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Wednesday, July 8, 2020 | History

2 edition of observation study of the RV Tauri stars found in the catalog.

observation study of the RV Tauri stars

David Lorraine DePuy

observation study of the RV Tauri stars

by David Lorraine DePuy

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Published in [Toronto] .
Written in English

    Subjects:
  • Tauri stars

  • Edition Notes

    ContributionsToronto, Ont. University.
    The Physical Object
    Pagination188 leaves.
    Number of Pages188
    ID Numbers
    Open LibraryOL19123920M

    Because they still hide some secrets about a dramatic stage most stars go through at some point in their evolution Come and join us for a conversation on A Project for the Observation of RV Tauri Variable Stars. Our speaker this time is a LaGuardia student -- Amaru Alzogaray, who will speak about his research proposal on studying Variable Stars. Numerical Investigation of the Stability of Motion of a Mass Element Ejected from a Component of a Binary Star System.- Resonance in RV Tauri Stars.- The Determination of Intrinsic Polarization for RV Tauri Stars.- Multi-Color Interferometric Observations of Mira Stars.- Origin and Propagation of Shocks in the Atmospheres of Mira-Type Stars

    A Study of the Spectroscopic Variability of Select RV Tauri and Semiregular Stars. ABSTRACT ACKNOWLEDGEMENTS. Support for this work was provided by the NSF PAARE program to South Carolina State University under award AST We thank the director of KPNO for his generous allocation of telescope time to this project over the years. RV Tauri Stars. RV Tauri type stars are yellow supergiant stars (spectral type G or K). They have periods from 30 to days. They show brightness variations of up to 3 magnitudes. Their ‘light curve’ shows alternating deep and shallow minima. Sometimes they show superimposed very long period variations from to days ( to 25 years).

    Other articles where RV Tauri star is discussed: star: Pulsating stars: semiregular variables such as the RV Tauri stars show complex light and spectral changes. They do not repeat themselves from one cycle to the next; their behaviour suggests a simultaneous operation of two or more modes of oscillation. Betelgeuse is an example of an irregular red variable. Wolf-Rayet stars as a diagnostic of internal mixing processes in massive mass losing stars.- A systematic study of stellar models for c/o-rich Wolf-Rayet stars.- Overabundance of sodium in the atmospheres of massive supergiants as a possible manifestation of NeNa cycle.- Photometric and polarimetric observations of the RV Tauri star ar.


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Observation study of the RV Tauri stars by David Lorraine DePuy Download PDF EPUB FB2

Abstract. Several problems of the theory of the RV Tauri stars are reviewed on the basis of the numerical nonlinear modelling. We analyse the nature of the alternating pulsations of these variables, and discuss their relation to the period doubling phenomenon in W Virginis by: 5.

Multiwavelength observations of RV Tauri stars. I - AC Herculis Article (PDF Available) in Astronomy and Astrophysics July with 16 Reads. The brighter RV Tauri stars have recently been studied on the Harvard collection of stellar photographs.

Of the twenty-nine stars now assigned to the class, fourteen proved to be bright enough for intensive study. Simultaneous spectroscopic and polarimetric observations are presented for the RV Tauri stars AC Her U Mon, V Vul, SS Gem, and TW Cam and for the RV Tauri-like.

A variety of aspects of R Coronae Borealis and RV Tauri variables are investigated. Simultaneous optical and infrared observations of both types of star allow stellar and dust shell parameters to be inferred. For R Coronae Borealis stars, light is thrown on mass loss mechanisms via statistical and model studies of deep : Michael John Goldsmith.

observed (O- C) diagrams of RV Tauri stars. In the present paper, we analyze the times of minimum of 15 RV Tauri stars, to see if this model fits the observations. OBSERVATIONS We have analyzed the times of minima of the 15 RV Tauri stars listed in Table 1.

They are the stars for which Zsoldos has accumulated times of minimum from the litera. ABSTRACT We present a detailed study based on infrared photometry of all Galactic RV Tauri stars from the General Catalogue of Variable Stars (GCVS).

RV Tauri stars are the brightest among the population II Cepheids. They are thought to evolve away from the asymptotic giant branch (AGB) towards the white dwarf observation study of the RV Tauri stars book.

