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Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos November July EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN Chair H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN COPYRIGHT NOTICE IBVS is published on b ehalf of the th and nd Commissions of the IAU by the Konkoly Observatory Budap est Hungary Individual issues could b e downloaded for scientic and educational purp oses free of charge Bibliographic information of the recent issues could b e entered to indexing sys tems No IBVS issues may b e stored in a public retrieval system in any form or by any means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS C STERKEN A JONES B VOS I ZEGELAAR AM van GENDEREN M de GROOT On the Cyclicity of the S Dor Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: : J BOROVICKA L SAROUNOVA The Period and Lightcurve of NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::: W LILLER AF JONES A New Very Long Period Variable Star in Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::: EA KARITSKAYA VP GORANSKIJ Unusual Fading of V Cygni Cyg X in Early November ::::::::::::::::::::::::::::::::::::::: -
List of Easy Double Stars for Winter and Spring = Easy = Not Too Difficult = Difficult but Possible
List of Easy Double Stars for Winter and Spring = easy = not too difficult = difficult but possible 1. Sigma Cassiopeiae (STF 3049). 23 hr 59.0 min +55 deg 45 min This system is tight but very beautiful. Use a high magnification (150x or more). Primary: 5.2, yellow or white Seconary: 7.2 (3.0″), blue 2. Eta Cassiopeiae (Achird, STF 60). 00 hr 49.1 min +57 deg 49 min This is a multiple system with many stars, but I will restrict myself to the brightest one here. Primary: 3.5, yellow. Secondary: 7.4 (13.2″), purple or brown 3. 65 Piscium (STF 61). 00 hr 49.9 min +27 deg 43 min Primary: 6.3, yellow Secondary: 6.3 (4.1″), yellow 4. Psi-1 Piscium (STF 88). 01 hr 05.7 min +21 deg 28 min This double forms a T-shaped asterism with Psi-2, Psi-3 and Chi Piscium. Psi-1 is the uppermost of the four. Primary: 5.3, yellow or white Secondary: 5.5 (29.7), yellow or white 5. Zeta Piscium (STF 100). 01 hr 13.7 min +07 deg 35 min Primary: 5.2, white or yellow Secondary: 6.3, white or lilac (or blue) 6. Gamma Arietis (Mesarthim, STF 180). 01 hr 53.5 min +19 deg 18 min “The Ram’s Eyes” Primary: 4.5, white Secondary: 4.6 (7.5″), white 7. Lambda Arietis (H 5 12). 01 hr 57.9 min +23 deg 36 min Primary: 4.8, white or yellow Secondary: 6.7 (37.1″), silver-white or blue 8. -
Morphology and Kinematics of the Gas Envelope of the Mira Binary W Aquilae 3
Research in Astron. Astrophys. Vol.0 (200x) No.0, 000–000 Research in http://www.raa-journal.org http://www.iop.org/journals/raa Astronomy and Astrophysics Morphology and kinematics of the gas envelope of the Mira binary W Aquilae ⋆ D. T. Hoai, P. T. Nhung, P. N. Diep, N. T. Phuong, P. Tuan-Anh, N. T. Thao and P. Darriulat Department of Astrophysics, Vietnam National Satellite Center, VAST, 18 Hoang Quoc Viet, Cau Giay, Hanoi, Vietnam; [email protected] Abstract We analyse ALMA observations of the 12CO(3-2) emission of the circumstellar envelope (CSE) of the Mira variable binary star W Aql. These provide, for the first time, spatially resolved Doppler velocity spectra of the CSE up to angular distances to the central star of ∼ 5′′ (meaning some 2000 AU). The exploratory nature of the observations (only five minutes in each of two different configurations) does not allow for a detailed modelling of the properties of the CSE but provides important qualitative information on its morphology and kinematics. Emission is found to be enhanced along an axis moving from east/west to north-east/south-west when the angular distance from the central star projected on the plane of the sky increases from zero to four arcseconds. In parallel, the Doppler velocity distribution displays asymmetry along an axis moving from east/west to north-west/south-east. The results are discussed in the context of earlier observations, in particular of the dust morphology. Key words: stars: AGB and post-AGB − (Star:) circumstellar matter − Star: individual (W Aql) − Stars: mass-loss − radio lines: stars. -
Agrarian Metaphors 397
