Last edited by Akill
Tuesday, October 13, 2020 | History

2 edition of Stellar chromospheres found in the catalog.

Stellar chromospheres

International Astronomical Union. Colloquium

Stellar chromospheres

proceedings.

by International Astronomical Union. Colloquium

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Published by Scientific and Technical Information Office, National Aeronautics and Space Administration; [for sale by the Supt. of Docs., U.S. Govt. Print. Off.] in Washington .
Written in English

    Subjects:
  • Stellar chromospheres -- Congresses.

  • Edition Notes

    Includes bibliographies.

    StatementEdited by S. D. Jordan and E. H. Avrett. Prepared by Goddard Space Flight Center.
    SeriesNASA SP, -317, NASA SP ;, 317.
    ContributionsJordan, Stuart D., ed., Avrett, Eugene H., 1933- ed., Goddard Space Flight Center.
    Classifications
    LC ClassificationsQB809 .I58 1972
    The Physical Object
    Paginationix, 318 p.
    Number of Pages318
    ID Numbers
    Open LibraryOL5389210M
    LC Control Number72600300

      Cool Stars, Stellar Systems, and the Sun by Jeffrey L. Linsky, , available at Book Depository with free delivery worldwide. Unfortunately, this book can't be printed from the OpenBook. If you need to print pages from this book, we recommend downloading it as a PDF. Visit to get more information about this book, to buy it in print, or to download it as a free PDF. Below is the uncorrected machine-read text.

    In preparation for the launch of NASA's AXAF X-ray Observatory in , Professor Walker's group will be utilizing both space observations and ground-based observations (from the Hobby Eberly Telescope) to study phenomena associated with stellar chromospheres and coronae, supernova remnents, the interstellar medium, and clusters of galaxies. of stellar structure, stellar rotation, pulsation, and evolution up to the supernova and compact object stages. The course will also include radiation transport in stellar photospheres, chromospheres, coronas, and winds. We will occasionally touch on topics in planetary astrophysics, especially in .

    Finally the structural components that are accessible, such as the convestion zone, chromosphere, corona, and mass outflow are described. The book will interest any student with a knowledge of physics and mathematics who needs to learn about stellar atmospheres. stellar outer atmosphere. 2. H–R diagram Figure 1 is a schematic view of the cool-half of the H–R diagram. This is the domain of surface convection, defining the so-called “late-type” stars. This is where chromospheres are found ubiquitously, and nearly exclusively. The .


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Stellar chromospheres by International Astronomical Union. Colloquium Download PDF EPUB FB2

The focus is on stellar “chromospheres,” an important byproduct of magnetic “activity,” because this is a key area in solar physics today and one in which the stars can be most informative.

The main topic is why chromospheres exist: the warm, extensive outer atmospheres of cool stars, a consequence of nonradiative heating mainly. The focus is on stellar “chromospheres,” an important byproduct of magnetic “activity,” because this is a key area in solar physics today and one in which the stars can be most informative.

The main topic is why chromospheres exist: the warm, extensive outer atmospheres of cool stars, a consequence of nonradiative heating mainly Author: Thomas R.

Ayres. STELLAR CHROMOSPHERES, NASA SP Paperback – January 1, by E. JORDAN, S. D.; AVRETT (Editor) See all formats and editions Hide other formats and editions. Price New from Used from Paperback, "Please retry" — Manufacturer: National Aeronautics and Space Administration.

Get this from a library. Stellar chromospheres: proceedings of the International Astronomical Union Colloquium held at NASA Goddard Space Flight Center, February[Stuart D Jordan; Eugene H Avrett; International Astronomical Union. Colloquium; Goddard Space Flight Center.].

Volume 1: The global properties of stars and the observational techniques used to determine them are examined Stellar chromospheres book an introduction for undergraduate students. Chapters are devoted to stellar positions, proper motions, brightness, color-magnitude diagrams, luminosities, angular radii, and effective temperatures.

Also considered are stellar masses and radii, spectral classification, population II Cited by: 1. Observations indicating the presence of stellar chromospheres, that is hot envelopes around stars are summarized.

Undisputed indicators (called type I) for hot stellar envelopes are spectral lines of highly Stellar chromospheres book atoms, Fe ii emission lines and flares in late type stars and the presence of the He i Å line.

