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Uva-DARE (Digital Academic Repository) UvA-DARE (Digital Academic Repository) Line spectra of some giant and dwarf K-type stars Koelbloed, D. Publication date 1953 Document Version Final published version Link to publication Citation for published version (APA): Koelbloed, D. (1953). Line spectra of some giant and dwarf K-type stars. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:04 Oct 2021 l ACADEl'vlISCll PR()EI~'SCHRI TER VERKRUGINCi V/\N DE CHr\/\D V/\N DOCTO,R IN DE WIS- EN NATUURKUNDE /\AN DE UNlVER­ SITEIT VAN r\MS'TERDld\i[, OJ' GEZAG VAN DE RECTOR },,1AGNIPrc-::US NIH DR G. VAN DEN BERGl'!. HOOGLEHAAR IN DE FACUL'I'ElT DER R.ECHTS­ GELEERDHEID, IN HET OPENB/\AIZ 'I'E VERDEDIGEN IN I)E AULA DEE UNIVERSITEIT 01' WOENSDACi 3 JlJNI 19.'5:), I)E8 NA1\iJrDDAGS 'rr: 3 UUR PREGlES DOOR DAViD KOELBLOED GEBOREN TE AMSTERDAM University ofAmsterdam Institute "Anton Pannekoek" LIBRARY OF ASTRONOMY Kmislaall 403, 1098 SJ Amsterdam The Netherlands. 'ret +31 20··5257489 1953 DRUKKERIj WED. G. VAN SOEST --. AMSTERDAM I-let in dit proefschrift aangeb(xJen werk werd llitgevoerd In ovedeg met ])rof. Dr A, Pannekoek en is goedgekeurd door de Promo[(Jr Prof. Dr Ii, Zanstra Aan mijn Moeder Aan myn Vrouw Aan Ineke STELUNGEN. 1. VoJgens Parenago zou er een discontinuiteit in de kinennatische en physische eigenschappetl cler sterren van de hoofdrecks bestaan, Dit zou van grate betekenis voor de cosmogonie kunnen zijn. De real iteit van zijnuitkornsten moel: echter, op grond van de \vaarnemingsgegevens, betwijfeld worden. P. P. Pan:enago, PubL Sternben:g State, l\strol1. Institute 20, 81:, 1951. n, Fen nader onderzoek naar turbulcntie in atmospberen van K-sterren is gewenst Ler toetsing van de theorc~l:ische uitkornsten betreHencle de Jigging van de bovengrens van de convectieve laag. III. De wijze, waarop Lauwerier aXloma's voor projectieve meetkunde invoert, is door het ongeoor­ [oofde gebruik vall het syrnbool 00, inexact. De opmerking, dat het symbooI verrneden kan worden door hornogenc getallcnparen te gebruiken, is in het stadium van de ontwikkeling der theorie onjuist, 1-1, l\.. Lauwerier, Axiomatische onderzoekingen oven: de vlakke meetkunde. Dis". 1948,. p. It e,'i. IV. Bij de herekening van intensiteitsvercleling in continue spectrurn van een cK5 ster, client rekening gehoudel1 te worden met de rnogelijkheid van Rayleigh. verstrooilng door neutrale waterstofatornen, \1, Er is gE~en reden om, op grond van het schiHen'model, de door Daniels, c.s. gemeten waarde van het magnetische mOlllent van de 58Co-kern in twijfel te trekken. J. !\t Dannels, c.s" Phil. lV[ag, series 7, Vol 43, p, 1297., 1.952, VI. UiL statistische ovcrwegingen mag verwacht worden, dat het systematisch onderzoek van zwakke eclipsvariabelen, in de lvfelkweg, weinig H'sultaten van statistische\vaarde zal opleveren. vn, De aHeiding, die \Iv'aldmeier geeft voor de betrekking tussen de electronen-temperatuur van cen gasnevel en de ternperatllur van de centrak~ ster, is onjuist. 1vt Waidmeier: Einfllhrung in die Astrophysik, p, 348, 1948. vm, Oat rel1zen van s populatie II in algemeen cen kIeinerc iichtkracht zouden bezitten dan voIgens de nOn1JaJc massa Iichtkracht \;vet verwacht wordt, kan bestreden \vorden, C, Payne,Caposchkin: Stars in the making, Cambridge, Mass., p.145" 1952. IX, De 11 it ele verhouding del' Lij nintensiteiten bepaalde verschillen in magnitude tussen de beic1e com­ ponenten van een spectl,oscopisclw dubbelster, rnoeten met voorzichtigheid gebruikt'.vorden bij de studie van dl~ massa,lLchtkracht wet en hij het af1eiden van de elementen van het stelsel met behulp van Lichtkromme, ingeval van een eclipsvariabele. R. M. Dom. Aslroph. Obs. Victoria, Vol 8, J19, 1950,Llarvard Obs. Mon" No 7, 231, 1948. De "stratiJicatie" van elernenten in de atll10spbeer van .Arcturus, gevonden door S. E. A. van Dijk.e. is cell, schijnbare. S. E. t\. van Dijke, Ap. J. 104, 44, 1946, Xl. In K"sterren lijkt de abundantic van titanium ten opzichte van die van ijzer grater in de reuzen dan in de chvergen, Er zijn aamvijzingen een dee1 van zulke abundantie-verschiHen schijnbaar is en anlstan! door het gebruik van cen te ig atrnospheriscb model. Dit proefschrift. p.. 37, XII. De verklaring, die UnsLild en Struve geven vom de verschiHen in turbulent.e snelheden tussen ionen en. alomen, gevondcn door K., O. Wright in de atmospheren van enige sterren, is in sommige gevallen niet bcvredigcnd. l\., Unsold en O. Struve, Ap. J. 110, +60, 1949, TABLE OF CONTENTS. Samenvatting s Summary .. 7 1. Introduction () 2. The spectral plates 9 Chapter I. The derivation of the line intensities, 3. The derivation of the intensity curves. 