Ankara Üniversitesi Akademik Arşiv Sistemi

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Ankara Üniversitesi Akademik Arşiv Sistemi ANKARA ÜNİVERSİTESİ FEN BİLİMLERİ ENSTİTÜSÜ YÜKSEK LİSANS TEZİ DÜŞÜK GENLİKLİ δ SCUTI YILDIZI 20 CVn’NİN ELEMENT BOLLUK ÇALIŞMASI Tolgahan KILIÇOĞLU ASTRONOMİ VE UZAY BİLİMLERİ ANABİLİM DALI ANKARA 2008 Her hakkı saklıdır ÖZET Yüksek Lisans Tezi DÜŞÜK GENLİKLİ δ SCUTI YILDIZI 20 CVn’NİN ELEMENT BOLLUK ÇALIŞMASI Tolgahan KILIÇOĞLU Ankara Üniversitesi Fen Bilimleri Enstitüsü Astronomi ve Uzay Bilimleri Anabilim Dalı Danışman : Yrd. Doç. Dr. Kutluay YÜCE Eş Danışman: Prof. Dr. Saul J. ADELMAN Bu tez çalışmasında, 20 CVn (F3 III) yıldızının, Dominion Astrofizik Gözlemevi’ndeki (Victoria, Kanada) 1.2 m’lik teleskoba bağlı Coude tayfçekerindeki Reticon ve CCD algılayıcılarla elde edilen yüksek kaliteli tayflar kullanılarak atmosfer parametreleri ve element bollukları tespit edilmiştir. Optik bölgenin λλ3820-4940 Å dalgaboyu aralığını içeren tayflar, Dr. Graham Hill ve arkadaşları (Hill et al. 1982a,b) tarafından yazılan REDUCE ve VLINE programları kullanılarak ölçülmüştür. Her tayf çizgisine ait merkezi dalgaboyu, eşdeğer genişlik, derinlik ve yarı maksimumdaki tam genişlik değerleri bulundu. Atmosfer analizi, Dr. Robert L. Kurucz (Kurucz 1993)’un yerel termodinamik denge varsayımlı, paralel düzlem geometrili ATLAS9 ve O’nun ilgili programları kullanılarak gerçekleştirildi. 20 CVn’nin çizgi tanısı yapıldıktan sonra, atmosferindeki atom ve iyonlar tespit edilmiş oldu. Çizgi tanısı, benzer tür yıldızlar için yapılacak tayfsal çalışmalar için yararlı olacaktır. Etkin sıcaklık ve yüzey çekim ivmesi, gözlemsel ve kuramsal Hγ profillerinin karşılaştırılmasından, spektrofotometrik akıların, teorik profil ve akılarla karşılaştırılmasından ve nötr ve bir kez iyonlaşmış demir çizgileri kullanılarak demir elementinin iyonizasyon dengesinden elde edilmiştir. 20 CVn için elde -1 edilen değerler: Te = 6950 K and log g = 2.80 dir. Mikrotürbülans hızı 2.6 km sn olarak hesaplandı. Dönme hızı (v sin i), bazı metal çizgilerine yapılan Gauss fitlerinden 5.6 km sn-1 olarak elde edildi. C, Mg, Si, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, Eu, Gd, Tb, ve Tm elementlerinin bollukları belirlendi. Bolluk analizi sonuçları, 20 CVn’nin atmosferindeki element bolluklarının Güneş’in değerlerine yakın olduğunu göstermektedir. Bununla beraber Normal yıldızlarda beklenen bazı bolluk farklılıklarını da içermektedir. Bu farklılıklar demir grubu elementlerde biraz fazlalık, nadir toprak elementlerinde ise aşırıbolluk olarak kendini gösterir. Güneş değerlerinde olan Ca ve Sc, bize 20 CVn’nin bir klasik Am yıldızı olmadığını gösterir. Yıldız, marjinal Am yıldızlarının özelliklerine sahiptir. Hesapladığımız [Fe/H] = 0.06 değeri, demir bolluklarının Güneş’den anlamlı bir miktarda fazla olmadığını göstermektedir. Ocak 2008, 200 sayfa ANAHTAR KELİMELER: 20 CVn, F tayf türü yıldızlar, δ Scuti yıldızları, atmosfer parametreleri, model atmosfer, mikrotürbülans hızları, element bollukları. i Abstract Master Thesis AN ELEMENTAL ABUNDANCE ANALYSIS OF LOW AMPLITUDE δ SCUTI STAR: 20 CVn Tolgahan KILIÇOĞLU Ankara University Graduate School of Natural and Applied Science Astronomy and Space Sciences Department Supervisor : Asst. Prof. Dr. Kutluay YÜCE Co-Supervisor : Prof. Dr. Saul J. ADELMAN In this thesis study, the atmosphere parameters and elemental abundances of 20 CVn (F3 III) were determined using high quality spectral data obtained with Reticon and CCD detectors at the long camera of the coude spectrograph of the 1.2 m telescope at the Dominion Astrophysical Observatory (Victoria, Canada). The spectra covering λλ3820-4940Å of the optical spectral region were measured using programs REDUCE and VLINE written by Dr. Graham Hill and his associates (Hill et al. 1982a,b). I found for each line, its stellar wavelength, equivalent width, line depth, and line width. The atmosphere analysis was performed using the LTE plane parallel model atmospheres code ATLAS9 and its associated programs of Dr. Robert L. Kurucz (Kurucz 1993). After the line identifications for 20 CVn were finished, the atoms and ions in its atmosphere were found. The line identification should be useful for the spectral studies of similar type stars. The effective temperature and surface gravity were found from fitting the observed Hγ profiles and spectrophotometric fluxes with the theoretical fluxes and profiles, and the ionization equilibria of iron from neutral and singly-ionized lines: The adopted values of 20 CVn are Te = 6950 K and log g = 2.80. The microturbulent velocity was calculated to be 2.6 km s-1. The projected rotational velocity (v sin i) was derived as 5.6 km s-1 from the Gaussian fitting of several metal lines. The abundance of C, Mg, Si, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, Eu, Gd, Tb, and Tm were determined. The results of the abundance