396 Agrarian Metaphors 397 The Bible provided homilists with a rich store of "agricultural" metaphors and symbols) The loci classici are passages like Isaiah's "Song of the Vineyard" (Is. 5:1-7), Ezekiel's allegories of the Tree (Ez. 15,17,19:10-14,31) and christ's parables of the Sower (Matt. 13: 3-23, Mark 4:3-20, Luke 8:5-15) ,2 the Good Seed (Matt. 13:24-30, Mark 4:26-29) , the Barren Fig-tree (Luke 13:6-9) , the Labourers in the Vineyard (Matt. 21:33-44, Mark 12:1-11, Luke 20:9-18), and the Mustard Seed (Matt. 13:31-32, Mark 4:30-32, Luke 13:18-19). Commonplace in Scripture, however, are comparisons of God to a gardener or farmer,5 6 of man to a plant or tree, of his soul to a garden, 7and of his works to "fruits of the spirit". 8 Man is called the "husbandry" of God (1 Cor. 3:6-9), and the final doom which awaits him is depicted as a harvest in which the wheat of the blessed will be gathered into God's storehouse and the chaff of the damned cast into eternal fire. Medieval scriptural commentaries and spiritual handbooks helped to standardize the interpretation of such figures and to impress them on the memories of preachers (and their congregations). The allegorical exposition of the res rustica presented in Rabanus Maurus' De Universo (XIX, cap.l, "De cultura agrorum") is a distillation of typical readings: Spiritaliter ... in Scripturis sacris agricultura corda credentium intelliguntur, in quibus fructus virtutuxn germinant: unde Apostolus ad credentes ait [1 Cor. -
Molecular Line Study of the S-Type AGB Star W Aquilae ALMA Observations of CS, Sis, Sio and HCN
Astronomy & Astrophysics manuscript no. WAql-v6-revision_02_final c ESO 2018 October 5, 2018 Molecular line study of the S-type AGB star W Aquilae ALMA observations of CS, SiS, SiO and HCN M. Brunner1, T. Danilovich2; 3, S. Ramstedt4, I. Marti-Vidal2, E. De Beck2, W.H.T. Vlemmings2, M. Lindqvist2, and F. Kerschbaum1 1 Department for Astrophysics, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna e-mail: [email protected] 2 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden 3 Department of Physics and Astronomy, Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium 4 Department of Physics and Astronomy, Uppsala University, 75120 Uppsala, Sweden Received Month nr, YYYY; accepted Month nr, YYYY ABSTRACT Context. With the outstanding spatial resolution and sensitivity of the Atacama Large Millimeter/sub-millimeter Array (ALMA), molecular gas other than the abundant CO can be observed and resolved in circumstellar envelopes (CSEs) around evolved stars, such as the binary S-type Asymptotic Giant Branch (AGB) star W Aquilae. Aims. We aim to constrain the chemical composition of the CSE and determine the radial abundance distribution, the photospheric peak abundance, and isotopic ratios of a selection of chemically important molecular species in the innermost CSE of W Aql. The derived parameters are put into the context of the chemical evolution of AGB stars and are compared with theoretical models. Methods. We employ one-dimensional radiative transfer modeling – with the accelerated lambda iteration (ALI) radiative transfer code – of the radial abundance distribution of a total of five molecular species (CS, SiS, 30SiS, 29SiO and H13CN) and determine the best fitting model parameters based on high-resolution ALMA observations as well as archival single-dish observations. -
The XMM-Newton View of the Yellow Hypergiant IRC+10420 And
The XMM-Newton view of the yellow hypergiant IRC +10420 and its surroundings$ M. De Becker, D. Hutsem´ekers1, E. Gosset1 Department of Astrophysics, Geophysics and Oceanography, University of Li`ege, 17, All´ee du 6 Aoˆut, B5c, B-4000 Sart Tilman, Belgium Abstract Among evolved massive stars likely in transition to the Wolf-Rayet phase, IRC +10420 is probably one of the most enigmatic. It belongs to the category of yellow hypergiants and it is characterized by quite high mass loss episodes. Even though IRC +10420 benefited of many observations in several wavelength domains, it has never been a target for an X-ray observatory. We report here on the very first dedicated observation of IRC +10420 in X-rays, using the XMM-Newton satellite. Even though the target is not detected, we derive X-ray flux upper limits of the order of 1–3 × 10−14 ergcm−2 s−1 (between 0.3 and 10.0keV), and we discuss the case of IRC +10420 in the framework of emission models likely to be adequate for such an object. Using the Optical/UV Monitor on board XMM-Newton, we present the very first upper limits of the flux density of IRC +10420 in the UV domain (between 1800 and 2250Å and between 2050 and 2450Å). Finally, we also report on the detection in this field of 10 X-ray and 7 UV point sources, and we briefly discuss their properties and potential counterparts at longer wavelengths. Key words: stars: early-type, stars: individual: IRC +10420, X-rays: stars PACS: 97.10.Me, 97.30.Sw, 95.85.Nv 1. -
The Evening Sky Map