Because they still hide some secrets about a dramatic stage most stars go through at some point in their evolution Come and join us for a conversation on A Project for the Observation of RV Tauri Variable Stars.

Our speaker this time is a LaGuardia student -- Amaru Alzogaray, who will speak about his research proposal on studying Variable Stars. RV Tauri stars are further classified into two photometric sub-types based on their light curves: RVa: these are RV Tauri variables which do not vary in mean brightness; RVb: these are RV Tauri variables which show periodic variations in their mean brightness, so that their maxima and minima change on to day timescales.

This book provides a concise overview of variable stars, including a historical with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and public interest in astronomy.

This book is (W Virginis stars) RV Tauri variables RR Lyrae stars Delta. We made the multicolor Polarimetric observations of 17 RV Tauri stars. We report the characteristics of intrinsic polarization of these stars.

The interstellar polarizations were determined by the modified near-neighbor method. stellar dust around many of the RV Tauri stars, which has been interpreted as being due to strong, dusty mass-loss during AGB evolution (Jura).

From CO observations,Alcolea & Bujarrabal() suggest a mass loss rate of 4 10 7 to 7 10 6 M yr 1 within the last to years for most of the RV Tauri stars. Because of their position on the H-R di.

modulation in maximum light van der Bilt observed. The "RV Tauri stars" were mentioned as a distinct subtype in Harlow Shapley's paper on Cepheids in clusters, and by the time Russell, Dugan, and Stewart's Astronomy was published inthe RV Tauri stars were listed as a distinct class of variable star.

RV Tauri stars — variables in transition. A Spectroscopic Study of the RV Tauri Stars TT Oph and UZ Oph - NASA/ADS TT and UZ Orphiuchus are listed as RV Tauri types in the General Catalog of Variable Stars, although Percy and Mohammed (, JAAVSO, 32, 9) question this classification.

We have acquired spectra of these objects with the Coude Feed Telescope at KPNO over the past decade. An unconventional class of stars, known as semiregular variables, or "RV Tauri stars," exhibits complex changes in brightness as well as dramatic spectral changes over timescales of years.

Students analyze spectra taken one to two times a year with the Kitt Peak Coudé Spectrograph to determine each star's current spectral class and surface. The observational history of the important variable star RV Tauri had humble beginnings in with a simple and concise discovery paper by Lydia Ceraski (or "Mme.

Ceraski" as she was often cited) announcing the discovery of three new variables from photographic plates taken by Blazhko (the other two being the Mira RY And and the Cepheid RW Cas).

Abstract The project of time series analysis for the photometric observations of a representative group of RV Tauri type stars is described. This class of variables consists of about supergiants in the Milky Way.

Their light curves show in general two unequal minima with several individual features which are not explained by now. to RV Tauri variables. obtained severalLaney () JHK observations each of 19 LMC type II Cepheid candidates, conÐrming that four had infrared excesses in the K band.

An excess in the near infrared is not a sure indicator of variable type, however. A few rare RV Tauri stars show no excess, and a number of W Vir stars show some degree of.

RV Tau gives an insight into the lives and deaths of stars like the Sun. Evolution models show it takes about 10 billion years for a 1 solar mass (1 M ☉) star to reach the Asymptotic Giant Branch.

The study of period changes in RV Tauri stars conducted by Erleksova () presented (O C) diagrams that were interpreted in terms of a series of abrupt period changes. Percy et al. () studied the periods of U Mon and R Sct and claimed to have found single abrupt decreases, which, when averaged over the interval of observation, were.

RV Tauri stars form an enigmatic subgroup of pulsating yellow supergiants. Their most characteristic photomet-ric feature is the alternation of shallow and deep min-ima. Their periods are usually between 50 and days, the visual amplitudes can be sometimes higher than 1m.

RV Tauri stars have F{K spectral types though occa.Here, we present a systematic study of the IR properties of RV Tauri stars and we use all Galactic RV Tauri stars listed in the GCVS (Samus et al. ) as our IR photometry is a good tracer of the temperature gradient of the circumstellar dust (if present), which we want to correlate with the properties of the central object.category of RV Tauri stars.

Although the entire RV Tau research project is working to combine photometric and spectroscopic analysis, our portion of the research for the summer of focused on testing various methods of period determination for the RV Tau visual lightcurves.