Astrophysical processes in upper main sequence stars

by A. N. Cox

Publisher: Geneva Observatory in Sauverny, Switzerland

Written in English
Published: Downloads: 114
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Edition Notes

StatementA.N. Cox, S. Vauclair, J.-P. Zahn.
SeriesThirteenth Advanced course of the Swiss Society of Astronomy and Astrophysics
ID Numbers
Open LibraryOL14863768M

Get this from a library! Les étoiles de composition chimique anormale du debut de la sequence principale = Upper main sequence chemically peculiar stars: communications présentées au vingt-troisième Colloque international d'astrophysique, tenu à Liège du 23 au 26 juin [Université de Liège. Institut d'astrophysique.;]. @article{osti_, title = {Physics of stellar evolution and cosmology}, author = {Goldberg, H.S. and Scadron, M.D.}, abstractNote = {Astrophysical phenomena are examined on a fundamental level, stressing basic physical laws, in a textbook suitable for a one-semester intermediate course. The ideal gas law, the meaning of temperature, black-body radiation, discrete spectra, and the Doppler. The phrase chemically peculiar star without further specification usually means a member of one of the hot main sequence types described above. Many of the cooler chemically peculiar stars are the result of the mixing of nuclear fusion products from the interior of the star to its surface; these include most of the carbon stars and S-type stars. Among main-sequence stars, the most massive stars are more luminous, redder, cooler, and have larger radii than less massive stars. False To measure the parallax of the most distant stars measurable, we would make two measurements of the star's position separated by.

An O-type main-sequence star (O V) is a main-sequence (core hydrogen-burning) star of spectral type O and luminosity class V. These stars have between 15 and 90 times the mass of the Sun and surface temperatures betw are betw and 1,, times as luminous as the Sun. Get this from a library! Les Étoiles de composition chimique anormale du debut de la sequence principale = Upper main sequence chemically peculiar stars: communications présentées au XXIIIe Colloque international d'astrophysique, tenu à Liège du 23 au 26 juin [Université de Liège. Institut d'astrophysique.;]. Mature stars. Eventually the core exhausts its supply of hydrogen and the star begins to evolve off of the main sequence. Without the outward pressure generated by the fusion of hydrogen to counteract the force of gravity the core contracts until either electron degeneracy becomes sufficient to oppose gravity or the core becomes hot enough (around MK) for helium fusion to begin. The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous is a period of stellar evolution undertaken by all low- to intermediate-mass stars (–10 solar masses) late in their lives.. Observationally, an asymptotic-giant-branch star will appear as a bright red giant with a luminosity ranging up to thousands of times.

The Upper Scorpius association is quite young and only stars earlier (hotter) than type A3 have reached the main sequence; less massive stars, such as 1RXS J−, are still in the process of contraction during the pre-main sequence phase. Originally, the association was estimated to be around 5 million years old, but a recent Constellation: Scorpius. A recent news article 1 reported that certain types of stars 2 in our Milky Way Galaxy have more lithium (Li) in their stellar atmosphere than the current models predict. Before , it was generally believed that Li abundances in “unevolved” low-mass stars 3 with low metallicity 4 were constant as predicted by Big Bang nucleosynthesis models. However, in that year a closer analysis of. Stars above this luminosity would be too unstable and simply do not form. Red supergiants have masses between about 10 M ☉ and 40 M ☉. Main-sequence stars more massive than about 40 M ☉ do not expand and cool to become red supergiants. Red supergiants at the upper end of the possible mass and luminosity range are the largest known.

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Book-Review - Astrophysical Processes in Upper Main Sequence Stars - Saas-Fee 13TH - MARCited by: 1.

Astrophysical processes in upper main sequence stars: thirteenth advanced course of the Swiss Society of Astronomy and Astrophysics. astrophysical processes in upper main sequence stars Download astrophysical processes in upper main sequence stars or read online books in PDF, EPUB, Tuebl, and Mobi Format.

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Pub Date: Bibcode: .C Keywords: MAINSEQUENCE STARS; The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Author: A. Cox, S. Vauclair, J. Zahn. There is a natural astrophysical division of the main sequence which occurs for early F stars.

Stars cooler than this have deep surface convection zones, radiative cores, generate their energy by the proton-proton cycle, rotate relatively slowly and any global magnetic field present is weak, although strong fields may exist in tangled flux tubes, as in sunspots in the Sun.

Stars hotter than early. Cambridge Core - Astrophysics - Astrophysics Processes - by Hale Bradt. Bridging the gap between physics and astronomy textbooks, this book provides step-by-step physical and mathematical development of fundamental astrophysical processes underlying a wide range of phenomena in stellar, galactic, and extragalactic by: 7.

Review chapter in book: 'The Tidal Disruption of Stars by Massive Black Holes', Space Science Reviews, Springer. Comments welcome: Subjects: High Energy Astrophysical Phenomena () Cite as: arXiv [] (or arXivv1 [] for.

Bridging the gap between physics and astronomy textbooks, this book provides physical explanations of twelve fundamental astrophysical processes underlying a wide range of phenomena in stellar, galactic, and extragalactic astronomy. The book has been written for upper-level undergraduates and graduate students, and its strong pedagogy ensuresFile Size: KB.

In: Cowley C.R., Dworetsky M.M., Mégessier C. (eds) Upper Main Sequence Stars with Anomalous Abundances. Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Reviews), vol Author: Graham Hill, Saul J.

Adelman. Structure and Evolution of Single Stars: An introduction is intended for upper-level undergraduates and beginning graduates with a background in physics. Following a brief overview of the background observational material, the basic equations describing the structure and evolution of single stars Author: James MacDonald.