I N E D R I A C A S T N E O D I T A C L E O R N I G D S T S H A E P H M O O R C I . Z N O p l f e i n h d o P t O o N ) l h a r g Z i u s , o I l C t P h R I r e o R N ( O o r C r H e t L p h p E E i s t D H a ( r g T F i . O B NORTH D R e N M h t E A X O e s A H U M C T . I P N S L E E P Z “ E A N H O NORTHERN HEMISPHERE M T R T Y N H E ” K E η ) W S . T T E W U B R N W D E T T W T H h A The Evening Sky Map e MAY 2021 E . C ) Cluster O N FREE* EACH MONTH FOR YOU TO EXPLORE, LEARN & ENJOY THE NIGHT SKY r S L a o K e Double r Y E t B h R M t e PERSEUS A a A r CASSIOPEIA n e S SKY MAP SHOWS HOW Get Sky Calendar on Twitter P δ r T C G C A CEPHEUS r E o R e J s O h Sky Calendar – May 2021 http://twitter.com/skymaps M39 s B THE NIGHT SKY LOOKS T U ( O i N s r L D o a j A NE I I a μ p T EARLY MAY PM T 10 r 61 M S o S 3 Last Quarter Moon at 19:51 UT. -
Lunar Mansion Names in South-West China
Onoma 51 Journal of the International Council of Onomastic Sciences ISSN: 0078-463X; e-ISSN: 1783-1644 Journal homepage: https://onomajournal.org/ Lunar mansion names in South-West China: An etymological reconstruction of ancestral astronomical designations in Moso, Pumi, and Yi cultures compared with Chinese and Tibetan contexts DOI: 10.34158/ONOMA.51/2016/6 Xu Duoduo National University of Singapore (NUS), Asia Research Institute (ARI), Singapore [email protected] To cite this article: Xu Duoduo. 2016. Lunar mansion names in South-West China: An etymological reconstruction of ancestral astronomical designations in Moso, Pumi, and Yi cultures compared with Chinese and Tibetan contexts. Onoma 51, 113–143. DOI: 10.34158/ONOMA.51/2016/6 To link to this article: https://doi.org/10.34158/ONOMA.51/2016/6 © Onoma and the author. Lunar mansion names in South-West China: An etymological reconstruction of ancestral astronomical designations in Moso, Pumi, and Yi cultures compared with Chinese and Tibetan contexts Abstract: The present study aims at an etymological reconstruction of lunar mansion designations of the Moso, Pumi, and Yi people from South-West China. Those lunar mansions are generally named after animals. A systematic examination on these astronomical names reveals frequent borrowing processes among these cultures, extended to Tibetan and Chinese contexts. Three patterns of direct borrowing of the lunar mansion names can be highlighted in addition to compatible morphological structures in some designation. This comparative research also provides innovative 114 XU DUODUO solutions to several issues still unsolved from the current studies on lunar mansions focused on specific ethnic groups. -
Ephemerides Astronomicae. Anni...Ad Meridianum Mediolanensem
Informazioni su questo libro Si tratta della copia digitale di un libro che per generazioni è stato conservata negli scaffali di una biblioteca prima di essere digitalizzato da Google nell’ambito del progetto volto a rendere disponibili online i libri di tutto il mondo. Ha sopravvissuto abbastanza per non essere più protetto dai diritti di copyright e diventare di pubblico dominio. Un libro di pubblico dominio è un libro che non è mai stato protetto dal copyright o i cui termini legali di copyright sono scaduti. La classificazione di un libro come di pubblico dominio può variare da paese a paese. I libri di pubblico dominio sono l’anello di congiunzione con il passato, rappresentano un patrimonio storico, culturale e di conoscenza spesso difficile da scoprire. Commenti, note e altre annotazioni a margine presenti nel volume originale compariranno in questo file, come testimonianza del lungo viaggio percorso dal libro, dall’editore originale alla biblioteca, per giungere fino a te. Linee guide per l’utilizzo Google è orgoglioso di essere il partner delle biblioteche per digitalizzare i materiali di pubblico dominio e renderli universalmente disponibili. I libri di pubblico dominio appartengono al pubblico e noi ne siamo solamente i custodi. Tuttavia questo lavoro è oneroso, pertanto, per poter continuare ad offrire questo servizio abbiamo preso alcune iniziative per impedire l’utilizzo illecito da parte di soggetti commerciali, compresa l’imposizione di restrizioni sull’invio di query automatizzate. Inoltre ti chiediamo di: + Non fare un uso commerciale di questi file Abbiamo concepito Google Ricerca Libri per l’uso da parte dei singoli utenti privati e ti chiediamo di utilizzare questi file per uso personale e non a fini commerciali. -
From Supergiant to Solar-Mass Star: Study Finds HD 179821 Less Massive Than Previously Thought 8 February 2019, by Tomasz Nowakowski