10 4. The continuous background , . II, 5. An absorption band of unknown origin in the spectrum of 61 Cygni, 13 6. The derivation of equivalent widths. 15 a. The empirical line profile. 15 b. The instrumental prol1le . 15 c. The theoretical profile . 17 c1. The instrumentally broadened theoretical proille ]II) e. The analysis of the blends . 119 7. The catalogue of line intensities . 20 8. The hydrogen lines. 21 9. The comparison of equivalent widths with tl10se of other observers 22 10, The curves of growth. n 11. The Carter effect. 29 ]2, Comparison of curves of growth with those obtai.ned by other observers 29 Chapter n. Temperature and electron preSSUI·,e (Homogeneous model). 13. The excitation temperature. 31 14. The ionization temperature and electron pressure, 32 15. Rayleigh scattering by neutral Ii atoms in the K-type giants 38 16. Discussion of the results for Fe and Ti. , . , . , 40 17. Comparison of electron pressure with l\ifiss van Dijke's results . 41 18, Cornparison of excitation temperature and ionization temperature. 41 19. Comparison of ionization temperature and effective tem.perature . 43 20. The ionization temperature derived from the lines of other elements. "14 Chapter III. Theoretical results for faint Hnes of Fe and 1'1 (Stratified model). 21. Introduction. The theory of faint lines 46 22, The relation between gas pressure, electron pressure and temperature 48 23. The continuous absorption coefficient. , . 51 24. Model atmospheres of K-type stars, , , . .. .,.. 52 a. Introduction. .. .. .... 52 b. The construction of models with mechanical quadrature. 53 c. An analytical construction . 54 d. Numerical results for tIle atmospheric curves. .. 58 e. The upper boundary of the zone of convection. 59 25. On. the distribution of absorbing atoms and ions with optical depth 61 26. The weighting functions.. 63 27. The numerical resuJts for the atDlospheric integrals and. the theoretical excitation temperatures .. .. .. (i5 28. The"Adams-Russell" phenomenon. 68 29. Critical remarks on the use of the homogeneous model. 69 Chapter IV. The pmblern of gra.vity.. 30. Cornputation of the gravity gcfl derived from the spectrum . 73 31. Computation of the true surface gravity, derived from mass and radius. 76 32. Comparison of th.e effective with the true gravity 77 33. On the influence of motions of gases on gw 79 3"1·. OverhlJninous stars . 82 The spectral line catalogue 83 Bihliography . 92 S/\MENVATTING. De in dit proefschrlift bewerkte spectra van K ZIJI1 opgenomcn Professor A. Pannekoek op het Observatorium te Victoria, IlIet het doel 0111 uit de spectraal1ijn~ intensiteiten atmospherische temperaturen en de versnelJing van de 2.waartekrachl: nan. ste1'­ oppervlak af te leiden. Onderzocht worden de dwergcn 61 Cygni en 70 Ophiuchi, bekende dubbelsterren, de reuzen a Boot!s en a T,mei, benevens de superreus ~ Cygni. Ten gevolge van de grate gecompIiceerdheid cler K-spectra men tot nu toe WClilIg aanJacht aan deze spectra besteed. Door het gedeeltdijk autornatiseren van de reductietechnid~ is het thans mogelijk de bewerking dezer spectra minder tijdrovend te maken. Het gemeten spectraalgebied strck!: zich Ult van 4100 Lot 4770 A.De dispersie bedraagt 10 A/:mm bij A 4375 A. In hoofdstuk I wordt de methode van het bepa1en van Iijnintensiteiten besproken. In het continue spectrum van 61 Cygni w()rdt een depressie van onbekende ()orsprong ge­ vanden. De intensiteitsdistributie van deze inzinking is vrij symn1etrisch, bereikt een minimurn van 70 van de inten:siteit van het naastliggende continuuln bij 4780 A en sLrekt uit van 4770 tot 4790 A. Met behulp van de equivalente breedten en ..Allen's Nf waarden, vcrkregen uit het zonne· spectrum, zijn groeikrommen geconstrueerd en de verschillen van de logarithmen van het aantal werkzame atomen met die van de zon bepaald. Turbulente sne1heden del' atmospherische gassen worden vervolgens uit de posities der graeikrom.men afgeleicL Nadat deexcitatietemperaturen berekend zijn uit de lijnmtensit,eiten del' ijzer-atomen, worden in hoofdstuk II de lonizatietemperatuur en de e1ectronendruk afge:leid llit de .iintensiteitcn van atoom- en ionlijnen van Fe en Ti, aan de hand van een eenvoudig miodel (homogeen model). Hierbij is verondersteld dat de gemi.ddelde optische diepten van jijnformatie voor atomcn en i(lnen gelijk zijn aan elkaar en avereenkomen met die van de zan. Aangenomen is dat de continue absorptie hoofdzakelijk door negatieve waterstof-ioncn veroOl'zaakt wordt en dat de abundanties in ster en zan dezdfde zijn.
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