Whether indicators (called type II) like emission cores in the Ca ii H and K and. Purchase The Sun as a Guide to Stellar Physics - 1st Edition. Print Book & E-Book. ISBNCOVID Resources. Reliable information about the coronavirus (COVID) is available from the World Health Organization (current situation, international travel).Numerous and frequently-updated resource results are available from this ’s WebJunction has pulled together information and resources to assist library staff as they consider how to handle coronavirus.

Stellar Chromospheres. Stellar chromospheres and transition regions contain the moderate temperature (5, K) gas located between the photosphere and corona. These regions are best studied using the emission lines they emit in the ultraviolet.

The present conference on cool stars, stellar systems, and the sun encompasses stellar chromospheres and coronae, binary stars, the stellar evolution of contracting stars and red giants, stellar evolution abundances of the elements, mass loss and envelopes, and stellar pulsation.

Specific issues addressed include theories regarding the acoustic. Solar Dynamo Theory Paul Charbonneau Annual Review of Astronomy and Astrophysics The Structure of the Solar Chromosphere B.

Pagel Annual Review of Astronomy and Astrophysics Stellar Model Chromospheres and Spectroscopic Diagnostics Jeffrey L.

Linsky. Not Available adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86AAuthor: C.

Jeffery, R. Griffin, D. Stickland. Abstract. Chromospheres, coronae, and winds similar to those observed on the Sun have been detected in a variety of cool stars.

In many cases, especially for main-sequence stars, there is good evidence that the processes leading to non-radiative plasma heating and wind acceleration are the same as for the Sun, although the radiative losses from stellar chromospheres and coronae are often some Cited by: 4.

This book represents the proceedings of a NATO Advanced Study Institute which was held at Bonas from August 25 till Sep­ tember 5, and was devoted to the study of "Solar Phenomena in Stars and Stellar Systems". It is intended for a broad audi­ ence. Students and post-doctoral scientists for.

The IAU Symposium on `Stellar Surface Structure' consequently focused on spatially resolved stellar observations throughout the H-R diagram, from O- and B-stars to late M-stars. Two further sections in this book summarize the current observational data on surface inhomogeneities in stellar photospheres, chromospheres, and coronae.

Cool Stars, Stellar Systems, and the Sun Proceedings of the Fifth Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun Held in Boulder, Colorado, July 7–11, Heating of stellar chromospheres and coronae observational constraints and evidence for saturation.

Book Title Cool Stars, Stellar Systems, and the Sun Book Subtitle. The chromosphere (literally, "sphere of color") is the second of the three main layers in the Sun's atmosphere and is roughly 3, to 5, kilometers deep. Its rosy red color is only apparent during eclipses. The chromosphere sits just above the photosphere and below the solar transition layer of the chromosphere atop the photosphere is homogeneous.

@article{osti_, title = {Stellar model chromospheres. A survey of CaII lambda line profiles in late-type stars of differing chromospheric activity}, author = {Linsky, J L and Hunten, D M and Sowell, R and Glackin, D L and Kelch, W L}, abstractNote = {We have obtained profiles of the Ca II infrared triplet line lambda in 49 stars of spectral type FK3.

The observational evidence for the presence of chromospheres in late-type stellar atmospheres is discussed, taking into account spectral diagnostics and line formation, an observational summary.

The influence of the non-greyness of the absorption coefficient. The pressure stratification. Theory of line formation. The hydrogen lines. Spectrum analysis. Basics about non-local thermodynamic equilibrium. The hydrogen convection zone. Stellar chromospheres, transition layers, and coronae.

Stellar winds. STARS AND STELLAR EVOLUTION Stellar Dynamos and Chromospheres 23 The Sun is still the gateway to a deeper understanding of all stars because it is typical in so many ways.

Solar seismology has used oscillations to image phenomena such as the rotational profile of the core and the subsurface convective structure of sunspots. Han wasn't sure how they actually mined the gas, but he knew that tibanna gas was very valuable, so the miners must be doing well.

Before it was discovered in Bespin's atmosphere, tibanna gas had usually been found in stellar chromospheres and nebular clusters— which made harvesting it hazardous, to say the least/5(39).Stellar chromospheres - H-alpha and CA II K profiles Article (PDF Available) in The Astrophysical Journal Supplement Series November with 11 Reads How we measure 'reads'.