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2 edition of Study of the pulsation properties of small-amplitude yellow supergiants. found in the catalog.

Study of the pulsation properties of small-amplitude yellow supergiants.

Armando Arellano Ferro

Study of the pulsation properties of small-amplitude yellow supergiants.

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Published .
Written in English


The Physical Object
Pagination210 leaves.
Number of Pages210
ID Numbers
Open LibraryOL14724548M


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Study of the pulsation properties of small-amplitude yellow supergiants. by Armando Arellano Ferro Download PDF EPUB FB2

Here, we analyze the amplitude variability in 29 pulsating yellow supergiants (5 RVa, 4 RVb, 9 SRd, 7 long-period Cepheid, and 4 yellow hypergiant stars), using visual observations from the AAVSO The large-amplitude pulsation of a model yellow supergiant star is investigated by using a hydrodynamic code.

The parameters of the model were M=1M_⦿, L=L⦿ and T_ =://   Amplitude Variations in Pulsating Yellow Supergiants John R. Percy and Rufina Y.H. Kim Department of Astronomy and Astrophysics University of Toronto Toronto ON Canada M5S 3H4 Abstract It was recently discovered that the amplitudes of pulsating red giants and super-giants vary significantly on time scales of pulsation ://   Arellano-Ferro, Armando, / Study of the pulsation properties of small-amplitude yellow supergiants, Armstrong, W.

S./ A laboratory method of testing a tube sensitometer, Bakos, Gustav A., / Spectroscopic and photometric investigation of EE Pegasi, The period variation of the double mode high amplitude δ Scuti variable VZ Cnc Study of the Pulsation Properties of Small-Amplitude Yellow Supergiants A study of 14 galactic small A study of 14 galactic small-amplitude yellow supergiant variables has been carried out in order to determine their pulsational properties.

They can be divided into two groups: periodic short /_Period_and_amplitude_variations_of_Polaris. Study of the IR-excess supergiant HD The star HD is one of a small group of supergiants becoming known as 89 Herculis stars or UU Herculis stars. Questions arise regarding the /_Study_of_the_IR-excess_supergiant_HD_   changes in amplitude resulted in small changes in period, due to non-linear effects in the pulsation.

Indeed, they did—but only in carbon (C-type) red giants. That led us, in the present study, to investigate whether there were any other differences in the pulsation properties of C red giants and normal oxygen (M) red ://    Pulsation amplitude variations in RY Sgr Most of the famous Cepheid pulsating variables have constant pulsation amplitudes, but this is not true of other types, especially low-gravity stars: pulsating red giants (Percy and Abachi ), pulsating red supergiants (Percy and Khatu ) and some pulsating yellow supergiants (Percy and Kim ).

Red supergiants are stars with a supergiant luminosity class (Yerkes class I) of spectral type K or M.[1] They are the largest stars in the universe in terms of volume, although they are not the most massive or luminous.

Betelgeuse and Antares are the brightest and best known red supergiants (RSGs), indeed the only first magnitude red supergiant ://   Classical Cepheids (also known as Population I Cepheids, Type I Cepheids, or Delta Cepheid variables) are a type of Cepheid variable are population I variable stars that exhibit regular radial pulsations with periods of a few days to a few weeks and visual amplitudes from a few tenths of a magnitude to about 2 magnitudes.

There exists a well-defined relationship between a   TwoDecades of Hypergiant Research Alex Lobel Harvard-Smithsonian CenterforAstrophysics, 60Garden Street, Cambridge MA,USA Abstract. This article is a brief review of the research by Dr. de Jager and co-workers over the past twenty years into the physics of hy-pergiant atmospheres.

Various important results on the microturbulence,   The pulsation amplitude varies between and in visual light, non-periodically but on a time scale of about 20 pulsation periods.