analysis show that 20 CVn's abundances are close to solar values, something that is expected for normal stars. It exhibits slightly enhanced iron peak metals and overabundances of some Rare Earths. The Ca and Sc abundances, which are solar, show us 20 CVn is not a classical Am star. It has a marginal Am star charateristic. Our [Fe/H] = 0.06 value shows that the Fe abundance do not exhibit any significant overabundance respect to solar. January 2008, 200 pages Key Words: 20 CVn, F type stars, δ Scuti stars, atmosphere parameters, model atmospheres, microturbulent velocity, elemental abundances. ii TEŞEKKÜR Yaptığım çalışmaların her aşamasında bilgi ve tecrübeleriyle bana yol gösteren, bana daima vakit ayıran, tayf konusunda yetişmemi ve ince ayrıntıları görmemi sağlayan danışmanım ve değerli hocam Sayın Yrd. Doç. Dr. Kutluay YÜCE’ye, 20 CVn yıldızının gözlemsel verilerini Dominion Astrofizik Gözlemevi (Kanada)’nde gözlemci olarak temin edip benimle paylaşan ve tayfsal analizler konusunda bana önemli bilgiler sunan, kendisiyle Fransa’da düzenlenen NLTE konulu bir çalıştayda tanışma imkanı bulduğum danışmanım Sayın Prof. Dr. Saul J. ADELMAN’a, 20 CVn’nin tayfsal gözlemlerinin yapılabilmesi için gerekli gözlem zamanlarını tahsis eden Dominion Astrofizik Gözlemevi müdürü Dr. James HESSER’e, yıldızın gözlenen tayflarını bir boyutlu tayflara dönüştüren Austin F. GULLIVER’e, tayf ölçümlerinde gerekli olan REDUCE ve ilgili programlarını benimle paylaşan Dr. Graham HILL’e, maddi ve manevi desteklerini hiç esirgemeyen anneme ve babama çok teşekkür ederim. Tolgahan KILIÇOĞLU Ankara, Ocak 2008 iii İÇİNDEKİLER ÖZET........................................................................................................................... i ABSTRACT................................................................................................................. ii TEŞEKKÜR................................................................................................................ iii SİMGELER DİZİNİ................................................................................................... vi ŞEKİLLER DİZİNİ.................................................................................................... viii ÇİZELGELER DİZİNİ.............................................................................................. ix 1. GİRİŞ....................................................................................................................... 1 2. KAYNAK ÖZETLERİ.......................................................................................... 3 2.1 δ Scuti Yıldızlarının Genel Özellikleri............................................................... 3 2.1.1 δ Scuti türü yıldızların kimyasal element bolluk çalışmaları........................ 7 2.1.2 δ Scuti yıldızlarının HR diyagramındaki yerleri............................................ 10 2.1.3 Alt gruplar.......................................................................................................... 12 2.2 Alt Karasızlık Kuşağı’ndaki Kimyasal Türler................................................... 12 2.2.1 Normal yıldızlar................................................................................................. 13 2.2.2 Kimyasal tuhaf yıldızlar: CP/Ap...................................................................... 14 2.2.3 Am yıldızları....................................................................................................... 15 2.2.4 ρ Pup yıldızları................................................................................................... 16 2.2.5 λ Boo yıldızları................................................................................................... 17 2.3 DAO Verileriyle Bolluk Analizleri Gerçekleştirilen Yıldızlar......................... 18 2.4 20 CVn Yıldızı..................................................................................................... 20 2.4.1 Fotometrik Gözlemler....................................................................................... 20 2.4.2 Atmosfer Parametreleri..................................................................................... 23 2.4.3 Element Bolluk Analizleri................................................................................. 24 2.4.4 Radyal Hız Değişimi.......................................................................................... 25 3. MATERYAL VE YÖNTEM................................................................................. 27 3.1 20 CVn Yıldızının Tayfsal Gözlemleri................................................................ 27 3.2 Tayfların Ölçümü................................................................................................. 28 3.3 Radyal Hız Ölçümü.............................................................................................
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