From supergiant to solar-mass star: Study finds HD 179821 less massive than previously thought 8 February 2019, by Tomasz Nowakowski observations of HD 179821 have been conducted, the exact distance to this star remains a subject of debate. Some studies suggest that it is located about 19,500 light years from the Earth, while others cite a much closer distance of some 12,700 light years. Discrepancy in the distance estimates leaves uncertainties regarding the star's mass and evolutionary status. Gaia's second data release, known as Data Release 2 (DR2), has the potential to resolve such uncertainties as it offers high-precision positions, parallaxes and proper motions for more than 1.3 billion sources in the sky. A team of astronomers led by Mudumba Parthasarathy of the Indian Institute of Astrophysics in Bangalore used DR2 data to obtain the parallax of HD 179821, which allowed them to make new distance calculations. The parallax of HD 179821 was found to be approximately 0.31 mas. Employing an inference HD 179821. Credit: Hubble Legacy Archive procedure developed by other researchers in 2018, Parthasarathy's team calculated that this value corresponds to a distance of about 9,600 light years. Gaia parallax also allowed them to find that A post-asymptotic giant branch (post-AGB) star the star is located some 850 light years below the known as HD 179821 turns out to be significantly Galactic plane. less massive than previously thought, according to a new study. Using new data from ESA's Gaia Furthermore, the derived distance and other satellite, astronomers found that HD 179821 is not parameters provided by previous studies, such as a supergiant, which was suggested by previous spectral type and observed V magnitude, were observations, but is rather a solar-mass star. -
Reduced Maximum Mass-Loss Rate of OH/IR Stars Due to Overlooked Binary Interaction
The University of Manchester Research Reduced maximum mass-loss rate of OH/IR stars due to overlooked binary interaction DOI: 10.1038/s41550-019-0703-5 Document Version Accepted author manuscript Link to publication record in Manchester Research Explorer Citation for published version (APA): Decin, L., Homan, W., Danilovich, T., de Koter, A., Engels, D., Waters, L. B. F. M., Muller, S., Gielen, C., Garca- Hernandez, D. A., Stancliffe, R., Van de Sande, M., Molenberghs, G., Kerschbaum, F., Zijlstra, A., & El Mellah, I. (2019). Reduced maximum mass-loss rate of OH/IR stars due to overlooked binary interaction. Nature Astronomy, 3(5), 408-415. https://doi.org/10.1038/s41550-019-0703-5 Published in: Nature Astronomy Citing this paper Please note that where the full-text provided on Manchester Research Explorer is the Author Accepted Manuscript or Proof version this may differ from the final Published version. If citing, it is advised that you check and use the publisher's definitive version. General rights Copyright and moral rights for the publications made accessible in the Research Explorer are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. Takedown policy If you believe that this document breaches copyright please refer to the University of Manchester’s Takedown Procedures [http://man.ac.uk/04Y6Bo] or contact [email protected] providing relevant details, so we can investigate your claim. Download date:08. Oct. 2021 Reduced maximum mass-loss rate of OH/IR stars due to overlooked binary interaction L. -
Molecular Line Study of the S-Type AGB Star W Aquilae: ALMA Observations of CS, Sis, Sio and HCN
Molecular line study of the S-type AGB star W Aquilae: ALMA observations of CS, SiS, SiO and HCN Downloaded from: https://research.chalmers.se, 2021-10-05 12:42 UTC Citation for the original published paper (version of record): Brunner, M., Danilovich, T., Ramstedt, S. et al (2018) Molecular line study of the S-type AGB star W Aquilae: ALMA observations of CS, SiS, SiO and HCN Astronomy and Astrophysics, 617 http://dx.doi.org/10.1051/0004-6361/201832724 N.B. When citing this work, cite the original published paper. research.chalmers.se offers the possibility of retrieving research publications produced at Chalmers University of Technology. It covers all kind of research output: articles, dissertations, conference papers, reports etc. since 2004. research.chalmers.se is administrated and maintained by Chalmers Library (article starts on next page) Astronomy & Astrophysics manuscript no. WAql-v6-revision_02_final c ESO 2018 October 5, 2018 Molecular line study of the S-type AGB star W Aquilae ALMA observations of CS, SiS, SiO and HCN M. Brunner1, T. Danilovich2; 3, S. Ramstedt4, I. Marti-Vidal2, E. De Beck2, W.H.T. Vlemmings2, M. Lindqvist2, and F. Kerschbaum1 1 Department for Astrophysics, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna e-mail: [email protected] 2 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden 3 Department of Physics and Astronomy, Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium 4 Department of Physics and Astronomy, Uppsala University, 75120 Uppsala, Sweden Received Month nr, YYYY; accepted Month nr, YYYY ABSTRACT Context.