Introduction R Coronae Borealis (RCB) stars are rare carbon-rich, hydrogen-poor, highly-evolved yellow supergiants which undergo fadings of up to 10 magnitudes, then slowly return   The method, although calibrated using yellow supergiants, was established with the aim of studying Cepheid variables, and was used recently by Kovtyukh et al.

to examine the pulsation modes of three s-Cepheids, with fairly robust results: V Cyg (first overtone), V Per (fundamental mode), and V Cas (fundamental mode). It is ideal for   As the pulsation amplitude grows gradually, the surface velocity eventually reaches the sound speed. Since our code cannot describe shock waves, we investigate the pulsation properties only with the subsonic results.

Figure 1 shows the pulsation period P and the growth rate η of the fundamental mode at different reference points on the H-R   John Percy -- Astronomy Education, Outreach, Communication, and Research.

Brief Bio of John Percy: at For a list of some of my recent publications, please see the end of this page. Here are some documents and links that you ~percy/ The method, although calibrated using yellow supergiants, was established with the aim of studying Cepheid variables, and was used recently by Kovtyukh et al.

(b) to examine the pulsation modes of three s-Cepheids, with fairly robust results: V Cyg (first overtone), V Per (fundamental mode), and V Cas (fundamental mode)   brightness variations.

The variability amplitude, the light-curve shape, and the magnitude of V Cyg at maximum light changed noticeably from cycle to cycle. We observed both small-amplitude variations with ΔV =0m.2 in, and and varia-tions with depths up to 0m.6as well as deep photomet-ric minima with an amplitude up to 1m A SOFIA FORCAST Grism Study of the Mineralogy of Dust in the Winds of Proto-planetary Nebulae: RV Tauri Stars and SRd Variables Full Record Other Related Research   tion maximum, called max1, of which the amplitude is sometimes slightly higher than for normal pulsation max-ima.

The duration of the entire eruption episode is about twice the duration of an ordinary pulsation. Because of such markers we identified one new eruption in Fig.2 (B panel):in(themaximumnamedno.8).Thiseruption   Classical Cepheids After Years of Study that their fundamental properties are well enough understood.

Introduction They are currently yellow supergiants in a variety of short-lived evolutionary stages between that of B dwarfs and their later existence as red supergiants The RV Tauri-type variable R Scuti was discovered in by the English observer E.

Piggot, when only a handful of variables were known to exist. This finding followed in a parade of well-known variables, including: omicron Cet (Mira), beta Per (Algol), chi Cyg, R Hya, R Leo, beta Lyr, delta Cep, eta Aql, alpha Her, and R CrB (with the   MNRAS ,1{14() Preprint 10 December Compiled using MNRAS LATEX style le v A new outburst of the yellow hypergiant star ˆCas M.

Kraus 1?, I. Kolka 2, A. Aret;, D. Nickeler1, G. Maravelias3 4, T. Eenm ae 2, A. Lobel5, V. Klochkova6 1 Astronomick y us tav, Akademie v ed Cesk e republiky, Fri covaOnd rejov, Czech Republic 2Tartu Observatory,   Two Decades of Hypergiant Research A. Lobel Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA, USA Abstract.

This article is a brief review of the research by Dr. de Jager and co-workers over the past twenty years into the physics of hy-pergiant atmospheres. Various important results on the microturbulence,   Most large-amplitude pulsators like Cepheids: due to hydrogen and helium ionization zones, which thermodynamically drive the pulsation – like a car engine.

Sun and orange and red giants: stochastic excitation of the pulsation by the random convective motions in the outer layers of the ~percy/variablestarspdf. On the basis of radial velocities obtained at the Lick Observatory by Paddock in the yearsan attempt is made to discover the nature of the semiregular variability alpha.

Cygni (A2 Ia). Harmonic analysis of the velocities obtained in suggests that this variability   The typical amplitude of variation in the V band is about 1 mag, while in the near-infrared the amplitude is smaller, about mag in the K band, and even smaller in the mid-infrared band (Levesque et al.

; Yang et al. According to the characteristics of light variation, the RSG variability is divided into two categories: one is   Observations of Pulsating Stars Noel Richardson Ap 1 Introduction Pulsating stars are stars that show some sort of instability, often which can be called vibration or oscillation just as easily as pulsation.