The chemically peculiar (CP) stars of the upper main sequence are perfect tracers for several astrophysical processes.

Their study especially in open clusters further helps to establish their evolutionary by: 5. In this article we first review the main physical effects to be considered in the building of evolutionary models of rotating stars on the Upper Main-Sequence (MS).

The internal rotation law evolves as a result of contraction and expansion, meridional circulation, diffusion processes, and mass loss. In turn, differential rotation and mixing exert a feedback on circulation and diffusion, so Cited by: We review some of the mixing processes that may influence the evolution of massive stars, such as penetrative convection, and put our emphasis on those which occur in the radiative envelope.

There the main transport mechanisms are a thermally driven meridian circulation, which departs significantly from the classical Eddington-Sweet description Cited by: 8. In: Cowley C.R., Dworetsky M.M., Mégessier C.

(eds) Upper Main Sequence Stars with Anomalous Abundances. Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Reviews), vol Cited by: 2.

Herbig Ae Stars. In their premain sequence phase, intermediate mass stars appear to be moderate X-ray sources (e.g., and references therein). Their X-ray emission characteristics are overall similar to the lower mass TTS (hot, variable), possibly implying that the same X-ray emission processes are at work in the two classes of stars or that the Cited by: 7.

Optical region spectra for a number of upper main sequence chemically peculiar (CP) stars have been observed to study singly and doubly ionized praseodymium and neodymium lines.

In order to improve existing atomic data of these elements, laboratory measurements have been carried out with the Lund VUV Fourier Transform Spectrometer (FTS).

From these measurements wavelengths and. The main process responsible for the energy produced in most main sequence stars is the proton-proton (pp) chain.

It is the dominant process in our Sun and all stars of less than solar masses. The net effect of the process is that four hydrogen nuclei, protons, undergo a sequence of fusion reactions to produce a helium-4 nucleus.

In: Cowley C.R., Dworetsky M.M., Mégessier C. (eds) Upper Main Sequence Stars with Anomalous Abundances. Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Reviews), vol Author: R.E.

Gershberg. THE ASTROPHYSICAL JOURNAL,¨,December1 Rotationally induced mixing processes widen the main sequence and increase the core hydrogen-burning lifetime, similar to the eƒects of convective over- Massive main-sequence stars are rapid rotators.

Equato-rial rotation velocities span the range kmv rot. Stars on the horizontal branch are about a factor of 30 to more luminous than stars of about the same mass at the tip of the main sequence.

We will show that stars on the horizontal branch have He-fusion in their cores surrounded by a H-fusion shell. The cool end of the horizontal branch reaches the red giant branch. This query page only provides access to articles that have been scanned by the ADS.

If you want to access every article from a particular journal, please use the Journal/Volume/Page Query Page. All articles are copyrighted by the publisher of the article. O and B stars tend to be blueish in color, while A and F stars tend to be white in color, G are more yellow, while K and M are pink to red in color.

90% of stars fit on this Main Sequence of stars, however some odd-balls lay outside of this Main Sequence, including, the highly luminous Giant Stars (Supergiants, Bright Giants, Giants and.

The lifetimes of these stars in different phases of stellar evolution are significantly extended, namely, in the pre-main sequence, main sequence, and red giant phases.

In particular, more» intermediate-mass stars in the red giant phase experience significant. Capture on the Main Sequence During the main sequence (MS) phase of stellar evolution, stars derive their energy from thermonuclear burning of hydrogen to helium. Stars on the main sequence range in mass from about Q to MO, and are divided into two categories: upper (M 2 &) and lower (M s MO) main sequence.

Because. The chemically peculiar (CP) stars on the upper main sequence belong in the standard framework within which we understand stellar evolution and the history of matter. Recent work has made it clear that the unusual chemistry and magnetic structure of these objects is of relevance across the broad domain of stellar astronomy.

from the upper main Book Edition: Ed. This second volume of a comprehensive three-volume work on theoretical astrophysics deals with stellar physics. After reviewing the key observational results and nomenclature used in stellar astronomy, the book develops a solid understanding of central concepts including stellar structure and evolution, the physics of stellar remnants, pulsars, binary stars, the sun and planetary systems Cited by: Main Theoretical astrophysics vol.1 astrophysical processes T.

Padmanabhan. Graduate students and researchers in astrophysics and cosmology need a solid grasp of a wide range of physical processes. This authoritative textbook helps readers develop the necessary toolkit of theory.

The book is modular in design, allowing the reader to pick. Spectropolarimetry has been used for decades to detect magnetic fields in stars through-out the HR diagram (Donati & Landstreet ).

Our particular interest in this paper, however, is in instrumentation that enables the measurement of strong, large-scale magnetic fields in the chemically peculiar stars (Ap/Bp) of the upper main sequence.

Journal: Saas-Fee Advanced Cou Astrophysical Processes in Upper Main Sequence Stars, given at the Swiss Society for Astronomy and Astrophysics (SSAA), in Les Diablerets, Switzerland. Edited by B. Hauck and A. Maeder. Publisher: Geneva Observatory, CH Sauverny, Switzerland,p Bibliographic Code:.

Astronomers divide the main sequence into upper and lower parts, based on which of the two is the dominant fusion process. In the lower main sequence, energy is primarily generated as the result of the proton-proton chain, which directly fuses hydrogen together in a series of stages to produce helium.

Stars in the upper main sequence have.The chemically peculiar (CP) stars of the upper main sequence, between spectral types B2 and F5, are excellent samples for testing astrophysical processes such as diffusion, mass-loss, and global.The solar system thus serves as a “laboratory” for the investigation of processes common to all astrophysical plasmas.

At the center of this laboratory sits our Sun, a “cool” (6, K) main-sequence star with a hot (1, K) corona.