its , − 9 M ± ⊙ T .9dxad+1.00 and dex 0.09 ± eff nteH-iga.Hwvr the However, HR-diagram. the on .3dex. 0.13 and ) M ⊙ 6.4 n o hi NC ratios, [N/C] their for and ) Sodium . − .6(nlog (in 0.06 LMNA BNACSI UEGAT 409 SUPERGIANTS IN ABUNDANCES ELEMENTAL M M ± ⊙ .3dxrespec- dex 0.13 hrfr,we Therefore, . ⊙ ± g lhuhthis although , .7dx For dex. 0.17 respectively. ) ± .0dex 0.10 § M and 6 ⊙ it . dex. 0.3 oslrmtliiy(hronl&Lgre2010). Lagarde & for process (Charbonnel Even extra-mixing metallicity by solar or to dregde-up first the from azo21)idct htsdu osntso a show Lat- not ( & stars Karakas does low-mass in in sodium enrichment 8 that significant predictions indicate Fig. The 2014) (see tanzio models debated. the by still made is assumption although 1990) this Denissenkova & (Denissenkov event u bet ssmlrt htosre ntethin the in [ observed that i.e., to population, similar disk is objects our hman 19)fritreit asstars Eid mass El intermediate for by ( (1995) predicted Champagne in [Na/Fe] obser- are & the our uncertainties) and with that their +0.24 agreement note (within +0.22, We results results +0.16, and vational respectively. (2011) of dex al. [Na/Fe] +0.37 et of Lind values from in taken was Na o D145,soigatnec iia othat to similar tendency +0.12 for a and observed 45675 showing HD 194951, for HD +0.25 for of (6743–6757 [S/Fe] at a syn- region obtained estimated spectral was the abundance sulfur thesizing The dex. 0.18 hwamds niheto Zr of enrichment 180028 HD modest and 45674 a HD value. show solar the abundances By i.e., [X/Fe] to show similar stars overabundant, neutron-capture sample 2005). all and is in al. Iron-peak elements 180028 HD et dex. +0.44 (Caffau for = [S/Fe] value S solar contrast, to near ity aatcceia vlto o ouainIstars. I from Population expected for evolution trends chemical the galactic follow elements) capture ao.W a e,i eea,ta bnacsof abundances that pen- CNO, general, (e.g., filled in stars red sample see, our a can filled We with blue abundances tagon. a CNO with and represented circle are The supergiants pentagon). (open cool 224893 HD 194951 and HD square) triangle), (open (open 45674 180028 HD HD of circle), namely symbols stars (open uncertainties, different their sample with with shown the together atomic are in paper versus present abundances abundances the The Fig- [X/H] the (2014). number. shows Luck by 5 abundances ure CNO 1978) (1977; mean Luck and by G–K studied of stars sample supergiant a young from derived abundances mean the respectively. dex, +0.32 and dex +0.45 ≈ .-. dex). 0.2-0.3 o-T orcino bu of about of correction non-LTE A h ednysonb h lh-lmnsof alpha-elements the by shown tendency The u XH bnacscnb oprdwith compared be can abundances [X/H] Our 6.6 oprsnWt te Supergiants Other With Comparison . > M α 2 6.5 eeet nteds o metallic- for disc the in -elements M eve Elements Heavier . ⊙ hsercmn osntexceed not does enrichment this α F]rne from ranges /Fe] α epa n neutron and Fe-peak , II − n La and .0dxto dex 0.10 M − ≤ ) We A). ˚ .2to 0.02 2 II M ⊙ of ) © Copyright 2016: Instituto de Astronomía, Universidad Nacional Autónoma de México e,so in fitra iig en[N/C] mean A nitro- mixing. +0.90 and internal of carbon of ratio both signs which determine show for to gen, able 224893), HD were and we 194951 HD stars using 45674, Three (HD abundances widths. equivalent and and synthesis atmo- spectral masses determined We parameters, spheric type spectra. 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Adams, im- that work. suggestions this and ref- proved comments anonymous fruitful an for we thank eree authors which The for thankful. databases are ADS-NASA and SIMBAD satisfactorily be determined. not could status I, evolutionary Population its the of but on typical 180028, HD abundances shows region. contrary, loop red-blue lo- the are in objects cated These post-first phase. the (post-1DUP) reached 224893 have dregde-up HD that the population of and disc supergiants thin for 194951 HD typical values abundance 45674, HD have that clude radial discarded. be in can variability binarity sample little hence The very and re- 1DUP. shows velocities, a the stars be during three only mixing of can deep it and of predict stars sult which these enhancement in nitrogen (2000), observed surface was Maeder A dex. & mo- =+0.72 [N/C] Meynet non-rotating by of preditions dels the with agreement lrt .20,AA 2,919 10 424, 522, A&A, A&A, 2004, 2010, A. N. 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