Just like in musical instruments such as violins, stars can vibrate with multiple frequencies at once. Pulsations ~wiita/ Properties of the SX Phoenecis Stars in the Metal-Poor Globular Cluster NGCand Pulsation Modes of Three of the Newly-Discovered SX Phe Stars in 47 TUC Nemec, J.

?book_id=   The goalofthe present study is to consider the pulsation properties ofmassive stars during the later evolutionary stage of gravitational contraction of the helium core and to determine the role of radial stellar pulsations in variability of yellow ://   Beta Canis Majoris (β Canis Majoris, abbreviated Beta CMa, β CMa), also named Mirzam / ˈ m ɜːr z əm /, is a star in the southern constellation of Canis Major, the "Great Dog", located at a distance of about light-years ( parsecs) from the Sun.

In the modern constellation it lies at the position of the dog's front :// Binary stars. There are many single or isolated stars like the Sun, but about half of all stars in the sky are found in multiple systems.

Of the 25 nearest star systems within 4 pc (13 ly) of the Sun, 8 actually are multiple systems (7 binaries and 1 triple system). information about stellar properties, which can then be extrapolated to other types of stars. Information about mass, radius, internal and external structure, composition, temperature and luminosity can be gained by the study of variable stars.

At last another thing to say is that the archives of the AAVSO currently over million   Red supergiants are cool and large. They have spectral types of K and M, hence temperatures below 4, K. They are typically several hundred to over a thousand times the radius of the Sun, although size is not the primary factor in a star being designated as a supergiant.

A bright cool giant star can easily be larger than a hotter ://   uniform and systematic study of the stellar spectra. The stellar atmosphere models calculated by us include many elements and ionic species neglected in previous analyses, which allowed us to improve the fits to the observed spectra considerably and provided an additional diagnostic line: the Nevii λ ˚A, which had not been modelled in [WCE]   The focus of this book is, however, not the study of these well-known pulsators but stars with solar-like pulsations—the small-amplitude oscillations that are continually excited (in a stochastic manner) and damped by turbulence in   Pulsation model calculations by Heger et al.

() have shown that very large pulsation periods, amplitudes and mass-loss rates may be expected to occur at and beyond central helium exhaustion over the time-scale of the last few 10 4 yr. The physical reason for this is the resonant character of pulsations when the pulsation period and the   curve, pulsation theory (without mathematical proof), distance modulation, and needs for research.

Direct quotations are provided to express the idea. more effectively, and special references are used for completeness. * Student trainee from University of South Florida, Tampa, Florida.

NASA - GEORGE C. MARSHALL SPACE FLIGHT CENTER   Below is an ordered list of the largest stars currently known by radius expressed in units compared to the radius of the Sun (, km;mi). The exact order of this list remains very incomplete, as there currently remains great uncertainties especially when deriving various important parameters used in calculations, such as stellar Caveats  Extragalactic large stars  List  References:JoeyPknowsalotaboutthat/sandbox.

The MACHO Project Large Magellanic Cloud Variable Star Inventory. VIII. The Recent Star Formation History of the LMC from the Cepheid Period Distribution arXiv:astro-ph/v1 16 Nov C. Alcock Lawrence Livermore National Laboratory  › 百度文库 › 专业资料.

'yellow-red' and the 'blue' dynamic instability regions. No model calculations are so far available above and below the upper and lower dashed horizontal lines, respectively. that this extent is not large enough, because Ar/R is still considerable at TR = The question that is relevant to the present study is that of the delineation  Formamidinium lead bromide and iodide (FAPbX3, X = Br, I) in the form of colloidal nanocrystals (NCs) exhibit outstanding photoluminescence properties in the green and infrared regions of the electromagnetic spectrum, characterized by narrow emission line widths (below 90 meV) and high quantum yields (above 90%).

The controlled formation of Br-I mixed halide NCs is a facile strategy for Properties of galactic B[e] supergiants III. MWC We present the results of optical and near-IR spectroscopic and mid-IR imaging observations of the emission-line star MWC Its properties and evolutionary state are still under debate (a B[e] supergiant or a Herbig Be star).

Properties of galactic B[e] supergiants ://?id=