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3 edition of Stellar Lyman alpha emission and the local interstellar medium found in the catalog.

Stellar Lyman alpha emission and the local interstellar medium

Theodore Simon

Stellar Lyman alpha emission and the local interstellar medium

final report for National Aeronautics and Space Administration, Grant NAG 5-1823

by Theodore Simon

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Published by Institute for Astronomy, University of Hawaii, National Aeronautics and Space Administration, National Technical Information Service, distributor in Honolulu, Hawaii, [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Stars -- Spectra.

  • Edition Notes

    Statementprincipal investigator: Theodore Simon.
    Series[NASA contractor report] -- NASA CR-192635., NASA contractor report -- NASA CR-192635.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL14690474M

      In this paper, we discuss the nature of the Lyman-break galaxies and their properties, including star-formation rate, stellar and total mass, chemical abundance, morphology, and interstellar medium (ISM) kinematics, and outline their contribution to the stellar content of the universe and their connection to the galaxies observed in the present   The distribution of ionized hydrogen (known by astronomers as H II from old spectroscopic terminology) in the parts of the Galactic interstellar medium visible from the Earth's northern hemisphere as observed with the Wisconsin Hα Mapper (Haffner et al. ).. In astronomy, the interstellar medium (ISM) is the matter and radiation that exists in the space between the star systems in a ://

      Exploration of the Outer Heliosphere and the Local Interstellar Medium: The National Academies Press. doi: / of the hydrogen wall and then, only a few more years after that, using the same Lyman-alpha absorption technique, the discovery of hydrogen walls about other stars in our galactic neighborhood and the associated   The interstellar medium (hereafter ISM) was first discovered in , with the observation of stationary calcium absorption lines superimposed on the Doppler shifting spectrum of a spectroscopic binary. Since the calcium lines were not changing in wavelength, they could not originate in the stellar atmospheres of ~woosley/lectures_fall/lecturepdf.

      Astrospheres, stellar winds, and the interstellar medium BRIAN E. WOOD AND JEFFREY L. LINSKY The spatial extent of the solar wind While orbiting the Sun, the Earth and the other planers in our solar system are exposed to an outflow of plasma from the Sun. This is the solar wi nd, which   List of the largest nebulae; Nebula Maximum dimension (in light-years/parsecs) Type Notes LAB Giant Concentration (coinciding with SSA22 Protocluster): ,, ly (61,, pc) complex of LαBs: Also on record as one of the largest structures in the universe.: NGC Halo Cloud: 1,, ly (, pc) H I region


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Stellar Lyman alpha emission and the local interstellar medium by Theodore Simon Download PDF EPUB FB2

Stellar Lyman-alpha emission and the local interstellar medium Article (PDF Available) in The Astrophysical Journal (2) February with 11 Reads How we measure 'reads' The model emission was then subtracted from the observed image, leaving behind the corrected stellar Lyman alpha emission.

The details of this fitting procedure are described. Having devised a successful method for removing the unwanted geocoronal emission, the correction procedure was applied to archival images which, from inspection of   The UV spectra now available in the IUE archives have been systematically searched for the presence of Lyman-alpha emission in late-type stars.

The results provide the first survey of the behavior of the Ly-alpha emission line across most of the cool half of the H-R diagram. The normalized Ly-alpha emission flux is strongest in the chromospherically active RS CVn stars and in the dMe :// LL/abstract.

Under the auspices of this ADP program, a systematic study was made of IUE archival images in order to extract spectra of the Lyman alpha region and to measure the stellar Lyman alpha flux for as many late-type stars as possible. The Lyman alpha resonance line is a powerful cooling channel for the hot chromospheres of solar-type stars, but has not been studied before in any systematic fashion Get this from a library.

Stellar Lyman alpha emission and the local interstellar medium: final report for National Aeronautics and Space Administration, Grant NAG [Theodore Simon; United States. National Aeronautics and Space Administration.] Stellar lyman alpha emission and the local interstellar medium.

By Theodore Simon. Abstract. Under the auspices of this ADP program, a systematic study was made of IUE archival images in order to extract spectra of the Lyman alpha region and to measure the stellar Lyman alpha flux for as many late-type stars as possible. The Lyman alpha Lyman Alpha absorption in the interstellar medium.

of the local interstellar medium. features seen against the stellar Lyman-alpha emission line and to derive densities and D/H ratios for   Dissecting the Neutral Medium in Detail. FROM SMALL TO LARGE SCALES: COMPLETING THE QUANTITATIVE PICTURE WITH HST IMAGING Resolved Analyses: A Case Study of Haro 11 Extended Halos.

LYMAN ALPHA SURVEYS AT LOW REDSHIFT Evolution of Lyman alpha Galaxies into the Nearby Universe The Properties of Nearby Lyman alpha Galaxies Stellar This chapter summarizes the community’s basic understanding of the physics of the outer heliosphere, focusing on the influence exerted on the solar wind by the interstellar medium ().In particular, it describes several approaches that allow us to infer the properties and structure of the heliospheric :// the interstellar medium have been summarized in Chapter 1, to indicate the general nature of the physical system which is subject to the various processes discussed in the following chapters.

Chapters 2 through 6 discuss various local phenomena occumng in the gas, whereas Chapters 7,8, and 9 Stellar Lyman-alpha emission and the local interstellar medium.

The UV spectra now available in the IUE archives have been systematically searched for the presence of Lyman-alpha emission in late-type stars. The results provide the first survey of the behavior of the Ly-alpha emission line across most of the cool half of the H-R diagram Stellar populations in the Local Group Galaxy formation and evolution Interstellar medium of star-forming galaxies at high redshift Distribution of molecular gas and dust in strongly lensed galaxies Blind searches on Submm observations These quantities were determined by modeling the interstellar hydrogen and deuterium Lyman alpha lines and the resonance lines of Fe II and Mg II against the background stellar emission-line profiles.

We now report on our preliminary analysis of these spectral lines for the line of sight toward Procyon ( pc).

Abstract We will observe w spectral resolution the stellar Lyman alpha emission line and interstellar hydrogen and deuterium absorption towards local late-type stars to derive the H and D column densities and D/H ratios along different lines of The XMM-Newton view of stellar coronae: High-resolution X-ray spectroscopy of Capella Deuterium and the Local Interstellar Medium Properties for the Procyon and Capella Lines of Sight The first images from an optical aperture synthesis array: mapping of Capella with COAST at two ://   Doppler-shifted hydrogen Lyman-alpha (Ly α) emission from galaxies is currently measured and used in cosmology as an indicator of star formation.

Until now, the Milky Way emission has not been detected, owing to far brighter local sources, including the H Glow, i.e., solar Lyα radiation backscattered by interstellar atoms that / Acknowledgements.

Firstly it is my pleasure to thank the organizers of 46th Saas Fee school Lyman-alpha as an astrophysical and cosmological tool for this exciting invitation and their warmest hospitality: Anne Verhamme, Pierre North, Hakim Atek, Sebastiano Cantalupo, and Myriam Burgener Frick.

While on the subject, I also need to thank them for their patience in waiting for this ://   The process of fine structure cooling is dominant in most regions of the Interstellar Medium, except regions of hot gas and regions deep in molecular clouds.

It occurs most efficiently with abundant atoms having fine structure levels close to the fundamental level such as: CII and OI in the neutral medium and OII, OIII, NII, NIII, NeII and   stellar lyman alpha emission and the local interstellar medium (nasa-cr) stellar lyman alpha emission and the local interstellar medium final technical keport, 15 nov.

- 14 nov. (hawaii univ.) 50 p g n unclas principal investigator: dr. theodore simon november 15 - november 14   @article{osti_, title = {Hydrogen and deuterium in the local interstellar medium}, author = {Murthy, J N}, abstractNote = {This work reports on the results of a series of IUE observations of interstellar HI and DI alpha.

absorption against the chromospheric alpha. emission of the nearby late-type ://. stellar grain per hour? Neglect the motion of the spacecraft relative to the Sun, and assume that the interstellar grains are unaffected by solar gravity, radiation pressure, and the solar wind (and interplanetary magnetic field).

The distance to the nearby star Proxima Centauri is D= pc. The ISM between the Sun and Proxima Cen~draine/book/  This grant covers studies of the local interstellar medium from. absorption lines observed in the spectra of. nearby, late-type stars. Since the resonance lines of interstellar hydrogen and deuterium appear.

in absorption against the strong chromospheric emission line of hydrogen. Lyman-a, it is   present measurements of the velocity, covering fraction and optical depth of neutral gas in front of two well known local blue compact galaxies that show Lyman alpha in emission: ESO IG 04 and Haro We thus test observationally the hypothesis that Lyman alpha can escape through neutral gas by being Doppler shifted out of ://